PhD Thesis (PDF) - Department of Astronomy - University of Virginia
PhD Thesis (PDF) - Department of Astronomy - University of Virginia
PhD Thesis (PDF) - Department of Astronomy - University of Virginia
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LOW-MASS X-RAY BINARIES, DIFFUSE GAS, AND GLOBULAR CLUSTERS<br />
IN EARLY-TYPE GALAXIES<br />
Gregory Robert Sivak<strong>of</strong>f<br />
Wilmington, Delaware<br />
B.S./B.A., Brandeis <strong>University</strong>, 2000<br />
M.S., <strong>University</strong> <strong>of</strong> Manchester, 2001<br />
M.S., <strong>University</strong> <strong>of</strong> <strong>Virginia</strong>, 2003<br />
A Dissertation Presented to the Graduate<br />
Faculty <strong>of</strong> the <strong>University</strong> <strong>of</strong> <strong>Virginia</strong><br />
in Candidacy for the Degree <strong>of</strong><br />
Doctor <strong>of</strong> Philosophy<br />
<strong>Department</strong> <strong>of</strong> <strong>Astronomy</strong><br />
<strong>University</strong> <strong>of</strong> <strong>Virginia</strong><br />
August, 2006<br />
Craig L. Sarazin<br />
Kelsey E. Johnson<br />
Robert T. Rood<br />
Bradley B. Cox<br />
Joel N. Bregman
Abstract<br />
Chandra X-ray Telescope observations are used to resolve the X-ray content <strong>of</strong> nearby<br />
early-type galaxies into low-mass X-ray binaries (LMXBs) and diffuse interstellar<br />
gas. The ∼50–200 bright LMXBs present in each early-type galaxy are an incredible<br />
complementary sample to the ∼150 Milky Way LMXBs. Large LMXB samples reveal<br />
general LMXB properties and rare LMXB phenomena. The diffuse gas can be used<br />
to trace the history, mass, and dynamics <strong>of</strong> the galaxy environment. We present<br />
detailed studies <strong>of</strong> the LMXBs and diffuse gas in four early-type galaxies and a study<br />
<strong>of</strong> the connection between LMXBs and globular clusters (GCs) in eleven early-type<br />
galaxies. NGC 4365 and 4382 are galaxies with relatively small contributions <strong>of</strong> gas<br />
to their X-ray emission. Although the faintness <strong>of</strong> the X-ray gas limits our ability to<br />
study it; we find some evidence that its temperature increases with increasing radius<br />
and that the gas in NGC 4382 may be rotating significantly. The LMXB luminosity<br />
functions in both galaxies are consistent with single power-law fits that are cut<strong>of</strong>f at<br />
high luminosities. Since it is farther away and its X-ray emission is gas dominated,<br />
only the brightest X-ray sources in NGC 1600 can be detected. NGC 1600 has a<br />
surprising number <strong>of</strong> ultraluminous X-ray candidates. We also find two phases <strong>of</strong><br />
gas in NGC 1600; a s<strong>of</strong>t inner component is attributed to the interstellar medium <strong>of</strong><br />
NGC 1600, while a hotter outer component is attributed to the intragroup medium<br />
<strong>of</strong> the NGC 1600 group. Multi-epoch observations <strong>of</strong> NGC 4697, one <strong>of</strong> the nearest,<br />
massive early-type galaxies whose X-ray emission is LMXB-dominated, reveal sources<br />
with extreme flaring on minutes to hours timescales, sources variable on days to years<br />
timescales, and 34 LMXBs in GCs used to probe the GC/LMXB connection. We<br />
extend this last study to ten other early-type Virgo cluster galaxies. Hubble Space<br />
Telescope Advanced Camera for Surveys observations reveal brighter, redder, and<br />
ii
smaller GCs are more likely to contain LMXBs. We present the most direct evidence<br />
to date that the formation <strong>of</strong> LMXBs in GCs depends on the stellar encounter rates<br />
and metallicities <strong>of</strong> GCs.<br />
iii
Acknowledgements<br />
My decision to attend the <strong>Astronomy</strong> <strong>Department</strong> at the <strong>University</strong> <strong>of</strong> <strong>Virginia</strong> has<br />
proved to be one <strong>of</strong> the best decisions I have made in my life; my five years here have<br />
been incredible. I have had the chance to learn from and work with an incredibly<br />
talented cadre <strong>of</strong> faculty, collaborators, postdocs, graduate students, and staff. But<br />
more important to me, I feel that I have been adopted into an incredible family <strong>of</strong><br />
warm, caring people whose support goes well beyond the call <strong>of</strong> duty. Adding the<br />
people here to my already rich tapestry <strong>of</strong> family and friends makes me realize just<br />
how lucky I am. Needless to say, I am bound to overlook people who richly deserve<br />
acknowledgment. Those that know me well, know I already feel guilty about it.<br />
I have to thank my advisor, Craig Sarazin, first. He has been a true mentor<br />
throughout my entire time here. Although he is always involved in many projects, he<br />
has the infinite supply <strong>of</strong> patience (and time) needed to match my endless supply <strong>of</strong><br />
questions. I appreciate his open door and the many discussions (whether astronomical<br />
or gastronomical) we have had. Without his encouragement to write proposals from<br />
my second year on, I know I would not have the opportunities that now lie ahead. I<br />
hope I can become a quarter <strong>of</strong> the accomplished scientist that Craig is.<br />
Second, I would like to thank the other members on my thesis committee, Joel<br />
Bregman, Brad Cox, Kelsey Johnson, and Bob Rood. They not only spent their time<br />
reading through this work and pointing out some necessary corrections, but also gave<br />
me some good ideas for future avenues <strong>of</strong> exploration.<br />
Next, I would like to thank the various funding agencies, resources, collaborators,<br />
and other scientists who made important direct contributions to the work presented<br />
here. Financial support was provided by the National Aeronautics and Space Admin-<br />
istration through Chandra Award Numbers GO1-2078X, GO1-3100X, GO2-3100X,<br />
iv
GO2-3099X, GO3-4099X, AR3-4005X, GO4-5093X, AR4-5008X, and GO5-6086X, is-<br />
sued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian<br />
Astrophysical Observatory for and on behalf <strong>of</strong> NASA under contract NAS8-39073.<br />
Support for Program Numbers HST-GO-10003.01-A, HST-GO-10597.03-A, and HST-<br />
GO-10582.02-A was provided by NASA through grants from the Space Telescope<br />
Science Institute, which is operated by AURA under NASA contract NAS5-26555.<br />
Partial support was also provided by the Celerity Foundation and the F. H. Levinson<br />
Fund, as well through my receipt <strong>of</strong> Achievement Reward for College Scientists and<br />
<strong>Virginia</strong> Space Grant Consortium Aerospace Graduate Research fellowships.<br />
This research has made use <strong>of</strong>: (1) the NASA/IPAC Extragalactic Database<br />
(NED), which is operated by the Jet Propulsion Laboratory, California Institute <strong>of</strong><br />
Technology, under contract with the National Aeronautics and Space Administration;<br />
(2) the SIMBAD database, operated at CDS, Strasbourg, France; (3) the Digitized<br />
Sky Surveys, produced at the Space Telescope Science Institute under US Govern-<br />
ment grant NAG W-2166; (4) the HyperLeda data base http://leda.univ-lyon1.fr/;<br />
(5) data products from the Two Micron All Sky Survey, which is a joint project<br />
<strong>of</strong> the <strong>University</strong> <strong>of</strong> Massachusetts and the Infrared Processing and Analysis Cen-<br />
ter/California Institute <strong>of</strong> Technology, funded by the National Aeronautics and Space<br />
Administration and the National Science Foundation; (6) SAOImage DS9, developed<br />
by Smithsonian Astrophysical Observatory.<br />
I had incredible co-authors that strengthened all <strong>of</strong> the published work in this<br />
thesis. Craig, <strong>of</strong> course, helped co-author and review all <strong>of</strong> the chapters. Additional<br />
co-authors <strong>of</strong> the published chapters include: (Chapter 2) Jimmy Irwin; (Chapter 3)<br />
Jeff Carlin; and (Chapter 4) Andres Jordán. Among the unpublished chapters, I must<br />
especially thank Pat Côté, Adrienne Juett, and Andres for their strong level <strong>of</strong> input<br />
v
and help with revisions.<br />
Additional thanks in Chapter 2 must be extended to Arunav Kundu for several<br />
very helpful conversations, as well as providing us with his unpublished list <strong>of</strong> globular<br />
clusters in NGC 4365, and Mike Skrutskie for his help and advice in using the 2MASS<br />
catalog. Adrienne Juett and Eric Pfahl made helpful comments on Chapter 4. I had<br />
very helpful discussions with Kris Beckwith, Peter Frinchaboy, Rachel Osten, and<br />
Roseanne di Stefano while writing Chapter 5. I could not have performed the X-ray<br />
analysis for Chapter 6 without my many conversations with Elizabeth Blanton.<br />
In the beginning ...<br />
My training as an astronomer began when I started research in astrophysics as a<br />
sophomore at Brandeis <strong>University</strong>. I am in the debt to David Roberts who prompted<br />
me to inquire about available positions. I began working with John Wardle, my<br />
first astronomical advisor. With his guidance, and that <strong>of</strong> Dan Homan, I started<br />
to become the astronomer I am today. Thanks along the way also must go to Bob<br />
Phillips, who mentored me as an undergraduate researcher at Haystack Observatory,<br />
and Neal Jackson, who was my advisor for my first post-baccalaureate degree in<br />
astronomy at Jodrell Bank Observatory.<br />
And now some more general acknowledgments for help over the past five years...<br />
The open door is one <strong>of</strong> the finest qualities <strong>of</strong> our department. Everyone in this<br />
department seemed available to answer my various science questions. However, there<br />
are three doors I walked into more than any other (for science help). Although<br />
Bob Rood was department chair, he always seemed to have time to talk about either<br />
science or the department (and occasionally photography). His responsiveness helped<br />
instill the pride and ownership I feel for this department. Although Adrienne Juett<br />
was only here for my last two years, I had some <strong>of</strong> my most useful science discussions in<br />
vi
her room (my apologies to her <strong>of</strong>ficemates, Alex Constandache and Poonam Chandra).<br />
Having a second expert in X-ray binaries in our research group tremendously honed<br />
my scientific knowledge and goals. Plus, she was also always there to talk through<br />
topics outside <strong>of</strong> science. Without the constant help <strong>of</strong> Ed Murphy, I would never<br />
have been able to strongly pursue my interest in education and public outreach. Our<br />
field needs more scientists and educators like Ed.<br />
I would like to thank all the postdocs and long-term visitors that have made their<br />
way through the X-ray group; Liz Blanton, Tracy Clarke, Yutaka Fujita, Molly Hicks,<br />
Adrienne Juett, Thomas Reiprich, and Motokazu Takizawa. They were always there<br />
to help me and provide pro<strong>of</strong> that there was light at the end <strong>of</strong> the tunnel.<br />
We have an incredible staff in this department. <strong>University</strong> life always requires<br />
navigating the <strong>University</strong> bureaucracy and without <strong>Virginia</strong> Bossong, Jackie Harding,<br />
or Barbara Johnson, I would never have made my way through it. Jim Barr and<br />
Charles Lam were always there to help repair things, whether for work (e.g., numerous<br />
power supplies for my UPS) or personal. Given the technical nature <strong>of</strong> astronomy,<br />
it goes without saying that system administrators like Andrew Markwick-Kemper,<br />
Howard Powell, and Kiriaki Xiluri were indispensable.<br />
Now on to the all-important acknowledgments <strong>of</strong> graduate students and my other<br />
Charlottesville friends. Without these people, I would never have made it through<br />
with even the little shred <strong>of</strong> sanity I have left. Life here is so intertwined that many <strong>of</strong><br />
them should be thanked in multiple places. Rather than kill more trees, I am going<br />
to thank them once and let them figure out where else in these acknowledgments<br />
they belong. Doing this somewhat temporally, I’d like to thank: Josh Kempner<br />
for providing a lot <strong>of</strong> guidance with regards to Charlottesville, computing, and X-<br />
ray astronomy; Jeff Crane for being one <strong>of</strong> my early department role models (<strong>of</strong><br />
vii
course, I have never gotten the hang <strong>of</strong> letting things roll <strong>of</strong>f my back the way he<br />
can); Scott Randall, for not only begin a great friend, but also introducing me to<br />
a place where one can always hide away to feel safe (Shirtworld); Jeffrey Anderson<br />
and Heather Hershley for nights <strong>of</strong> roleplaying, Xbox, Munchkin, and red velvet<br />
cake; David Rosario for being a great <strong>of</strong>fice-mate and introducing me to wallyball,<br />
which naturally leads to also thanking John Karpovich, John Jones, Duane Merill,<br />
and Glenn Wasson for all the (literally) <strong>of</strong>f-the-wall spikes; Jodie Martin, for being<br />
the only other person I have met who knows what skirt steak is before I met them<br />
(I guess Texans are good for something); Megan Crane and Ally Polak for instilling<br />
Halloween visions <strong>of</strong> a deranged, knife-wielding angel chasing a bunch <strong>of</strong> grapes; Matt<br />
Garvin, a wholesome person who could (gleefully) play Grand Theft Auto while saying<br />
how wrong it is; Jeff Oishi for his intricate choreography when presenting his middle<br />
fingers as his jovial greeting; Alok Singhal for his actions in the secret cow level <strong>of</strong><br />
Diablo; Jennifer Bartlett for taking over the Public Outreach committee spot when I<br />
needed to concentrate on work; Tanim Islam, for several interesting parties (a bowlful<br />
<strong>of</strong> cigarettes?); Marios Chatzikos, for being my second great <strong>of</strong>fice-mate and always<br />
proving that when one wants help with English, look to an international student;<br />
the poker regulars, Jeff Carlin, Ori Fox, NJ Gauthier, Nate Jones, Rick Mellon, and<br />
Ricardo Munoz, for helping me relieve stress one $5 buy-in at a time (except for<br />
those more expensive wall-<strong>of</strong>-shame nights); Jeff Bary, for starting the Big Bangers<br />
intramural franchise (are we home or away?); Dawn Peterson, Steph Brown, Kelli<br />
Joseph, Ricardo Schiavon, and the rest <strong>of</strong> the Big Bangers volleyball team (oh-ee-oh-<br />
ee-oh-ee-ohhh); Genevieve de Messieres, Joleen Miller, Megan Thomes, and the rest <strong>of</strong><br />
the happy hour crew (the new department social chairs?); Jill Klinger, David Nidever,<br />
and Amy Reines for making Sushi night at my place a success; Sri Kanneganti (our<br />
viii
US Court expert from India), for all our interesting discussions outside <strong>of</strong> astronomy;<br />
Mei-Yin Chou, Cheng-Yu Kuo, Chan Park, Ka-Wah Wong for sharing their cultures<br />
(especially their food) with me; Sean and Tia Matt for Wings night; and the BSG<br />
crew, Nicole Gugliucci, Jarron Leisenring, (future member) Jacob Simon, Isabelle<br />
Stanton, Mike Thomas, and Gail Zasowski, for lifting me up in my final year when I<br />
needed it most.<br />
Those people in Charlottesville who know me have probably notice four missing<br />
people; I would like to especially thank these very close friends I have made here.<br />
Peter Frinchaboy and I met as prospective students in 2000, and he was the first<br />
person I re-met when I arrived in 2001. Since then, we have been fast friends, talking<br />
to each other nearly every day. We have been co-conspirators in our attempts to<br />
improve the department (whether they realized it or not). Both <strong>of</strong> us have used each<br />
other as sounding boards for our projects and frustrations, and so much more I do not<br />
have room to thank him for. I have had the pleasure <strong>of</strong> watching his family blossom<br />
as he and his wife Jennifer raise their son Xander (with a little help from the rest <strong>of</strong><br />
us in the department). I wish them all the best in Madison and beyond.<br />
Mark Morgan and I met when I began playing wallyball. For virtually every<br />
Tuesday over the past five years, Mark has been the leader <strong>of</strong> our wallyball group,<br />
kept its score in amusing ways, and then marched us out to a local restaurant for<br />
some food and libations. Mark seemed to have a sixth sense for when I needed to<br />
talk about what was going on at work or in the rest <strong>of</strong> my life. I am going to miss<br />
these talks, our Thursday night roleplaying sessions, chili nights, and other cooking<br />
sessions, which were always great pick-me-ups.<br />
I met Howard Powell when he started working as a system administrator in our<br />
department. He has always been a tremendous help, especially for the graduate<br />
ix
students. I can not recall the countless hours he has spent helping me install various<br />
X-ray s<strong>of</strong>tware packages. But more importantly, we became good friends. I will miss<br />
our discussions <strong>of</strong> everything technical, late night video game sessions, and countless<br />
lunch runs.<br />
Dan Wik and I met when he began his graduate student days in the department<br />
two years ago. But it was not until I started lifting with him that we began to<br />
become good friends. Our talks <strong>of</strong> astronomy, politics, and virtually everything else<br />
made lifting longer, but much more enjoyable. He has extended spotting me in the<br />
weight room to my life beyond. I am forever in his debt for his friendship and all his<br />
help in my final year here.<br />
Next, I would like to thank my friends that predate my Charlottesville years. My<br />
closest friends from Delaware, Barbara Eucalano, Chad Leigh, Brett and Lea Ann<br />
Skipper, and Mike and Christy Pollack have provided me with support for over 14<br />
years now. We may not meet up or talk as <strong>of</strong>ten as we once did, but I value each<br />
time we do. Now we will have a whole new town to explore. The same goes for my<br />
college buddies, Mike Descy, Dave Erenberg, and Myq Kaplan. They always know<br />
how to make me act a little less serious, a trait I am thankful for.<br />
Most <strong>of</strong> all, I have been supported by my family; my grandfather Murray Sivak<strong>of</strong>f<br />
and grandmother Shirley Barouch; parents Ilene and Sheldon Sivak<strong>of</strong>f; and sister and<br />
brother-in-law Beth and Jay Band. A conversation my father and I had in a car one<br />
fateful afternoon helped me realize that the Universe is a big place that might have<br />
some intellectual space I could mark as my own. This and my family’s emphasis on<br />
education throughout my life started my path in astronomy. More importantly, I<br />
never could have finished without my entire family being behind me. This work is<br />
dedicated to them.<br />
x
Table <strong>of</strong> contents<br />
Abstract ii<br />
Acknowledgements iv<br />
List <strong>of</strong> Figures xvi<br />
List <strong>of</strong> Tables xviii<br />
1 General Introduction 1<br />
1.1 Early-type Galaxies and Their X-ray Emission . . . . . . . . . . . . . 1<br />
1.2 Hot, Diffuse Interstellar Gas . . . . . . . . . . . . . . . . . . . . . . . 2<br />
1.3 Low-Mass X-ray Binaries . . . . . . . . . . . . . . . . . . . . . . . . . 4<br />
1.4 The Galactic Connection Between Low-Mass X-ray Binaries and Globular<br />
Clusters . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 7<br />
1.5 The Chandra X-ray Observatory . . . . . . . . . . . . . . . . . . . . . 10<br />
1.6 The Hubble Space Telescope . . . . . . . . . . . . . . . . . . . . . . . 11<br />
1.7 Contents <strong>of</strong> the <strong>Thesis</strong> . . . . . . . . . . . . . . . . . . . . . . . . . . 12<br />
2 Chandra Observations <strong>of</strong> Low-Mass X-Ray Binaries and Diffuse Gas<br />
in the Early-Type Galaxies NGC 4365 and NGC 4382 (M85) 13<br />
2.1 Introduction . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 13<br />
2.2 Observation and Data Reduction . . . . . . . . . . . . . . . . . . . . 16<br />
2.3 X-ray Image . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 18<br />
2.4 Resolved Sources . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 28<br />
2.4.1 Detections . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 28<br />
2.4.2 Identifications . . . . . . . . . . . . . . . . . . . . . . . . . . . 29<br />
2.4.3 X-ray Luminosities and Luminosity Functions . . . . . . . . . 31<br />
2.4.4 Hardness Ratios . . . . . . . . . . . . . . . . . . . . . . . . . . 34<br />
2.4.5 Variability . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 37<br />
2.4.6 Spatial Distribution . . . . . . . . . . . . . . . . . . . . . . . . 37<br />
2.5 Spectral Analysis . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 42<br />
2.5.1 X-ray Spectra <strong>of</strong> Resolved Sources . . . . . . . . . . . . . . . . 46<br />
2.5.2 X-ray Spectra <strong>of</strong> Unresolved Emission . . . . . . . . . . . . . . 49<br />
xi
2.5.3 Total X-ray Spectra . . . . . . . . . . . . . . . . . . . . . . . . 53<br />
2.5.4 Discrete versus Diffuse Emission . . . . . . . . . . . . . . . . . 55<br />
2.6 Spatial Distribution <strong>of</strong> the Diffuse Gaseous<br />
Emission . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 56<br />
2.7 Conclusions . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 58<br />
3 Chandra Observations <strong>of</strong> Diffuse Gas and Luminous X-Ray Sources<br />
Around the X-Ray–Bright Elliptical NGC 1600 61<br />
3.1 Introduction . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 61<br />
3.2 Observation and Data Reduction . . . . . . . . . . . . . . . . . . . . 64<br />
3.3 X-ray Image . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 65<br />
3.4 Resolved Sources . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 72<br />
3.4.1 Detections . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 72<br />
3.4.2 Identifications . . . . . . . . . . . . . . . . . . . . . . . . . . . 74<br />
3.4.3 X-ray Luminosities and Luminosity Functions . . . . . . . . . 75<br />
3.4.4 Hardness Ratios . . . . . . . . . . . . . . . . . . . . . . . . . . 82<br />
3.4.5 Variability . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 86<br />
3.5 Unresolved X-ray Emission . . . . . . . . . . . . . . . . . . . . . . . . 87<br />
3.5.1 Radial Pr<strong>of</strong>ile <strong>of</strong> the Unresolved X-ray Emission . . . . . . . . 88<br />
3.5.2 Structural Features in the Unresolved X-ray Emission . . . . . 92<br />
3.5.3 Central X-ray Structure and Multiwavelength Comparisons . . 97<br />
3.6 Spectral Analysis . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 100<br />
3.6.1 X-ray Spectrum <strong>of</strong> Resolved Sources . . . . . . . . . . . . . . 103<br />
3.6.2 X-ray Spectra <strong>of</strong> Unresolved Emission . . . . . . . . . . . . . . 105<br />
3.7 Mass Determination . . . . . . . . . . . . . . . . . . . . . . . . . . . 110<br />
3.8 Conclusions . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 112<br />
4 Luminous X-Ray Flares from Low-Mass X-Ray Binary Candidates<br />
in the Early-Type Galaxy NGC 4697 116<br />
4.1 Introduction . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 116<br />
4.2 Observations and Data Reduction . . . . . . . . . . . . . . . . . . . . 118<br />
4.3 Detection <strong>of</strong> Flaring Sources . . . . . . . . . . . . . . . . . . . . . . . 118<br />
4.4 Discussion . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 124<br />
4.4.1 CXOU J124837.8−054652 (Source A) and<br />
CXOU J124831.0−054828 (Source B): Type-I X-ray Superbursts?124<br />
4.4.2 CXOU J124839.0−054750 (Source C) . . . . . . . . . . . . . . 126<br />
4.5 Conclusions . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 128<br />
5 Multi-Epoch Chandra X-ray Observations <strong>of</strong> Low Mass X-ray Binary<br />
Candidates in the Early-Type Galaxy NGC 4697 129<br />
5.1 Introduction . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 129<br />
5.2 Observations and Data Reduction . . . . . . . . . . . . . . . . . . . . 134<br />
xii
5.2.1 Chandra X-ray Observatory . . . . . . . . . . . . . . . . . . . 134<br />
5.2.2 Hubble Space Telescope . . . . . . . . . . . . . . . . . . . . . . 136<br />
5.3 X-ray Image . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 136<br />
5.4 X-ray Source Detection . . . . . . . . . . . . . . . . . . . . . . . . . . 141<br />
5.5 Optical Counterpart Identification . . . . . . . . . . . . . . . . . . . . 152<br />
5.5.1 Existing Catalog Identifications . . . . . . . . . . . . . . . . . 152<br />
5.5.2 HST-ACS Identifications . . . . . . . . . . . . . . . . . . . . . 156<br />
5.6 GC/LMXB Connection . . . . . . . . . . . . . . . . . . . . . . . . . . 160<br />
5.7 X-ray Luminosities and Luminosity Functions . . . . . . . . . . . . . 167<br />
5.8 Hardness Ratios . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 186<br />
5.9 Spectral Analysis . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 189<br />
5.9.1 Best-Fit Spectra <strong>of</strong> LMXBs . . . . . . . . . . . . . . . . . . . 191<br />
5.9.2 Spectra Grouped by Position . . . . . . . . . . . . . . . . . . 192<br />
5.9.3 Spectra Grouped by GC Association . . . . . . . . . . . . . . 193<br />
5.9.4 Spectra Grouped by Luminosity . . . . . . . . . . . . . . . . . 194<br />
5.9.5 Individual Source Spectra . . . . . . . . . . . . . . . . . . . . 195<br />
5.10 X-ray Source Variability . . . . . . . . . . . . . . . . . . . . . . . . . 198<br />
5.10.1 Intraobservation Variability . . . . . . . . . . . . . . . . . . . 199<br />
5.10.2 Interobservation Variability . . . . . . . . . . . . . . . . . . . 206<br />
5.11 Conclusions . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 225<br />
6 The Low-Mass X-ray Binary and Globular Cluster Connection in<br />
Virgo Cluster Early-type Galaxies: Optical Properties 230<br />
6.1 Introduction . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 230<br />
6.2 Sample . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 233<br />
6.2.1 Galaxy Sample . . . . . . . . . . . . . . . . . . . . . . . . . . 233<br />
6.2.2 X-ray Analysis . . . . . . . . . . . . . . . . . . . . . . . . . . 234<br />
6.2.3 Optical Analysis . . . . . . . . . . . . . . . . . . . . . . . . . 242<br />
6.2.4 Matching LMXBs And GCs . . . . . . . . . . . . . . . . . . . 249<br />
6.3 Properties <strong>of</strong> GCs with and without LMXBs . . . . . . . . . . . . . . 251<br />
6.3.1 Luminosity and Mass . . . . . . . . . . . . . . . . . . . . . . . 253<br />
6.3.2 Color . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 253<br />
6.3.3 Size . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 255<br />
6.3.4 Galactocentric Distance . . . . . . . . . . . . . . . . . . . . . 256<br />
6.3.5 Relaxation Time . . . . . . . . . . . . . . . . . . . . . . . . . 257<br />
6.3.6 Dynamical Rates . . . . . . . . . . . . . . . . . . . . . . . . . 258<br />
6.4 Multi-Variable Relation Between LMXBs and GCs . . . . . . . . . . 258<br />
6.4.1 Technique . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 258<br />
6.4.2 Effect <strong>of</strong> GC Mass and Color . . . . . . . . . . . . . . . . . . 261<br />
6.4.3 Effect <strong>of</strong> GC Size . . . . . . . . . . . . . . . . . . . . . . . . . 262<br />
6.4.4 Simultaneous Effect <strong>of</strong> GC Mass, Color, and Size . . . . . . . 263<br />
6.4.5 Implications <strong>of</strong> Simultaneous Fit . . . . . . . . . . . . . . . . 265<br />
xiii
6.5 Conclusions . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 272<br />
7 Summary and Future Directions 276<br />
7.1 Summary . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 276<br />
7.1.1 Luminosity Functions <strong>of</strong> Low-Mass X-Ray Binaries . . . . . . 276<br />
7.1.2 The Connection Between Globular Clusters and Low-Mass Xray<br />
Binaries . . . . . . . . . . . . . . . . . . . . . . . . . . . . 278<br />
7.1.3 Spectra <strong>of</strong> Low-Mass X-Ray Binaries . . . . . . . . . . . . . . 279<br />
7.1.4 Variability in Low-Mass X-Ray Binaries . . . . . . . . . . . . 280<br />
7.1.5 Spectra <strong>of</strong> Diffuse Gas . . . . . . . . . . . . . . . . . . . . . . 281<br />
7.1.6 Gas Pr<strong>of</strong>iles <strong>of</strong> Diffuse Gas . . . . . . . . . . . . . . . . . . . . 282<br />
7.2 Future Directions . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 282<br />
7.2.1 X-ray Properties <strong>of</strong> the GC-LMXB connection . . . . . . . . . 283<br />
7.2.2 X-ray Observations <strong>of</strong> Early-type Galaxies . . . . . . . . . . . 283<br />
7.2.3 Optical Observation <strong>of</strong> Early-type Galaxies . . . . . . . . . . . 284<br />
7.2.4 Closing Remarks . . . . . . . . . . . . . . . . . . . . . . . . . 286<br />
A Encounter Rate Parameter Γh<br />
B Optical Properties <strong>of</strong> Globular Clusters 290<br />
C Optimal Preparation <strong>of</strong> Bovine Diaphragm for Human Consumption<br />
402<br />
C.1 Introduction . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 402<br />
C.2 Technique . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 403<br />
C.3 Conclusions . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 404<br />
C.4 Sivak<strong>of</strong>f Signature Soy Sauce Skirt Steak . . . . . . . . . . . . . . . . 405<br />
xiv<br />
287
List <strong>of</strong> Figures<br />
1.1 Hubble Tuning Fork . . . . . . . . . . . . . . . . . . . . . . . . . . . 3<br />
2.1 Adaptively Smoothed False-Color X-Ray Images <strong>of</strong> NGCs 4365 & 4382 19<br />
2.2 Optical Images <strong>of</strong> NGCs 4365 & 4382 . . . . . . . . . . . . . . . . . . 20<br />
2.3 Luminosity Functions <strong>of</strong> Discrete X-Ray Sources in NGCs 4365 & 4382 31<br />
2.4 Hardness Ratio Diagrams <strong>of</strong> Discrete X-Ray Sources in NGCs 4365 &<br />
4382 . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 35<br />
2.5 Accumulated Fractional X-Ray Light Curves <strong>of</strong> Highly Variable Discrete<br />
X-ray Sources in NGCs 4365 & 4382 . . . . . . . . . . . . . . . 38<br />
2.6 X-Ray Light Curve <strong>of</strong> Source 86 in NGC 4365 . . . . . . . . . . . . . 38<br />
2.7 Position Angles <strong>of</strong> Discrete X-Ray Sources in NGC 4365 & 4382 . . . 39<br />
2.8 Radial Distribution <strong>of</strong> Discrete X-Ray Sources in NGCs 4365 & 4382 40<br />
2.9 X-Ray Spectrum <strong>of</strong> Resolved Sources in NGCs 4365 & 4382 . . . . . 47<br />
2.10 X-Ray Spectrum <strong>of</strong> Unresolved Emission in NGCs 4365 & 4382 . . . 50<br />
2.11 Surface Brightness Pr<strong>of</strong>iles <strong>of</strong> Unresolved S<strong>of</strong>t-Band X-Ray Emission<br />
in NGCs 4365 & 4382 . . . . . . . . . . . . . . . . . . . . . . . . . . . 57<br />
3.1 Adaptively Smoothed True-Color X-Ray Image <strong>of</strong> NGC 1600 . . . . . 67<br />
3.2 Optical Image <strong>of</strong> NGC 1600 . . . . . . . . . . . . . . . . . . . . . . . 68<br />
3.3 Luminosity Function <strong>of</strong> Discrete X-Ray Sources in NGC 1600 . . . . 77<br />
3.4 Hardness Ratio Diagrams <strong>of</strong> Discrete X-Ray Sources in NGC 1600 . . 84<br />
3.5 Surface Brightness Pr<strong>of</strong>ile <strong>of</strong> Unresolved X-Ray Emission in NGC 1600 89<br />
3.6 Hardess Ratio Pr<strong>of</strong>iles <strong>of</strong> Unresolved X-Ray Emission in NGC 1600 . 90<br />
3.7 Large-Scale Structural Features <strong>of</strong> Unresolved Emission in NGC 1600 92<br />
3.8 Surface Brightness Pr<strong>of</strong>iles by Position Angles <strong>of</strong> Unresolved X-Ray<br />
Emission in NGC 1600 . . . . . . . . . . . . . . . . . . . . . . . . . . 94<br />
3.9 Comparison <strong>of</strong> Excess X-Ray Emission and Emission-Line Filaments<br />
in NGC 1600 . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 98<br />
3.10 Comparison <strong>of</strong> Excess X-Ray Emission With Radio Emission and Dust<br />
Map in NGC 1600 . . . . . . . . . . . . . . . . . . . . . . . . . . . . 99<br />
3.11 X-Ray Spectrum <strong>of</strong> Resolved Sources in NGC 1600 . . . . . . . . . . 104<br />
3.12 X-Ray Spectrum <strong>of</strong> Unresolved Emission in NGC 1600 . . . . . . . . 106<br />
3.13 Gas and Mass Pr<strong>of</strong>iles in NGC 1600 . . . . . . . . . . . . . . . . . . . 111<br />
xv
5.1 Raw X-ray Greyscale X-ray Image <strong>of</strong> NGC 4697: S3 FOV . . . . . . . 137<br />
5.2 Raw X-ray Greyscale Image <strong>of</strong> NGC 4697: Central 3 ′ × 3 ′ FOV . . . 138<br />
5.3 Adaptively Smoothed True-Color X-ray Image <strong>of</strong> NGC 4697: S3 FOV 139<br />
5.4 Adaptively Smoothed True-Color X-ray Image <strong>of</strong> NGC 4697: Central<br />
3 ′ × 3 ′ FOV . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 140<br />
5.5 Percentage <strong>of</strong> GCs with an LMXB vs. Limiting X-ray Luminosity in<br />
NGC 4697 . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 160<br />
5.6 Color Magnitude Diagram <strong>of</strong> GCs in NGC 4697 . . . . . . . . . . . . 161<br />
5.7 Cumulative Luminosity Functions <strong>of</strong> Discrete X-ray Sources in NGC<br />
4697: Individual Observations . . . . . . . . . . . . . . . . . . . . . . 174<br />
5.8 Cumulative Luminosity Functions <strong>of</strong> Discrete X-ray Sources in NGC<br />
4697: Constant Sources . . . . . . . . . . . . . . . . . . . . . . . . . . 179<br />
5.9 Differential Instantaneous Luminosity Function <strong>of</strong> Discrete X-ray<br />
Sources in NGC 4697 . . . . . . . . . . . . . . . . . . . . . . . . . . 182<br />
5.10 Cumulative Luminosity Functions <strong>of</strong> Discrete X-ray Sources in NGC<br />
4697: GC-LMXBs vs. Field-LMXBs . . . . . . . . . . . . . . . . . . . 183<br />
5.11 Luminosity and Hardness Ratios Spatial Functions <strong>of</strong> Discrete X-ray<br />
Sources in NGC 4697 . . . . . . . . . . . . . . . . . . . . . . . . . . . 185<br />
5.12 Hardness Ratio Diagram <strong>of</strong> Discrete X-ray Sources in NGC 4697 . . . 187<br />
5.13 X-ray Spectrum <strong>of</strong> LMXBs in NGC 4697 . . . . . . . . . . . . . . . . 192<br />
5.14 X-ray Light Curve <strong>of</strong> Source 156 in NGC 4697 . . . . . . . . . . . . . 201<br />
5.15 Photon Impulse Diagram <strong>of</strong> Source 57 in NGC 4697 . . . . . . . . . . 204<br />
5.16 Accumulated Fractional X-ray Light Curve <strong>of</strong> Source 155 in NGC 4697 205<br />
5.17 Percentages <strong>of</strong> Variable Discrete X-ray Sources in NGC 4697 . . . . . 211<br />
6.1 Magnitudes and Colors <strong>of</strong> GCs . . . . . . . . . . . . . . . . . . . . . . 244<br />
6.2 Galactocentric Distances and Sizes <strong>of</strong> GCs . . . . . . . . . . . . . . . 245<br />
6.3 Corrected Sizes and Colors <strong>of</strong> GCs . . . . . . . . . . . . . . . . . . . 247<br />
6.4 Relaxation Times and Magnitudes <strong>of</strong> GCs . . . . . . . . . . . . . . . 248<br />
6.5 Corrected Sizes and Magnitudes <strong>of</strong> GCs . . . . . . . . . . . . . . . . . 249<br />
6.6 Percentage <strong>of</strong> GCs with LMXBs: Base . . . . . . . . . . . . . . . . . 252<br />
6.7 Percentage <strong>of</strong> Red-GCs and Blue-GCs with LMXBs . . . . . . . . . . 254<br />
6.8 Percentage <strong>of</strong> GCs with LMXBs: GC Mass and Color Fit Overlaid . . 262<br />
6.9 Percentage <strong>of</strong> GCs with LMXBs: GC Mass, Color, and Size Fit Overlaid263<br />
6.10 Two-Dimensional Confidence Intervals <strong>of</strong> Mass and Radius Exponents 270<br />
6.11 Two-Dimensional Confidence Intervals <strong>of</strong> Density and Metallicity Exponents<br />
. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 271<br />
A.1 R 5/2 L −3/2 as a Function <strong>of</strong> GC Concentration . . . . . . . . . . . . . 289<br />
xvi
List <strong>of</strong> Tables<br />
1.1 Galactic Low-Mass X-ray Binaries in Globular Clusters . . . . . . . . 10<br />
2.1 Discrete X-ray Sources in NGC 4365 . . . . . . . . . . . . . . . . . . 21<br />
2.2 Discrete X-ray Sources in NGC 4382 . . . . . . . . . . . . . . . . . . 25<br />
2.3 X-ray Spectral Fits <strong>of</strong> NGC 4365 . . . . . . . . . . . . . . . . . . . . 44<br />
2.4 X-ray Spectral Fits <strong>of</strong> NGC 4382 . . . . . . . . . . . . . . . . . . . . 45<br />
3.1 Discrete X-ray Sources in NGC 1600 . . . . . . . . . . . . . . . . . . 69<br />
3.2 X-ray Spectral Fits <strong>of</strong> NGC 1600 . . . . . . . . . . . . . . . . . . . . 102<br />
4.1 Observed Properties <strong>of</strong> Short-Timescale Flares in NGC 4697 . . . . . 122<br />
4.2 Inferred Properties <strong>of</strong> Short-Timescale Flares in NGC 4697 . . . . . . 122<br />
5.1 Discrete X-ray Sources in NGC 4697 . . . . . . . . . . . . . . . . . . 142<br />
5.2 Optical Properties <strong>of</strong> Ground-Based Optical Sources Matched to X-ray<br />
Sources in NGC 4697 . . . . . . . . . . . . . . . . . . . . . . . . . . . 153<br />
5.3 Optical Properties <strong>of</strong> HST Sources Matched with X-ray Sources in<br />
NGC 4697 . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 158<br />
5.4 Fits to the Expected Number <strong>of</strong> LMXBs per GC (λ) . . . . . . . . . 165<br />
5.5 X-ray Spectral Fits for Point Sources in NGC 4697 . . . . . . . . . . 168<br />
5.6 Instantaneous Luminosities <strong>of</strong> X-ray Sources . . . . . . . . . . . . . . 170<br />
5.7 Combined Luminosities & Hardness Ratios <strong>of</strong> X-ray Sources . . . . . 175<br />
5.8 Possible Periodically Variable Sources . . . . . . . . . . . . . . . . . . 200<br />
5.9 KS Test for Intraobservation Variability . . . . . . . . . . . . . . . . . 200<br />
5.10 Possible Flaring Sources in NGC 4697 . . . . . . . . . . . . . . . . . . 203<br />
5.11 Sources Which Vary between Pairs <strong>of</strong> Observations . . . . . . . . . . 208<br />
5.12 States <strong>of</strong> Variable X-ray Sources . . . . . . . . . . . . . . . . . . . . . 214<br />
6.1 Galaxy Properties <strong>of</strong> Sample . . . . . . . . . . . . . . . . . . . . . . . 233<br />
6.2 Properties <strong>of</strong> Chandra Observations . . . . . . . . . . . . . . . . . . 235<br />
6.3 GC-LMXB Matches by Galaxies . . . . . . . . . . . . . . . . . . . . 240<br />
6.4 Fits <strong>of</strong> the Expected Number λt <strong>of</strong> LMXBs per GC . . . . . . . . . . 260<br />
B.1 Optical Properties <strong>of</strong> Globular Clusters (With LMXBs) . . . . . . . 292<br />
xvii
xviii<br />
B.2 Optical Properties <strong>of</strong> Globular Clusters (Without LMXBs) . . . . . . 297
Chapter 1<br />
General Introduction<br />
1.1 Early-type Galaxies and Their X-ray Emission<br />
Hubble (1936) first began the classification <strong>of</strong> galaxies by their optical morphol-<br />
ogy. In his classical tuning fork diagram (Figure 1.1), early-type galaxies [elliptical<br />
galaxies (Es) and lenticular galaxies (S0s)] form the base <strong>of</strong> the tuning fork. The ellip-<br />
tical galaxies are dominated by ellipsoidal shapes, called bulges, while the lenticulars<br />
have bulges plus a contribution from a disk. Compared to late-type galaxies (spi-<br />
ral and irregular galaxies), early-type galaxies exhibit much smoother distributions<br />
<strong>of</strong> optical light and larger bulge-to-disk ratios. Broadly speaking, the morphological<br />
differences between early-type and late-type galaxies are related to the level <strong>of</strong> recent<br />
star formation. Early-type galaxies tend not to have had much large-scale recent star<br />
formation.<br />
Einstein X-ray Observatory observations revealed that early-type galaxies are lu-<br />
minous X-ray sources (Forman, Jones, & Tucker 1985). Although sensitive enough<br />
to detect the X-ray emission from nearby galaxies, these early observations had low<br />
spatial resolution. As such, the X-ray emission appeared diffuse. At a given optical<br />
1
luminosity, LB, the X-ray luminosity LX was found to range over about two orders <strong>of</strong><br />
magnitude for early-type galaxies. In galaxies with a relatively high X-ray-optical ra-<br />
tio LX/LB (X-ray bright galaxies), the emission is dominated by a hot (kT ∼ 1 keV)<br />
optically-thin, diffuse interstellar gas (e.g., Forman et al. 1985; Trinchieri, Fabbiano,<br />
& Canizares 1986). On the other hand, in galaxies with relatively low LX/LB ratios<br />
(X-ray faint galaxies), the X-ray spectra showed two distinct spectral components: a<br />
hard (∼5–10 keV) thermal bremsstrahlung component (Matsumoto et al. 1997) and a<br />
very s<strong>of</strong>t (∼0.2 keV), optically-thin plasma component (Fabbiano, Kim, & Trinchieri<br />
1994; Pellegrini 1994; Kim et al. 1996). Since the hard component is actually found<br />
in both X-ray–bright and X-ray–faint early-type galaxies, with a luminosity that is<br />
roughly proportional to the optical luminosity <strong>of</strong> the galaxy, the hard component was<br />
thought to have a stellar origin. Kim et al. (1992) suggested that the hard component<br />
is due to low-mass X-ray binaries (LMXBs) like those observed in the bulge <strong>of</strong> the<br />
Milky Way. High resolution, sensitive X-ray observations were needed to confirm this<br />
picture. Chandra observations <strong>of</strong> the X-ray faint elliptical galaxy, NGC 4697 (Sarazin,<br />
Irwin, & Bregman 2000, 2001), were the first to resolve the majority <strong>of</strong> hard emission<br />
into X-ray point sources, whose properties are consistent with LMXBs.<br />
1.2 Hot, Diffuse Interstellar Gas<br />
The diffuse interstellar gas in early-type galaxies is believed to originate from stel-<br />
lar mass loss, with a small but energetically important contribution from supernovae<br />
(SNe; Mathews & Brighenti 2003). As stars evolve, they eject gas, and the rates for<br />
the stellar populations in early-type galaxies are ˙ M ∼ 1.3[LB/(10 11 LB,⊙)] M⊙ yr −1 .<br />
Due to the motions <strong>of</strong> the gas-losing stars, this gas is shocked and heated to roughly<br />
the stellar kinematic temperature T ≈ µmpσ 2 /k ∼ 10 7 K, or kT ∼ 1 keV. Here,<br />
2
Fig. 1.1.— Hubble Tuning Fork, courtesy <strong>of</strong> http://hubblesite.org. Early-type galaxies,<br />
ellipticals (Es) and lenticulars (S0s), form the base <strong>of</strong> the tuning fork.<br />
µ is the mean particle mass in terms <strong>of</strong> the proton mass mp and σ is the stellar<br />
velocity dispersion. SNe can also add heavy elements and heat to the gas. For a<br />
typical early-type galaxy, Type Ia SNe may be capable <strong>of</strong> driving a galactic outflow<br />
at current times for galaxies with shallow enough potential wells and a small amount<br />
<strong>of</strong> interstellar gas. In the past when early-type galaxies primarily formed, they may<br />
have had very high rates <strong>of</strong> core-collapse supernovae that expelled enriched gas from<br />
the galaxy. In groups and clusters <strong>of</strong> galaxies, some <strong>of</strong> this gas can eventually fall<br />
back through the deeper potential well <strong>of</strong> the local environment and return to the<br />
galaxy. In general, the gravitational potential wells <strong>of</strong> groups and clusters are deeper<br />
than those <strong>of</strong> galaxies, and intragroup and intracluster gas is hotter than the gas in<br />
galaxies.<br />
Since different SNe types have varying abundance patterns, abundance measure-<br />
ments have the capacity to help disentangle the origin <strong>of</strong> the gas. In particular, the<br />
radial pattern <strong>of</strong> abundance may trace the flow <strong>of</strong> hot gas.<br />
By measuring the gas density and temperature pr<strong>of</strong>iles, the total mass pr<strong>of</strong>ile<br />
3
(including dark-matter) <strong>of</strong> a galaxy can be determined if the gas is in hydrostatic<br />
equilibrium and the gas pressure dominates (Mathews & Brighenti 2003). When<br />
combined with the optical pr<strong>of</strong>ile, X-ray derived total mass pr<strong>of</strong>iles also yield the<br />
mass-to-light ratio.<br />
1.3 Low-Mass X-ray Binaries<br />
Among stellar sources <strong>of</strong> X-ray emission (e.g., active M stars, RS CVn binaries),<br />
active X-ray binaries are typically the most luminous, LX > 10 36 ergs s −1 (White et al.<br />
1995). In these systems, a stellar-mass compact object [a neutron star (NS) or a black<br />
hole (BH)] accretes material from a donor star. As the material is captured onto an ac-<br />
cretion disk, the material is heated and emits X-rays. The mass <strong>of</strong> the compact object<br />
is thought to regulate the maximum X-ray luminosity in the case <strong>of</strong> spherically sym-<br />
metric steady-state accretion (Frank et al. 2002). The largest possible amount <strong>of</strong> emis-<br />
sion is the Eddington limit luminosity, which is LEdd = 1.3 × 10 38 (Mco/M⊙) ergs s −1<br />
for the accretion <strong>of</strong> hydrogen-dominated material, where Mco is the mass <strong>of</strong> the com-<br />
pact object. For accretion <strong>of</strong> matter that is predominately made <strong>of</strong> heavier elements,<br />
the Eddington luminosity is twice as large. If the luminosity exceeds the Eddington<br />
value, radiation pressure on the accreting material is larger than gravity, and steady,<br />
spherically-symmetric accretion cannot occur.<br />
X-ray binary star systems in our Galaxy are divided into two general classes, high-<br />
mass X-ray binaries (HMXBs) and low-mass X-ray binaries (LMXBs) (White et al.<br />
1995). The “mass” in this classification system refers to the mass <strong>of</strong> the donor star,<br />
Mdonor. Thus, both HMXBs and LMXBs may contain relatively massive BHs, say with<br />
MBH ∼ 10 M⊙. In HMXBs, the donor star is an O or B star, with Mdonor 5 M⊙.<br />
These stars have relatively short lifetimes, τdonor 100 Myr (Sparke & Gallagher<br />
4
2000). In most HMXBs, the accreted material is captured from the strong stellar<br />
wind <strong>of</strong> the O or B star, although mass transfer via Roche-lobe overflow can also<br />
occur in some HMXBs (White et al. 1995). Approximately half <strong>of</strong> the ∼300 Milky<br />
Way X-ray binaries are HMXBs (Liu et al. 2000, 2001). Typically, HMXBs have<br />
wide orbital separations and relatively long orbital periods (∼ 1 – 10 2 days). Given<br />
the short lifetimes <strong>of</strong> O and B stars, HMXBs can only occur in a region with recent<br />
star formation. This means that HMXBs occur predominately in late-type galaxies<br />
(spirals and irregulars).<br />
In LMXBs, the donor star has a relatively low mass (Mdonor 2 M⊙), so that these<br />
are stars <strong>of</strong> later spectral type than A (White et al. 1995). Such stars have relatively<br />
long lifetimes (τdonor 1 Gyr), and reach the age <strong>of</strong> the Universe for Mdonor 0.8 M⊙.<br />
Since main sequence low mass stars have relatively weak stellar winds, most LMXBs<br />
accrete through Roche-lobe overflow. This typically requires much tighter orbits and<br />
shorter orbital periods. Among the ∼ 150 Galactic LMXBs, typical orbital periods<br />
range from tens <strong>of</strong> minutes to tens <strong>of</strong> days, with a median <strong>of</strong> ∼ 9 hours (Liu et al.<br />
2001) Since the donor stars <strong>of</strong> LMXBs live for very long periods, LMXBs can occur in<br />
regions either with or without recent star formation. Thus, LMXBs are expected to<br />
be the dominant class <strong>of</strong> X-ray binaries in early-type galaxies. [Although supernova<br />
remnants (SNRs) and radio pulsars (RPs) can reach X-ray luminosities comparable<br />
to X-ray binaries at early times, very few bright, young SNRs or RPs are expected<br />
in E/S0 galaxies, and the bright X-ray sources (LX > 10 37 ergs s −1 ) are expected to<br />
be predominantly LMXBs.] In fact, Roche lobe overflow generally requires that the<br />
donor star evolve <strong>of</strong>f the mass sequence (Verbunt & van den Heuvel 1995). This<br />
suggests that there may be a delay time (comparable to the main sequence lifetime<br />
<strong>of</strong> the donor stars) between star formation and the onset <strong>of</strong> LMXB activity.<br />
5
Much <strong>of</strong> the work in this thesis concerns the LMXBs in relatively nearby early-<br />
type galaxies. The work was made possible by the high spatial resolution and high<br />
sensitivity <strong>of</strong> the Chandra X-ray Observatory. Prior to the launch <strong>of</strong> Chandra, LMXBs<br />
were mainly studied in our galaxy (the Milky Way) and in the companion galaxies<br />
(the Large and Small Magellanic Clouds, and the Andromeda galaxy, M31). Studies<br />
<strong>of</strong> LMXBs in the Milky Way and in E/S0s are very complementary. Galactic LMXBs<br />
can be studied in great detail during both active (LX 10 36 ergs s −1 ) and quiescent (<br />
10 34 ergs s −1 ) states across all wavelengths. Optical/IR studies <strong>of</strong> individual LMXBs<br />
can provide important information about the donor star. Radio observations can<br />
detect the presence <strong>of</strong> jets, allowing the study <strong>of</strong> the connection between accretion<br />
physics and jet formation. Detailed variability and spectral studies can allow the<br />
orbital parameters to be derived, which allows the masses <strong>of</strong> the compact object and<br />
donor star to be determined. The X-ray spectra and time variability can be measured<br />
in great detail, which gives information on the accretion physics. All <strong>of</strong> this can<br />
provide a detailed understanding <strong>of</strong> the formation and evolution <strong>of</strong> a small sample <strong>of</strong><br />
Galactic LMXBs. However, there are several limitations in studying Galactic LMXBs.<br />
Many are observed through the extinction <strong>of</strong> the Galactic disk, which can make it<br />
difficult to detect the systems optically. As a result, distances are known for only<br />
a small subset <strong>of</strong> Galactic LMXBs, which implies that their luminosities and other<br />
properties are poorly known. The absorption columns vary from source to source,<br />
and in many cases is not known for a given LMXB. It is difficult to observe the whole<br />
Galaxy at once, so one may miss interesting sources, and we cannot have a complete<br />
census <strong>of</strong> the LMXB population <strong>of</strong> the Milky Way at a single instance. Perhaps<br />
most importantly the size <strong>of</strong> the observed sample <strong>of</strong> Galactic LMXBs is very limited,<br />
particularly if one considers the more luminous sources. With so few sources, we may<br />
6
not get a complete picture <strong>of</strong> the LMXB phenomena, and may completely miss rare<br />
but very powerful types <strong>of</strong> LMXBs.<br />
For observations <strong>of</strong> nearby E/S0 galaxies, we typically can only detect bright<br />
active LMXBs ( 10 37 ergs s −1 ), and these LMXBs cannot be studied in as great a<br />
level <strong>of</strong> detail as in the Milky Way. However, there are distinct advantages to E/S0<br />
observations. All LMXBs in a given E/S0 share a common Galactic absorption column<br />
and a common distance, which makes it easy to determine accurate luminosities. In<br />
most cases, nearby E/S0 galaxies fit within the field-<strong>of</strong>-view (FOV) <strong>of</strong> a Chandra<br />
observation, and thus all <strong>of</strong> the LMXBs in a given galaxy can be observed at the<br />
same time. Thus, the instantaneous luminosity function (LF) <strong>of</strong> LMXBs can be easily<br />
determined. Furthermore, individual E/S0s <strong>of</strong>ten have 50–200 sources brighter than<br />
∼ 5×10 37 ergs s −1 , as opposed to the small number <strong>of</strong> bright sources in the Galaxy.<br />
There are ∼30 early-type galaxies with good Chandra observations. Thus, it is much<br />
easier to study the properties <strong>of</strong> the population <strong>of</strong> LMXBs in external galaxies, and<br />
to do statistical studies. Moreover, there is a much greater chance <strong>of</strong> detecting rare<br />
but luminous states <strong>of</strong> these systems.<br />
1.4 The Galactic Connection Between Low-Mass<br />
X-ray Binaries and Globular Clusters<br />
Except for some galactic nuclei, the stellar densities in the field in galaxies are<br />
quite low. For example, the local stellar mass density near the Sun is ∼ 0.1 M⊙ pc −3<br />
(Binney & Merrifield 1998). At such low densities, individual stars in galaxies do not<br />
interact with one another, either physically (collisions or tidal interactions) or even<br />
gravitationally, unless they are formed together in a binary system. Thus, in the field<br />
7
<strong>of</strong> a galaxy, the low density implies that essentially all <strong>of</strong> the binary systems are pri-<br />
mordial systems which formed together. In the Milky Way, the ∼ 140 LMXBs found<br />
in the field (hereafter, Field-LMXBs) are most likely primordial binaries. Roughly<br />
half <strong>of</strong> the Milky Way stars are located in binaries. However, if one compares the<br />
number <strong>of</strong> stars in the Milky Way (total stellar luminosity <strong>of</strong> L∗ ∼ 10 10 L⊙) with the<br />
number <strong>of</strong> Field-LMXBs, it is clear that it must be relatively difficult to produce an<br />
active LMXB from a primordial binary. This is not terribly surprising; the binary<br />
progenitor <strong>of</strong> a primordial LMXB must initially be sufficiently separated to avoid<br />
having the stars merge, and the binary must survive the supernova event associated<br />
with the formation <strong>of</strong> the compact object. Despite the likely loss <strong>of</strong> a significant frac-<br />
tion <strong>of</strong> the mass and gravitational binding energy in the supernova, the binary must<br />
end up close enough that the binary system can evolve to the point where Roche-lobe<br />
overflow begins.<br />
On the other hand, galaxies also contain very dense, spherical star clusters con-<br />
taining up to millions <strong>of</strong> stars. These systems are called globular clusters (GCs). The<br />
stellar densities in GCs are much higher than in the field. Among Galactic GCs, the<br />
median central stellar density is 4 × 10 3 M⊙ pc −3 , and the densest GC has a central<br />
stellar density <strong>of</strong> nearly 10 6 M⊙ pc −3 . At such high densities, stellar interactions can<br />
occur. These stellar interactions can create (and destroy) binaries. This raises the<br />
possibility that a binary system can be created (through two-body tidal capture, or<br />
three-body or four-body exchange interactions) in GCs. This can allow a single NS<br />
or BH to acquire a donor star, or a compact object in a wide binary can move to a<br />
more compact system. For example, a typical three-body exchange interaction tends<br />
to create a tighter binary containing the more massive stars. Since most normal stars<br />
in GCs have masses <strong>of</strong> 0.8 M⊙, and NS and BHs always are more massive than<br />
8
this, the result <strong>of</strong> dynamical interactions in GCs will tend to be the creation <strong>of</strong> tight<br />
binaries containing compact objects. In fact, in the Milky Way, LMXBs are much<br />
more likely to be found in GCs than in the field, given the number <strong>of</strong> stars in GCs;<br />
∼ 10% <strong>of</strong> Galactic LMXBs are found in GCs, while GCs contain only ∼ 0.06% <strong>of</strong> the<br />
optical light <strong>of</strong> the Milky Way. Clark (1975) suggested that dynamical interactions<br />
in GCs could account for this association <strong>of</strong> LMXBs with GCs.<br />
At least thirteen LMXBs are associated with 12 GCs. (If the two transient LMXBs<br />
in NGC 6440 were different LMXBs, then there are 14 LMXBs in 12 GCs.) We list the<br />
LMXB names and corresponding GC names in Table 1.1. Nearly all <strong>of</strong> these sources<br />
show Type-I X-ray bursts. These bursts are thermonuclear flashes that must occur on<br />
a physical surface. This indicates that the compact objects in the bursting LMXBs<br />
are NSs. A few <strong>of</strong> these sources are transient and are not currently active. Given<br />
these relatively low numbers <strong>of</strong> LMXBs and associated GCs, it is difficult to perform<br />
detailed studies <strong>of</strong> the Galactic LMXB-GC connection; however some patterns have<br />
emerged. First, the Galactic GCs with LMXBs tend to have high central densities<br />
(Grindlay 1993). This suggests that dynamical interactions play a role in the GC-<br />
LMXB connection. This result is supported by recent work by Bregman et al. (2006),<br />
which indicated that the Galactic GCs with LMXBs tend to have a higher dynamical<br />
interaction rate than those without LMXBs. The second pattern is that the GCs<br />
with LMXBs tend to be found in the disk <strong>of</strong> our Galaxy (Grindlay 1993). This may<br />
indicate that tidal shocking and disruptive encounters with the disk play a role in<br />
the formation <strong>of</strong> LMXBs. Perhaps it is more likely that this is due to a preference <strong>of</strong><br />
LMXBs for GCs with higher metallicities, which is a property <strong>of</strong> the disk GCs.<br />
A much larger sample is needed to probe the LMXB-GC connection. The com-<br />
bination <strong>of</strong> Chandra X-ray Observatory and Hubble Space Telescope observations <strong>of</strong><br />
9
Table 1.1. Galactic Low-Mass X-ray Binaries in Globular Clusters<br />
Log LX<br />
LMXB Globular Cluster [ergs s −1 ] Note<br />
0512-401 NGC 1851 36.2 B<br />
1724-307 Terzan 2 36.5 B<br />
1730-335 Liller 1 37.0 B,T<br />
1732-304 Terzan 1 36.3 B<br />
1745-203 NGC 6440 37.4 R,T<br />
J1748.9-2021 NGC 6440 37.4 B,R,T<br />
1745-248 Terzan 5 35.8 B,T<br />
1746-370 NGC 6441 36.6 B<br />
1747-313 Terzan 6 36.7<br />
1820-303 NGC 6624 37.8 B<br />
1832-330 NGC 6652 36.4 B<br />
1850-087 NGC 6712 36.1 B<br />
AC 211 M 15 36.0 D<br />
M15 X-2 M 15 36.1 B,D<br />
NOTE.—M15 LMXBs from White & Angelini (2001). All<br />
other luminosities from Verbunt & Murdin (2000) and notes<br />
from Liu et al. (2001).<br />
B Type-I X-ray bursts indicate LMXB contains a NS.<br />
D Two LMXBs previously called 2127+117.<br />
R Transient LMXB may be a recurring transient.<br />
T LMXB is transient.<br />
early-type galaxies allows for the accurate identification <strong>of</strong> LMXBs and GCs. A large<br />
sample <strong>of</strong> these objects can be an excellent probe <strong>of</strong> the LMXB-GC connection.<br />
1.5 The Chandra X-ray Observatory<br />
Since studies <strong>of</strong> the diffuse interstellar gas and LMXBs in early-type galaxies<br />
require sensitive, high resolution X-ray observations, the Chandra X-ray Observatory<br />
is the ideal instrument for observing the X-ray emission in early-type galaxies. In<br />
particular, its spatial resolution is nearly an order <strong>of</strong> magnitude better than any<br />
previous <strong>of</strong> current X-ray telescope. The primary detector for such observations<br />
10
is the Advanced CCD Imaging Spectrometer (ACIS). As a non-dispersive imaging<br />
spectrometer, the location, time, and energy <strong>of</strong> every detected photon in the 0.08–<br />
10 keV range is recorded. Since an early-type galaxy will typically fit on a single 1024×<br />
1024 chip with 0.492 ′′ ×0.492 ′′ pixels, the more sensitive, backside illuminated S3 chip<br />
is typically used. At ∼ 1.5 keV, the effective area including the quantum efficiency<br />
(QE) <strong>of</strong> the S3 chip is ∼ 650 cm 2 , and the 1σ point spread function (PSF) is ∼ 0. ′′ 5<br />
near the optical axis <strong>of</strong> the telescope (Weisskopf et al. 2002). (As a point source moves<br />
<strong>of</strong>f-axis, its PSF becomes larger and more complex.) The combination <strong>of</strong> sensitivity<br />
and resolution is sufficient to detect bright, active LMXBs (LX 10 37 ergs s −1 ) at the<br />
distance <strong>of</strong> the Virgo cluster in reasonable exposure times.<br />
1.6 The Hubble Space Telescope<br />
Like Chandra, the Hubble Space Telescope (HST) is part <strong>of</strong> NASA’s Great Ob-<br />
servatories program. Since HST orbits above the atmosphere <strong>of</strong> the Earth, it is a<br />
diffraction-limited instrument. While ground-based instruments typically have ∼ 1 ′′<br />
resolution, HST can achieve ∼ 0.1 ′′ resolution or better. The Wide Field Channel <strong>of</strong><br />
the Advanced Camera for Surveys (ACS) has a 202 ′′ × 202 ′′ field-<strong>of</strong>-view (FOV), can<br />
observe light from 3700–11,000 ˚A, and has a peak efficiency <strong>of</strong> 48% (Pavlovsky et al.<br />
2004), including the effects <strong>of</strong> quantum efficiency and the optics (Pavlovsky et al.<br />
2004). The half-light diameter <strong>of</strong> a typical GC (∼ 6 pc, Harris 1996) at the distance<br />
<strong>of</strong> the Virgo cluster corresponds approximately to ∼ 1.6 pixel, where 1 pixel ∼ 0.049 ′′ .<br />
The PSF <strong>of</strong> the HST-ACS is well enough calibrated that one can detect such a spatial<br />
extent and measure the half-light radius <strong>of</strong> the GC. With HST-ACS, we can not only<br />
detect the majority <strong>of</strong> GCs at the distance <strong>of</strong> the Virgo cluster, but can also measure<br />
their sizes.<br />
11
1.7 Contents <strong>of</strong> the <strong>Thesis</strong><br />
In this thesis, we present detailed studies <strong>of</strong> the LMXBs and diffuse gas in four<br />
early-type galaxies and a study <strong>of</strong> the connection between LMXBs and GCs in eleven<br />
early-type galaxies.<br />
In Chapter 2, we present the detailed studies <strong>of</strong> LMXBs and diffuse gas in the<br />
E/S0 galaxies NGC 4365 and NGC 4382 (M85). This study <strong>of</strong> two X-ray faint E/S0<br />
galaxies on the far end <strong>of</strong> the Virgo Cluster (∼ 20 and 18 Mpc away) was published<br />
in 2003 December in the Astrophysical Journal, 599, 218–236.<br />
We discuss the diffuse gas and luminous X-ray sources around the X-ray–bright<br />
elliptical NGC 1600 in Chapter 3. This galaxy lies at the center <strong>of</strong> a group <strong>of</strong> galaxies<br />
∼ 60 Mpc away. We published this study in 2004 December in the Astrophysical<br />
Journal, 617, 262–280.<br />
We present our discovery <strong>of</strong> luminous X-ray flares from LMXB candidates in the<br />
nearest (11 Mpc), optically luminous, elliptical galaxy, NGC 4697. This work, which<br />
was published 2005 May in the Astrophysical Journal Letters, 624, L17–L20, includes<br />
the description <strong>of</strong> a new flare detection we developed, and its application to multi-<br />
epoch observations <strong>of</strong> NGC 4697.<br />
We are preparing to submit two additional papers on the multi-epoch observations<br />
<strong>of</strong> NGC 4697. Chapter 5 combines the discussion <strong>of</strong> the detection <strong>of</strong> LMXBs and their<br />
connection to GCs with our detailed analysis <strong>of</strong> the spectral and variability properties<br />
from five Chandra observations and one HST-ACS observation <strong>of</strong> NGC 4697.<br />
Finally, we discuss our study <strong>of</strong> the connection between LMXBs and GCs, which<br />
combines analysis <strong>of</strong> Chandra and HST-ACS observations <strong>of</strong> eleven early-type Virgo<br />
Cluster galaxies. We are preparing to submit Chapter 6 as a paper that focuses on<br />
the optical properties <strong>of</strong> the GCs with and without LMXBs.<br />
12
Chapter 2<br />
Chandra Observations <strong>of</strong><br />
Low-Mass X-Ray Binaries and<br />
Diffuse Gas in the Early-Type<br />
Galaxies NGC 4365 and NGC 4382<br />
(M85)<br />
2.1 Introduction<br />
Early-type galaxies are luminous X-ray sources (Forman, Jones, & Tucker 1985).<br />
For galaxies <strong>of</strong> a given optical luminosity, the X-ray–to–optical luminosity ratio<br />
(LX/LB) ranges over 2 orders <strong>of</strong> magnitude for galaxies (Canizares, Fabbiano, &<br />
Trinchieri 1987; White & Davis 1997). We refer to galaxies with relatively high<br />
LX/LB ratios as “X-ray bright” and to galaxies with relatively low LX/LB ratios as<br />
13
“X-ray faint.” Hot (kT ∼ 1 keV) interstellar gas dominates the X-ray emission in X-<br />
ray bright galaxies (e.g., Forman et al. 1985; Trinchieri, Fabbiano, & Canizares 1986),<br />
whereas X-ray faint galaxies exhibit two distinct spectral components: a hard (∼5–<br />
10 keV) component (Matsumoto et al. 1997) and a very s<strong>of</strong>t (∼0.2 keV) component<br />
(Fabbiano, Kim, & Trinchieri 1994; Pellegrini 1994; Kim et al. 1996). Since the hard<br />
component is actually found in both X-ray–bright and X-ray–faint early-type galax-<br />
ies, with strengths roughly proportional to the optical luminosity <strong>of</strong> the galaxy, Kim<br />
et al. (1992) suggested that the hard component is due to low-mass X-ray binaries<br />
(LMXBs) like those observed in the Milky Way’s bulge.<br />
Chandra observations <strong>of</strong> the X-ray faint elliptical galaxy, NGC 4697 (Sarazin,<br />
Irwin, & Bregman 2000, 2001), resolved the majority <strong>of</strong> emission into X-ray point<br />
sources, whose properties are consistent with LMXBs. Chandra observations show<br />
that a significant fraction <strong>of</strong> the LMXBs are coincident with globular clusters (Sarazin<br />
et al. 2000; Angelini et al. 2001). Taken together, the X-ray spectra <strong>of</strong> LMXBs in<br />
early-type galaxies are hard and can be fitted by thermal bremsstrahlung with a<br />
temperature <strong>of</strong> ∼7 keV. However, there is a considerable variety in observed X-ray<br />
spectra and colors <strong>of</strong> individual sources. Some <strong>of</strong> the LMXBs have very s<strong>of</strong>t X-ray<br />
spectra, similar to those <strong>of</strong> Galactic supers<strong>of</strong>t sources (Sarazin et al. 2000). The<br />
luminosity function <strong>of</strong> LMXBs in early-type galaxies in the luminosity range 5 × 10 37<br />
to 10 39 ergs s −1 appears to generally be fitted by a broken power-law (Sarazin et al.<br />
2000, 2001), with a break luminosity that is comparable to the Eddington luminosity<br />
for spherical accretion onto a 1.4 M⊙ neutron star. This suggests that the sources<br />
with luminosity 2 × 10 38 ergs s −1 are accreting black holes.<br />
In addition to the LMXBs, the Chandra observations <strong>of</strong> NGC 4697 also detected<br />
diffuse emission from interstellar gas. The gas is quite cool, with temperatures ∼0.3<br />
14
keV (Sarazin et al. 2000, 2001).<br />
With Chandra’s ability to study both the LMXB population and diffuse X-ray<br />
emission <strong>of</strong> early-type galaxies, it is useful to extend such studies to other early-type<br />
galaxies. Since diffuse emission could dominate the LMXBs in X-ray–bright galaxies,<br />
the ideal targets for studying the LMXB population <strong>of</strong> early-type galaxies are X-<br />
ray–faint galaxies. In this chapter we present the results <strong>of</strong> two such observations.<br />
Both NGC 4365 and NGC 4382 are early-type galaxies located in the Virgo Cluster.<br />
NGC 4365 is an E3 galaxy. NGC 4382 (M85) is an S0 galaxy with an interacting<br />
companion NGC 4394, which together with several other nearby galaxies (VCC 797,<br />
IC 3292) form a galaxy group RSCG 54 (Barton et al. 1996). Since NGC 4382 has<br />
somewhat bluer colors than are typical for an S0 galaxy, and its disk shows a spiral<br />
pattern, it is sometimes classified as an Sa. It was the host <strong>of</strong> the Type Ia supernova<br />
SN1960r (e.g., Porter 1993). The distances to these galaxies are 20.4 (NGC 4365)<br />
and 18.5 Mpc (NGC 4382), based on the method <strong>of</strong> surface brightness fluctuations<br />
(Tonry et al. 2001). For comparison, NGC 4697 has a distance <strong>of</strong> 11.7 Mpc using the<br />
same technique. All three galaxies have similar X-ray luminosities and LX/LB ratios<br />
(O’Sullivan, Forbes, & Ponman 2001).<br />
In § 2.2 we discuss the observations and data reduction <strong>of</strong> these galaxies. The<br />
X-ray images are presented in § 2.3. The properties <strong>of</strong> resolved sources are given and<br />
discussed in § 2.4. We discuss the X-ray spectral properties in § 2.5. The spatial<br />
distribution <strong>of</strong> the diffuse X-ray–emitting gas is determined in § 2.6. We summarize<br />
our conclusions in § 2.7.<br />
15
2.2 Observation and Data Reduction<br />
NGC 4365 was observed on 2001 June 2–3 with a live exposure <strong>of</strong> 40,429 s, while<br />
NGC 4382 was observed on 2001 May 29–30 for 39,749 s. Both galaxies were observed<br />
with the ACIS-235678 chips operated at a temperature <strong>of</strong> −120 ◦ C and with a frame<br />
time <strong>of</strong> 3.2 s. We determined the pointings so that the entire galaxy was located on<br />
the S3 chip and so that the center <strong>of</strong> each galaxy was not on a node boundary <strong>of</strong><br />
the chip. Although a number <strong>of</strong> serendipitous sources were seen on the other chips,<br />
the analysis <strong>of</strong> both galaxies in this chapter is based on data from the S3 chip alone.<br />
The data were telemetered in Faint mode, and only events with ASCA grades <strong>of</strong> 0,<br />
2, 3, 4, and 6 were included. Photon energies were determined using the gain file<br />
acisD2000-08-12gainN0003.fits. We excluded bad pixels, bad columns, and columns<br />
adjacent to bad columns or chip node boundaries.<br />
Chandra is known to encounter periods <strong>of</strong> high background (“background flares”),<br />
which especially affect the backside-illuminated S1 and S3 chips. 1 We determined the<br />
background count rate for each galaxy, using the S1 chip to avoid the enhanced<br />
flux due to the galaxy on the S3 chip. For both NGC 4365 and NGC 4382, no<br />
background flares were seen. The backgrounds for extended regions were taken from<br />
the deep blank sky backgrounds compiled by Maxim Markevitch 3 , and were adjusted<br />
to the aspect histories <strong>of</strong> our observations using his MAKE ACISBG program 3 The<br />
normalization <strong>of</strong> the background was increased very slightly to match the 5–10 keV<br />
count rate <strong>of</strong> the blank-sky background with a galaxy emission-free region <strong>of</strong> each<br />
galaxy on the S3 chip. We included the “background” due to the readout artifact in<br />
ACIS using his MAKE READOUT BG program 3 .<br />
On the S3 image <strong>of</strong> NGC 4365, there were two X-ray sources with positions that<br />
1 See http://cxc.harvard.edu/contrib/maxim/acisbg/.<br />
16
agreed with positions from the USNO-A2.0 (Monet et al. 1998) or the Two Micron<br />
All Sky Survey (2MASS; Cutri et al. 2001) catalogs. Source 98 in Table 2.1, an<br />
X-ray source near the edge <strong>of</strong> the field where the Chandra point-spread-function<br />
(PSF) is quite broad and the X-ray position is uncertain, corresponded to USNO-<br />
A2.0 0900−07143676. For this source, the optical and X-ray positions agree to within<br />
∼0. ′′ 4. The second possible optical identification is between the optical nucleus <strong>of</strong><br />
NGC 4365 itself and source 1 in Table 2.1. Unfortunately, the central region <strong>of</strong> this<br />
galaxy is crowded with sources, and it is uncertain whether the source closest to<br />
the nucleus is, in fact, an active galactic nucleus (AGN), a nearly coincident X-ray<br />
binary, or a combination <strong>of</strong> sources. Confusion limits the accuracy with which the<br />
positions <strong>of</strong> sources near the center <strong>of</strong> NGC 4365 can be determined. In the absence<br />
<strong>of</strong> more direct evidence, we will assume that the positions in NGC 4365 are accurate<br />
to 1 ′′ . In NGC 4382, there were two X-ray sources with optical identifications and<br />
positions from the Tycho-2 catalog (Høg et al. 2000), the 2MASS catalog, and/or<br />
the USNO-A2.0 optical catalog. The first source, source 38 in Table 2.2, corresponds<br />
to J1225+182, a z = 1.19 quasar (Knezek & Bregman 1998), and is the brightest<br />
X-ray source in the S3 field. The second source, which was just below the detection<br />
threshold for inclusion in Table 2.2, corresponds to BD +18 ◦ 2609, a G5 star with a<br />
proper motion <strong>of</strong> ∼90 mas yr −1 (Høg et al. 1998). The X-ray positions agreed with<br />
the optical positions to better than 0. ′′ 4 in both cases with no evidence for a systematic<br />
<strong>of</strong>fset. We believe that the X-ray positions for NGC 4382 are generally accurate to<br />
∼0. ′′ 5.<br />
We performed initial data reduction and some <strong>of</strong> the data analysis using the Chan-<br />
dra analysis package CIAO 2 . We extracted spectra using the CALCRMF 3 s<strong>of</strong>tware<br />
2 See http://asc.harvard.edu/ciao/.<br />
3 See http://asc.harvard.edu/cont-s<strong>of</strong>t/s<strong>of</strong>tware/.<br />
17
kindly provided by Alexey Vikhlinin and Jonathon McDowell. The spectra were fit-<br />
ted using XSPEC. 4 Since launch, the ACIS quantum efficiency (QE) has undergone<br />
continuous degradation. 5 We used the XSPEC ACISABS model to correct X-ray<br />
spectra for this effect.<br />
2.3 X-ray Image<br />
The X-ray images <strong>of</strong> NGC 4365 and NGC 4382 show both resolved point sources<br />
and diffuse emission. To best image this combination, we adaptively smoothed the<br />
Chandra S3 image using a minimum signal–to–noise ratio (S/N) per smoothing beam<br />
<strong>of</strong> 3. After correcting for exposure and background, we removed regions <strong>of</strong> less than<br />
20 ks to avoid artifacts at the chip’s edge. Figure 2.1 displays gray-scale images with<br />
a logarithmic surface brightness scale ranging between 1.56 × 10 −6 and 3.3 × 10 −4<br />
counts pixel −1 s −1 . In both galaxies, the majority <strong>of</strong> the X-ray luminosity emission<br />
has been resolved into point sources.<br />
In Figure 2.2, we show the Digital Sky Survey (DSS) optical images centered on<br />
NGC 4365 and NGC 4382 using a logarithmic gray scale. The overlaid circles indicate<br />
the positions <strong>of</strong> the X-ray point sources listed in Tables 2.1 and 2.2. Only a small<br />
fraction <strong>of</strong> the weaker point sources are not evident in Figure 2.1. In NGC 4365,<br />
the diffuse emission qualitatively has the same ellipticity and position angle (P.A.) as<br />
the optical emission. On the other hand, the X-ray emission in NGC 4382 appears<br />
rounder than the optical emission.<br />
4 See http://heasarc.gsfc.nasa.gov/docs/s<strong>of</strong>tware/lheas<strong>of</strong>t/.<br />
5 See http://cxc.harvard.edu/cal/Acis/Cal prods/qeDeg/.<br />
18
24:00<br />
22:00<br />
7:20:00<br />
18:00<br />
16:00<br />
18:00<br />
16:00<br />
14:00<br />
12:00<br />
18:10:00<br />
08:00<br />
12:24:50 45 12:24:40 35 12:24:30 25 12:24:20 15 12:24:10<br />
12:25:50 45 12:25:40 35 12:25:30 25 12:25:20 15 12:25:10 05<br />
Fig. 2.1.— Adaptively smoothed Chandra S3 image (0.3–10 keV) <strong>of</strong> NGC 4365<br />
(top) and NGC 4382 (bottom), corrected for exposure and background. The scale is<br />
logarithmic and ranges from 1.56 × 10 −6 to 3.3 × 10 −4 counts pixel −1 s −1 .<br />
19
24:00<br />
22:00<br />
7:20:00<br />
18:00<br />
16:00<br />
18:00<br />
16:00<br />
14:00<br />
12:00<br />
18:10:00<br />
08:00<br />
12:24:50 40 30 20 10<br />
12:25:50 40 30 20 10<br />
Fig. 2.2.— Logarithmic gray-scale DSS optical image <strong>of</strong> NGC 4365 (top) and<br />
NGC 4382 (bottom). The circles indicate the positions <strong>of</strong> the X-ray sources listed<br />
in Tables 2.1 and 2.2. The relative surface brightness range covered by the gray scale<br />
is narrower than in Figure 2.1.<br />
20
Table 2.1. Discrete X-ray Sources in NGC 4365<br />
Source d Count Rate<br />
Number Name R.A. Decl. (arcsec) (10−4 s−1 ) S/N LX H21 H31 Notes<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11)<br />
1.......... CXOU J122428.3+071904 12 24 28.32 7 19 04.1 1.0 37.34±3.18 11.75 152.49 −0.12 +0.12<br />
−0.11<br />
−0.48+0.13<br />
−0.11 a,b,c<br />
2.......... CXOU J122428.1+071902 12 24 28.18 7 19 02.9 1.4 14.23±1.98 7.17 58.10 −0.25 +0.23<br />
−0.21<br />
−0.28+0.23<br />
−0.20 a,b<br />
3.......... CXOU J122428.4+071906 12 24 28.44 7 19 06.0 3.5 48.89±3.61 13.53 199.64 −0.08 +0.09<br />
−0.09<br />
−0.35+0.11<br />
−0.10 a,b<br />
4.......... CXOU J122428.5+071905 12 24 28.59 7 19 05.5 5.2 8.86±1.56 5.69 36.16 +0.23 +0.34<br />
−0.41<br />
+0.12+0.38<br />
−0.42 a,b<br />
5.......... CXOU J122427.8+071907 12 24 27.89 7 19 07.3 6.5 4.59±1.16 3.95 18.75 −0.38 +0.56<br />
−0.38<br />
−0.37+0.59<br />
−0.39 c,d<br />
6.......... CXOU J122428.3+071857 12 24 28.36 7 18 57.0 7.0 5.94±1.35 4.39 24.26 +0.70 +0.25<br />
−0.77<br />
−0.74+1.74<br />
−0.26<br />
7.......... CXOU J122428.6+071908 12 24 28.67 7 19 08.0 7.4 13.66±1.97 6.93 55.76 −0.21 +0.24<br />
−0.22<br />
−0.17+0.23<br />
−0.22<br />
8.......... CXOU J122428.7+071853 12 24 28.70 7 18 53.7 12.0 3.37±1.01 3.34 13.76 −0.08 +0.57<br />
−0.52<br />
−0.22+0.66<br />
−0.51 c,d<br />
9.......... CXOU J122428.9+071856 12 24 28.97 7 18 56.6 12.8 7.11±1.43 4.98 29.04 +0.36 +0.26<br />
−0.34<br />
−0.05+0.43<br />
−0.41 c,d<br />
10........ CXOU J122429.1+071859 12 24 29.18 7 18 59.6 14.3 5.40±1.28 4.23 22.04 +0.48 +0.30<br />
−0.47<br />
+0.00+0.57<br />
−0.57 c,d<br />
11........ CXOU J122428.4+071849 12 24 28.43 7 18 49.4 14.6 3.53±1.04 3.39 14.42 +0.06 +0.46<br />
−0.48<br />
−0.36+0.73<br />
−0.45<br />
12........ CXOU J122427.1+071901 12 24 27.18 7 19 01.6 16.2 7.18±1.45 4.95 29.33 +0.27 +0.29<br />
−0.35<br />
−0.19+0.49<br />
−0.41 c,d<br />
13........ CXOU J122429.3+071850 12 24 29.33 7 18 50.4 20.8 4.16±1.14 3.67 17.00 −0.74 +0.87<br />
−0.22<br />
−0.38+0.52<br />
−0.35 c,d<br />
14........ CXOU J122429.7+071904 12 24 29.72 7 19 04.1 21.7 16.48±2.12 7.78 67.31 +0.05 +0.17<br />
−0.17<br />
−0.27+0.22<br />
−0.19<br />
15........ CXOU J122428.9+071844 12 24 28.92 7 18 44.0 22.1 6.53±1.31 5.00 26.66 +0.18 +0.28<br />
−0.32<br />
−0.54+0.61<br />
−0.32<br />
16........ CXOU J122427.2+071844 12 24 27.29 7 18 44.4 24.2 5.74±1.30 4.42 23.45 −0.06 +0.34<br />
−0.33<br />
−0.37+0.46<br />
−0.33 e<br />
17........ CXOU J122426.6+071856 12 24 26.61 7 18 56.3 25.7 3.22±0.97 3.31 13.14 +0.61 +0.30<br />
−0.71<br />
−0.20+1.00<br />
−0.71 c,d<br />
18........ CXOU J122427.3+071926 12 24 27.31 7 19 26.1 26.4 11.78±1.80 6.56 48.11 +0.10 +0.21<br />
−0.22<br />
−0.22+0.28<br />
−0.24 c,d<br />
19........ CXOU J122429.8+071916 12 24 29.85 7 19 16.6 26.9 14.33±1.97 7.28 58.51 −0.03 +0.17<br />
−0.17<br />
−0.71+0.25<br />
−0.15<br />
20........ CXOU J122428.1+071836 12 24 28.17 7 18 36.0 27.8 4.53±1.13 4.00 18.50 +0.06 +0.42<br />
−0.44<br />
−0.03+0.48<br />
−0.46<br />
21........ CXOU J122429.3+071839 12 24 29.32 7 18 39.0 29.3 3.89±1.07 3.63 15.88 +0.08 +0.54<br />
−0.60<br />
+0.04+0.56<br />
−0.59 e<br />
22........ CXOU J122427.4+071934 12 24 27.49 7 19 34.4 32.7 3.93±1.06 3.72 16.04 +0.29 +0.37<br />
−0.48<br />
+0.08+0.48<br />
−0.52<br />
23........ CXOU J122428.5+071831 12 24 28.50 7 18 31.1 32.9 21.17±2.38 8.90 86.44 +0.02 +0.15<br />
−0.15<br />
−0.43+0.19<br />
−0.15<br />
24........ CXOU J122427.8+071830 12 24 27.88 7 18 30.5 33.8 13.64±1.93 7.06 55.69 −0.01 +0.21<br />
−0.21<br />
−0.10+0.24<br />
−0.23<br />
25........ CXOU J122428.7+071938 12 24 28.72 7 19 38.7 35.5 6.86±1.38 4.97 27.99 +0.25 +0.27<br />
−0.32<br />
+0.00+0.36<br />
−0.36 c,d<br />
26........ CXOU J122429.1+071937 12 24 29.13 7 19 37.9 36.5 2.69±0.89 3.04 11.00 +0.38 +0.40<br />
−0.62<br />
+0.06+0.61<br />
−0.66 c,d<br />
27........ CXOU J122429.9+071832 12 24 29.97 7 18 32.5 40.4 3.51±1.01 3.48 14.32 +0.33 +0.37<br />
−0.51<br />
−0.16+0.67<br />
−0.55<br />
Continued on Next Page. . .<br />
21
Table 2.1—Continued<br />
Source d Count Rate<br />
Number Name R.A. Decl. (arcsec) (10−4 s−1 ) S/N LX H21 H31 Notes<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11)<br />
28........ CXOU J122430.9+071852 12 24 30.92 7 18 52.8 41.2 2.79±0.90 3.10 11.40 −0.14 +0.60<br />
−0.51<br />
+0.11+0.46<br />
−0.51<br />
29........ CXOU J122429.8+071938 12 24 29.82 7 19 38.5 41.7 2.65±0.89 3.00 10.83 +0.29 +0.42<br />
−0.58<br />
+0.05+0.57<br />
−0.60 e<br />
30........ CXOU J122428.4+071946 12 24 28.42 7 19 46.9 43.2 6.67±1.36 4.91 27.23 −0.32 +0.32<br />
−0.26<br />
−0.44+0.36<br />
−0.26<br />
31........ CXOU J122427.6+071947 12 24 27.63 7 19 47.1 44.3 2.66±0.89 3.00 10.87 +0.00 +0.47<br />
−0.47<br />
−0.87+1.87<br />
−0.13 e<br />
32........ CXOU J122430.4+071933 12 24 30.48 7 19 33.6 44.5 4.05±1.08 3.74 16.54 +0.31 +0.38<br />
−0.51<br />
+0.08+0.53<br />
−0.58<br />
33........ CXOU J122426.8+071944 12 24 26.89 7 19 44.7 45.7 5.03±1.51 3.33 20.53 +0.45 +0.30<br />
−0.45<br />
−0.73+1.67<br />
−0.27<br />
34........ CXOU J122429.1+071949 12 24 29.10 7 19 49.3 47.2 2.94±0.93 3.17 11.99 −0.55 +0.75<br />
−0.34<br />
−0.68+0.93<br />
−0.28 c,d<br />
35........ CXOU J122431.2+071925 12 24 31.20 7 19 25.7 49.0 5.08±1.20 4.24 20.76 −0.59 +0.35<br />
−0.21<br />
−0.77+0.46<br />
−0.17<br />
36........ CXOU J122428.4+071813 12 24 28.48 7 18 13.9 50.0 7.66±1.48 5.18 31.27 +0.88 +0.11<br />
−0.92<br />
+0.83+0.16<br />
−1.06<br />
37........ CXOU J122425.3+071828 12 24 25.35 7 18 28.0 56.2 2.79±0.92 3.04 11.40 −0.43 +0.73<br />
−0.41<br />
−0.43+0.73<br />
−0.41 c,d<br />
38........ CXOU J122427.7+071806 12 24 27.74 7 18 06.9 57.4 18.65±2.27 8.23 76.14 −0.33 +0.15<br />
−0.13<br />
−0.91+0.26<br />
−0.07<br />
39........ CXOU J122431.8+071923 12 24 31.89 7 19 23.4 57.5 3.22±0.96 3.37 13.15 +0.48 +0.40<br />
−0.79<br />
+0.37+0.48<br />
−0.82<br />
40........ CXOU J122425.2+071826 12 24 25.24 7 18 26.6 58.3 3.60±1.03 3.48 14.69 −0.02 +0.38<br />
−0.38<br />
−0.83+1.42<br />
−0.17 c,d<br />
41........ CXOU J122431.4+071827 12 24 31.45 7 18 27.5 59.8 5.43±1.22 4.45 22.19 −0.16 +0.35<br />
−0.31<br />
−0.32+0.40<br />
−0.31<br />
42........ CXOU J122424.6+071833 12 24 24.66 7 18 33.9 61.3 11.86±1.79 6.63 48.44 +0.13 +0.21<br />
−0.22<br />
−0.16+0.28<br />
−0.25<br />
43........ CXOU J122425.1+071947 12 24 25.16 7 19 47.9 63.9 3.95±1.06 3.74 16.11 +0.50 +0.32<br />
−0.57<br />
+0.24+0.51<br />
−0.68<br />
44........ CXOU J122428.5+072009 12 24 28.56 7 20 09.5 65.8 3.22±1.07 3.02 13.14 +0.00 +0.45<br />
−0.45<br />
−0.67+1.09<br />
−0.30 c,d<br />
45........ CXOU J122430.3+072005 12 24 30.30 7 20 05.1 68.4 4.21±1.19 3.55 17.21 +0.24 +0.41<br />
−0.53<br />
+0.15+0.46<br />
−0.54 c,d<br />
46........ CXOU J122423.7+071922 12 24 23.73 7 19 22.7 69.9 2.62±0.86 3.05 10.70 +0.00 +0.45<br />
−0.45<br />
−0.67+1.09<br />
−0.30<br />
47........ CXOU J122425.2+071804 12 24 25.29 7 18 04.6 73.9 10.72±1.68 6.39 43.76 +0.09 +0.20<br />
−0.21<br />
−0.59+0.35<br />
−0.22<br />
48........ CXOU J122423.1+071836 12 24 23.15 7 18 36.9 80.6 2.70±0.89 3.02 11.01 +0.20 +0.54<br />
−0.70<br />
+0.06+0.64<br />
−0.69 c,d,e<br />
49........ CXOU J122432.5+071955 12 24 32.50 7 19 55.2 81.5 3.17±0.96 3.29 12.94 +0.50 +0.36<br />
−0.70<br />
+0.40+0.43<br />
−0.74<br />
50........ CXOU J122429.4+072027 12 24 29.42 7 20 27.1 85.1 6.29±1.31 4.79 25.69 −0.21 +0.31<br />
−0.27<br />
−0.69+0.59<br />
−0.23 c,d<br />
51........ CXOU J122430.7+071746 12 24 30.75 7 17 46.5 85.7 3.65±1.03 3.55 14.89 +0.09 +0.41<br />
−0.44<br />
−0.50+0.84<br />
−0.40<br />
52........ CXOU J122425.6+071746 12 24 25.69 7 17 46.0 86.7 16.83±2.10 8.02 68.71 +0.01 +0.16<br />
−0.16<br />
−0.45+0.22<br />
−0.18<br />
53........ CXOU J122422.4+071851 12 24 22.40 7 18 51.4 88.0 5.85±1.26 4.64 23.89 +0.59 +0.25<br />
−0.45<br />
+0.49+0.31<br />
−0.51 c,d<br />
54........ CXOU J122432.2+072010 12 24 32.29 7 20 10.5 89.7 4.01±1.05 3.81 16.37 −0.14 +0.39<br />
−0.35<br />
−0.50+0.57<br />
−0.32<br />
Continued on Next Page. . .<br />
22
Table 2.1—Continued<br />
Source d Count Rate<br />
Number Name R.A. Decl. (arcsec) (10−4 s−1 ) S/N LX H21 H31 Notes<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11)<br />
55........ CXOU J122426.7+071736 12 24 26.76 7 17 36.6 90.0 4.84±1.14 4.25 19.75 −0.75 +0.73<br />
−0.21<br />
−0.63+0.49<br />
−0.24<br />
56........ CXOU J122429.0+071729 12 24 29.03 7 17 29.8 94.7 5.73±1.24 4.62 23.39 +0.12 +0.36<br />
−0.39<br />
+0.22+0.32<br />
−0.38<br />
57........ CXOU J122431.8+072028 12 24 31.85 7 20 28.2 99.9 2.81±0.88 3.20 11.50 −0.25 +0.49<br />
−0.39<br />
−1.00+2.00<br />
−0.00<br />
58........ CXOU J122425.1+071734 12 24 25.13 7 17 34.9 100.4 10.92±1.70 6.42 44.58 +0.41 +0.20<br />
−0.24<br />
+0.11+0.29<br />
−0.31<br />
59........ CXOU J122424.0+071745 12 24 24.04 7 17 45.1 100.7 3.35±0.96 3.49 13.67 −0.33 +0.57<br />
−0.40<br />
−0.13+0.47<br />
−0.42 c,d<br />
60........ CXOU J122431.1+071724 12 24 31.18 7 17 24.7 108.2 7.62±1.42 5.35 31.11 +0.02 +0.30<br />
−0.30<br />
+0.03+0.31<br />
−0.31<br />
61........ CXOU J122424.9+072046 12 24 24.92 7 20 46.9 114.4 2.87±0.95 3.03 11.73 −0.08 +0.52<br />
−0.48<br />
−0.27+0.65<br />
−0.47<br />
62........ CXOU J122435.9+071925 12 24 35.93 7 19 25.9 116.3 3.82±1.03 3.72 15.59 +0.00 +0.83<br />
−0.83<br />
+0.69+0.25<br />
−0.72<br />
63........ CXOU J122420.7+071938 12 24 20.72 7 19 38.0 117.2 6.59±1.34 4.93 26.93 +0.12 +0.30<br />
−0.33<br />
−0.11+0.38<br />
−0.35<br />
64........ CXOU J122421.6+071757 12 24 21.62 7 17 57.6 118.8 3.94±1.04 3.80 16.10 +1.00 +0.00<br />
−0.48<br />
+1.00+0.00<br />
−0.37<br />
65........ CXOU J122435.3+071805 12 24 35.30 7 18 05.4 119.9 10.81±1.70 6.34 44.13 −0.08 +0.21<br />
−0.20<br />
−0.71+0.39<br />
−0.18<br />
66........ CXOU J122425.8+071706 12 24 25.81 7 17 06.1 123.2 3.41±0.96 3.54 13.92 −0.33 +0.46<br />
−0.34<br />
−0.66+0.74<br />
−0.27<br />
67........ CXOU J122423.3+071720 12 24 23.35 7 17 20.6 126.4 3.60±0.99 3.62 14.70 +0.29 +0.42<br />
−0.57<br />
+0.17+0.49<br />
−0.59<br />
68........ CXOU J122435.8+071806 12 24 35.88 7 18 06.2 127.2 3.87±1.04 3.73 15.82 +0.31 +0.38<br />
−0.51<br />
+0.08+0.51<br />
−0.56<br />
69........ CXOU J122426.3+071653 12 24 26.39 7 16 53.2 133.5 48.43±3.54 13.67 197.75 +0.65 +0.08<br />
−0.10<br />
+0.64+0.09<br />
−0.11<br />
70........ CXOU J122426.7+071650 12 24 26.70 7 16 50.2 135.6 8.21±1.47 5.58 33.52 +0.24 +0.24<br />
−0.27<br />
−0.16+0.35<br />
−0.31<br />
71........ CXOU J122420.1+071739 12 24 20.18 7 17 39.4 146.8 16.46±2.08 7.89 67.20 +0.04 +0.16<br />
−0.16<br />
−0.44+0.23<br />
−0.18<br />
72........ CXOU J122437.0+071757 12 24 37.08 7 17 57.3 147.1 3.59±1.01 3.57 14.65 +0.46 +0.30<br />
−0.46<br />
−0.29+0.77<br />
−0.51<br />
73........ CXOU J122423.9+071651 12 24 23.95 7 16 51.0 147.4 5.06±1.17 4.34 20.66 +0.47 +0.26<br />
−0.38<br />
−0.33+0.72<br />
−0.47<br />
74........ CXOU J122438.4+071902 12 24 38.46 7 19 02.8 151.8 4.67±1.21 3.86 19.05 −0.10 +0.49<br />
−0.45<br />
+0.15+0.39<br />
−0.44<br />
75........ CXOU J122419.2+072019 12 24 19.25 7 20 19.3 153.9 2.88±0.90 3.20 11.78 +0.38 +0.50<br />
−0.87<br />
+0.55+0.36<br />
−0.82<br />
76........ CXOU J122418.0+071839 12 24 18.01 7 18 39.1 154.4 3.36±0.97 3.46 13.70 −0.28 +0.47<br />
−0.37<br />
−1.00+2.00<br />
−0.00<br />
77........ CXOU J122418.0+071803 12 24 18.04 7 18 03.5 163.6 3.45±0.98 3.52 14.08 +0.00 +0.45<br />
−0.45<br />
−0.11+0.51<br />
−0.46<br />
78........ CXOU J122422.1+071646 12 24 22.19 7 16 46.1 164.7 9.95±1.62 6.14 40.63 +0.15 +0.24<br />
−0.26<br />
+0.10+0.26<br />
−0.27<br />
79........ CXOU J122434.9+072116 12 24 34.93 7 21 16.1 165.4 2.86±0.95 3.02 11.67 +0.09 +0.55<br />
−0.61<br />
+0.17+0.50<br />
−0.60<br />
80........ CXOU J122423.4+072136 12 24 23.44 7 21 36.5 168.7 2.77±0.91 3.03 11.29 +0.07 +0.47<br />
−0.50<br />
−0.37+0.82<br />
−0.48<br />
81........ CXOU J122436.4+071706 12 24 36.47 7 17 06.7 169.2 3.34±0.96 3.49 13.63 −0.27 +0.51<br />
−0.39<br />
−0.56+0.66<br />
−0.32<br />
Continued on Next Page. . .<br />
23
Table 2.1—Continued<br />
Source d Count Rate<br />
Number Name R.A. Decl. (arcsec) (10−4 s−1 ) S/N LX H21 H31 Notes<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11)<br />
82........ CXOU J122417.9+071741 12 24 17.91 7 17 41.4 174.7 4.85±1.15 4.23 19.78 +0.38 +0.37<br />
−0.56<br />
+0.51+0.29<br />
−0.50<br />
83........ CXOU J122417.8+071715 12 24 17.80 7 17 15.6 189.5 7.11±1.38 5.17 29.02 +0.40 +0.25<br />
−0.33<br />
+0.03+0.41<br />
−0.42<br />
84........ CXOU J122436.6+072129 12 24 36.65 7 21 29.3 191.8 9.43±1.81 5.22 38.51 −0.11 +0.29<br />
−0.27<br />
−0.12+0.35<br />
−0.32<br />
85........ CXOU J122425.1+072211 12 24 25.19 7 22 11.2 192.9 3.33±1.03 3.24 13.59 +0.39 +0.34<br />
−0.49<br />
+0.18+0.46<br />
−0.56<br />
86........ CXOU J122438.3+072107 12 24 38.31 7 21 07.0 193.7 28.87±2.88 10.01 117.88 −0.25 +0.12<br />
−0.11<br />
−0.61+0.15<br />
−0.12 e<br />
87........ CXOU J122427.2+072231 12 24 27.28 7 22 31.2 207.9 8.82±1.87 4.72 36.03 +0.32 +0.34<br />
−0.44<br />
+0.32+0.36<br />
−0.49<br />
88........ CXOU J122414.7+072004 12 24 14.74 7 20 04.9 210.3 37.47±3.20 11.72 153.01 −0.22 +0.11<br />
−0.10<br />
−0.54+0.12<br />
−0.10 c<br />
89........ CXOU J122424.8+072229 12 24 24.83 7 22 29.4 211.9 4.53±1.35 3.36 18.48 +0.73 +0.24<br />
−1.10<br />
+0.76+0.22<br />
−1.08<br />
90........ CXOU J122441.0+072047 12 24 41.05 7 20 47.8 216.9 4.95±1.38 3.59 20.21 +0.86 +0.14<br />
−1.67<br />
+0.85+0.15<br />
−1.67<br />
91........ CXOU J122438.9+071625 12 24 38.96 7 16 25.8 224.3 12.21±1.84 6.65 49.87 +0.05 +0.20<br />
−0.20<br />
−0.50+0.32<br />
−0.23<br />
92........ CXOU J122438.9+072152 12 24 38.93 7 21 52.4 231.6 7.80±1.61 4.83 31.85 +0.57 +0.28<br />
−0.52<br />
+0.68+0.21<br />
−0.44<br />
93........ CXOU J122425.4+072258 12 24 25.42 7 22 58.7 238.6 7.47±1.62 4.60 30.48 +0.30 +0.26<br />
−0.32<br />
−0.33+0.66<br />
−0.44<br />
94........ CXOU J122435.9+071533 12 24 35.94 7 15 33.3 239.6 5.70±1.30 4.39 23.26 +0.11 +0.34<br />
−0.37<br />
−0.05+0.42<br />
−0.40<br />
95........ CXOU J122420.8+072237 12 24 20.84 7 22 37.0 240.1 6.85±1.55 4.41 27.96 +0.50 +0.25<br />
−0.38<br />
−0.10+0.62<br />
−0.55<br />
96........ CXOU J122440.9+072204 12 24 40.90 7 22 04.1 260.6 55.42±3.99 13.88 226.30 −0.19 +0.08<br />
−0.08<br />
−0.48+0.10<br />
−0.09<br />
97........ CXOU J122437.9+072311 12 24 37.91 7 23 11.0 285.9 22.69±2.74 8.27 92.64 −0.01 +0.16<br />
−0.16<br />
−0.25+0.21<br />
−0.19 c<br />
98........ CXOU J122419.9+072332 12 24 19.91 7 23 32.6 296.1 3.83±1.27 3.02 15.64 +0.08 +0.53<br />
−0.58<br />
+0.12+0.58<br />
−0.67 c<br />
99........ CXOU J122416.0+072324 12 24 16.03 7 23 24.3 317.7 36.75±4.33 8.65 150.05 +0.49 +0.15<br />
−0.18<br />
+0.43+0.17<br />
−0.20 f<br />
NOTE.—Units <strong>of</strong> right ascension are hours, minutes, and seconds, and units <strong>of</strong> declination are degrees, arcminutes, and arcseconds. The units for<br />
LX are 1037 ergs s−1 in the 0.3–10 keV band.<br />
a Sources near the center may be confused with nearby sources, making their positions, fluxes, and extents uncertain.<br />
b Source is noticeably more extended than PSF.<br />
c Possible faint optical counterpart.<br />
d Globular cluster is possible optical counterpart.<br />
e Source may be variable.<br />
f Source is at the edge <strong>of</strong> the S3 detector, and flux is uncertain due to large exposure correction.<br />
24
Table 2.2. Discrete X-ray Sources in NGC 4382<br />
Source d Count Rate<br />
Number Name R.A. Decl. (arcsec) (10−4 s−1 ) S/N LX H21 H31 Notes<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11)<br />
1.......... CXOU J122524.0+181127 12 25 24.06 18 11 27.7 1.8 22.79±2.55 8.93 89.66 −0.16 +0.13<br />
−0.13<br />
−0.36+0.14<br />
−0.13 a<br />
2.......... CXOU J122523.9+181121 12 25 23.99 18 11 21.7 4.2 16.44±2.15 7.63 64.71 −0.10 +0.17<br />
−0.16<br />
−0.39+0.20<br />
−0.17<br />
3.......... CXOU J122523.9+181131 12 25 23.90 18 11 31.1 5.5 10.90±1.79 6.09 42.88 −0.08 +0.25<br />
−0.24<br />
−0.68+0.46<br />
−0.21<br />
4.......... CXOU J122523.5+181126 12 25 23.58 18 11 26.7 6.6 11.87±1.88 6.33 46.71 −0.04 +0.27<br />
−0.27<br />
−0.07+0.29<br />
−0.27<br />
5.......... CXOU J122524.5+181134 12 25 24.54 18 11 34.9 11.5 11.97±1.84 6.52 47.11 +0.35 +0.24<br />
−0.29<br />
+0.28+0.26<br />
−0.30<br />
6.......... CXOU J122523.6+181136 12 25 23.60 18 11 36.4 12.2 5.10±1.24 4.12 20.06 +0.26 +0.37<br />
−0.46<br />
+0.18+0.42<br />
−0.49<br />
7.......... CXOU J122523.7+181139 12 25 23.75 18 11 39.9 14.6 9.64±1.66 5.79 37.92 −0.20 +0.20<br />
−0.18<br />
−0.65+0.27<br />
−0.17<br />
8.......... CXOU J122524.7+181141 12 25 24.70 18 11 41.0 17.7 11.31±1.79 6.33 44.48 +0.69 +0.17<br />
−0.31<br />
+0.46+0.29<br />
−0.43<br />
9.......... CXOU J122525.6+181141 12 25 25.65 18 11 41.5 27.7 5.24±1.25 4.20 20.63 −0.09 +0.45<br />
−0.41<br />
+0.22+0.32<br />
−0.37<br />
10........ CXOU J122522.8+181053 12 25 22.84 18 10 53.6 36.5 7.19±1.43 5.01 28.28 −0.41 +0.27<br />
−0.21<br />
−0.97+1.90<br />
−0.03<br />
11........ CXOU J122524.8+181048 12 25 24.83 18 10 48.7 38.9 3.32±0.99 3.36 13.08 −0.36 +0.63<br />
−0.41<br />
−0.21+0.54<br />
−0.43<br />
12........ CXOU J122524.9+181205 12 25 24.95 18 12 05.7 41.8 27.91±2.76 10.12 109.83 +0.11 +0.14<br />
−0.15<br />
+0.00+0.15<br />
−0.15<br />
13........ CXOU J122526.9+181149 12 25 26.94 18 11 49.7 47.7 24.71±2.59 9.55 97.24 −0.03 +0.14<br />
−0.14<br />
−0.45+0.17<br />
−0.14<br />
14........ CXOU J122520.5+181121 12 25 20.53 18 11 21.8 50.1 2.74±0.91 3.01 10.78 −0.41 +0.86<br />
−0.47<br />
+0.14+0.45<br />
−0.51<br />
15........ CXOU J122522.1+181043 12 25 22.15 18 10 43.5 50.3 17.38±2.22 7.82 68.40 +0.21 +0.18<br />
−0.19<br />
−0.02+0.22<br />
−0.22<br />
16........ CXOU J122520.6+181052 12 25 20.69 18 10 52.5 58.3 2.80±0.93 3.01 11.03 −0.11 +0.68<br />
−0.59<br />
+0.17+0.49<br />
−0.59<br />
17........ CXOU J122527.4+181157 12 25 27.47 18 11 57.8 58.4 10.08±1.67 6.03 39.65 +0.22 +0.24<br />
−0.27<br />
+0.06+0.29<br />
−0.30<br />
18........ CXOU J122519.7+181125 12 25 19.75 18 11 25.0 61.2 4.49±1.14 3.92 17.66 −0.07 +0.38<br />
−0.36<br />
−0.53+0.71<br />
−0.34<br />
19........ CXOU J122527.2+181215 12 25 27.29 18 12 15.4 67.8 7.24±1.56 4.65 28.48 −0.14 +0.32<br />
−0.30<br />
−0.31+0.40<br />
−0.31<br />
20........ CXOU J122521.7+181026 12 25 21.72 18 10 26.3 68.1 9.07±1.57 5.79 35.69 +0.09 +0.28<br />
−0.29<br />
+0.09+0.28<br />
−0.29<br />
21........ CXOU J122528.3+181205 12 25 28.35 18 12 05.7 73.2 6.11±1.40 4.35 24.04 +1.00 +0.00<br />
−0.29<br />
+1.00+0.00<br />
−0.26<br />
22........ CXOU J122521.6+181232 12 25 21.68 18 12 32.1 74.2 3.54±1.01 3.51 13.91 −0.33 +0.57<br />
−0.40<br />
+0.05+0.39<br />
−0.40<br />
Continued on Next Page. . .<br />
25
Table 2.2—Continued<br />
Source d Count Rate<br />
Number Name R.A. Decl. (arcsec) (10−4 s−1 ) S/N LX H21 H31 Notes<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11)<br />
23........ CXOU J122518.4+181137 12 25 18.42 18 11 37.0 80.9 14.54±1.98 7.36 57.22 −0.20 +0.22<br />
−0.20<br />
−0.11+0.21<br />
−0.20<br />
24........ CXOU J122519.8+181235 12 25 19.82 18 12 35.3 91.8 3.61±1.01 3.59 14.19 +0.54 +0.30<br />
−0.55<br />
−0.07+0.73<br />
−0.67<br />
25........ CXOU J122520.7+180955 12 25 20.72 18 09 55.7 101.8 4.65±1.14 4.09 18.29 −0.12 +0.39<br />
−0.36<br />
−0.35+0.53<br />
−0.37<br />
26........ CXOU J122520.3+181301 12 25 20.32 18 13 01.7 109.5 40.73±3.37 12.10 160.27 +0.21 +0.10<br />
−0.10<br />
−0.60+0.15<br />
−0.12<br />
27........ CXOU J122525.5+180936 12 25 25.51 18 09 36.8 111.1 3.82±1.02 3.73 15.02 +0.67 +0.30<br />
−1.09<br />
+0.82+0.16<br />
−0.89<br />
28........ CXOU J122531.6+181051 12 25 31.68 18 10 51.8 114.1 5.66±1.26 4.49 22.26 −0.33 +0.35<br />
−0.28<br />
−0.47+0.41<br />
−0.27<br />
29........ CXOU J122527.4+181314 12 25 27.48 18 13 14.1 118.8 3.33±0.98 3.38 13.09 −0.48 +0.58<br />
−0.34<br />
−0.48+0.63<br />
−0.35<br />
30........ CXOU J122521.6+180929 12 25 21.61 18 09 29.0 121.9 21.55±2.39 9.01 84.78 +0.10 +0.16<br />
−0.16<br />
+0.02+0.17<br />
−0.17<br />
31........ CXOU J122518.1+181255 12 25 18.19 18 12 55.7 122.5 2.68±0.87 3.06 10.55 −0.41 +0.88<br />
−0.47<br />
−0.04+0.57<br />
−0.54<br />
32........ CXOU J122516.8+181234 12 25 16.82 18 12 34.3 123.5 8.37±1.51 5.53 32.93 +0.22 +0.23<br />
−0.25<br />
−0.57+0.46<br />
−0.26<br />
33........ CXOU J122530.4+181311 12 25 30.41 18 13 11.8 139.5 12.51±1.88 6.65 49.24 +0.47 +0.18<br />
−0.23<br />
+0.20+0.27<br />
−0.30<br />
34........ CXOU J122522.2+181344 12 25 22.22 18 13 44.0 140.5 7.37±1.46 5.04 28.99 +0.55 +0.24<br />
−0.38<br />
+0.47+0.28<br />
−0.42<br />
35........ CXOU J122515.0+181018 12 25 15.01 18 10 18.8 145.1 4.20±1.11 3.77 16.52 +0.71 +0.25<br />
−0.79<br />
+0.41+0.49<br />
−0.95<br />
36........ CXOU J122513.8+181248 12 25 13.80 18 12 48.9 167.9 2.70±0.88 3.05 10.62 −0.77 +0.98<br />
−0.21<br />
−0.35+0.50<br />
−0.36<br />
37........ CXOU J122517.6+181350 12 25 17.64 18 13 50.2 170.7 22.95±2.61 8.79 90.29 −0.05 +0.16<br />
−0.16<br />
−0.10+0.17<br />
−0.17<br />
38........ CXOU J122517.1+181346 12 25 17.17 18 13 46.8 171.6 156.44±7.25 21.60 615.56 −0.19 +0.05<br />
−0.05<br />
−0.59+0.06<br />
−0.05 b,c<br />
39........ CXOU J122512.9+181016 12 25 12.98 18 10 16.2 172.3 16.00±2.06 7.76 62.94 +0.00 +0.20<br />
−0.20<br />
−0.05+0.20<br />
−0.20<br />
40........ CXOU J122528.0+181417 12 25 28.06 18 14 17.2 180.7 3.56±1.04 3.42 14.08 −0.15 +0.60<br />
−0.51<br />
−0.15+0.56<br />
−0.47<br />
41........ CXOU J122518.1+180841 12 25 18.12 18 08 41.5 184.8 8.19±2.66 3.09 32.24 −0.14 +0.60<br />
−0.51<br />
−0.14+0.60<br />
−0.51 d<br />
42........ CXOU J122536.5+181002 12 25 36.58 18 10 02.6 197.2 6.43±1.37 4.70 25.31 −0.23 +0.31<br />
−0.27<br />
−0.49+0.43<br />
−0.28<br />
43........ CXOU J122511.1+181006 12 25 11.18 18 10 06.1 199.9 2.70±0.89 3.05 10.64 +0.47 +0.35<br />
−0.59<br />
−0.45+1.23<br />
−0.51<br />
44........ CXOU J122528.6+180808 12 25 28.66 18 08 08.6 208.0 3.20±0.94 3.39 12.59 −0.36 +0.63<br />
−0.41<br />
−0.26+0.57<br />
−0.44<br />
Continued on Next Page. . .<br />
26
Table 2.2—Continued<br />
Source d Count Rate<br />
Number Name R.A. Decl. (arcsec) (10−4 s−1 ) S/N LX H21 H31 Notes<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11)<br />
45........ CXOU J122523.3+180758 12 25 23.33 18 07 58.1 208.0 22.72±4.02 5.66 89.40 +0.00 +0.24<br />
−0.24<br />
−0.50+0.36<br />
−0.24 d<br />
46........ CXOU J122538.8+181137 12 25 38.83 18 11 37.1 211.1 5.71±1.41 4.06 22.48 +1.00 +0.00<br />
−0.40<br />
+1.00+0.00<br />
−0.09<br />
47........ CXOU J122522.4+181457 12 25 22.48 18 14 57.1 212.3 15.34±2.27 6.75 60.36 −0.24 +0.22<br />
−0.20<br />
−0.43+0.30<br />
−0.23<br />
48........ CXOU J122538.7+181205 12 25 38.75 18 12 05.1 213.2 6.64±1.53 4.33 26.13 +0.66 +0.26<br />
−0.68<br />
+0.67+0.25<br />
−0.67 b<br />
49........ CXOU J122512.8+181409 12 25 12.80 18 14 09.3 228.8 20.54±2.72 7.55 80.83 +0.10 +0.17<br />
−0.18<br />
−0.35+0.25<br />
−0.21<br />
50........ CXOU J122508.0+181229 12 25 08.00 18 12 29.9 237.3 3.75±1.11 3.37 14.73 +0.30 +0.34<br />
−0.43<br />
−0.65+1.25<br />
−0.33<br />
51........ CXOU J122540.6+181224 12 25 40.60 18 12 24.6 243.2 10.99±1.94 5.67 43.24 +0.13 +0.24<br />
−0.25<br />
−0.08+0.33<br />
−0.32<br />
52........ CXOU J122509.2+181336 12 25 09.27 18 13 36.7 247.8 9.67±2.13 4.55 38.07 +0.36 +0.31<br />
−0.41<br />
+0.28+0.35<br />
−0.45 d<br />
53........ CXOU J122506.1+181045 12 25 06.15 18 10 45.8 258.0 12.67±1.95 6.49 49.83 +0.11 +0.22<br />
−0.23<br />
−0.19+0.30<br />
−0.27 b<br />
54........ CXOU J122505.9+181158 12 25 05.91 18 11 58.9 260.5 9.25±1.67 5.53 36.41 +0.12 +0.25<br />
−0.27<br />
−0.48+0.57<br />
−0.33 e<br />
55........ CXOU J122504.7+181133 12 25 04.74 18 11 33.5 275.1 13.21±1.98 6.66 51.98 +0.58 +0.20<br />
−0.30<br />
+0.59+0.19<br />
−0.29<br />
56........ CXOU J122543.4+181048 12 25 43.44 18 10 48.3 278.9 8.82±2.98 3.02 34.69 +0.45 +0.36<br />
−0.60<br />
−0.14+0.88<br />
−0.70 d<br />
57........ CXOU J122503.7+181124 12 25 03.70 18 11 24.1 289.9 14.61±2.52 5.82 57.48 −0.12 +0.23<br />
−0.22<br />
−0.49+0.31<br />
−0.22 b,d<br />
58........ CXOU J122546.0+181302 12 25 46.05 18 13 02.9 328.3 12.11±2.49 4.86 47.65 +0.24 +0.32<br />
−0.38<br />
−0.40+1.03<br />
−0.52<br />
NOTE.—Units <strong>of</strong> right ascension are hours, minutes, and seconds, and units <strong>of</strong> declination are degrees, arcminutes, and arcseconds. The units for<br />
LX are 1037 ergs s−1 in the 0.3–10 keV band.<br />
a Sources near the center may be confused with nearby sources, making their positions, fluxes, and extents uncertain.<br />
b Source is noticeably more extended than PSF.<br />
c Possible faint optical counterpart.<br />
d Globular cluster is possible optical counterpart.<br />
e Source may be variable.<br />
f Source is at the edge <strong>of</strong> the S3 detector, and flux is uncertain due to large exposure correction.<br />
27
2.4 Resolved Sources<br />
2.4.1 Detections<br />
The discrete X-ray source populations on the ACIS-S3 images <strong>of</strong> the two galaxies<br />
were determined using the wavelet detection algorithm (CIAO wavdetect program),<br />
and were confirmed with a local cell detection method and by visual inspection. The<br />
wavelet source detection threshold was set at 10 −6 , which implies that 1 false source<br />
(as a result <strong>of</strong> statistical fluctuation in the background) would be detected in the entire<br />
S3 image. We further restricted the sources by requiring sufficient source counts to<br />
determine the source flux at the ≥3 σ level. Over most <strong>of</strong> the image, the minimum<br />
detectable flux was about 2.7 × 10 −4 counts s −1 in the 0.3–10 keV band for both<br />
galaxies. The detection limit is slightly higher at large distances where the PSF is<br />
larger, and near the center <strong>of</strong> the galaxy where confusion with other discrete sources<br />
or diffuse gaseous emission may affect the sensitivity. For all source analyses, we used<br />
a local background with an area 3 times that <strong>of</strong> each source’s region from wavdetect.<br />
There were a few cases <strong>of</strong> nearby sources where the source regions or background<br />
regions were altered slightly to avoid overlaps, without affecting the net count rates.<br />
Tables 2.1 and 2.2 list the discrete sources detected by this technique in NGC 4365<br />
and NGC 4382, respectively. In each case, the sources are ordered with increasing<br />
projected distance d from the center <strong>of</strong> the galaxy. Columns (1)–(7) provide the<br />
source number, the IAU name, the source position (J2000.0), the projected distance<br />
d from the center <strong>of</strong> each galaxy, the count rate with its 1 σ error, and the S/N for<br />
the count rate. The fluxes were corrected for exposure and the instrument PSF. Since<br />
we did not detect a distinct source that was unambiguously associated with an AGN<br />
at the center <strong>of</strong> either NGC 4365 or NGC 4382 (see § 2.4.2), we adopted the central<br />
28
optical/IR positions <strong>of</strong> R.A. = 12 h 24 m 28. s 26 and decl. = +7 ◦ 19 ′ 3. ′′ 8 for NGC 4365 and<br />
R.A. = 12 h 25 m 24. s 04 and decl. = +18 ◦ 11 ′ 25. ′′ 9 for NGC 4382 from 2MASS (Cutri et al.<br />
2001). As noted in § 2.2, the overall absolute errors are probably 1 ′′ for NGC 4365<br />
and ∼0. ′′ 5 for NGC 4382 near the centers <strong>of</strong> the fields, with larger errors farther out<br />
for both observations.<br />
Our detection limit for sources should result in 1 false source (as a result <strong>of</strong> a<br />
statistical fluctuation) in the entire S3 field <strong>of</strong> view for each galaxy. However, some <strong>of</strong><br />
the detected sources may be unrelated foreground or (more likely) background objects.<br />
Based on the source counts in Brandt et al. (2000) and Mushotzky et al. (2000), we<br />
would expect ≈12 such unrelated sources in each observation. These should be spread<br />
out fairly uniformly over each S3 image (Figure 2.1), except for the reduced sensitivity<br />
at the outer edges <strong>of</strong> the field due to reduced exposure and increased PSF. Thus, the<br />
unrelated sources should mainly be found at larger distances from the optical centers<br />
<strong>of</strong> the galaxies (the latter entries <strong>of</strong> Tables 2.1 and 2.2), while the sources associated<br />
with the galaxies should be concentrated to their centers.<br />
2.4.2 Identifications<br />
In addition to the identifications mentioned in § 2.2, we visually examined the first<br />
and second generation DSS images for position matches. Both source 98 (USNO-A2.0<br />
0900−07143676) <strong>of</strong> NGC 4365, and source 38 (J1225+182) <strong>of</strong> NGC 4382 were visible.<br />
In addition, sources 88 and 97 <strong>of</strong> NGC 4365 and sources 48, 53, and 57 <strong>of</strong> NGC 4382<br />
had possible optical counterparts. None <strong>of</strong> these five sources corresponded to objects<br />
listed in NED or SIMBAD.<br />
In both galaxies, the area enclosed by source 1 is coincident with our adopted<br />
optical/IR positions <strong>of</strong> the galaxy center. In NGC 4365, the centroid <strong>of</strong> source 1 is <strong>of</strong>f<br />
29
y an amount that is consistent with our positional uncertainty, while in NGC 4382,<br />
the centroid is <strong>of</strong>f by 3 times our positional uncertainty. It is unclear whether<br />
either <strong>of</strong> these sources is an AGN in the galaxy center or an LMXB projected near<br />
the center. We also examined hard-band (2–10 keV) images <strong>of</strong> both galaxies in which<br />
AGNs might be more obvious, particularly as the diffuse emission from the galaxies is<br />
s<strong>of</strong>t. We did not see any new sources near the center, nor were either <strong>of</strong> the centermost<br />
sources particularly hard. Thus, we have no unambiguous evidence for AGNs in these<br />
galaxies. Conservatively, we adopt the luminosity <strong>of</strong> the centermost source in each<br />
galaxy (1.5 × 10 38 ergs s −1 in NGC 4365 and 9.0 × 10 37 ergs s −1 in NGC 4382) as the<br />
upper limit to the central AGN luminosity.<br />
We examined NGC 4382 for a source associated with SN 1960r. Source 27 is<br />
the closest detected source; however, it is ∼20 ′′ from the Porter (1993) position. We<br />
placed a 2. ′′ 0 radius circular aperture, similar to that <strong>of</strong> source 27 plus 0. ′′ 5 to account<br />
for our positional uncertainty, and a 4. ′′ 0 radius circular aperture to determine the<br />
local background. No net counts were detected, and we can place a 3 σ upper limit<br />
<strong>of</strong> 6.3 × 10 37 ergs s −1 .<br />
For NGC 4365, A. Kundu kindly provided a list <strong>of</strong> 325 globular cluster positions<br />
from data presented in Kundu & Whitmore (2001). The WFPC2 field <strong>of</strong> view overlaps<br />
37 X-ray point sources from Table 2.1. After solving for a small <strong>of</strong>fset, 18 <strong>of</strong> the 37<br />
sources have a globular cluster within 1. ′′ 02. The expected number <strong>of</strong> associations<br />
from random positions is ∼0.6 based on the density <strong>of</strong> the globular clusters. This<br />
number is consistent with Kundu et al. (2003), who adopted less strict source detection<br />
criteria. Recently Larsen et al. (2003) published a short list <strong>of</strong> globular clusters with<br />
spectroscopy. In addition to globular clusters identifications from Kundu & Whitmore<br />
(2001), globular cluster 1 from Larsen et al. (2003) agrees with the position <strong>of</strong> our<br />
30
log N(>L)<br />
2.0<br />
1.5<br />
1.0<br />
0.5<br />
0.0<br />
NGC 4365<br />
38.2 38.4 38.6 38.8 39.0 39.2 39.4<br />
log L X [0.3-10 keV] (ergs/s)<br />
log N(>L)<br />
2.0<br />
1.5<br />
1.0<br />
0.5<br />
0.0<br />
NGC 4382<br />
38.2 38.4 38.6 38.8 39.0 39.2 39.4 39.6 39.8<br />
log L X [0.3-10 keV] (ergs/s)<br />
Fig. 2.3.— Histogram <strong>of</strong> the observed cumulative luminosity function <strong>of</strong> all resolved<br />
sources within the Chandra S3 fields <strong>of</strong> NGC 4365 (left) and NGC 4382 (right). The<br />
continuous curves are the sums <strong>of</strong> the respective best-fit LMXB luminosity functions<br />
(eq. 2.1) and the expected background source counts. Poisson error bars are displayed<br />
for every fifth interval. As this is a cumulative distribution, the errors are correlated.<br />
source 59. Sources with candidate globular clusters are noted in Table 2.1. There<br />
were no available lists <strong>of</strong> globular clusters for NGC 4382.<br />
2.4.3 X-ray Luminosities and Luminosity Functions<br />
When converting the source count rates into unabsorbed X-ray (0.3–10 keV) lu-<br />
minosities, we assumed that each source was at the distance <strong>of</strong> the target galaxy.<br />
We then used the best-fit Chandra X-ray spectrum <strong>of</strong> the inner (one effective radius<br />
for NGC 4365, two effective radii for NGC 4382) resolved sources (Tables 2.3 and<br />
2.4, row 3). The conversion factors were 4.08 × 10 41 ergs count −1 for NGC 4365 and<br />
3.93 × 10 41 ergs count −1 for NGC 4382. Column 8 <strong>of</strong> Tables 2.1 and 2.2 list the X-ray<br />
luminosities in units <strong>of</strong> 10 37 ergs s −1 , which range roughly from 1.1×10 38 to 2.3×10 39<br />
ergs s −1 for NGC 4365 and 1.1 × 10 38 to 6.2 × 10 39 ergs s −1 for NGC 4382.<br />
In Figure 2.3, we display the cumulative luminosity functions <strong>of</strong> all resolved sources<br />
in the S3 field. Each cumulative luminosity function should be the sum <strong>of</strong> the point-<br />
source (LMXB) population <strong>of</strong> the target galaxy and the foreground/background pop-<br />
31
ulation. We fit the luminosity function using the same techniques as we have used<br />
previously (Sarazin et al. 2000, 2001; Blanton, Sarazin, & Irwin 2001; Irwin, Sarazin,<br />
& Bregman 2002); a single power-law, a broken power-law, and a cut<strong>of</strong>f power-law<br />
were all used to model the LMXB population. The background source population was<br />
modeled as discussed in the previous references. For NGC 4365, a single power-law<br />
fit was acceptable (at ∼54% confidence level). However, the single power-law fit for<br />
NGC 4382 was rejected at the greater than 94% confidence level. Attempts at broken<br />
power-law fits were more successful (∆χ 2 = −6.2 and −19.0, with 2 less degrees <strong>of</strong><br />
freedom [d<strong>of</strong>] compared to the single power-law); however, the power-law exponents<br />
at high luminosities were steep (∼9), so that these models effectively had a cut<strong>of</strong>f<br />
above the break luminosity. As a result, we fit the luminosity functions with a cut<strong>of</strong>f<br />
power-law model (∆χ 2 = −7.3 and −19.3, with 1 less d<strong>of</strong> compared to the single<br />
power-law):<br />
dN<br />
dL37<br />
⎧<br />
⎪⎨<br />
=<br />
⎪⎩<br />
N0( LX<br />
Lc )−α LX ≤ Lc<br />
0 LX > Lc<br />
32<br />
, (2.1)<br />
where LX is the X-ray luminosity, L37 ≡ LX/(10 37 ergs s −1 ), and Lc is the cut<strong>of</strong>f<br />
luminosity. The best fits were determined by the maximum likelihood method, and<br />
the errors (90% confidence interval) were determined by Monte Carlo techniques. For<br />
NGC 4365, N0 = 2.28 +4.31<br />
−0.59 × 10 −2 , α = 1.91 +0.23<br />
−0.30, and Lc = 226 +57<br />
−90 × 10 37 ergs s −1 ;<br />
while for NGC 4382, N0 = 0.19 +0.14<br />
−0.06, α = 0.93 +0.38<br />
−0.51, and Lc = 110 +21<br />
−23 × 10 37 ergs s −1 .<br />
At the faint end <strong>of</strong> the luminosity function, incompleteness may play a role. Since<br />
the incompleteness is a complicated function <strong>of</strong> source counts, spectra, background,<br />
the PSF, and the detection band, we used simulations to understand the incomplete-<br />
ness. With MARX 6 simulations, we found that incompleteness can lead to a depressed<br />
6 See http://space.mit.edu/CXC/MARX/.
luminosity function for luminosities ∼30% higher than the minimum detectable lu-<br />
minosity in these galaxies. In our cases, that corresponds to ∼1.4 × 10 38 ergs s −1 (14<br />
counts) for both galaxies. This is in rough agreement with other reported simulations<br />
(Kim & Fabbiano 2003). The largest effect <strong>of</strong> incompleteness for our fits would be in<br />
their power-law slopes. When we fit the luminosity function at a minimum <strong>of</strong> 2×10 38<br />
ergs s −1 , we find agreement within the errors reported above.<br />
The X-ray luminosity functions <strong>of</strong> LMXBs have been determined with Chandra<br />
in a number <strong>of</strong> other early-type galaxies. In most cases, the observations are lim-<br />
ited to LX 10 38 ergs s −1 . The best-fit slope α <strong>of</strong> NGC 4365 is steeper than the<br />
low-luminosity slope αl in NGC 1553 (Blanton et al. 2001), NGC 4649 (Randall<br />
et al. 2004), and NGC 4697 (Sarazin et al. 2001), although the values for NGC 4365,<br />
NGC 4649, and NGC 4697 agree within the 90% confidence intervals. The slope in<br />
NGC 4365 is also flatter than the high luminosity slope αh in these three galaxies, and<br />
the single power-law slope in NGC 1316 (Kim & Fabbiano 2003). The 90% confidence<br />
intervals <strong>of</strong> NGC 4382 α overlap with αl in NGC 1553, NGC 4649, and NGC 4697.<br />
The cut<strong>of</strong>f luminosities <strong>of</strong> NGC 4365 and NGC 4382 [≈(0.9–3.2) ×10 39 ergs s −1 ]<br />
are much higher than the break or cut<strong>of</strong>f luminosities <strong>of</strong> NGC 1291, NGC 1553,<br />
NGC 4649, and NGC 4697 (≈(2–6) ×10 38 ergs s −1 ; Sarazin et al. 2001; Blanton et al.<br />
2001; Irwin et al. 2002; Randall et al. 2004). The differences probably are too large to<br />
be explained by distance errors. When we fitted the luminosity functions in NGC 4365<br />
and NGC 4382 with broken power-laws, the break values were somewhat lower than<br />
the cut<strong>of</strong>f luminosities but consistent within the errors. Moreover, the break lumi-<br />
nosities were significantly larger than the values found in NGC 1291, NGC 1553, and<br />
NGC 4697. A very high break luminosity or single power-law fit was found previously<br />
for NGC 1316 (Kim & Fabbiano 2003); this galaxy had a single power-law fit, but a<br />
33
eak at greater than 5 × 10 38 ergs s −1 could not be excluded.<br />
In Sarazin et al. (2000), we argued that a break luminosity similar to the Ed-<br />
dington luminosity <strong>of</strong> a 1.4M⊙ spherically accreting neutron star indicated that the<br />
LMXBs above the break contain accreting black holes. The large luminosities <strong>of</strong> the<br />
cut<strong>of</strong>f or broken power-laws for NGC 1316, NGC 4365, and NGC 4382 seem less<br />
consistent with this interpretation, barring a large error in the distance.<br />
In the luminosity function <strong>of</strong> NGC 4382, the best-fit clearly misses the brightest<br />
source, source 38. Since source 38 is a bright background AGN, this is not indicative<br />
<strong>of</strong> a poor fit.<br />
2.4.4 Hardness Ratios<br />
We determined X-ray hardness ratios for the sources, using the same techniques<br />
and definitions we used previously (Sarazin et al. 2000, 2001; Blanton et al. 2001; Irwin<br />
et al. 2002). Hardness ratios or X-ray colors are useful for crudely characterizing the<br />
spectral properties <strong>of</strong> sources, and can be applied to sources that are too faint for<br />
detailed spectral analysis. We define two hardness ratios as H21 ≡ (M − S)/(M + S)<br />
and H31 ≡ (H −S)/(H +S), where S, M, and H are the total counts in the s<strong>of</strong>t (0.3–1<br />
keV), medium (1–2 keV), and hard (2–10 keV) bands, respectively. Since the hardness<br />
ratios measure observed counts, Galactic absorption, as well as QE degradation, must<br />
be taken into account when interpreting the ratios. The hardness ratios and their 1 σ<br />
errors are listed in columns (9) and (10) <strong>of</strong> Tables 2.1 and 2.2. Figure 2.4 plots H31<br />
versus H21 for the 48 and 39 sources <strong>of</strong> NGC 4365 and NGC 4382, respectively, with<br />
at least 20 net counts. The hardness ratios for the sum <strong>of</strong> those sources are (H21,<br />
H31) = (0.04, −0.25) for NGC 4365 and (0.02, −0.25) for NGC 4382. Sources with<br />
∼40 net counts had errors similar to the median <strong>of</strong> the uncertainties, ∼0.26. The<br />
34
H31<br />
1.0<br />
0.5<br />
0.0<br />
-0.5<br />
-1.0<br />
NGC 4365<br />
-1.0 -0.5 0.0 0.5 1.0<br />
H21<br />
H31<br />
1.0<br />
0.5<br />
0.0<br />
-0.5<br />
-1.0<br />
NGC 4382<br />
-1.0 -0.5 0.0 0.5 1.0<br />
H21<br />
Fig. 2.4.— Hardness ratios for the sources <strong>of</strong> NGC 4365 (left) and NGC 4382 (right)<br />
with at least 20 net counts. Here, H21 ≡ (M −S)/(M +S) and H31 ≡ (H −S)/(H +<br />
S), where S, M, and H are the counts in the s<strong>of</strong>t (0.3–1 keV), medium (1–2 keV),<br />
and hard (2–10 keV) bands, respectively. The area <strong>of</strong> each circle is proportional to<br />
the observed number <strong>of</strong> net counts. The solid curve and large diamonds show the<br />
hardness ratios for power-law spectral models with Galactic absorption; the small<br />
diamonds show the ratios for NH = 5 × 10 21 cm −2 ; the diamonds indicate values <strong>of</strong><br />
the power-law photon number index from Γ = 0 (upper right) to 3.2 (lower left) in<br />
increments <strong>of</strong> 0.4. The dashed curve encloses the area with power-law photon indices<br />
between 0 and 3.2 and absorption columns between Galactic and 5 × 10 21 cm −2 . The<br />
1 σ error bars at the upper left illustrate the median <strong>of</strong> the uncertainties. As a result<br />
<strong>of</strong> the QE degradation, an effective absorption <strong>of</strong> ∼6 × 10 20 cm −2 was added to these<br />
spectral models.<br />
errors scale roughly with the inverse square root <strong>of</strong> the net counts.<br />
As was also seen in the bulge <strong>of</strong> NGC 1291, NGC 1553, and NGC 4697 (Sarazin<br />
et al. 2000, 2001; Blanton et al. 2001; Irwin et al. 2002), most <strong>of</strong> the sources lie along<br />
a broad diagonal swath extending roughly from (H21, H31) ≈ (−0.3, −0.7) to (0.4,<br />
0.5). In Figure 2.4, the solid line corresponds to Galactic absorption, QE degradation,<br />
and power-law spectra with photon indices <strong>of</strong> Γ = 0–3.2. Most <strong>of</strong> the sources (37/48<br />
and 26/39) are displaced to the right <strong>of</strong> the solid curve. Were the solid curve a good<br />
fit to the data, one would expect to find roughly equal numbers <strong>of</strong> sources on each<br />
35
side <strong>of</strong> the curve. Assuming that this is the case, the probability <strong>of</strong> seeing ≤ 9/48 and<br />
13/39 sources to the left <strong>of</strong> the line is 0.01% and 2.66% for NGC 4365 and NGC 4382,<br />
respectively. The spectra seem to be more complex than a single power-law with<br />
varying indices.<br />
Between NGC 4697 and the bulge <strong>of</strong> NGC 1291, there were four sources with<br />
(H21, H31) ≈ (−1, −1). These supers<strong>of</strong>t sources have, essentially, no emission above<br />
1 keV. Based on scaling to the three sources in NGC 4697, one might have expected<br />
approximately five to six supers<strong>of</strong>t sources in NGC 4365 and ∼3 supers<strong>of</strong>t sources in<br />
NGC 4382. However, no supers<strong>of</strong>t sources are observed in either galaxy.<br />
In Figure 2.4, there are three NGC 4365 sources (sources 36, 69, and 92) and<br />
four NGC 4365 sources with very hard spectra [hardness ratios (H21, H31) > (0.5,<br />
0.5)]. These may be unrelated, strongly absorbed AGNs, similar to the sources that<br />
produce the hard component <strong>of</strong> the X-ray background and that appear strongly at<br />
the faint fluxes in the deep Chandra observations <strong>of</strong> blank fields (Brandt et al. 2000;<br />
Mushotzky et al. 2000; Giacconi et al. 2001). There also are two sources with hardness<br />
ratios <strong>of</strong> around (−0.4, −1): these are source 38 <strong>of</strong> NGC 4365 and source 10 <strong>of</strong><br />
NGC 4382, although the hardness ratio <strong>of</strong> the latter is highly uncertain. Studies<br />
<strong>of</strong> other galaxies (Sarazin et al. 2001) and deep blank-sky images (e.g., Giacconi<br />
et al. 2001) suggest that many <strong>of</strong> the sources, similarly lacking hard emission, may<br />
be unrelated background sources. However, such sources, especially when at smaller<br />
radii, may be part <strong>of</strong> the host galaxy. Although the identification <strong>of</strong> source 38 <strong>of</strong><br />
NGC 4382 with a z = 1.19 quasar marks it as a background object, it occupies a<br />
typical part <strong>of</strong> the figure [(H21, H31) ≈ [−0.2, −0.6)].<br />
36
2.4.5 Variability<br />
We searched for variability in the X-ray emission <strong>of</strong> the resolved sources over the<br />
duration <strong>of</strong> the Chandra observation using the Kolmogorov-Smirnov (K-S) test (see<br />
Sarazin et al. 2001). In most cases, the tests were inconclusive. For NGC 4365, six<br />
sources (sources 16, 21, 29, 31, 48, and 86) had a greater than 95% probability that<br />
they were variable. For NGC 4382, only source 54 had a greater than 95% probability<br />
that it was variable. Figure 2.5 displays the total count histograms <strong>of</strong> the three sources<br />
in NGC 4365 (sources 16, 29, and 86) that had a greater than 99% probability that<br />
they were variable and NGC 4382 source 54 which had a 97% probability that it was<br />
variable. NGC 4365 source 16 seems to be gradually fading. Similarly, NGC 4365<br />
source 29 also seems to fade gradually but has only 15 net counts. The X-ray light<br />
curve for NGC 4365 source 86 is shown in Figure 2.6. This source appears to have<br />
turned on after the start <strong>of</strong> the observation, and undergone a large outburst after<br />
about 1<br />
3<br />
<strong>of</strong> NGC 4365’s exposure. It then decreased and probably underwent at least<br />
one more outburst before gradually fading as the observation was ending. The light<br />
curve <strong>of</strong> NGC 4382 source 54 suggests that it underwent an outburst after about 3<br />
8<br />
<strong>of</strong> NGC 4382’s exposure, and that the outburst gradually faded. Variable sources are<br />
noted in Tables 2.1 and 2.2.<br />
2.4.6 Spatial Distribution<br />
As in Sarazin et al. (2001), we have performed two comparisons <strong>of</strong> the spatial<br />
distribution <strong>of</strong> the X-ray sources with that <strong>of</strong> the optical light; we have fitted the<br />
position angle (P.A.) distribution and the radial distribution. For both galaxies,<br />
we limited the analysis to all sources within 3 ′ <strong>of</strong> the galaxy center to ensure that<br />
the circular area lies completely on the chip. In this area, we expect approximately<br />
37
Fraction <strong>of</strong> Counts<br />
1<br />
1<br />
NGC 4365 Src. 16<br />
NGC 4365 Src. 29<br />
1 NGC 4365 Src. 86<br />
1 NGC 4382 Src. 54<br />
0<br />
0 10000 20000<br />
Exposure Time (s)<br />
30000 40000<br />
Fig. 2.5.— Solid histogram: Accumulated fraction <strong>of</strong> events for sources as a function<br />
<strong>of</strong> exposure time. Dashed line: Predicted distribution under the hypothesis that the<br />
source plus background rate is constant. The three NGC 4365 sources shown are<br />
those with variability detected at the greater than 99% confidence level. NGC 4382<br />
Source 54 had variability detected at the greater than 96.8% confidence level.<br />
Fig. 2.6.— X-ray light curve <strong>of</strong> source 86 in NGC 4365. The points with 1 σ error<br />
bars are the source count rate, uncorrected for background, accumulated in 2021 s<br />
time bins. The horizontal dashed line is the background count rate scaled to the<br />
source region size.<br />
38
Number<br />
10<br />
8<br />
6<br />
4<br />
2<br />
NGC 4365<br />
Optical<br />
Maximum Likelihood<br />
0<br />
0 20 40 60 80 100 120 140 160 180<br />
PA mod 180 (degrees)<br />
Number<br />
6<br />
4<br />
2<br />
NGC 4382<br />
Optical<br />
Maximum Likelihood<br />
0<br />
0 20 40 60 80 100 120 140 160 180<br />
PA mod 180 (degrees)<br />
Fig. 2.7.— Solid histogram: Distribution <strong>of</strong> the position angles <strong>of</strong> the X-ray sources<br />
within 3 ′ <strong>of</strong> the center <strong>of</strong> NGC 4365 (left) NGC 4382 and (right) in 10 ◦ bins, as<br />
a function <strong>of</strong> the P.A. (modulo 180 ◦ ). P.A. is measured from north to east. The<br />
curves are the expected number <strong>of</strong> background sources plus the predicted distribution<br />
based on optical photometry and the best-fit elliptical distribution determined by a<br />
maximum likelihood fit to the observed values.<br />
five background sources in each exposure. We have adopted the Third Reference<br />
Catalogue <strong>of</strong> Bright Galaxies (RC3) values for the optical photometry’s effective radii,<br />
P.A., and ellipticity (de Vaucouleurs et al. 1992). At an effective radius <strong>of</strong> 49. ′′ 8,<br />
NGC 4365 has P.A. = 40 ◦ and e = 0.28; while at an effective radius <strong>of</strong> 54. ′′ 6, NGC 4382<br />
has e = 0.22. There is no P.A. listed for NGC 4382 in RC3. Fisher (1997) found that<br />
NGC 4382 has an isophotal twist, with its P.A. ranging from 60 ◦ at its center to 0 ◦<br />
at large radii. We adopted the latter P.A. for NGC 4382. These elliptical isophotes<br />
contain one-half <strong>of</strong> the optical light.<br />
In Figure 2.7 we show the observed distributions <strong>of</strong> position angles (modulo 180 ◦ ,<br />
measuring P.A. from north to east). In addition to the observed distribution and the<br />
expected optical distribution, we have fitted a distribution representing the number<br />
<strong>of</strong> expected background sources plus the number <strong>of</strong> sources expected from a set <strong>of</strong><br />
sources with constant projected density on elliptical isophotes. For NGC 4365 and<br />
NGC 4382, ∆χ 2 between the optical fits and the maximum likelihood fits indicates<br />
that the optical fits are acceptable at the 83% and 54% confidence level. The best-fit<br />
39
log N(
LMXBs has an effective radius <strong>of</strong> 129 ′′ . Both fits indicate that there are more X-ray<br />
sources at larger radii than expected from the optical light distribution. Radial fits<br />
from circular isophotes yield similar results. Since NGC 4382 is an S0 galaxy, this<br />
disagreement may reflect the contribution <strong>of</strong> X-ray sources associated with the disk<br />
<strong>of</strong> the galaxy. However, this would not explain the difference between the LMXB<br />
distribution and the optical light distribution in NGC 4365.<br />
We note that a significant fraction <strong>of</strong> the LMXBs in NGC 4365 are associated<br />
with globular clusters (§ 2.4.2), as is generally true <strong>of</strong> elliptical galaxies (Angelini,<br />
Loewenstein, & Mushotzky 2001; Sarazin et al. 2000). In elliptical galaxies (including<br />
NGC 4365), the globular cluster population is more broadly distributed than that<br />
<strong>of</strong> the optical light and field stars (e.g., Harris 1991). This might help to explain<br />
the broader distribution <strong>of</strong> the LMXBs. Figure 2.8 suggests that there may be two<br />
populations <strong>of</strong> LMXBs, one with a small effective radius perhaps consistent with the<br />
optical distribution, and one with a larger effective radius. It is possible that these<br />
two distributions represent the LMXBs formed in globular clusters and those formed<br />
from field binary star systems. However, we note that in NGC 4697, the LMXBs<br />
followed the optical light distribution (Sarazin et al. 2001). More elliptical galaxies<br />
need to be observed to resolve this question.<br />
To test whether the LMXBs in these galaxies could discriminate between such<br />
models, we added either a second de Vaucouleurs model or an exponential model to the<br />
optical light distribution. For either additional component, there were only minimal<br />
improvements to the fits (∆χ 2 −0.6 for NGC 4365 and −0.8 for NGC 4382,<br />
with one less d<strong>of</strong> compared to the single pr<strong>of</strong>ile), indicating that the current data<br />
cannot statistically discriminate between single de Vaucouleurs distributions with<br />
large effective radii or multiple component distributions.<br />
41
2.5 Spectral Analysis<br />
We extracted spectra <strong>of</strong> the sources and diffuse emission in both galaxies. We<br />
restricted the spectral analysis to the 0.7 – 9 keV range. The lower limit was taken<br />
to avoid calibration uncertainties, while there are few non-background counts beyond<br />
9 keV. We also found a possible spectral artifact around 1.6–1.9 keV, which has been<br />
noticed by others. 7 We believe that this artifact is minor enough that it should not<br />
effect continuum models (bremsstrahlung or power-law); however, we chose to excise<br />
the 1.6–1.9 keV band when we fitted line models (MEKAL). All <strong>of</strong> the spectra were<br />
grouped to have at least 25 counts per spectral bin prior to background correction<br />
to enable our use <strong>of</strong> χ 2 statistics. The use <strong>of</strong> minimum counts per spectral bin and<br />
restricted energy ranges can result in bins being excluded in the allowed energy range.<br />
The results <strong>of</strong> the spectral fits are summarized in Tables 2.3 and 2.4. Spec-<br />
tra were extracted for the resolved point sources (“Sources”), the unresolved diffuse<br />
emission excluding the point sources (“Unresolved”), and the total emission (sources<br />
and unresolved emission). The total emission spectra were studied for comparison<br />
to instruments with poorer spatial resolution that cannot resolve the point sources.<br />
The third column gives the geometric region for the spectrum; “Field” implies the<br />
entire S3 chip. The value <strong>of</strong> the absorbing column density (NH) applied to all com-<br />
ponents <strong>of</strong> the model emission spectrum is given in the fourth column. In this and<br />
other columns, values in parentheses are fixed (not allowed to vary). The fixed value<br />
<strong>of</strong> NH is the Galactic value from Dickey & Lockman (1990). As in Sarazin et al.<br />
(2001), a two component model was necessary to fit the total spectrum data. A hard<br />
component, modeled by thermal bremsstrahlung or by a power-law spectrum, was<br />
used to model the resolved and unresolved LMXBs. An additional s<strong>of</strong>t line emitting<br />
7 See http://asc.harvard.edu/cal/Links/Acis/acis/Cal projects/index.html.<br />
42
component (“MEKAL”) was used for gaseous diffuse emission. We used the XSPEC<br />
ACISABS model to correct for the QE degradation. For the hard component, the<br />
fifth, sixth, and seventh columns give the spectral model, the temperature Th (for<br />
bremsstrahlung) or photon number spectral index Γ, and the unabsorbed flux <strong>of</strong> the<br />
hard component, F h X<br />
(0.3–10 keV). Similarly, the eighth, ninth, and tenth columns<br />
give the temperature Ts, overall heavy-element abundance relative to solar, and flux<br />
for the s<strong>of</strong>t MEKAL component. For the unresolved emission, the spectra exclude<br />
regions around each <strong>of</strong> the resolved sources. The last two columns give the number<br />
<strong>of</strong> net counts in each spectrum and χ 2 per d<strong>of</strong> for the best-fit model. All errors<br />
reported in the spectral analysis are 90% confidence level errors. Parentheses are<br />
used to indicate a frozen parameter, and square brackets are used when an error is<br />
unconstrained.<br />
The background spectra for the resolved sources were determined locally, using<br />
the same nearby regions as discussed in § 2.4. For the spectra <strong>of</strong> the resolved diffuse<br />
emission and the total spectrum (sources and unresolved emission), the background<br />
was taken from the deep blank-sky backgrounds compiled by Maxim Markevitch 3 .<br />
The spectra <strong>of</strong> several spatial regions were analyzed. In NGC 4365, the spectra <strong>of</strong><br />
sources, unresolved emission, and total emission were derived from an inner region,<br />
which was determined by the elliptical optical isophote containing one-half <strong>of</strong> the<br />
optical light. We refer to this region as within “one effective radius.” The semimajor<br />
axis <strong>of</strong> this isophote is defined as aeff. In NGC 4365, this isophote has aeff = 58. ′′ 5, a<br />
semi-minor axis <strong>of</strong> 42. ′′ 5, and a P.A. <strong>of</strong> 40 ◦ (de Vaucouleurs et al. 1992). In NGC 4382,<br />
43
Table 2.3. X-ray Spectral Fits <strong>of</strong> NGC 4365<br />
Hard Component S<strong>of</strong>t Component (MEKAL)<br />
NH Model kTh or Γ F h X kTs Abund. F s X<br />
Row Origin Region (10 20 cm −2 ) (keV) ( a ) (keV) (solar) ( a ) Counts χ 2 /d<strong>of</strong><br />
1.......... Sources
Table 2.4. X-ray Spectral Fits <strong>of</strong> NGC 4382<br />
Hard Component S<strong>of</strong>t Component (MEKAL)<br />
NH Model kTh or Γ F h X kTs Abund. F s X<br />
Row Origin Region (10 20 cm −2 ) (keV) ( a ) (keV) (solar) ( a ) Counts χ 2 /d<strong>of</strong><br />
+ 7.54<br />
1.......... Sources
the corresponding isophote did not have sufficient counts from resolved sources for<br />
spectral analysis. Therefore, we chose the innermost region <strong>of</strong> NGC 4382 to be twice<br />
as large (2 aeff), which gave an elliptical region with a semi-major axis <strong>of</strong> 123 ′′ , a<br />
semi-minor axis <strong>of</strong> 95. ′′ 5, and a P.A. <strong>of</strong> 0 ◦ (de Vaucouleurs et al. 1992; Fisher 1997).<br />
This isophote contains 69% <strong>of</strong> the optical light. We fitted the sources (resolved<br />
emission), unresolved emission, and total emission in these innermost regions. We<br />
also examined the spectra <strong>of</strong> the sources for the entire field. In order to search for<br />
changing unresolved emission with radius, we chose to analyze the elliptical annulus<br />
between one and three effective radii for both galaxies, corresponding to ∼28.8%<br />
<strong>of</strong> the optical light. For both galaxies, we used the same P.A. as the innermost<br />
region. In NGC 4365, there were enough counts from resolved sources between one<br />
and three effective radii to also analyze that spectrum. Finally, we analyzed the<br />
total emission spectra in the three effective radii region. The counts <strong>of</strong> the source<br />
spectrum plus the unresolved spectrum in a region will not exactly equal the counts <strong>of</strong><br />
the total spectrum for a variety <strong>of</strong> reasons: the different spectra (source, unresolved,<br />
and total) were binned separately, all <strong>of</strong> the counts for a point source were assigned<br />
to a region if the source’s center was inside the region, and the source spectra used a<br />
local background compared to the blank-sky background used by the unresolved and<br />
total spectra.<br />
2.5.1 X-ray Spectra <strong>of</strong> Resolved Sources<br />
NGC 4365<br />
For NGC 4365, we extracted the spectrum <strong>of</strong> all resolved sources within one<br />
effective radius. The observed spectrum is shown in the left-hand panels <strong>of</strong> Figure 2.9.<br />
As has been found in other early-type galaxies (Sarazin et al. 2001), the combined<br />
46
Fig. 2.9.— Top panels: Cumulative X-ray spectra <strong>of</strong> all <strong>of</strong> the resolved sources in the<br />
inner effective radius <strong>of</strong> NGC 4365 (left) and inner two effective radii <strong>of</strong> NGC 4382<br />
(right) with 1 σ error bars overlayed by the solid histograms <strong>of</strong> the best-fit model<br />
spectra (Table 2.3 and 2.4 row 3). Bottom panels: Contribution to χ 2 with the sign<br />
indicating the sign <strong>of</strong> the residual.<br />
spectra <strong>of</strong> the sources were reasonably well-fitted by either a thermal bremsstrahlung<br />
model with kTh = 6.08 keV (Table 2.3, row 1) or a power-law model with a photon<br />
number spectral index <strong>of</strong> Γ = 1.67 (row 3). The power-law model gave a slightly<br />
better fit, so we adopted this model as our best-fit. The fits were not improved<br />
significantly when the absorbing column was allowed to vary (rows 2 and 4), so we<br />
fixed the hydrogen column at the Galactic value, NH = 1.63 × 10 20 cm −2 (Dickey<br />
& Lockman 1990). The adopted best-fit power-law model with Galactic absorption<br />
and residuals to the fit are shown in the left-hand panels <strong>of</strong> Figure 2.9. Although the<br />
hardness ratios indicate that each source is probably fitted by a more complex model<br />
than a power-law and Galactic absorption, the summation <strong>of</strong> counts from objects with<br />
different emission properties can be well fitted with a single power-law and Galactic<br />
absorption. Extending the spectrum down to 0.3 keV to see how the restricted energy<br />
range used in fitting affects the absorbing column does result in a somewhat higher<br />
absorption value; however, we believe that the calibration at low energies is still too<br />
unreliable to confidently claim an excess absorption.<br />
We also searched for any radial variation in the spectra <strong>of</strong> the sources. We ex-<br />
47
tracted the spectrum from an elliptical annulus between one and three effective radii.<br />
We first fitted this region using the source best-fit model from the inner one effec-<br />
tive radius region, which provided an acceptable fit (row 5). When we allowed the<br />
power-law index to vary (row 6), we found a better fit (∆χ 2 = −2.9 with 1 less d<strong>of</strong>);<br />
however, the two values <strong>of</strong> Γ agree their 90% confidence limits. Freeing the absorp-<br />
tion also yielded a better fit, (∆χ 2 = −1.9 with one fewer d<strong>of</strong>); however, Galactic<br />
absorption was allowed at the 90% confidence limit.<br />
We also attempted to fit the collective spectrum <strong>of</strong> all <strong>of</strong> the resolved sources on<br />
the S3 chip, which had 2660 net counts. Again, freeing the power-law index from the<br />
best-fit value for the inner effective radii produced a better fit; however, the power-law<br />
index is still consistent with the best-fit 90% confidence limit (rows 8 and 9). Freeing<br />
the absorbing column did not produce a better fit (rows 9 and 10). We find no clear<br />
trend between radius and spectral fit. This is consistent with results from a study <strong>of</strong><br />
the sources in 15 galaxies by Irwin et al. (2003).<br />
NGC 4382<br />
For NGC 4382, the lower number <strong>of</strong> sources and counts required using the inner<br />
two effective radii to attain 921 net counts in the spectrum. For this region, the<br />
adopted best-fit model had a power-law index <strong>of</strong> 1.52 with the Galactic absorption<br />
column <strong>of</strong> 2.45 × 10 20 cm −2 (Table 2.4, row 3). Neither using a bremsstrahlung model<br />
(row 1) nor freeing the absorbing column (rows 2 and 4) gave a better fit. Again, we<br />
remark that although hardness ratios indicate that each source is probably fitted by<br />
a more complex model than a power-law and Galactic absorption, the summation <strong>of</strong><br />
counts from objects with different emission properties can be well fitted with a single<br />
power-law and Galactic absorption. The best-fit indicated no excess absorption when<br />
48
we extended the spectrum down to 0.3 keV.<br />
Since there were not enough resolved source counts between one and three effective<br />
radii, we determined the spectrum <strong>of</strong> the entire field (which, <strong>of</strong> course, includes the<br />
inner two effective radius region discussed above). There were no large statistically-<br />
significant differences in the fits for the entire field and for the inner region (rows<br />
5–7). Within the 90% confidence level, the sources could be fitted by a power-law fit<br />
with indices between 1.45 and 1.65 (inclusive <strong>of</strong> the inner two effective radius fit) and<br />
an absorbing column <strong>of</strong> 11 × 10 20 cm −2 . Note that an important contribution to the<br />
spectrum in the outer parts <strong>of</strong> the observation <strong>of</strong> NGC 4382 is source 38, which is a<br />
known background AGN. However, this AGN has X-ray hardness ratios that indicate<br />
that it does not have a particularly hard or absorbed spectrum (Table 2.2). The<br />
X-ray hardness ratios for this source are similar to the average values for the LMXBs<br />
in NGC 4382. Since we can rarely identify an AGN with a particular source, AGNs<br />
always contribute to spectra describing the resolved sources. Removing source 38<br />
from the spectral analysis would hinder comparisons with other galaxies’ resolved<br />
sources.<br />
2.5.2 X-ray Spectra <strong>of</strong> Unresolved Emission<br />
NGC 4365<br />
Again, we began by exploring the spectrum <strong>of</strong> the inner effective radius, which<br />
had 935 net counts. This spectrum is shown in the left-hand panels <strong>of</strong> Figure 2.10.<br />
First, we attempted to model the unresolved emission with a s<strong>of</strong>t MEKAL component<br />
representing the emission by diffuse interstellar gas (Table 2.3, row 11). In general,<br />
none <strong>of</strong> the spectral fits were improved by allowing the absorbing column to vary<br />
(e.g., row 12), so we discuss only fits with a fixed Galactic column. Values from both<br />
49
Fig. 2.10.— Top panels: Cumulative X-ray spectra <strong>of</strong> the unresolved emission in the<br />
inner effective radius <strong>of</strong> NGC 4365 (left) and inner two effective radii <strong>of</strong> NGC 4382<br />
(right) with 1 σ error bars overlayed by the solid histograms <strong>of</strong> the best-fit model<br />
spectra (Table 2.3, row 13, Table and 2.4, row 11). Bottom panels: Contribution to<br />
χ 2 with the sign indicating the sign <strong>of</strong> the residual.<br />
MEKAL-only fits are consistent with previous ROSAT measurements from Davis &<br />
White (1996). The fits to the unresolved emission using only a s<strong>of</strong>t MEKAL model<br />
showed large residuals at high energies. Of course, the unresolved emission includes<br />
unresolved point sources, as well as diffuse gas, and the unresolved point sources will<br />
have a hard spectrum if they are like the resolved sources. Thus, we added a hard<br />
component to the fit with the same spectral shape as the best-fit model for the source.<br />
This produced a dramatic reduction in χ 2 by 37 for 1 less d<strong>of</strong>, clearly indicating that<br />
values from single temperature fits, like in Davis & White (1996), may be suspect.<br />
Allowing the power-law index to vary did not improve the fit significantly. Therefore,<br />
we adopted the model with a power-law index <strong>of</strong> 1.67, a MEKAL temperature <strong>of</strong><br />
0.56 +0.05<br />
−0.08 keV, and an abundance in solar units <strong>of</strong> 0.35 (row 13) as our best-fit model<br />
for unresolved emission (Figure 2.10). Although the line emission strength from<br />
heavy elements is well constrained, minimal emission from hydrogen leads to poorly<br />
constrained (>0.08) abundances. These best-fit values are consistent with some <strong>of</strong><br />
the s<strong>of</strong>t temperatures and abundances found from two-temperature fits to ASCA<br />
observations (Buote & Fabian 1998).<br />
50
We also examined whether the unresolved emission’s spectrum changed with ra-<br />
dius. The unresolved spectrum between one and three effective radii had 1155 net<br />
counts. We first fitted this spectrum with the best-fit model for unresolved emission<br />
(row 14). Then, we allowed the s<strong>of</strong>t component model to vary in the fit. This produced<br />
a much better fit (∆χ 2 = −37) with a statistically significant higher temperature (row<br />
15). This suggests that there is a positive radial gradient in the temperature <strong>of</strong> the<br />
gas. If there is a significant gradient, this would also affect the spectra in the inner<br />
parts <strong>of</strong> the galaxy. We would be observing both cooler gas located near the center <strong>of</strong><br />
the galaxy, and hotter gas at larger radii seen in projection against the center. Thus,<br />
we tried fitting the emission from the inner effective radius with two s<strong>of</strong>t components<br />
and a hard component; that model did not improve on the single s<strong>of</strong>t+hard model<br />
spectral fit we report in Table 2.3. A temperature gradient may exist in the diffuse<br />
gas; however, deeper observations <strong>of</strong> NGC 4365 are necessary to do a more detailed<br />
deprojection.<br />
In addition to a possible temperature gradient in the diffuse emission, the spectral<br />
fits <strong>of</strong> the sources and unresolved emission point to a possible change in the unresolved<br />
sources with respect to radius. In the resolved sources, the model fluxes for sources in<br />
the inner effective radius and sources between one and three effective radii are about<br />
the same. The correction for increased contribution by background sources based on<br />
the luminosity function we fitted earlier suggests that the flux from resolved sources<br />
between one and three effective radii should be ∼0.9 times the flux from resolved<br />
sources in the inner effective radius. The luminosity function <strong>of</strong> background sources<br />
in a particular field can differ from an average field either by total number <strong>of</strong> sources<br />
or by having a brighter than expected background source in the field. Source 69 is<br />
a very hard and bright source that might be such an unusually bright AGN. This<br />
51
source accounts for ∼ 1<br />
4<br />
<strong>of</strong> the hard counts in the one to three effective radii resolved<br />
source region. If we were to exclude this source, the flux ratio between the two regions<br />
would be ∼0.65. One would expect that if the unresolved source distribution is the<br />
same as the resolved source distribution, we should find a flux ratio between ∼0.6<br />
and 1.0 for the unresolved sources. Instead, the best-fit unresolved emission between<br />
one and three effective radii is a purely s<strong>of</strong>t component fit. At best, we can limit<br />
the ratio to be 0.15. This suggests that the unresolved source radial distribution<br />
may decline more rapidly than the resolved source distribution. Poisson errors in<br />
the 2–9 keV count rate <strong>of</strong> the one to three effective radii unresolved emission are too<br />
large to statistically confirm this result. Deeper X-ray observations <strong>of</strong> NGC 4365 are<br />
needed to resolve enough sources to allow the faint source and bright source radial<br />
distribution to be compared.<br />
NGC 4382<br />
The spectrum <strong>of</strong> the unresolved emission <strong>of</strong> the inner two effective radii (Fig-<br />
ure 2.10, right-hand panels) had 2620 counts. We initially fitted the spectrum with a<br />
model containing only a s<strong>of</strong>t MEKAL component representing emission from diffuse<br />
interstellar gas (row 8). The best-fit models with varying absorption gave values be-<br />
low the Galactic column, but with an upper limit that included the Galactic value<br />
(Table 2.4, row 9). Thus, we chose to use the Galactic column for all remaining fits<br />
<strong>of</strong> this galaxy’s spectra. As with NGC 4365, the addition <strong>of</strong> a hard component rep-<br />
resenting unresolved sources led to a much better statistical fit (row 10). Allowing<br />
the parameters <strong>of</strong> the hard component to vary did not result in a significantly bet-<br />
ter fit, and the hard component parameters were very poorly constrained. Thus, we<br />
fixed the shape <strong>of</strong> the spectrum <strong>of</strong> the hard component to the adopted model for the<br />
52
esolved sources in the galaxy. This leads to an acceptable fit (row 10); however, its<br />
abundance is abnormally high and poorly constrained as a result <strong>of</strong> minimal emission<br />
from hydrogen. Therefore, we have frozen the abundance at 0.5 solar for all remain-<br />
ing s<strong>of</strong>t component fits in this galaxy. This choice (row 11) is very close to the best<br />
fit (∆χ 2 = 0.3). This best-fit model has a temperature <strong>of</strong> 0.28 +0.04<br />
−0.03 and is shown in<br />
Figure 2.10.<br />
We extracted the unresolved emission spectrum from a larger (but overlapping)<br />
elliptical annulus extending from one to three effective radii. The spectrum in this<br />
region was reasonably fitted by the same gas temperature and abundance that pro-<br />
vided the best fit within two effective radii (row 12). When the gas temperature was<br />
allowed to vary (row 13), the best-fit temperature increased; however, that increase<br />
was not statistically significant. Unlike in NGC 4365, we find no change in the flux<br />
ratio <strong>of</strong> the resolved and unresolved sources with increasing radius.<br />
2.5.3 Total X-ray Spectra<br />
NGC 4365<br />
We first extracted the spectrum <strong>of</strong> all <strong>of</strong> the emission within one effective radius.<br />
The spectrum in this region is consistent with the best-fit spectra for the resolved<br />
and unresolved emission (row 16); when the spectral parameters <strong>of</strong> the hard and s<strong>of</strong>t<br />
components were allowed to vary, the fits were not significantly improved (rows 17<br />
and 18) and did not constrain the abundance. We also attempted a model with a<br />
bremsstrahlung hard component (row 19). This fit, slightly better than the power-law<br />
model, was more successful at constraining the abundance (5.21 keV). We therefore adopted<br />
the sum <strong>of</strong> the best-fit spectra for the resolved and unresolved emission as our best-fit<br />
53
for the total emission. The total emission within three effective radii yielded the same<br />
fit within the overlap <strong>of</strong> the two region’s errors for a power-law hard component model.<br />
Again, a bremsstrahlung hard component could better constrain the s<strong>of</strong>t component<br />
abundance at the expense <strong>of</strong> constraining the hard component temperature. The<br />
abundance is significantly lower than the best-fit unresolved abundance; however, the<br />
statistics can not discriminate between the power-law fit, with its poorly constrained<br />
abundance (>0.01 solar), and the bremsstrahlung fit to within a 90% confidence level.<br />
Therefore, we do not claim any abundance gradient in the total emission.<br />
In Matsumoto et al. (1997), a bremsstrahlung model with a temperature <strong>of</strong><br />
12.0 +29.3<br />
− 5.5 keV or a power-law model with index 1.8 +0.4<br />
−0.4 was fitted to the hard compo-<br />
nent, while the s<strong>of</strong>t component was fitted by either a MEKAL or a Raymond-Smith<br />
model with temperature ∼0.5 keV and poorly constrained abundance (>0.016 solar).<br />
These results are consistent with what we have found.<br />
NGC 4382<br />
The results for NGC 4382 were similar to those for NGC 4365. Within two<br />
effective radii, the total spectrum was fitted well by the combination <strong>of</strong> the best-fit<br />
hard component from the resolved sources and the best-fit s<strong>of</strong>t component from the<br />
diffuse emission (Table 2.4, row 14). Freeing the hard and s<strong>of</strong>t spectral parameters did<br />
not improve the fit significantly (rows 15 and 16). A bremsstrahlung hard component<br />
did not produce a better fit and poorly constrained the bremsstrahlung temperature<br />
greater than 10.38 keV. There was no significant change between the total emission<br />
within two effective radii and the total emission within three effective radii.<br />
Once again, the results were similar to Matsumoto et al. (1997). They used<br />
the same hard component model discussed above for NGC 4365 and fitted a s<strong>of</strong>t<br />
54
temperature ∼0.3 keV. Matsumoto et al. (1997) were able to constrain the abundance<br />
using the Raymond-Smith model to 0.029–0.21 solar, but could not constrain the<br />
abundance for the MEKAL model.<br />
2.5.4 Discrete versus Diffuse Emission<br />
We used both counts (0.3–10.0 keV) and spectral fitting results to determine the<br />
fraction <strong>of</strong> the X-ray emission that was due to diffuse gas versus the fraction due to<br />
point sources, whether resolved or not. The unresolved emission is a combination <strong>of</strong><br />
unresolved point sources and truly diffuse gaseous emission. We used the resolved<br />
source hardness ratios <strong>of</strong> each region to separate unresolved counts into point sources<br />
and diffuse gas. We also compared the hard flux (point sources) to the s<strong>of</strong>t flux<br />
(diffuse gas) in the total emission spectra. Uncertainty in the spectral models used<br />
led to a much wider range <strong>of</strong> derived flux ratios than count ratios. Since the gas is<br />
s<strong>of</strong>ter than the sources, absorption affects the diffuse emission more. Therefore, the<br />
unabsorbed flux ratio <strong>of</strong> point sources to total emission need not be larger than the<br />
count ratio <strong>of</strong> point sources to total emission, as one would expect.<br />
For the inner one effective radius <strong>of</strong> NGC 4365 the point sources are responsible<br />
for 75 ± 7% <strong>of</strong> the total counts and ∼70% <strong>of</strong> the unabsorbed flux (Table 2.3, rows<br />
16–19). Approximately 60% <strong>of</strong> the point-source counts are resolved. The unresolved<br />
point-source flux overlaps with 90% confidence level fluxes obtained from the derived<br />
luminosity function extended down to 10 36 ergs s −1 . Moving to the region within<br />
three effective radii the point sources are responsible for 75 ± 6% <strong>of</strong> the total counts<br />
and ∼55% <strong>of</strong> the unabsorbed flux (rows 20 and 21).<br />
In the inner two effective radii <strong>of</strong> NGC 4382 the point sources account for 55 ±<br />
5% <strong>of</strong> the total counts and ∼50% <strong>of</strong> the unabsorbed flux (Table 2.4, rows 14–17),<br />
55
with ∼40% <strong>of</strong> the point-source counts resolved. Again, the unresolved point-source<br />
flux overlaps with 90% confidence level fluxes obtained from the derived luminosity<br />
function extended down to 10 36 ergs s −1 . In the inner three effective radii, the point<br />
sources account for 56 ± 6% <strong>of</strong> the total counts and ∼50% <strong>of</strong> the unabsorbed flux<br />
(rows 18 and 19).<br />
For both galaxies, it was crucial that a majority <strong>of</strong> the sources were resolved.<br />
For power-law models, the 90% confidence limit on the power-law index was cut by<br />
a factor <strong>of</strong> 2–3 when sources were resolved. If one uses bremsstrahlung models, the<br />
bremsstrahlung temperature had no upper constraint unless the sources’ spectra could<br />
be fitted separately.<br />
2.6 Spatial Distribution <strong>of</strong> the Diffuse Gaseous<br />
Emission<br />
We derived the radial distribution <strong>of</strong> the diffuse gas, based on the surface bright-<br />
ness distribution in the s<strong>of</strong>t band (0.3–1 keV). We excluded regions around each <strong>of</strong> the<br />
resolved sources in determining the diffuse surface brightness. Although the diffuse<br />
gas generally dominates in the s<strong>of</strong>t band, this emission still contains a contribution<br />
from unresolved sources (§ 2.5.2). To remove the effect <strong>of</strong> the unresolved point sources,<br />
we have assumed that the spectrum <strong>of</strong> the sum <strong>of</strong> all resolved sources in the S3 field<br />
is representative <strong>of</strong> the spectrum <strong>of</strong> the unresolved sources. Based on the observed<br />
spectra, we also assume that the diffuse gas produces no significant hard-band (2–10<br />
keV) emission. Thus, we determined the surface brightness pr<strong>of</strong>ile in the hard band<br />
(removing resolved sources), and scale this by the ratio <strong>of</strong> s<strong>of</strong>t- to hard-band emission<br />
expected based on the best-fit spectrum <strong>of</strong> the resolved point sources. This s<strong>of</strong>t-band<br />
56
log I X (counts/sec/arcmin 2 )<br />
-1.0<br />
-1.5<br />
-2.0<br />
-2.5<br />
-3.0<br />
NGC 4365<br />
-3.5<br />
0.0 0.5 1.0 1.5 2.0 2.5<br />
log r (arcsec)<br />
log I X (counts/sec/arcmin 2 )<br />
-1.0<br />
-1.5<br />
-2.0<br />
-2.5<br />
-3.0<br />
NGC 4382<br />
-3.5<br />
0.0 0.5 1.0 1.5 2.0 2.5<br />
log r (arcsec)<br />
Fig. 2.11.— Surface brightness pr<strong>of</strong>iles <strong>of</strong> the s<strong>of</strong>t-band (0.3–1 keV) diffuse gaseous<br />
emission <strong>of</strong> NGC 4365 (left) and NGC 4382 (right) as a function <strong>of</strong> projected radius<br />
r with 1 σ error bars. The dashed curve shows the RC3 de Vaucouleurs pr<strong>of</strong>ile with<br />
an effective radius determined from the distribution <strong>of</strong> optical light in the galaxy, but<br />
with the normalization varied to fit the X-ray surface brightness. The solid curve is<br />
the best-fit beta model. All fits were for r < 2 ′ .<br />
surface brightness pr<strong>of</strong>ile for the sources was subtracted from the observed s<strong>of</strong>t-band<br />
pr<strong>of</strong>ile, and we attribute the remainder to diffuse gas. We performed this operation<br />
in regular circular annuli out to ∼3 ′ and corrected the pr<strong>of</strong>iles for background and<br />
exposure.<br />
Figure 2.11 displays the observed s<strong>of</strong>t band gaseous surface brightness pr<strong>of</strong>iles as<br />
a function <strong>of</strong> projected radius, r. The dashed lines display the best-fit de Vaucouleurs<br />
pr<strong>of</strong>iles with effective radii fixed at the values for the optical light in the galaxies (49. ′′ 8<br />
for NGC 4365 and 54. ′′ 6 for NGC 4382). The normalization was varied to achieve the<br />
best fit. NGC 4365 is acceptably fitted by such a pr<strong>of</strong>ile, with a χ 2 <strong>of</strong> 29.8 for 29 d<strong>of</strong>.<br />
NGC 4382 is unacceptably fitted by the de Vaucouleurs pr<strong>of</strong>ile, and the diffuse gas<br />
surface brightness is consistently larger than the optical pr<strong>of</strong>ile at r 16 ′′ . Baggett,<br />
Baggett, & Anderson (1998) found that NGC 4382 could be decomposed into a bulge<br />
with an effective radius <strong>of</strong> 71. ′′ 4 and a disk with a scale length <strong>of</strong> 165. ′′ 5. Adjusting the<br />
normalization <strong>of</strong> the bulge plus disk pr<strong>of</strong>ile better fitted the X-ray pr<strong>of</strong>ile; however, it<br />
57
was still an unacceptable fit (χ 2 > 99 for 29 d<strong>of</strong>). Therefore, we attempted a standard<br />
beta model pr<strong>of</strong>ile,<br />
58<br />
<br />
2<br />
−3β+1/2<br />
r<br />
IX(r) = I0 1 +<br />
, (2.2)<br />
where rc is the core radius. The fit for NGC 4365 was much better than the de<br />
Vaucouleurs pr<strong>of</strong>ile, χ 2 <strong>of</strong> 17.7 for 27 d<strong>of</strong> with rc = 5. ′′ 1 +8.7<br />
−3.6 (0.50 kpc) and β =<br />
0.398 +0.083<br />
−0.045 (90% confidence errors). This near power-law fit is similar to those for<br />
NGC 1291 and NGC 4697 (Irwin et al. 2002; Sarazin et al. 2001). NGC 4382 had<br />
a similar quality beta model fit with rc = 35. ′′ 5 +21.8<br />
−13.0 (3.2 kpc) and β = 0.599 ±<br />
0.265. Since β is constrained by the outer data points, the much larger core radius <strong>of</strong><br />
NGC 4382 is responsible for the larger confidence limit <strong>of</strong> its β compared to NGC 4365.<br />
The beta models for both galaxies are similar to the pr<strong>of</strong>iles <strong>of</strong> X-ray–bright galaxies<br />
within the errors (Forman et al. 1985; Trinchieri et al. 1986). For NGC 4382, its large<br />
core radius, rounder X-ray emission than optical emission, and lower gas temperature<br />
at inner radii are roughly consistent with predictions by Brighenti & Mathews (1996)<br />
for a rotating interstellar gas distribution; however, the core radius is about half their<br />
predicted value for a galaxy in Virgo.<br />
2.7 Conclusions<br />
The ability <strong>of</strong> Chandra observations to separate X-ray emission into point sources<br />
(LMXBs and background sources) and diffuse emission (unresolved LMXBs and dif-<br />
fuse gas) plays a crucial part in exploring the properties <strong>of</strong> the X-ray–faint early-type<br />
galaxies NGC 4365 and NGC 4382. We detected 99 sources in NGC 4365 and 58<br />
sources in NGC 4382, while we expect that approximately 12 sources in each galaxy<br />
are due to unrelated background sources. Within one effective radius <strong>of</strong> NGC 4365,<br />
rc
∼45% <strong>of</strong> the counts are resolved into sources, ∼30% <strong>of</strong> the counts are attributed<br />
to unresolved LMXBs, and ∼25% are attributed to diffuse gas. This distribution<br />
is consistent with that <strong>of</strong> another X-ray–faint elliptical galaxy, NGC 4697 (Sarazin<br />
et al. 2001), after correcting for different sensitivities. Within two effective radii <strong>of</strong><br />
NGC 4382, ∼22% <strong>of</strong> the counts are resolved into sources, ∼33% <strong>of</strong> the flux is at-<br />
tributed to unresolved LMXBs, and ∼45% is attributed to diffuse gas. The higher<br />
diffuse gas fraction in this lenticular is consistent with NGC 1553 (Blanton et al.<br />
2001), also an X-ray–faint lenticular galaxy; however, NGC 4382 resolves less <strong>of</strong> its<br />
flux into sources than NGC 1553, despite a better sensitivity.<br />
The hardness ratios <strong>of</strong> the resolved sources tend to be harder (more H21) than a<br />
range <strong>of</strong> power-law indices with Galactic absorption. This suggests that the source<br />
emission spectra are more complex than single power-laws. No supers<strong>of</strong>t sources were<br />
found in either <strong>of</strong> the two galaxies. The spectra <strong>of</strong> the sum <strong>of</strong> all the sources were best<br />
fitted by a power-law model with Galactic absorption. The power-law <strong>of</strong> NGC 4382,<br />
1.52, was harder than that <strong>of</strong> NGC 4365, 1.67; however, the indices are the same<br />
within their 90% confidence interval and are consistent with the best-fit value <strong>of</strong> the<br />
sources simultaneously fitted in a survey <strong>of</strong> 15 galaxies (Irwin et al. 2003).<br />
For sources in NGC 4365, 18 sources out <strong>of</strong> 37 in a WFPC2 field <strong>of</strong> view had<br />
positions correlated with a globular cluster compared to the ∼0.6 expected from<br />
random association. An additional source’s position has also been identified with a<br />
globular cluster. Three <strong>of</strong> the sources in NGC 4365 are variable at the greater than<br />
99% confidence level. The spatial distributions <strong>of</strong> the sources are broader than the<br />
optical de Vaucouleurs distribution <strong>of</strong> each galaxy.<br />
The most surprising results from analysis <strong>of</strong> the sources are the luminosity fits.<br />
Both galaxies were best fitted with cut<strong>of</strong>f power-laws, where the cut<strong>of</strong>f luminosities<br />
59
were between ≈(0.9–3.1) ×10 39 ergs s −1 . Although broken power-laws were within<br />
the 90% confidence interval, the break luminosity was similar to the cut<strong>of</strong>f luminosity.<br />
This is in contrast to the prior break/cut<strong>of</strong>f luminosities <strong>of</strong> NGC 1291, NGC 1553,<br />
and NGC 4697 [≈(2–6) ×10 38 ergs s −1 ], which had been identified with the Eddington<br />
luminosity <strong>of</strong> a 1.4 M⊙ spherically accreting neutron star (Sarazin et al. 2001; Blan-<br />
ton et al. 2001; Irwin et al. 2002). It seems unlikely that the cut<strong>of</strong>f luminosities <strong>of</strong><br />
NGC 4365 and NGC 4382 can be attributed to that physical mechanism. One other<br />
X-ray–faint early-type galaxy, NGC 1316, indicates a break luminosity that may be<br />
as high as the cut<strong>of</strong>f luminosities found in NGC 4365 and NGC 4382; however, the<br />
galaxies in this chapter provide a tighter constraint on a cut<strong>of</strong>f/break luminosity well<br />
above the neutron star Eddington luminosity.<br />
In NGC 4365, the temperature <strong>of</strong> the diffuse gas is ∼0.6 keV and its abundance is<br />
poorly constrained (> 0.08 solar) in the inner effective radius. There is some evidence<br />
for a positive temperature gradient in NGC 4365; however, deeper observations are<br />
necessary to confirm any radial gradients in temperature or abundance. NGC 4382<br />
was best fitted with a temperature <strong>of</strong> ∼0.28 keV and a poorly constrained abundance<br />
(> 0.13 solar).<br />
The diffuse gas surface brightness pr<strong>of</strong>iles in both galaxies were fitted by standard<br />
beta model pr<strong>of</strong>iles. NGC 4365 had a small (5 ′′ , 0.5 kpc) core radius and β ∼ 0.40,<br />
similar to NGC 4697. NGC 4382 had a larger core radius (∼ 36 ′′ , 3.2 kpc) and β<br />
between ∼0.33 and 0.86. The larger core radius, combined with the X-ray emission<br />
being rounder than the optical emission, and evidence <strong>of</strong> a cooler central region may<br />
indicate rotation <strong>of</strong> the diffuse gas.<br />
60
Chapter 3<br />
Chandra Observations <strong>of</strong> Diffuse<br />
Gas and Luminous X-Ray Sources<br />
Around the X-Ray–Bright<br />
Elliptical NGC 1600<br />
3.1 Introduction<br />
X-ray emission in early-type galaxies generally comes from two sources, hot (kT ∼<br />
1 keV) interstellar gas and hard X-ray point sources whose properties are consistent<br />
with low-mass X-ray binaries (LMXBs). X-ray–bright galaxies (those with relatively<br />
high LX/LB ratios, where LX is X-ray luminosity and LB is blue optical luminos-<br />
ity) are dominated by the interstellar gas (e.g., Forman et al. 1985; Trinchieri et al.<br />
1986), while X-ray–faint galaxies (low LX/LB) have a large proportion <strong>of</strong> emission by<br />
LMXBs (Fabbiano et al. 1994; Pellegrini 1994; Kim et al. 1996; Sarazin et al. 2000).<br />
Since Fabbiano (1989), we have known that some <strong>of</strong> the <strong>of</strong>f-nuclear X-ray point<br />
61
sources in spiral and elliptical galaxies have luminosities significantly exceeding the<br />
Eddington limit for 1 M⊙. These ultra-luminous X-ray point sources (ULXs) appear<br />
to occur preferentially in star-forming regions, (e.g., the Antennae: Zezas & Fabbiano<br />
2002); however, early-type galaxies also contain bright point sources (e.g., NGC 1399<br />
Angelini et al. 2001). In early-type galaxies there appear to be X-ray point sources<br />
with LX < 2 × 10 39 ergs s −1 , consistent with accreting objects with masses 15 M⊙<br />
(Irwin et al. 2004). This mass limit is in line with current estimates <strong>of</strong> the upper mass<br />
limit <strong>of</strong> stellar mass black holes for progenitor masses 40 M⊙ (Fryer & Kalogera<br />
2001). Above 2 × 10 39 ergs s −1 , the number <strong>of</strong> sources in previously observed early-<br />
type galaxies may be consistent with the number <strong>of</strong> expected background sources<br />
(Irwin et al. 2004). For this reason, we adopt LX = 2 × 10 39 ergs s −1 as our minimum<br />
luminosity for a ULX candidate. Although the fainter ULXs could be explained by<br />
steady, spherically symmetric, Eddington-limited accretion onto stellar-mass black<br />
holes, some other mechanism is required for the brighter ULXs.<br />
ASCA results have indicated that the total luminosity <strong>of</strong> LMXBs in early-type<br />
galaxies correlates better with the number <strong>of</strong> globular clusters (GCs) than the optical<br />
luminosity <strong>of</strong> the galaxy (White et al. 2002). Chandra observations <strong>of</strong> early-type<br />
galaxies have also shown that a significant fraction (20%-70%) <strong>of</strong> the LMXBs are<br />
associated with globular clusters in the host galaxies (Sarazin et al. 2000, 2001; An-<br />
gelini et al. 2001; Kundu et al. 2003; Sarazin et al. 2003). It has been suggested that<br />
most, if not all, <strong>of</strong> the LMXBs were formed in GCs (Grindlay 1984; Sarazin et al.<br />
2000; White et al. 2002), and thus LMXBs can be used as tracers for GCs.<br />
In this chapter, we discuss Chandra observations <strong>of</strong> NGC 1600, an X-ray–bright<br />
E3 galaxy. NGC 1600 is the brightest member <strong>of</strong> the NGC 1600 group; NGC 1601<br />
(1. ′ 6 away) and NGC 1603 (2. ′ 5 away) are the two nearest galaxies, both <strong>of</strong> which are<br />
62
noninteracting members (de Vaucouleurs et al. 1992, hereafter RC3). We adopted the<br />
distance to NGC 1600 <strong>of</strong> 59.98 Mpc from Prugniel & Simien (1996), which assumes<br />
H0 = 75 km s −1 Mpc −1 and uses the Faber & Burstein (1988) model that accounts<br />
for the Virgocentric flow and the Great Attractor. NGC 1600 is a boxy elliptical with<br />
a radially anisotropic, axisymmetric, three-integral distribution function. Combined<br />
with its lack <strong>of</strong> significant rotation, its dynamics argue for a merger origin in which the<br />
effects <strong>of</strong> gas were not very important (Matthias & Gerhard 1999). Terlevich & Forbes<br />
(2002) estimated the age <strong>of</strong> NGC 1600 to be 7.3 Gyr with [Fe/H]= 0.41, while Trager<br />
et al. (2000) estimated an age <strong>of</strong> ∼8.8 Gyr with [Fe/H]∼0.15 through the inner 5. ′′ 7 and<br />
∼4.6 Gyr and [Fe/H]∼0.24 through the inner 22. ′′ 7. The colors (Sandage 1973; Frogel<br />
et al. 1978) <strong>of</strong> NGC 1600 are consistent with colors from NGC 3379, a prototypical<br />
elliptical galaxy, suggesting star-formation has not occurred recently. In addition to<br />
X-ray emitting gas, NGC 1600 also has cooler gas as indicated by Hα (Trinchieri & di<br />
Serego Alighieri 1991) and dust (Ferrari et al. 1999). Post-asymptotic giant branch<br />
(post-AGB) stars seem capable <strong>of</strong> producing the necessary ionization/heating for the<br />
Hα and dust.<br />
In § 3.2, we discuss the observations and data reduction <strong>of</strong> NGC 1600. After<br />
presenting the X-ray images in § 3.3, we discuss the properties <strong>of</strong> resolved sources<br />
in § 3.4. The spatial distribution <strong>of</strong> the diffuse X-ray emission and structures found<br />
in it are described in § 3.5, in which they are compared with structures in other<br />
wave bands. We discuss the X-ray spectral properties <strong>of</strong> the sources and unresolved<br />
emission in § 3.6. We estimate the gas and gravitational mass in § 3.7. Finally, we<br />
summarize our conclusions in § 3.8.<br />
63
3.2 Observation and Data Reduction<br />
NGC 1600 was observed in two intervals (observations 4283 and 4371) on 2002<br />
September 18–19 and September 20 with live exposures <strong>of</strong> 26,783 and 26,752 s, re-<br />
spectively. The ACIS-35678 chips were operated at a temperature <strong>of</strong> −120 ◦ C with<br />
a frame time <strong>of</strong> 3.2 s. We determined the pointings so that the entire galaxy was<br />
located on the S3 chip, with the galaxy center <strong>of</strong>fset from the node boundaries <strong>of</strong><br />
the chip. Although a number <strong>of</strong> serendipitous sources were seen on the other chips,<br />
the analysis in this chapter is based on data from the S3 chip alone. The data were<br />
telemetered and cleaned in Very Faint mode, and only events with ASCA grades <strong>of</strong><br />
0, 2, 3, 4, and 6 were included. Photon energies were determined using the gain file<br />
acisD2000-08-12gainN0003.fits and corrected for time dependence <strong>of</strong> the gain. 1 We<br />
excluded bad pixels, bad columns, and columns adjacent to bad columns or chip node<br />
boundaries.<br />
Chandra is known to encounter periods <strong>of</strong> high background (“background flares”),<br />
which especially affect the backside-illuminated S1 and S3 chips. 2 We determined the<br />
background count rate from the S1 chip to avoid the enhanced flux due to the galaxy<br />
on the S3 chip. Using Maxim Markevitch’s LC CLEAN program, 3 we found the<br />
exposure intervals that were unaffected by background flares. The first observation<br />
showed clear evidence <strong>of</strong> a major flare in the first 20% <strong>of</strong> the observation. The second<br />
observation had some small fluctuations greater than 20% from the mean rate. After<br />
these were filtered, observations 4283 and 4371 had flare-free exposure times <strong>of</strong> 21,562<br />
and 23,616 s, respectively. We created a merged events file for imaging analysis after<br />
checking that the observations were well registered; the separate events files were<br />
1 See http://hea-www.harvard.edu/∼alexey/acis/tgain.<br />
2 See http://cxc.harvard.edu/contrib/maxim/acisbg.<br />
3 See footnote 2.<br />
64
used for spectroscopic analysis. We took the backgrounds for extended regions from<br />
the deep blank-sky backgrounds compiled by Maxim Markevitch, 4 adjusted them to<br />
the aspect histories <strong>of</strong> our observations, and changed the normalizations slightly to<br />
match the hard count rate (pha = 2500 : 3000) <strong>of</strong> the blank-sky background with a<br />
relatively emission-free region on the S3 chip. For imaging analysis, we also included<br />
the “background” due to the readout artifact in ACIS using a script based on the<br />
MAKE READOUT BG program. 5 .<br />
We performed the data reduction and some <strong>of</strong> the data analysis using the Chandra<br />
analysis package CIAO, version 2.3, 6 and NASA’s FTOOLS. 7 Spectra were fit using<br />
XSPEC, 8 while correcting for the ACIS quantum efficiency (QE) degradation 9 . with<br />
the XSPEC acisabs model.<br />
3.3 X-ray Image<br />
NGC 1600 has a combination <strong>of</strong> diffuse emission and resolved point sources. In<br />
order to image the diffuse emission without deemphasizing the point sources, we<br />
adaptively smoothed the background-subtracted, exposure-corrected image using a<br />
minimum signal-to-noise ratio (S/N) per smoothing beam <strong>of</strong> 3. Figure 3.1 displays<br />
a true-color image <strong>of</strong> the adaptively smoothed X-ray image. This image was created<br />
by smoothing three exposure and background-corrected images in s<strong>of</strong>t (0.3–1 keV),<br />
medium (1–2 keV), and and hard (2–6 keV) bands using the same kernel required for<br />
the total band adaptively smoothed image, and then combining them with the color<br />
4 See footnote 2.<br />
5 See footnote 2.<br />
6 See http://asc.harvard.edu/ciao2.3.<br />
7 See http://heasarc.gsfc.nasa.gov/ftools.<br />
8 See http://heasarc.gsfc.nasa.gov/docs/s<strong>of</strong>tware/lheas<strong>of</strong>t.<br />
9 See http://cxc.harvard.edu/cal/Acis/Cal prods/qeDeg.<br />
65
coding red for s<strong>of</strong>t, green for medium, and blue for hard. A logarithmic intensity<br />
scale was chosen to range between total band surface brightnesses <strong>of</strong> 5 × 10 −7 and<br />
1 × 10 −3 counts arcsec −2 s −1 .<br />
In Figure 3.2 we show the corresponding Second Palomar Observatory Sky Survey<br />
(POSS II) optical (red) image using a linear gray scale. The field <strong>of</strong> view is the<br />
same as that in Figure 3.1. The largest galaxy near the upper center is NGC 1600<br />
and corresponds to the brightest peak in the diffuse X-ray emission. Another group<br />
member, NGC 1603, lies to the east <strong>of</strong> NGC 1600. The galaxy north <strong>of</strong> NGC 1600<br />
is the group member NGC 1601. In Figure 3.2 the overlaid regions indicate the<br />
positions <strong>of</strong> the X-ray sources discussed in § 3.4 and listed in Table 3.1. All <strong>of</strong> the<br />
sources with fluxes determined to more than 3 σ (squares) are clearly seen in the<br />
adaptively smoothed X-ray image (Fig. 3.1), except for the central three sources,<br />
which are embedded in strong diffuse emission. Very few <strong>of</strong> the weaker sources can<br />
be seen in Figure 3.1.<br />
The diffuse X-ray emission in Figure 3.1 shows several interesting structures. The<br />
central X-ray emission <strong>of</strong> NGC 1600 is elongated in a direction that is roughly aligned<br />
with the optical emission. However, there are some structures in the central X-ray<br />
emission, which are discussed below (§ 3.5.1). The emission around the elliptical<br />
galaxy NGC 1603 in the east appears somewhat extended, and there is a bridge <strong>of</strong><br />
X-ray emission extending from NGC 1603 in the west toward NGC 1600. There is<br />
an X-ray source associated with the lenticular galaxy NGC 1601, but it is unclear<br />
whether it is extended in this image. On larger scales, there is a slightly elongated<br />
region <strong>of</strong> very extended X-ray surface brightness, with excess diffuse emission, to the<br />
northeast <strong>of</strong> NGC 1600. (Adaptively smoothed images with the sources replaced by<br />
Poisson noise do not affect the gross morphology <strong>of</strong> the diffuse X-ray emission; that<br />
66
02:00.0<br />
03:00.0<br />
04:00.0<br />
05:00.0<br />
06:00.0<br />
07:00.0<br />
08:00.0<br />
09:00.0<br />
-5:10:00.0<br />
55.0 50.0 45.0 4:31:40.0 35.0 30.0 25.0<br />
Fig. 3.1.— Adaptively smoothed Chandra true-color S3 image (for 0.3–1 keV [red],<br />
1–2 keV [green], 2–6 keV [blue]) <strong>of</strong> NGC 1600, corrected for exposure and background.<br />
The total intensity scale is logarithmic and ranges from 5 × 10 −7 to 1 × 10 −3 counts<br />
arcsec −2 s −1 . The surrounding white square is the field <strong>of</strong> view <strong>of</strong> the Chandra S3<br />
image.<br />
67
02:00<br />
03:00<br />
04:00<br />
05:00<br />
06:00<br />
07:00<br />
08:00<br />
09:00<br />
-5:10:00<br />
71<br />
60 59<br />
40<br />
17<br />
18<br />
23<br />
13<br />
8 7<br />
10<br />
55 4:31:50 45 4:31:40 35 4:31:30 25<br />
Fig. 3.2.— Linear gray scale POSS II red optical image <strong>of</strong> NGC 1600. The squares<br />
and circles indicate the positions <strong>of</strong> the X-ray sources with S/N> 3 and S/N< 3 in<br />
Table 3.1, respectively. Sources mentioned in the text are labeled. The surrounding<br />
dark square is the field <strong>of</strong> view <strong>of</strong> the Chandra S3 image.<br />
2<br />
24<br />
3<br />
1<br />
33<br />
52<br />
30<br />
42<br />
36<br />
50<br />
63<br />
58<br />
68
Table 3.1. Discrete X-ray Sources in NGC 1600<br />
d a Count Rate<br />
Source Name R.A. Decl. (arcsec) (arcsec) (10 −4 s −1 ) S/N LX H21 0<br />
H31 0<br />
H32 0<br />
Notes<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13)<br />
1 ....... CXOU J043139.8−050511 04 31 39.88 −05 05 11.4 0.9 1.0 38.91±3.10 12.55 160.3 −0.50 +0.11<br />
−0.09<br />
−0.96 +0.09<br />
−0.03<br />
−0.88 +0.22<br />
−0.08<br />
a,b,d,e<br />
2 ....... CXOU J043140.0−050504 04 31 40.05 −05 05 04.7 6.4 6.5 15.00±1.94 7.75 61.8 −0.29 +0.25<br />
−0.21<br />
−0.88 +0.24<br />
−0.09<br />
−0.78 +0.36<br />
−0.15<br />
a,b<br />
3 ....... CXOU J043139.7−050456 04 31 39.71 −05 04 56.6 14.1 15.5 7.31±1.42 5.16 30.1 −0.48 +0.28<br />
−0.21<br />
−0.91 +0.43<br />
−0.08<br />
−0.77 +0.77<br />
−0.20<br />
a,b<br />
4 ....... CXOU J043138.1−050456 04 31 38.15 −05 04 56.9 29.0 42.3 1.78±0.70 2.55 7.3 −0.80 +1.09<br />
−0.19<br />
−0.67 +0.63<br />
−0.25<br />
+0.27 +0.67<br />
−1.11<br />
· · ·<br />
5 ....... CXOU J043140.1−050540 04 31 40.15 −05 05 40.7 30.6 33.2 4.26±1.05 4.05 17.5 −0.78 +0.66<br />
−0.18<br />
−0.48 +0.36<br />
−0.25<br />
+0.47 +0.42<br />
−0.87<br />
· · ·<br />
6 ....... CXOU J043139.7−050436 04 31 39.75 −05 04 36.3 34.2 36.1 1.55±0.65 2.37 6.4 +0.62 +0.36<br />
−1.41<br />
−0.22 +1.18<br />
−0.76<br />
−0.74 +0.98<br />
−0.23<br />
e<br />
7 ....... CXOU J043138.3−050536 04 31 38.30 −05 05 36.7 35.2 39.2 7.48±1.35 5.52 30.8 +0.30 +0.33<br />
−0.42<br />
+0.12 +0.38<br />
−0.42<br />
−0.18 +0.24<br />
−0.22<br />
· · ·<br />
8 ....... CXOU J043141.2−050543 04 31 41.23 −05 05 43.0 38.4 49.1 4.77±1.10 4.33 19.7 −0.42 +0.34<br />
−0.25<br />
−0.67 +0.34<br />
−0.19<br />
−0.35 +0.47<br />
−0.34<br />
e<br />
9 ....... CXOU J043137.3−050457 04 31 37.33 −05 04 57.2 40.2 59.4 3.48±0.93 3.73 14.3 −0.26 +0.41<br />
−0.34<br />
−0.67 +0.50<br />
−0.23<br />
−0.50 +0.57<br />
−0.33<br />
· · ·<br />
10...... CXOU J043139.8−050552 04 31 39.84 −05 05 52.3 41.9 43.4 8.32±1.42 5.87 34.3 −0.72 +0.17<br />
−0.11<br />
−0.86 +0.17<br />
−0.08<br />
−0.39 +0.48<br />
−0.33<br />
f<br />
11...... CXOU J043137.3−050536 04 31 37.31 −05 05 36.0 46.0 56.6 1.43±0.61 2.36 5.9 −0.72 +1.05<br />
−0.25<br />
−0.50 +0.75<br />
−0.37<br />
+0.35 +0.59<br />
−1.09<br />
· · ·<br />
12...... CXOU J043141.9−050550 04 31 41.99 −05 05 50.8 51.3 68.0 2.03±0.73 2.78 8.4 +0.25 +0.50<br />
−0.68<br />
−0.65 +1.16<br />
−0.32<br />
−0.78 +0.93<br />
−0.20<br />
· · ·<br />
13...... CXOU J043141.5−050421 04 31 41.50 −05 04 21.0 55.1 56.3 1.52±0.63 2.40 6.3 +0.06 +0.62<br />
−0.66<br />
−1.00 +0.66<br />
−0.00<br />
−1.00 +0.59<br />
−0.00<br />
e<br />
14...... CXOU J043139.8−050407 04 31 39.81 −05 04 07.1 63.4 66.1 3.65±0.94 3.90 15.0 −0.15 +0.42<br />
−0.37<br />
−0.53 +0.49<br />
−0.29<br />
−0.40 +0.48<br />
−0.33<br />
· · ·<br />
15...... CXOU J043136.0−050542 04 31 36.04 −05 05 42.2 65.5 83.2 1.66±0.65 2.56 6.9 −0.27 +0.91<br />
−0.60<br />
+0.01 +0.71<br />
−0.72<br />
+0.28 +0.51<br />
−0.73<br />
· · ·<br />
16...... CXOU J043135.1−050502 04 31 35.17 −05 05 02.6 70.7 103.9 9.47±1.51 6.26 39.0 −0.25 +0.22<br />
−0.20<br />
−0.61 +0.23<br />
−0.16<br />
−0.43 +0.27<br />
−0.21<br />
f<br />
17...... CXOU J043143.2−050411 04 31 43.27 −05 04 11.3 78.0 86.3 5.49±1.18 4.63 22.6 −0.48 +0.24<br />
−0.18<br />
−1.00 +0.12<br />
−0.00<br />
−1.00 +0.33<br />
−0.00<br />
f<br />
18...... CXOU J043145.0−050511 04 31 45.09 −05 05 11.1 78.0 113.5 1.66±0.65 2.54 6.8 −0.47 +0.59<br />
−0.34<br />
−0.81 +0.91<br />
−0.17<br />
−0.54 +1.12<br />
−0.41<br />
d<br />
19...... CXOU J043145.0−050438 04 31 45.06 −05 04 38.1 84.0 111.0 1.24±0.56 2.20 5.1 −0.35 +0.87<br />
−0.51<br />
−0.40 +0.88<br />
−0.47<br />
−0.06 +0.77<br />
−0.70<br />
· · ·<br />
20...... CXOU J043139.9−050339 04 31 39.93 −05 03 39.2 91.3 94.6 1.48±0.60 2.45 6.1 −0.02 +0.89<br />
−0.86<br />
+0.26 +0.65<br />
−1.00<br />
+0.28 +0.51<br />
−0.73<br />
· · ·<br />
21...... CXOU J043134.2−050431 04 31 34.25 −05 04 31.1 92.7 136.0 5.54±1.15 4.82 22.8 −0.72 +0.22<br />
−0.13<br />
−0.95 +0.36<br />
−0.04<br />
−0.73 +1.00<br />
−0.24<br />
f<br />
22...... CXOU J043143.6−050627 04 31 43.65 −05 06 27.6 95.6 125.5 3.75±0.97 3.85 15.5 +0.16 +0.54<br />
−0.65<br />
+0.04 +0.59<br />
−0.62<br />
−0.11 +0.40<br />
−0.37<br />
· · ·<br />
23...... CXOU J043141.7−050336 04 31 41.78 −05 03 36.9 97.9 97.9 2.73±0.83 3.30 11.2 −0.47 +0.67<br />
−0.37<br />
−0.60 +0.69<br />
−0.30<br />
−0.18 +0.75<br />
−0.59<br />
d<br />
24...... CXOU J043141.2−050654 04 31 41.25 −05 06 54.3 105.8 117.5 2.80±0.82 3.43 11.5 +0.01 +0.61<br />
−0.62<br />
−0.16 +0.69<br />
−0.56<br />
−0.17 +0.51<br />
−0.43<br />
e<br />
25...... CXOU J043141.6−050653 04 31 41.61 −05 06 53.5 106.3 120.4 12.63±1.71 7.38 52.0 +0.41 +0.25<br />
−0.34<br />
+0.36 +0.27<br />
−0.34<br />
−0.05 +0.17<br />
−0.17<br />
f<br />
26...... CXOU J043132.6−050513 04 31 32.61 −05 05 13.1 108.5 156.9 1.52±0.62 2.46 6.3 −0.61 +0.83<br />
−0.32<br />
−0.59 +0.73<br />
−0.31<br />
+0.03 +0.76<br />
−0.80<br />
· · ·<br />
Continued on Next Page. . .<br />
69
Table 3.1—Continued<br />
d a Count Rate<br />
Source Name R.A. Decl. (arcsec) (arcsec) (10 −4 s −1 ) S/N LX H21 0<br />
H31 0<br />
H32 0<br />
Notes<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13)<br />
27...... CXOU J043139.5−050711 04 31 39.58 −05 07 11.5 121.1 124.6 16.02±1.92 8.32 66.0 −0.29 +0.16<br />
−0.15<br />
−0.52 +0.16<br />
−0.13<br />
−0.27 +0.18<br />
−0.17<br />
f<br />
28...... CXOU J043132.1−050428 04 31 32.13 −05 04 28.6 123.0 181.5 3.31±0.89 3.71 13.6 −0.46 +0.33<br />
−0.24<br />
−0.83 +0.38<br />
−0.13<br />
−0.60 +0.63<br />
−0.29<br />
· · ·<br />
29...... CXOU J043144.8−050331 04 31 44.80 −05 03 31.9 123.1 132.8 11.38±1.64 6.92 46.9 −0.22 +0.19<br />
−0.17<br />
−0.68 +0.19<br />
−0.13<br />
−0.54 +0.22<br />
−0.17<br />
f<br />
30...... CXOU J043132.2−050422 04 31 32.25 −05 04 22.6 123.5 181.7 13.46±1.82 7.38 55.4 +0.30 +0.24<br />
−0.28<br />
+0.05 +0.29<br />
−0.30<br />
−0.26 +0.18<br />
−0.16<br />
e,f<br />
31...... CXOU J043147.5−050612 04 31 47.55 −05 06 12.6 130.5 190.2 0.68±0.43 1.56 2.8 −1.00 +0.60<br />
−0.00<br />
−1.00 +0.44<br />
−0.00<br />
+0.00 +1.00<br />
−1.00<br />
· · ·<br />
32...... CXOU J043147.1−050353 04 31 47.18 −05 03 53.5 133.6 163.0 3.34±0.91 3.69 13.8 −0.16 +0.48<br />
−0.42<br />
−0.31 +0.51<br />
−0.38<br />
−0.15 +0.44<br />
−0.39<br />
· · ·<br />
33...... CXOU J043136.1−050308 04 31 36.19 −05 03 08.3 133.9 162.7 1.71±0.65 2.65 7.1 −0.52 +0.63<br />
−0.33<br />
−0.81 +0.91<br />
−0.17<br />
−0.50 +1.13<br />
−0.45<br />
d<br />
34...... CXOU J043146.4−050338 04 31 46.48 −05 03 38.4 135.1 156.1 2.00±0.71 2.83 8.2 −0.43 +0.59<br />
−0.37<br />
−0.81 +0.91<br />
−0.17<br />
−0.58 +1.11<br />
−0.38<br />
· · ·<br />
35...... CXOU J043142.2−050257 04 31 42.24 −05 02 57.2 137.8 137.8 1.26±0.56 2.25 5.2 +0.31 +0.60<br />
−1.03<br />
−0.40 +1.24<br />
−0.56<br />
−0.64 +1.08<br />
−0.33<br />
· · ·<br />
36...... CXOU J043131.3−050411 04 31 31.34 −05 04 11.8 140.2 205.8 2.97±0.87 3.40 12.2 −0.59 +0.40<br />
−0.23<br />
−0.96 +1.88<br />
−0.04<br />
−0.86 +1.84<br />
−0.14<br />
· · ·<br />
37...... CXOU J043141.8−050252 04 31 41.84 −05 02 52.5 141.1 141.3 1.93±0.68 2.82 8.0 +0.41 +0.57<br />
−1.29<br />
+0.40 +0.58<br />
−1.28<br />
−0.01 +0.58<br />
−0.57<br />
· · ·<br />
38...... CXOU J043148.6−050415 04 31 48.60 −05 04 15.9 141.5 186.8 1.33±0.59 2.27 5.5 −0.35 +0.87<br />
−0.51<br />
−0.40 +0.88<br />
−0.47<br />
−0.06 +0.77<br />
−0.70<br />
· · ·<br />
39...... CXOU J043138.2−050245 04 31 38.21 −05 02 45.4 147.2 161.8 1.25±0.56 2.23 5.2 +0.57 +0.42<br />
−1.39<br />
−1.00 +2.00<br />
−0.00<br />
−1.00 +0.55<br />
−0.00<br />
· · ·<br />
40...... CXOU J043149.8−050539 04 31 49.86 −05 05 39.7 152.2 224.8 3.16±0.87 3.62 13.0 −1.00 +0.51<br />
−0.00<br />
−0.67 +0.57<br />
−0.24<br />
+1.00 +0.00<br />
−2.00<br />
d<br />
41...... CXOU J043147.0−050308 04 31 47.07 −05 03 08.7 162.5 180.7 2.88±0.84 3.45 11.9 −0.16 +0.48<br />
−0.42<br />
−0.52 +0.58<br />
−0.32<br />
−0.39 +0.55<br />
−0.37<br />
· · ·<br />
42...... CXOU J043132.2−050712 04 31 32.25 −05 07 12.0 166.6 187.2 4.88±1.13 4.31 20.1 +1.00 +0.00<br />
−1.47<br />
+1.00 +0.00<br />
−0.94<br />
+0.22 +0.30<br />
−0.35<br />
f<br />
43...... CXOU J043148.8−050328 04 31 48.83 −05 03 28.1 168.5 202.3 1.10±0.52 2.09 4.5 −0.35 +1.21<br />
−0.61<br />
+0.12 +0.76<br />
−0.93<br />
+0.45 +0.49<br />
−1.10<br />
· · ·<br />
44...... CXOU J043146.0−050735 04 31 46.08 −05 07 35.7 172.4 221.3 1.30±0.60 2.16 5.3 −0.21 +0.67<br />
−0.52<br />
−1.00 +0.21<br />
−0.00<br />
−1.00 +0.31<br />
−0.00<br />
· · ·<br />
45...... CXOU J043135.5−050222 04 31 35.50 −05 02 22.7 180.0 214.2 1.76±0.67 2.65 7.30 +0.46 +0.47<br />
−1.07<br />
−0.40 +1.24<br />
−0.56<br />
−0.73 +1.00<br />
−0.24<br />
· · ·<br />
46...... CXOU J043127.8−050537 04 31 27.82 −05 05 37.5 182.0 257.3 6.80±1.29 5.28 28.0 −0.04 +0.37<br />
−0.36<br />
−0.04 +0.36<br />
−0.35<br />
−0.00 +0.28<br />
−0.28<br />
f<br />
47...... CXOU J043142.9−050213 04 31 42.98 −05 02 13.3 183.2 183.2 1.90±0.89 2.14 7.8 +1.00 +0.00<br />
−2.00<br />
+1.00 +0.00<br />
−2.00<br />
−0.26 +0.77<br />
−0.54<br />
c<br />
48...... CXOU J043137.8−050818 04 31 37.80 −05 08 18.3 190.4 191.5 3.12±0.89 3.53 12.9 −0.65 +0.50<br />
−0.24<br />
−0.74 +0.50<br />
−0.19<br />
−0.18 +0.75<br />
−0.59<br />
· · ·<br />
49...... CXOU J043127.7−050405 04 31 27.75 −05 04 05.9 192.2 283.9 1.91±0.69 2.77 7.93 +0.21 +0.53<br />
−0.68<br />
−0.28 +0.80<br />
−0.54<br />
−0.46 +0.59<br />
−0.35<br />
e<br />
50...... CXOU J043130.4−050256 04 31 30.44 −05 02 56.1 194.6 269.3 75.83±4.18 18.14 312.4 −0.78 +0.03<br />
−0.03<br />
−0.99 +0.02<br />
−0.01<br />
−0.92 +0.12<br />
−0.05<br />
d<br />
51...... CXOU J043150.1−050304 04 31 50.16 −05 03 04.7 198.7 235.5 23.13±2.34 9.90 95.3 −0.54 +0.10<br />
−0.09<br />
−0.77 +0.09<br />
−0.07<br />
−0.39 +0.18<br />
−0.16<br />
f<br />
52...... CXOU J043134.2−050205 04 31 34.21 −05 02 05.2 203.7 247.9 5.99±2.74 2.21 24.7 +1.00 +0.00<br />
−2.00<br />
+1.00 +0.00<br />
−2.00<br />
+0.56 +0.39<br />
−1.09<br />
c<br />
Continued on Next Page. . .<br />
70
Table 3.1—Continued<br />
d a Count Rate<br />
Source Name R.A. Decl. (arcsec) (arcsec) (10 −4 s −1 ) S/N LX H21 0<br />
H31 0<br />
H32 0<br />
Notes<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13)<br />
53...... CXOU J043147.4−050212 04 31 47.45 −05 02 12.5 210.9 221.9 116.05±7.08 16.41 478.1 −0.41 +0.06<br />
−0.06<br />
−0.76 +0.05<br />
−0.04<br />
−0.50 +0.08<br />
−0.08<br />
c,f<br />
54...... CXOU J043134.6−050826 04 31 34.68 −05 08 26.8 211.0 212.6 4.45±1.10 4.05 18.3 +0.04 +0.38<br />
−0.40<br />
−0.65 +0.58<br />
−0.25<br />
−0.67 +0.50<br />
−0.23<br />
· · ·<br />
55...... CXOU J043153.6−050408 04 31 53.68 −05 04 08.6 215.4 293.8 26.29±2.64 9.94 108.3 −0.26 +0.13<br />
−0.12<br />
−0.61 +0.12<br />
−0.10<br />
−0.42 +0.15<br />
−0.13<br />
f<br />
56...... CXOU J043150.9−050730 04 31 50.96 −05 07 30.7 217.1 304.9 2.77±0.86 3.24 11.4 −0.13 +0.47<br />
−0.42<br />
−0.72 +0.71<br />
−0.23<br />
−0.65 +0.73<br />
−0.27<br />
· · ·<br />
57...... CXOU J043125.4−050540 04 31 25.43 −05 05 40.6 217.8 308.5 4.11±1.04 3.96 17.0 −0.04 +0.35<br />
−0.34<br />
−0.79 +0.58<br />
−0.17<br />
−0.78 +0.57<br />
−0.18<br />
· · ·<br />
58...... CXOU J043126.0−050639 04 31 26.07 −05 06 39.6 224.6 295.4 5.96±1.24 4.79 24.6 +0.61 +0.36<br />
−1.20<br />
+0.74 +0.24<br />
−1.13<br />
+0.24 +0.26<br />
−0.30<br />
f<br />
59...... CXOU J043153.0−050659 04 31 53.06 −05 06 59.0 225.0 327.7 4.65±1.07 4.35 19.2 −0.51 +0.27<br />
−0.20<br />
−0.78 +0.30<br />
−0.13<br />
−0.46 +0.50<br />
−0.32<br />
e,f<br />
60...... CXOU J043153.9−050656 04 31 53.90 −05 06 56.8 235.0 343.6 4.29±1.05 4.09 17.7 +0.69 +0.30<br />
−1.42<br />
+0.76 +0.24<br />
−1.41<br />
+0.13 +0.30<br />
−0.33<br />
· · ·<br />
61...... CXOU J043131.2−050832 04 31 31.21 −05 08 32.6 240.0 252.8 2.40±0.84 2.86 9.9 +0.56 +0.39<br />
−1.07<br />
−0.17 +1.03<br />
−0.76<br />
−0.66 +0.81<br />
−0.28<br />
· · ·<br />
62...... CXOU J043123.9−050546 04 31 23.95 −05 05 46.2 240.6 340.1 2.22±0.78 2.84 9.1 +1.00 +0.00<br />
−1.95<br />
+1.00 +0.00<br />
−1.55<br />
+0.11 +0.44<br />
−0.49<br />
· · ·<br />
63...... CXOU J043126.5−050729 04 31 26.51 −05 07 29.7 243.4 297.4 3.62±1.00 3.62 14.9 −0.46 +0.71<br />
−0.39<br />
−0.67 +0.96<br />
−0.29<br />
−0.31 +0.99<br />
−0.59<br />
d<br />
64...... CXOU J043155.4−050311 04 31 55.43 −05 03 11.5 261.2 335.9 6.25±1.27 4.92 25.7 −0.08 +0.30<br />
−0.29<br />
−0.60 +0.35<br />
−0.21<br />
−0.55 +0.34<br />
−0.22<br />
f<br />
65...... CXOU J043155.9−050255 04 31 55.98 −05 02 55.1 276.2 350.1 6.53±1.31 5.00 26.9 −0.03 +0.31<br />
−0.31<br />
−0.51 +0.37<br />
−0.25<br />
−0.48 +0.32<br />
−0.23<br />
f<br />
66...... CXOU J043124.2−050232 04 31 24.22 −05 02 32.3 282.3 405.2 0.82±0.47 1.76 3.4 +1.00 +0.00<br />
−2.00<br />
+1.00 +0.00<br />
−2.00<br />
−0.80 +1.79<br />
−0.20<br />
· · ·<br />
67...... CXOU J043130.2−050918 04 31 30.29 −05 09 18.3 286.1 297.3 14.34±1.99 7.21 59.1 −0.12 +0.19<br />
−0.18<br />
−0.67 +0.23<br />
−0.15<br />
−0.60 +0.24<br />
−0.17<br />
f<br />
68...... CXOU J043138.6−051011 04 31 38.65 −05 10 11.1 301.2 308.2 6.14±1.35 4.54 25.3 −0.45 +0.27<br />
−0.21<br />
−0.64 +0.29<br />
−0.18<br />
−0.27 +0.41<br />
−0.33<br />
f<br />
69...... CXOU J043150.8−050953 04 31 50.83 −05 09 53.3 326.8 412.8 4.10±1.17 3.50 16.9 +0.51 +0.45<br />
−1.22<br />
−0.65 +1.63<br />
−0.35<br />
−0.87 +1.75<br />
−0.13<br />
· · ·<br />
70...... CXOU J043127.7−051021 04 31 27.75 −05 10 21.0 359.5 373.9 43.34±3.52 12.32 178.6 +0.14 +0.12<br />
−0.12<br />
−0.39 +0.13<br />
−0.12<br />
−0.51 +0.09<br />
−0.08<br />
f<br />
71...... CXOU J043157.3−051006 04 31 57.39 −05 10 06.5 395.1 533.9 13.61±3.63 3.91 56.1 +0.04 +0.33<br />
−0.34<br />
−0.67 +0.44<br />
−0.22<br />
−0.69 +0.37<br />
−0.19<br />
c,e<br />
NOTE.—Units <strong>of</strong> right ascension are hours, minutes, and seconds, and units <strong>of</strong> declination are degrees, arcminutes, and arcseconds. The units for LX are 10 38 ergs s −1 in the<br />
0.3–10 keV band.<br />
a<br />
Sources near the center may be confused with nearby sources, making their positions, fluxes, and extents uncertain.<br />
b<br />
Source is noticeably more extended than PSF.<br />
c<br />
Source is at the edge <strong>of</strong> the S3 detector, and flux is uncertain because <strong>of</strong> large exposure correction.<br />
d<br />
Possible optical counterpart.<br />
e<br />
Source may be variable.<br />
f<br />
Source is part <strong>of</strong> analysis sample.<br />
71
is, these diffuse features are not due to the smearing <strong>of</strong> point sources.)<br />
3.4 Resolved Sources<br />
3.4.1 Detections<br />
We used a wavelet detection algorithm (the CIAO wavdetect program) with √ 2<br />
scales ranging from 1 to 32 pixels to identify the discrete X-ray source population<br />
on ACIS-S3. Since the wavelet source detection threshold was set at 10 −6 , 1 false<br />
source (due to a statistical fluctuation in the background) is expected in the entire<br />
S3 image. Source detection was first performed on the separate observations to check<br />
their astrometric registration; no significant <strong>of</strong>fset was found. To maximize the S/N,<br />
we analyzed the wavelet detection results from the combination <strong>of</strong> the two observa-<br />
tions. We required our sources to have wavdetect fluxes determined at the ≥3 σ level<br />
for all analyses except the identification <strong>of</strong> possible optical counterparts.<br />
At that level, the minimum detected count rate in the 0.3–6 keV band was 2.7 ×<br />
10 −4 counts s −1 ; however, the bright diffuse gaseous emission at the center <strong>of</strong> the<br />
galaxy makes it difficult to establish a minimum detectable flux over the entire image.<br />
For backgrounds <strong>of</strong> less than 0.05 counts pixel −1 and <strong>of</strong>f-axis distances appropriate<br />
to the S3 chip, sources with 20 counts should be detected at a roughly uniform<br />
completeness level ( 85%; Kim & Fabbiano 2003). For sources satisfying these<br />
criteria, the minimum detected flux was 4.7 × 10 −4 counts s −1 . To determine source<br />
characteristics other than their flux, we used a local background with an area 3 times<br />
that <strong>of</strong> each source’s wavdetect region. In a few cases <strong>of</strong> nearby sources, the source<br />
or background regions initially overlapped. We slightly altered these overlapping<br />
regions, preserving the ratio <strong>of</strong> areas and the net count rates.<br />
72
We also attempted detections in multiple bands (0.3–1, 1–2, and 2–6 keV) and<br />
compared detection rates with the total band (0.3–6 keV). In these sub-bands, 45%,<br />
68%, and 34% <strong>of</strong> the total-band sources were detected, respectively. There were two,<br />
one, and five sources detected in an individual sub-band that were not detected in the<br />
total band. None <strong>of</strong> these extra detections had fluxes that were significant at the ≥3<br />
σ level. Two, eight, and five sources were detected in only one sub-band in addition<br />
to the total band, with two, six, and one <strong>of</strong> those sources having total-band fluxes<br />
determined at ≥3 σ. In this X-ray–bright galaxy, performing detections by sub-bands<br />
provided no advantage.<br />
In Table 3.1 we list all discrete sources detected by wavdetect over the 0.3–6 keV<br />
range. The sources are ordered by increasing projected radial distance d from the<br />
center <strong>of</strong> the galaxy. Columns (1)–(8) provide the source number, the IAU name,<br />
the source position (J2000.0), the projected radial distance and semimajor distance a<br />
from the center <strong>of</strong> NGC 1600, the wavdetect count rate with its 1 σ error, and the S/N<br />
for the count rate. The fluxes were corrected for exposure and the instrument point-<br />
spread function (PSF). The first three sources are clearly extended; when the count<br />
rate was determined using 1. ′′ 5 circular regions centered on the source centroid, none<br />
<strong>of</strong> those sources were significant at the 3 σ level. Although the position <strong>of</strong> source 1 is<br />
close to the optical/IR nucleus <strong>of</strong> NGC 1600, we are not confident that it is a point<br />
source. Therefore, we adopted the 2MASS Point Source Catalog position <strong>of</strong> R.A. =<br />
4 h 31 m 39. s 87, decl. = -5 ◦ 5 ′ 10. ′′ 5 as the location <strong>of</strong> the center <strong>of</strong> NGC 1600. All listed<br />
positions include astrometry corrections based on optical/IR counterparts (§ 3.4.2);<br />
the overall absolute astrometric errors are probably ∼0. ′′ 5 near the field center, with<br />
larger errors farther out.<br />
In addition to the 1 false source in the entire S3 field <strong>of</strong> view, some <strong>of</strong> the de-<br />
73
tected sources may be foreground or (more likely) background objects unrelated to<br />
NGC 1600. If we consider the fluxes <strong>of</strong> all our detected sources, we expect ≈48 unre-<br />
lated sources based on the source counts in Brandt et al. (2000) and Mushotzky et al.<br />
(2000). Using the minimum detected ≥3 σ flux, we expect ≈15 unrelated sources.<br />
Incompleteness will reduce both <strong>of</strong> these estimates, especially the first number. Un-<br />
related sources should be spread out fairly uniformly over the S3 image (Fig. 3.1),<br />
except for the reduced sensitivity at the center due to bright diffuse emission and at<br />
the outer edges <strong>of</strong> the field due to reduced exposure and increased PSF. Sources close<br />
to NGC 1600 are more likely to be associated with the galaxy, while sources far from<br />
NGC 1600 are more likely unrelated to it.<br />
3.4.2 Identifications<br />
Sources in Table 3.1 were cross-correlated against optical/IR catalogs to identify<br />
possible counterparts and to improve the absolute astrometry <strong>of</strong> the observations. We<br />
used the Tycho-2 Catalog (Høg et al. 2000), the 2MASS 10 Point Source and Extended<br />
Source Catalogs, 11 and the USNO-B Catalog (Monet et al. 2003) to identify seven<br />
optical/IR counterparts to the X-ray sources. Four <strong>of</strong> these sources were used to de-<br />
termine the astrometry: source 18 corresponds to USNO-B1 0849−0044132, an R =<br />
19.4 mag object with a non-stellar PSF; source 23 corresponds to NGC 1601, a nearby<br />
lenticular galaxy north <strong>of</strong> NGC 1600; source 33 corresponds to<br />
2MASS 04313613−0503081, a J = 16.8 mag star; and source 50 corresponds to<br />
Tycho-2 4742-254-1, a B = 11.7 mag star. After correcting for an astrometric shift<br />
<strong>of</strong> about 0. ′′ 5, the residual astrometric errors are ≈ 0. ′′ 5.<br />
We did not use the remaining three sources for astrometry since they were as-<br />
10 See http://www.ipac.caltech.edu/2mass/releases/second/doc/explsup.html.<br />
11 When a source appeared in both 2MASS catalogs, the Point Source Catalog positions were used.<br />
74
sociated with extended X-ray or optical emission. The central source (source 1) is<br />
≈0. ′′ 9 from the optical center <strong>of</strong> the galaxy (after the astrometric correction discussed<br />
above). As the X-ray source is extended, we used a 1. ′′ 5 radius circular region cen-<br />
tered on the X-ray source to measure or limit the flux <strong>of</strong> any central point source;<br />
this gave a count rate <strong>of</strong> (7.6 ± 2.9) × 10 −4 counts s −1 (1 σ error bars). Since this<br />
source was neither particularly hard nor detected very significantly as a point source,<br />
we conservatively adopt its 3σ upper limit luminosity <strong>of</strong> 6.7 × 10 39 ergs s −1 as the<br />
upper limit for a central active galactic nucleus (AGN).<br />
Source 40 is ≈1. ′′ 7 from the 2MASS center <strong>of</strong> NGC 1603, a nearby elliptical<br />
galaxy east <strong>of</strong> NGC 1600. There is clearly extended X-ray emission centered east<br />
<strong>of</strong> the source position that appears more coincident with the galaxy center. Since<br />
NGC 1603 extended well beyond this X-ray source (20 mag arcsec −2 isophotal K<br />
fiducial elliptical aperture semimajor axis, r k20fe, <strong>of</strong> 18. ′′ 4), source 40 may be a<br />
point source <strong>of</strong>fset from the center <strong>of</strong> NGC 1603. Similarly, source 63 is ≈2. ′′ 9 from<br />
2MASX 04312667−0507309, a galaxy candidate whose r k20fe is 7. ′′ 2; source 63 may<br />
also be a point source <strong>of</strong>fset from this galaxy’s center. Although source 10 is close to<br />
an optical point source in Figure 3.2, the X-ray source is ≈3. ′′ 4 south <strong>of</strong> the optical<br />
object; thus, we do not consider this to be a reliable optical identification for the<br />
X-ray source.<br />
3.4.3 X-ray Luminosities and Luminosity Functions<br />
To convert the source count rates into unabsorbed X-ray luminosities, we used<br />
the adopted Chandra X-ray spectrum (§ 3.6.1; Table 3.2, row [3]) <strong>of</strong> the resolved<br />
sources to convert 0.3–6 keV count rates into 0.3–10 keV flux. We then assumed<br />
each source was at the distance <strong>of</strong> NGC 1600, 59.98 Mpc, yielding a conversion factor<br />
75
<strong>of</strong> 4.12 × 10 42 ergs count −1 . Column (8) <strong>of</strong> Table 3.1 lists the X-ray luminosities in<br />
units <strong>of</strong> 10 38 ergs s −1 , which range roughly from 2.8 × 10 38 to 4.8 × 10 40 ergs s −1 .<br />
Since sources 33 and 50 are likely foreground stars, their luminosities are probably<br />
overestimates.<br />
By restricting the sample to the sources with a uniform completeness <strong>of</strong> 85%<br />
(≥20 net counts, implying a count rate limit ≥ 4.7 × 10 −4 counts s −1 , and d > 40 ′′<br />
corresponding to a background 0.05 counts pixel −1 ; § 3.4.1), excluding the sources<br />
corresponding to NGC 1601 (source 23) and NGC 1603 (source 40), and excluding<br />
the very bright source corresponding to a foreground Tycho star (source 50), we<br />
created our analysis sample <strong>of</strong> 20 sources (see notes in Table 3.1). We expect 11 ± 2<br />
foreground/background sources based on the source counts in Brandt et al. (2000)<br />
and Mushotzky et al. (2000).<br />
In Figure 3.3 we display the cumulative luminosity function (LF) <strong>of</strong> our analy-<br />
sis sample. The LF should be the sum <strong>of</strong> the point source (LMXB) population <strong>of</strong><br />
NGC 1600 and the foreground/background population. We fit the LF using the same<br />
techniques we have used previously (Sarazin et al. 2000, 2001; Irwin et al. 2002); a<br />
single power law, a broken power law, and a cut<strong>of</strong>f power law were all used to model<br />
the LMXB population. The background source population was modeled as discussed<br />
in the previous references. A single power law fits the data very well based on the<br />
Kolmogorov-Smirnov (K-S) test:<br />
dN<br />
dL39<br />
76<br />
= N0L −α<br />
39 , (3.1)<br />
where L39 ≡ LX/(10 39 ergs s −1 ). The best fit was determined by the maximum<br />
likelihood method, and the errors (90% confidence interval) were determined by Monte<br />
Carlo techniques. We found N0 = 21.1 +73.0<br />
−10.0 and α = 2.00 +1.14<br />
−0.35. Although a cut<strong>of</strong>f
Fig. 3.3.— Histogram <strong>of</strong> the observed cumulative LF <strong>of</strong> resolved sources in our analysis<br />
sample. The continuous curve is the sum <strong>of</strong> the best-fit LMXB LFs (eq. 3.1) and<br />
the expected background source counts. The vertical line indicates the completeness<br />
limit <strong>of</strong> our sample.<br />
power law is not required by the fits, the total luminosity <strong>of</strong> all <strong>of</strong> the sources diverges<br />
at the high-luminosity limit for the best-fit LF. The lack <strong>of</strong> very bright sources (beyond<br />
those observed) in NGC 1600 can be explained by Poisson fluctuations; however, it<br />
seems likely either that the correct underlying LF <strong>of</strong> the sources in NGC 1600 is a bit<br />
steeper than the best-fit value or that it steepens or has a cut-<strong>of</strong>f at high luminosities<br />
beyond those observed.<br />
Early-type galaxies tend to have broken or cut<strong>of</strong>f power-law LFs with the break<br />
or cut<strong>of</strong>f occurring well below the luminosities measured in NGC 1600, while star-<br />
forming galaxies tend to have single power-law LFs that extend to low luminosities<br />
(Sarazin et al. 2001; Blanton et al. 2001; Finoguenov & Jones 2002; Zezas & Fabbiano<br />
2002; Jeltema et al. 2003; Chapter 2; Randall et al. 2004). The high luminosities <strong>of</strong><br />
the sources in NGC 1600 make it difficult to directly compare its LF with those <strong>of</strong><br />
77
other galaxies. Therefore, one must either extrapolate the NGC 1600 LF down to<br />
lower luminosities or extrapolate the LF <strong>of</strong> other galaxies to higher luminosities in<br />
order to compare them. The differential LF slopes at the highest luminosities in early-<br />
type galaxies tend to be steeper than 2.5 and tend to cluster around 1.5 in galaxies<br />
with some level <strong>of</strong> star formation. The best-fit slope <strong>of</strong> NGC 1600 is intermediate<br />
between the two; however, within the errors, the slope is more consistent with the<br />
other early-type galaxies. The normalization <strong>of</strong> NGC 1600 is higher by at least a<br />
factor <strong>of</strong> 4 than that <strong>of</strong> any <strong>of</strong> the galaxies in the above references. Extrapolating the<br />
best-fit LF, we would find ∼40 and ∼420 sources above 5×10 38 and 5×10 37 ergs s −1 ,<br />
respectively, a typical break luminosity and typical minimum observed luminosity in<br />
other early-type galaxies. If there is a break in the LF below 2 × 10 39 ergs s −1 , the<br />
numbers <strong>of</strong> fainter sources would be reduced.<br />
Only one <strong>of</strong> the sources in the analysis sample is fainter than 2 × 10 39 ergs s −1 .<br />
There are six additional sources that could qualify as ULX candidates, sources 1–<br />
3, 7, 52, and 71. Since sources 1–3 appear extended, we used a 1. ′′ 5 radius circular<br />
region to measure the flux <strong>of</strong> a possible point source. The count rates <strong>of</strong> sources<br />
1 and 2 are sufficient to qualify as ULX candidates; however, their fluxes are not<br />
determined at the 3 σ limit. Of the remaining candidates, only sources 7 and 71 are<br />
ULX candidates with well-determined fluxes. Source 7 is not included in the analysis<br />
sample, since it is only 35. ′′ 2 from the nucleus <strong>of</strong> NGC 1600. Source 71, a source at the<br />
edge <strong>of</strong> the chip, did not make it into the analysis sample because <strong>of</strong> its small number<br />
<strong>of</strong> counts, ∼17; its luminosity is boosted by a large exposure correction. Including<br />
sources 7 and 71, we observe 21 ULX candidates. At the flux limit corresponding to<br />
LX = 2 × 10 39 ergs s −1 , we expect 11 ± 2 foreground/background sources based on<br />
the source counts in Brandt et al. (2000) and Mushotzky et al. (2000) for the entire<br />
78
chip. The number <strong>of</strong> ULX candidates in excess <strong>of</strong> the expected background is 10 ± 5.<br />
Even if we consider sources with LX > 4×10 39 ergs s −1 , there are 10 ULX candidates<br />
and only approximately five unrelated foreground/background sources are expected.<br />
This corresponds to an excess <strong>of</strong> 5 ± 3.3. 12 The error budgets <strong>of</strong> both excesses are<br />
dominated by Poisson counting errors in NGC 1600.<br />
In a sample <strong>of</strong> 28 early-type galaxies, the number <strong>of</strong> sources with LX ≥ 2 ×<br />
10 39 ergs s −1 (0.3–10 keV) was equivalent to the expected number <strong>of</strong><br />
foreground/background sources (Irwin et al. 2004). 13 Although the number <strong>of</strong> ULX<br />
candidates is greater than the average number <strong>of</strong> unrelated sources, the number<br />
<strong>of</strong> ULX candidates in NGC 1600 could be a result <strong>of</strong> cosmic variance in the fore-<br />
ground/background sources. One item in support <strong>of</strong> this possibility is that the fitted<br />
slope <strong>of</strong> the LF is consistent with the typical slopes <strong>of</strong> foreground/background LFs<br />
(Brandt et al. 2001; Giacconi et al. 2001). To examine the possibility <strong>of</strong> cosmic<br />
variance, we compared the source densities we observed to the 0.5–2.0 keV source<br />
densities <strong>of</strong> the Chandra Deep Fields. 14<br />
Within two D25 (a ≤ 147. ′′ 3, where D25 is the diameter at which the surface<br />
brightness is 25 mag arcsec −2 ), the observed source density <strong>of</strong> ULX candidates in<br />
NGC 1600 is 2250 ± 796 deg −2 , while the remaining field <strong>of</strong> the S3 chip has a source<br />
density <strong>of</strong> 884 ± 245 deg −2 . In order to compare the background source densities<br />
with those in Brandt et al. (2001) and Giacconi et al. (2001), we converted our count<br />
rates to energy fluxes in the 0.5–2.0 keV band using a Γ = 1.4 power-law spectrum.<br />
Then, the minimum detectable 0.5–2.0 keV flux for our observation <strong>of</strong> NGC 1600 is<br />
12 We use √ N statistics since they better represent the true low-count Poisson lower limit 1 σ<br />
confidence level than the Gehrels approximation <strong>of</strong> 1 + (N + 0.75) 1/2 (cf. eqs. [7] and [11] and Table<br />
2 in Gehrels (1986)).<br />
13 This study used surface brightness fluctuation distances that are consistent with H0 = 74 ±<br />
4 km s −1 Mpc −1 (Tonry et al. 2001).<br />
14 We chose to use the 0.5–2.0 keV band, since all but one <strong>of</strong> the ULX candidates were detected<br />
in s<strong>of</strong>t as well as hard bands.<br />
79
1.36×10 −15 ergs cm −2 s −1 . The Chandra Deep Fields predict foreground/background<br />
source densities <strong>of</strong> ∼690±260 deg −2 (North) and 520±110 deg −2 (South). Assuming<br />
a background source density <strong>of</strong> 600 ± 100 deg −2 , there is an ∼2.1σ excess within 2D25<br />
<strong>of</strong> the galaxy corresponding to an excess <strong>of</strong> ∼6 ± 3 sources. The errors are dominated<br />
by counting errors in NGC 1600 as opposed to uncertainty in the background source<br />
density. The excess near the galaxy favors an association <strong>of</strong> ULX candidates with<br />
NGC 1600; however, cosmic variance cannot be ruled out.<br />
When one subdivides the ULX candidates into a fainter sample LX = (2–4) ×<br />
10 39 ergs s −1 and a brighter sample, LX > 4 × 10 39 ergs s −1 , we find that the brighter<br />
sample source densities are more consistent with the background than the fainter<br />
sample. In particular, there are no sources in the bright sample, which has better<br />
completeness than the faint sample, within 2 effective radii; in the faint sample, there<br />
are four sources. One possible explanation is that the overabundance <strong>of</strong> the bright<br />
ULX candidates is due to cosmic variance <strong>of</strong> foreground/background sources, while<br />
the overabundance <strong>of</strong> the faint ULX candidates is from sources within NGC1600.<br />
The ULX candidates could then be brought more in line with the findings <strong>of</strong> Ir-<br />
win et al. (2004) by a coincidence <strong>of</strong> cosmic variance and an ∼40% overestimate in<br />
the distance to NGC 1600. Such large differences do occasionally occur between re-<br />
cessional velocity distances and surface brightness fluctuation distances; however, in<br />
the case <strong>of</strong> NGC 1600, this would require NGC 1600 to have a peculiar velocity <strong>of</strong><br />
∼ +1300km s −1 . Since this peculiar velocity is more typical <strong>of</strong> cluster infall and there<br />
is no nearby large cluster, we do not think this model is likely.<br />
If cosmic variance does not explain the excess number <strong>of</strong> bright sources, then these<br />
bright sources are actually ULX candidates associated with NGC 1600. NGC 1399<br />
has three sources with LX ≥ 2 × 10 39 ergs s −1 , the largest number <strong>of</strong> sources at<br />
80
these luminosities among previously observed early-type galaxies. NGC 1407 may<br />
have five such sources; however, its distance is highly uncertain (Irwin et al. 2003).<br />
Although Jeltema et al. (2003) find that NGC 720 has nine ULX candidates, only<br />
one has a luminosity ≥2 × 10 39 ergs s −1 for H0 = 75 km s −1 Mpc −1 . Thus, we<br />
believe that NGC 1600 may have the largest number <strong>of</strong> ULX candidates brighter<br />
than 2 × 10 39 ergs s −1 observed in an early-type galaxy to date.<br />
There are a variety <strong>of</strong> models explaining the presence <strong>of</strong> ULX sources. Some <strong>of</strong><br />
these include favorable viewing angles <strong>of</strong> anisotropic radiation (King et al. 2001),<br />
super-Eddington accretion by high-mass X-ray binaries (HMXBs) at the thermal-<br />
timescale mass transfer rate (King 2002), accretion onto intermediate-mass black<br />
holes (Colbert & Mushotzky 1999), super-Eddington accretion <strong>of</strong> LMXBs in the s<strong>of</strong>t<br />
X-ray transient state (King 2002), and super-Eddington accretion from thin accretion<br />
disks <strong>of</strong> stellar mass black holes (Begelman 2002). If anisotropic radiation were the<br />
cause <strong>of</strong> ULXs in NGC 1600, one would predict the existence <strong>of</strong> a large population<br />
<strong>of</strong> ULXs seen at fainter fluxes, due to misalignment with the preferred axis <strong>of</strong> the<br />
anisotropic radiation, in addition to the intrinsically faint and isotropic radiating<br />
LMXB populations; our observation does not go deep enough to observe such sources.<br />
Since NGC 1600 has an observed age <strong>of</strong> 7.3 Gyr (Terlevich & Forbes 2002) and<br />
its photometric colors (Sandage 1973; Frogel et al. 1978) are typical for an elliptical<br />
galaxy, one would not expect its X-ray binaries to be HMXBs. Comparisons <strong>of</strong> the<br />
far-IR detections <strong>of</strong> NGC 1600 from IRAS in the 60 and 100 µm bands with the<br />
radio flux (Birkinshaw & Davies (1985)) could be consistent with either AGN or<br />
stellar heating <strong>of</strong> interstellar dust (Condon & Broderick 1991). Trinchieri & di Serego<br />
Alighieri (1991) and Ferrari et al. (1999) both found that post-AGB stars are the<br />
likely source <strong>of</strong> the ionization <strong>of</strong> the gas and heating <strong>of</strong> the dust in NGC 1600. Thus,<br />
81
the far-IR detections do not necessarily indicate that there is recent star formation,<br />
as needed for HMXBs. In addition, the cumulative spectrum <strong>of</strong> the ULX candidates<br />
in NGC 1600 is not consistent with the disk blackbody model found to fit well in<br />
ULXs associated with spiral galaxies (Makishima et al. 2000).<br />
Intermediate-mass black holes may be created if the progenitor mass <strong>of</strong> a star is<br />
40 M⊙ (Fryer & Kalogera 2001) and that star sinks to the center <strong>of</strong> a GC, where<br />
it can grow up to ∼10 3 M⊙ in 10 10 years (Miller & Hamilton 2002). Under this<br />
model, NGC 1600 would be expected to have a large number <strong>of</strong> GCs. The LMXB-<br />
GC connection in early-type galaxies (Sarazin et al. 2000, 2001; Angelini et al. 2001;<br />
Kundu et al. 2003; Sarazin et al. 2003) means that LMXBs in the s<strong>of</strong>t X-ray transient<br />
state or black hole LMXBs with thin accretion disks would also be consistent with<br />
a large number <strong>of</strong> GCs. Thus, it seems plausible that the large population <strong>of</strong> ULXs<br />
in NGC 1600, if it is not due to cosmic variance in the number <strong>of</strong> unrelated sources,<br />
requires a large population <strong>of</strong> GCs. Unfortunately, the GC population <strong>of</strong> NGC 1600<br />
does not appear to have been determined.<br />
3.4.4 Hardness Ratios<br />
Hardness ratios or X-ray colors are useful for crudely characterizing the spectral<br />
properties <strong>of</strong> sources and can be applied to sources that are too faint for detailed<br />
spectral analysis. We determined the observed X-ray hardness ratios for the sources,<br />
using the same techniques we used previously (Sarazin et al. 2000, 2001; Blanton et al.<br />
2001; Irwin et al. 2002). We define three hardness ratios as H21 ≡ (M − S)/(M + S),<br />
H31 ≡ (H − S)/(H + S), and H32 ≡ (H − M)/(H + M), where S, M, and H are the<br />
total counts in the s<strong>of</strong>t (0.3–1 keV), medium (1–2 keV), and hard (2–6 keV) bands,<br />
respectively. From our previous definitions, we have reduced the hard band from 2–10<br />
82
to 2–6 keV. Since the 6–10 keV range is dominated by background photons for most<br />
sources, this should increase the S/N <strong>of</strong> the hardness ratio techniques. The hardness<br />
ratios measure observed counts, which are affected by Galactic absorption and QE<br />
degradation in the Chandra ACIS detectors. In order to compare with other galaxies,<br />
it is useful to correct the hardness ratios for these two s<strong>of</strong>t X-ray absorption effects.<br />
Therefore, we have calculated the intrinsic hardness ratios, denoted by a superscript<br />
0, using a correction factor in each band appropriate to the best-fit spectrum <strong>of</strong><br />
the resolved sources. The intrinsic hardness ratios and their 1 σ errors are listed in<br />
columns (10)–(12) <strong>of</strong> Table 3.1.<br />
Although we have plotted H31 versus H21 in the past, plots <strong>of</strong> H32 versus H21<br />
allow for better separation <strong>of</strong> simple spectral models. In Figure 3.4 we plot both<br />
H31 0 versus H21 0 and H32 0 versus H21 0 for the 20 sources in the analysis sample.<br />
The hardness ratios for the sum <strong>of</strong> those sources are (H21 0 , H32 0 , H31 0 ) = (−0.26,<br />
−0.39, −0.59); the uncorrected hardness ratios are (H21, H32, H31) = (+0.11,<br />
−0.33, −0.24). Sources with ∼40 net counts had errors similar to the median <strong>of</strong> the<br />
uncertainties, ∼0.2. The errors scale roughly with the inverse square root <strong>of</strong> the net<br />
counts.<br />
In previously studied galaxies, most <strong>of</strong> the sources lie along a broad diagonal<br />
swath extending roughly from (H21, H31) ∼ (−0.3, −0.7) to (0.4, 0.5). Usually,<br />
these hardness ratios were not corrected for Galactic absorption and QE degradation;<br />
the latter effect was not known at the time <strong>of</strong> some <strong>of</strong> the previous studies. Since there<br />
are fewer sources and the absorption/degradation corrections tend to push sources<br />
to the lower left part <strong>of</strong> the diagram, this swath is less evident in NGC 1600. In<br />
Figure 3.4 the solid line corresponds to hardness ratios for power-law source spectra<br />
with Γ =0–3.2. In calculating these model hardness ratios, Galactic absorption and<br />
83
Fig. 3.4.— Hardness ratios for the sources in our analysis sample. Here, H21 0 ≡<br />
(M 0 −S 0 )/(M 0 +S 0 ), H31 0 ≡ (H 0 −S 0 )/(H 0 +S 0 ), and H32 0 ≡ (H 0 −M 0 )/(H 0 +M 0 ),<br />
where S 0 , M 0 , and H 0 are the counts in the s<strong>of</strong>t (0.3–1 keV), medium (1–2 keV),<br />
and hard (2–6 keV) bands, corrected for the effect <strong>of</strong> Galactic absorption and QE<br />
degradation according to the best-fit spectra <strong>of</strong> resolved sources. The area <strong>of</strong> each<br />
circle is proportional to the observed number <strong>of</strong> net counts. The solid curve and<br />
large diamonds show the hardness ratios for power-law spectral models; the dashed<br />
curve and small diamonds show the ratios for intrinsic absorption <strong>of</strong> NH = 4 × 10 21<br />
cm −2 ; the diamonds indicate values <strong>of</strong> the power-law photon number index <strong>of</strong> Γ = 0<br />
(upper right) to 3.2 (lower left) in increments <strong>of</strong> 0.4. Both models underwent the same<br />
correction as the sources. The 1 σ error bars at the upper left illustrate the median<br />
<strong>of</strong> the uncertainties.<br />
QE degradation were applied to the model spectra, and the hardness ratios were<br />
corrected for these effects using the best-fit spectral model <strong>of</strong> the resolved sources as<br />
described above. The dashed line corresponds to a similar model, with an intrinsic<br />
absorbing column <strong>of</strong> 4 × 10 21 cm −2 . Most <strong>of</strong> the sources are consistent with Γ =1.6–<br />
2.2, with the sum <strong>of</strong> these sources corresponding to Γ ≈ 1.7. The majority <strong>of</strong> the<br />
sources lie roughly between the two models in H31 0 versus H21 0 . In H32 0 versus<br />
H21 0 , we see that most <strong>of</strong> the sources have an H32 0 ∼ −0.5, but the two models<br />
still roughly contain the sources. When compared to the H31 0 versus H21 0 plot,<br />
the effects <strong>of</strong> absorption in the H32 0 versus H21 0 plot are larger, and the effects <strong>of</strong><br />
84
absorption and varying power-law index are more nearly orthogonal. Although it is<br />
suggestive that the sources tend to lie on one <strong>of</strong> the two tracks, the errors are large<br />
and the number <strong>of</strong> the sources is small, so this could be a coincidence.<br />
In NGC 4697 and the bulge <strong>of</strong> NGC 1291, a total <strong>of</strong> four sources had (H21,<br />
H31) ≈ (−1, −1). Scaling from the number <strong>of</strong> sources in NGC 4697, one would have<br />
expected only approximately two supers<strong>of</strong>t sources in NGC 1600, so the lack <strong>of</strong> any<br />
strong candidates is not surprising. Moreover, the supers<strong>of</strong>t sources in NGC 4697<br />
would all have been below our detection limit at the distance <strong>of</strong> NGC 1600. Another<br />
problem is that the s<strong>of</strong>t X-ray response <strong>of</strong> the Chandra ACIS-S3 detector was much<br />
worse at the time NGC 1600 was observed because <strong>of</strong> QE degradation. 15 Although<br />
the hardness ratios are corrected for this effect, the correction is based on the average<br />
(hard) spectrum <strong>of</strong> the sources; this correction would be too small for supers<strong>of</strong>t<br />
sources. Supers<strong>of</strong>t sources in NGC 1600 would have been difficult to detect unless<br />
they were very bright.<br />
Among the sources with known fluxes <strong>of</strong> more than 3σ, we find three sources (42,<br />
58, and 60) with very hard spectra, (H21 0 ,H31 0 ) > (0.5, 0.5), and three sources (17,<br />
36, and 50) with little hard emission, H31 0 ∼ −1.0. The very hard sources may<br />
be unrelated, strongly absorbed AGNs, similar to the sources that produce the hard<br />
component <strong>of</strong> the X-ray background and that appear strongly at the faint fluxes in the<br />
deep Chandra observations <strong>of</strong> blank fields (Brandt et al. 2000; Mushotzky et al. 2000;<br />
Giacconi et al. 2001); however, all three sources have large hardness ratio errors. The<br />
sources without hard emission may also be unrelated foreground/background sources,<br />
as indicated by studies <strong>of</strong> other galaxies (Sarazin et al. 2001) and deep blank-sky<br />
images (e.g., Giacconi et al. 2001); source 50 (see § 3.4.2) is clearly a foreground<br />
object, while source 36 has large hardness ratio errors.<br />
15 See footnote 9.<br />
85
The hardness ratios <strong>of</strong> sources 1–3 are s<strong>of</strong>ter than a majority <strong>of</strong> the sources in the<br />
analysis sample; however the errors <strong>of</strong> sources 2 and 3 could bring them more in line<br />
with the analysis sample. Since these extended sources appear s<strong>of</strong>ter, it is more likely<br />
that they are small-scale structures in the diffuse gas (see § 3.5.2) than that they are<br />
a number <strong>of</strong> confused sources.<br />
3.4.5 Variability<br />
With two observations we could test for variability on two time scales, intraob-<br />
servation, and interobservation. Since the midpoints <strong>of</strong> the observations were only<br />
∼60 ks apart, the timescales are not remarkably different. We searched for variabil-<br />
ity in the X-ray emission <strong>of</strong> the resolved sources over the duration <strong>of</strong> the Chandra<br />
observations individually and jointly using the K-S test (see Sarazin et al. 2001). In<br />
addition, we compared the count rates between the two observations. In Table 3.1<br />
we report the sources that had a more than 95% variability probability in any one <strong>of</strong><br />
these four tests. Among the 43 sources away from the edge <strong>of</strong> the chip detected with<br />
3 σ flux, sources 1, 8, 24, 30, and 59 were apparently variable. Source 1 had a 2.1 σ<br />
(96% probability) rate decline in count rate between the two observations; however,<br />
the variability was not significantly detected within the individual observations. This<br />
suggests that there may be a point source variable on a timescale more than 20 ks<br />
buried in the diffuse emission <strong>of</strong> this extended source. The flux in a 1. ′′ 5 circular re-<br />
gion centered on the position <strong>of</strong> source 1, which includes the galaxy center, is nearly<br />
constant between the two observations. This suggests that the buried variable point<br />
source, if it exists, is not a central AGN. For source 8, the K-S test on the joint<br />
observations yielded a 95% probability <strong>of</strong> variability. Source 24 shows a variability<br />
at the 99% probability in the first observation; in this observation, six <strong>of</strong> its seven<br />
86
counts occur within ∼ 4 ks. Source 30 undergoes a 2.0 σ (95% probability) rate<br />
increase between the two observations. Finally, source 59 has a 98% probability <strong>of</strong><br />
being variable in the joint observation K-S test. With 43 sources, approximately two<br />
false positives are expected at a more than 95% limit. Of the four sources variable at<br />
this limit, sources 24 and 59 show the strongest behavior <strong>of</strong> variability, both in the<br />
form <strong>of</strong> outbursts. Although source 71 shows 95% variability in the first observation,<br />
its light curve is irregularly sampled because <strong>of</strong> its location at the edge <strong>of</strong> the chip.<br />
Source 13, a weakly detected source, had a very high variability probability, 99%, in<br />
the second observation, since all three counts in that observation occurred in the last<br />
750 seconds. The remaining weak sources that are marked as potentially variable did<br />
not exhibit such clearly variable behavior as did Source 13.<br />
3.5 Unresolved X-ray Emission<br />
As mentioned in § 3.3, the morphology <strong>of</strong> the unresolved X-ray emission is com-<br />
plex. This emission is a combination <strong>of</strong> unresolved point sources and diffuse gaseous<br />
emission. Ideally, we would like to use the spectral properties <strong>of</strong> the gas and resolved<br />
sources (see § 3.6) to disentangle the two as in Sarazin et al. (2001) and Chapter 2;<br />
however, the changing diffuse gas temperature <strong>of</strong> NGC 1600 does not allow this sep-<br />
aration. For this reason, we chose to use the entire 0.3–6 keV band in analyzing the<br />
unresolved emission <strong>of</strong> NGC 1600. From the spectral fits, we estimate that unresolved<br />
point sources contribute ∼30% <strong>of</strong> the total unresolved counts. For comparisons with<br />
previous studies, we left in resolved sources with S/N < 3. As source 1 may be the<br />
peak <strong>of</strong> the unresolved emission, we did not exclude it. Since sources 2 and 3 were<br />
extended, we only excluded regions corresponding to 1. ′′ 5 circular regions located at<br />
their centers. We used the blank-sky background to statistically remove background<br />
87
events.<br />
3.5.1 Radial Pr<strong>of</strong>ile <strong>of</strong> the Unresolved X-ray Emission<br />
In order to compare the spatial distribution <strong>of</strong> the unresolved X-ray emission in<br />
NGC 1600 with the optical emission by stars, we adopted the Third Reference Cat-<br />
alogue <strong>of</strong> Bright Galaxies (RC3) values for the optical photometry’s effective radius<br />
(reff = 45. ′′ 4), position angle (P.A. = 15), and ellipticity (e = 0.324), which assumes<br />
a de Vaucouleurs pr<strong>of</strong>ile (RC3). The corresponding semimajor axis aeff is 55. ′′ 2. Al-<br />
though Rembold et al. (2002) find a different pr<strong>of</strong>ile in the infrared (a Sérsic pr<strong>of</strong>ile<br />
with n ∼ 1–2, an effective radius <strong>of</strong> ∼10 ′′ –15 ′′ , a semimajor axis P.A. ∼10–20, and<br />
ellipticity <strong>of</strong> 0.17–0.34), the values <strong>of</strong> the P.A. and ellipticity are roughly consistent<br />
with the optical pr<strong>of</strong>ile. The corresponding semimajor axis is 17. ′′ 6 using the optical<br />
ellipticity. Since the effective radius is only used for scaling in this chapter, the large<br />
discrepancy between the two radii does not make a difference in our study.<br />
We determined the surface brightness pr<strong>of</strong>ile (SBP; Fig. 3.5) and the hardness<br />
ratios (Fig. 3.6) for a series <strong>of</strong> elliptical annuli with semimajor widths <strong>of</strong> 5 ′′ , extending<br />
to 180 ′′ . We could have used much narrower annuli near the center <strong>of</strong> NGC 1600, but<br />
there is significant non-axially symmetric structure in the image there (§ 3.5.2). In the<br />
SBP, the dotted line displays the (optical) best-fit de Vaucouleurs pr<strong>of</strong>ile with effective<br />
semimajor axis fixed at 55. ′′ 2 and the dashed line displays the (J band) best-fit Sérsic<br />
n = 1.65 pr<strong>of</strong>ile with the effective semimajor axis fixed at 17. ′′ 6. The normalizations<br />
<strong>of</strong> the optical pr<strong>of</strong>iles were varied to achieve the best fit. It is clear that neither the<br />
optical nor the infrared pr<strong>of</strong>ile fits the unresolved X-ray emission well.<br />
88
log I X (counts/sec/arcmin 2 )<br />
0.5<br />
0.0<br />
-0.5<br />
-1.0<br />
-1.5<br />
-2.0<br />
-2.5<br />
0.0 0.5 1.0<br />
log a (arcsec)<br />
1.5 2.0<br />
NGC 1600<br />
Fig. 3.5.— SBPs, with 1 σ error bars, <strong>of</strong> the unresolved emission (0.3–6 keV) as a<br />
function <strong>of</strong> projected semimajor axis a. The dotted and dashed curves show the de<br />
Vaucouleurs pr<strong>of</strong>ile (RC3) and J-band Sérsic pr<strong>of</strong>ile, respectively, with fixed effective<br />
radii and normalizations varied to fit the X-ray surface brightness. The solid curve is<br />
the best-fit double beta model pr<strong>of</strong>ile. All fits were for a < 180 ′′ .<br />
We first tried to fit the SBP using a single-beta model pr<strong>of</strong>ile,<br />
89<br />
<br />
2<br />
−3β+1/2<br />
a<br />
IX(a) = I0 1 +<br />
, (3.2)<br />
where ac is the core semimajor axis. However, that model was clearly rejected with a<br />
χ 2 <strong>of</strong> 431 for 33 degrees <strong>of</strong> freedom (d<strong>of</strong>). The best-fit single-beta model has a small<br />
core radius ac, leading to essentially a power-law model. The model underestimates<br />
the emission in the inner 20 ′′ and beyond 90 ′′ while overestimating the emission be-<br />
tween 20 ′′ and 60 ′′ . Figure 3.5 clearly shows that there are at least two components<br />
to the X-ray SBP <strong>of</strong> NGC 1600. Thus, we tried to fit the SBP with a double beta<br />
ac
Fig. 3.6.— Hardness ratios with 1 σ error bars for the unresolved emission as a<br />
function <strong>of</strong> semimajor axis a. Here, H21 ≡ (M −S)/(M +S), H31 ≡ (H−S)/(H+S),<br />
and H32 ≡ (H − M)/(H + M), where S, M, and H are the observed counts in the<br />
s<strong>of</strong>t (0.3–1 keV), medium (1–2 keV), and hard (2–6 keV) bands.<br />
model:<br />
<br />
a<br />
IX(a) = I0,inner 1 +<br />
ac,inner<br />
<br />
2<br />
−3βinner+1/2 <br />
a<br />
+ I0,outer 1 +<br />
ac,outer<br />
2 −3βouter+1/2<br />
90<br />
.<br />
(3.3)<br />
The core radius <strong>of</strong> the outer component ac,outer is poorly determined and consis-<br />
tent with zero. That is, the outer part <strong>of</strong> the SBP could be fitted by a power-<br />
law surface brightness; however, a pure power-law form would produce a peak in<br />
the X-ray SBP at the very center which is not seen in the image. Therefore, we<br />
chose to freeze the outer core semimajor axis at 25 ′′ . We then found I0,inner =<br />
0.97 +0.08<br />
−0.07 counts s −1 arcmin −2 , ac,inner = 14.4 +3.3<br />
−2.3 arcsec (4.2 kpc in projection), βinner =<br />
1.18 +0.33<br />
−0.20, I0,outer = 0.039 +0.005<br />
−0.005 counts s −1 arcmin −2 , ac,outer ≡ 25. ′′ 0 (7.3 kpc in projec-
tion), and βouter = 0.36 +0.01<br />
−0.01. The values <strong>of</strong> this fit were consistent with the error bars<br />
from the double beta model pr<strong>of</strong>ile with a free outer core semimajor axis, and the χ 2<br />
<strong>of</strong> this fit, 39.0 for 30 d<strong>of</strong>, was only 0.9 higher. Therefore, we adopted this fit, the<br />
solid line in Figure 3.6, as the best-fit SBP model. To ensure that the inclusion <strong>of</strong><br />
source 1 did not affect the fit, we attempted to fit the same model without using the<br />
first annulus. The new fit was within the error bars <strong>of</strong> the above fit.<br />
A β <strong>of</strong> 1.18 is much larger than in most X-ray–bright galaxies (Forman et al.<br />
1985; Trinchieri et al. 1986). However, these previous fits were done with a single<br />
beta model and on much poorer resolution data. Below, we argue that the inner<br />
beta model component <strong>of</strong> the SBP is interstellar gas in NGC 1600, while the outer<br />
beta model component is intragroup gas. It may be that the intragroup medium has<br />
compressed the galactic gas, decreasing the value <strong>of</strong> ac and steepening the pr<strong>of</strong>ile<br />
(increasing β).<br />
Figure 3.6 shows the pr<strong>of</strong>iles <strong>of</strong> the hardness ratios for the unresolved emission. As<br />
was true for the SBP, the hardness ratio pr<strong>of</strong>iles show a break in behavior at a ∼ 25 ′′ .<br />
The inner regions <strong>of</strong> the galaxy are noticeably s<strong>of</strong>ter than the outer regions. It is<br />
unlikely that this trend is due to unresolved stellar point sources. The optical pr<strong>of</strong>ile<br />
<strong>of</strong> the galaxy is more centrally condensed than the X-ray SBP (Fig. 3.6), so unresolved<br />
stellar sources should contribute more in the inner regions. Yet, the average spectrum<br />
<strong>of</strong> the resolved sources is much harder than any <strong>of</strong> the diffuse emission and would not<br />
cause the central regions <strong>of</strong> the diffuse emission to be s<strong>of</strong>ter. A positive temperature<br />
gradient and/or abundance gradient in the diffuse gas in the inner regions is the likely<br />
cause for the s<strong>of</strong>ter emission; in § 3.6.2, we show that the X-ray spectra do indicate<br />
that this change in the hardness is due to a temperature gradient.<br />
91
02:30<br />
-5:03:00<br />
30<br />
-5:04:00<br />
30<br />
-5:05:00<br />
30<br />
-5:06:00<br />
30<br />
-5:07:00<br />
4:31:50 48 46 44 4:31:40 38 36 34 32<br />
30<br />
02:30<br />
-5:03:00<br />
30<br />
-5:04:00<br />
30<br />
-5:05:00<br />
30<br />
-5:06:00<br />
30<br />
-5:07:00<br />
4:31:50 48 46 44 4:31:40 38 36 34 32<br />
30<br />
02:30<br />
-5:03:00<br />
30<br />
-5:04:00<br />
30<br />
-5:05:00<br />
30<br />
-5:06:00<br />
30<br />
-5:07:00<br />
4:31:50 48 46 44 4:31:40 38 36 34 32<br />
30<br />
Fig. 3.7.— Left: Adaptively smoothed Chandra S3 image (0.3–6 keV) <strong>of</strong> NGC 1600,<br />
with sources removed and corrected for exposure and background. The gray scale<br />
is logarithmic and ranges from 1 × 10 −6 to 2.9 × 10 −4 counts arcsec −2 s −1 . Middle:<br />
Image on the left minus the best-fit double-beta model SBP. The gray scale is also<br />
logarithmic and ranges from 5 × 10 −7 to 1.4 × 10 −4 counts arcsec −2 s −1 . Right: Image<br />
<strong>of</strong> the hardness ratio H41 ≡ (H + M − S)/(H + M + S), Gaussian smoothed with<br />
σ = 5 ′′ . The gray scale is linear and ranges from −0.4 (black) to 0.4 (white). In each<br />
image, a cross marks the center <strong>of</strong> NGC 1600.<br />
3.5.2 Structural Features in the Unresolved X-ray Emission<br />
In Figure 3.7 we display images in which the resolved sources were replaced by the<br />
appropriate local Poisson noise. In each image, a cross marks the center <strong>of</strong> NGC 1600.<br />
On the left, we display the adaptively smoothed image <strong>of</strong> the total X-ray emission<br />
(0.3–6 keV) with logarithmic gray scale ranging from 1 × 10 −6 to 2.9 × 10 −4 counts<br />
arcsec −2 s −1 . From this image, we subtracted the double-beta elliptical SBP; the<br />
excess emission image is shown in Figure 3.7 (middle) with both limits <strong>of</strong> the gray<br />
scale reduced by a factor <strong>of</strong> two. The tail extending from NGC 1603 in the west toward<br />
NGC 1600 is shown clearly. This image shows extended, diffuse emission around both<br />
<strong>of</strong> the smaller galaxies NGC 1601 and NGC 1603. There is some interesting residual<br />
structure near the center <strong>of</strong> NGC 1600, which is discussed in more detail below<br />
(§ 3.5.3). The structure near the center includes an excess emission region to the<br />
west <strong>of</strong> the center <strong>of</strong> NGC 1600. On larger scales, there is excess X-ray emission to<br />
92
the east and northeast <strong>of</strong> NGC 1600. In Figure 3.7 (right) we display the hardness<br />
ratio image (5 ′′ Gaussian smoothed) <strong>of</strong> H41 ≡ (H + M − S)/(H + M + S) between<br />
−0.4 (black) and 0.4 (white). This displays the s<strong>of</strong>ter central emission well. One can<br />
also see that the NGC 1603 tail appears s<strong>of</strong>ter than its surroundings. These features<br />
are also evident in Figure 3.1.<br />
To quantify the surface brightness differences associated with the features in Fig-<br />
ure 3.7, we determined the X-ray surface brightness <strong>of</strong> the unresolved emission in<br />
a number <strong>of</strong> elliptical annular pie-shaped regions. For each annulus, we subdivided<br />
the region by P.A. (Fig. 3.8). To quantify nonuniform morphology, we first fitted<br />
a constant line to the surface brightnesses at each annulus (dashed line), iteratively<br />
excluding P.A. regions from the fit that diverged by more than 2 σ. In the innermost<br />
annulus, emission from unresolved point sources and any inaccuracies from using the<br />
optical isophotes will be largest. In addition, there appear to be small depressions<br />
in the emission just to the north and the south <strong>of</strong> the galaxy center and a larger<br />
depression at the east edge <strong>of</strong> the annulus. These make it difficult to accurately<br />
establish a baseline for this annulus. There is a clear excess <strong>of</strong> emission (P.A. = 255 ◦ –<br />
345 ◦ , 4.3 σ) to the west <strong>of</strong> the second annulus. This excess continues in the third<br />
annulus (P.A. = 255 ◦ –315 ◦ , 3.0 σ), where an excess also appears 180 ◦ away (P.A.<br />
= 105 ◦ –135 ◦ , σ 5.6). In the fourth and fifth annulus, the western excess has dis-<br />
appeared, while the eastern excess begins to take up most <strong>of</strong> the northeast quadrant<br />
(P.A. = 30 ◦ –120 ◦ , 4.0σ). In the fourth annulus, there is also an isolated excess in<br />
the south (∼3.5 σ). Finally, the last annulus clearly shows the NGC 1603 tail (∼4.5<br />
σ).<br />
The excess to the northeast <strong>of</strong> NGC 1600 in annuli 3–5 <strong>of</strong> Figure 3.8 may be due<br />
to gas associated with the NGC 1600 group potential rather than the galaxy. We<br />
93
Fig. 3.8.— SBPs, with 1 σ error bars, <strong>of</strong> the unresolved emission (0.3–6 keV) as a<br />
function <strong>of</strong> P.A. for annuli with varying projected semimajor radii a. The dashed<br />
line indicates the best-fit constant surface brightnesses <strong>of</strong> each annulus, iteratively<br />
excluding P.A. regions more than 2 σ from it. The last annuli excludes P.A. regions<br />
that extend beyond the S3 chip.<br />
note that this northeast excess starts at about the same radius where the X-ray SBP<br />
in Figure 3.5 has an inflection point and the larger scale component dominates. This<br />
suggests that the gas at these radii is responding to a potential with a larger scale.<br />
Both <strong>of</strong> these suggest that the outer gas is bound to the group and that the center<br />
<strong>of</strong> the group potential is to the northeast <strong>of</strong> NGC 1600.<br />
We believe that the tail west <strong>of</strong> NGC 1603 is the result <strong>of</strong> ram pressure stripping.<br />
NGC 1603 is at a projected distance from NGC 1600 <strong>of</strong> ∼44.5 kpc with its velocity<br />
redshifted from NGC 1600 by ∼ 284 km s −1 . Since NGC 1603 is part <strong>of</strong> the NGC 1600<br />
94
group, we assumed that they were at the same distance. Given the tail seen in the X-<br />
ray image, it is unlikely that the only component <strong>of</strong> the velocity <strong>of</strong> NGC 1603 relative<br />
to NGC 1600 is along the line <strong>of</strong> sight. We assume that the two transverse components<br />
<strong>of</strong> the relative velocity are each about the same as the line-<strong>of</strong>-sight component. Thus,<br />
the total relative velocity <strong>of</strong> NGC 1603 is about ≈ √ 3 × 284 km s −1 ≈ 490 km s −1 .<br />
This would be a reasonable value for a circular orbital velocity <strong>of</strong> NGC 1603 around<br />
NGC 1600, whose observed radial velocity dispersion is 321 km s −1 (Faber et al.<br />
1989). We argued above that there may be a significant potential associated with the<br />
NGC 1600 group, which would increase the estimated velocity.<br />
We estimated the gas densities and pressures in NGC 1603 and in its environment<br />
to see if ram pressure could be sufficient to strip gas and form the tail. For the gas<br />
in NGC 1603, we assumed three uniform-density spherical annuli with widths <strong>of</strong> 2 ′′<br />
each. Since the X-ray emission from NGC 1603 is s<strong>of</strong>ter than that from the center<br />
<strong>of</strong> NGC 1600, we assume a spectrum with kT = 0.6 keV and solar abundances for<br />
the gas in this galaxy. With these assumptions, we find that the electron number<br />
densities <strong>of</strong> the gas in NGC 1603 are 4.9 × 10 −2 , 1.9 × 10 −2 , and 5.4 × 10 −3 cm −3 and<br />
the pressures, Pgas, are 9.4 × 10 −11 , 3.6 × 10 −11 , and 1.0 × 10 −11 dyne cm −2 in the<br />
0 ′′ –2 ′′ , 2 ′′ –4 ′′ , and 4 ′′ –6 ′′ annuli, respectively. We estimated the density in the group<br />
gas around NGC 1603 from the X-ray surface brightness in a hemispherical annulus<br />
centered on NGC 1603 (radius from NGC 1600 <strong>of</strong> 6 ′′ –12 ′′ , P.A. = 0 ◦ –180 ◦ ). This<br />
surface brightness agrees within the errors with the prediction by the modeled SBP<br />
at the semimajor distance <strong>of</strong> NGC 1603 from NGC 1600. We assumed a spectrum<br />
with kT = 1.5 keV and solar abundances. This gave an ambient gas electron density<br />
<strong>of</strong> 4.0 × 10 −3 cm −3 at the projected semimajor distance <strong>of</strong> NGC 1603. Assuming<br />
a relative velocity <strong>of</strong> 490 km s −1 , the ram pressure <strong>of</strong> the ambient gas would be<br />
95
Pram ≈ 1.6 × 10 −11 dyne cm −2 . The ram pressure would be lower if NGC 1603 were<br />
at a larger radius than its projected radius (i.e., in front <strong>of</strong> or behind the center <strong>of</strong><br />
the NGC 1600 group). Roughly speaking, the condition for ram pressure to strip the<br />
gas is that Pram > Pgas, which appears plausible in the outer 4 ′′ –6 ′′ <strong>of</strong> NGC 1603.<br />
Since the tail points to the west towards the higher density gas near NGC 1600, the<br />
ambient gas density may have been higher in the past, making ram pressure stripping<br />
easier than it is at its present position.<br />
The NGC 1603 tail has a s<strong>of</strong>ter spectrum (Fig. 3.7, right) than the surrounding<br />
gas. Hardness ratios from counts in the same pie-shaped annuli used to construct<br />
Figure 3.8 confirm that the tail is s<strong>of</strong>ter in H21 by ≈2.6 σ. Thus, the jump in<br />
emission due to the tail is dominated by a jump in s<strong>of</strong>t emission, consistent with ram<br />
pressure stripping <strong>of</strong> cooler galactic gas by hotter group gas.<br />
NGC 1601 also has a velocity redshifted from NGC 1600 by ∼ 309 km s −1 , and its<br />
projected distance from NGC 1600 is only ∼28.5 kpc. Since the emission associated<br />
with NGC 1601 is fainter, its estimated thermal pressure is smaller than in NGC 1603.<br />
This, combined with its slightly higher velocity, suggests that ram pressure stripping<br />
should be stronger in NGC 1601 compared to NGC 1603. Although there is a hint <strong>of</strong><br />
a tail toward the east <strong>of</strong> NGC 1601 in Figure 3.7, it has only a 1.3 σ significance when<br />
the surface brightness in a hemispherical annulus east <strong>of</strong> NGC 1601 is compared with<br />
a similar annulus west <strong>of</strong> NGC 1601. There are a number <strong>of</strong> possible explanations <strong>of</strong><br />
why we do not see a significant tail around NGC 1601, while we see one for NGC 1603.<br />
First, NGC 1601 might have a small transverse velocity; the tail would then be<br />
projected onto NGC 1601 along our line <strong>of</strong> sight. In addition, the tail could be too<br />
faint, the projected velocity could be smaller than we estimated for NGC 1603, or<br />
projection effects could mean that NGC 1601 is actually in a lower density region in<br />
96
the group gas than we calculate from the SBP and its projected radius.<br />
3.5.3 Central X-ray Structure and Multiwavelength Com-<br />
parisons<br />
The X-ray emission near the center <strong>of</strong> the galaxy is elongated similarly to the<br />
optical emission (Figs. 3.1 and 3.2). However, the details <strong>of</strong> the central X-ray structure<br />
are complex. Figures 3.7 and 3.8 display the excess emission immediately west <strong>of</strong> the<br />
galaxy center, as well as holes in the emission immediately north and south <strong>of</strong> the<br />
galaxy center.<br />
One <strong>of</strong> the purposes <strong>of</strong> this Chandra observation was to compare the X-ray struc-<br />
ture with the extended emission-line filaments and dust. In Figure 3.9 we display<br />
the Hα +[N II] image (Trinchieri & di Serego Alighieri 1991) overlaid on the excess<br />
emission image <strong>of</strong> the inner 140 ′′ × 140 ′′ . The peak <strong>of</strong> the Hα corresponds to excess<br />
emission west <strong>of</strong> the galaxy center; however, the detailed structure <strong>of</strong> the Hα and<br />
excess X-ray emission do not have a one-to-one correspondence. Macchetto et al.<br />
(1996) find ∼5 ′′ × 5 ′′ <strong>of</strong> Hα+[N II] emission centered on the optical center, with a<br />
slight north-south elongation. There is excess X-ray emission centered on the galaxy;<br />
however, a correlation <strong>of</strong> excess emission is made difficult by the possible presence <strong>of</strong><br />
a central AGN and holes in the X-ray emission ∼2. ′′ 5 to the north and south <strong>of</strong> the<br />
galaxy center.<br />
In Figure 3.10 (left) we display the excess emission image <strong>of</strong> the inner 40 ′′ × 40 ′′ .<br />
It is overlaid by 4.885 GHz radio contours from Birkinshaw & Davies (1985). The<br />
double-radio lobe structure is oriented in the north-south direction, and the lobe<br />
positions are roughly consistent with holes in the X-ray emission. Although the<br />
southern lobe’s centroid is a bit <strong>of</strong>fset from the hole, the 5 ′′ Gaussian smoothed<br />
97
Fig. 3.9.— Hα +[N II] contours (Trinchieri & di Serego Alighieri 1991) overlaid on an<br />
adaptively smoothed image <strong>of</strong> unresolved X-ray emission (140 ′′ ×140 ′′ ) with a best-fit<br />
elliptical model for the SBP removed. The contours indicate line emission <strong>of</strong> 0, 1.7, 2,<br />
4.1, 6.2, 8.3, 12.4, 18.6, 27.6, and 41.4 ×10 −17 ergs cm −2 arcsec −2 . The cross indicates<br />
the center <strong>of</strong> the galaxy.<br />
image <strong>of</strong> H41 indicates that the lobe is cospatial with a region <strong>of</strong> s<strong>of</strong>ter emission.<br />
Considering the smoothing scale, this could be consistent with cool gas surrounding<br />
a radio bubble. No variation in H41 is observed near the northern lobe. These holes<br />
in X-ray emission may be due to the radio lobes, although this is uncertain.<br />
In Figure 3.10 we also display a V − R reddening map (Ferrari et al. 1999).<br />
The darker areas <strong>of</strong> the color index map correspond to regions <strong>of</strong> larger V − R<br />
and extinction AV . There is a clear filamentary structure to the west correspond-<br />
ing to a mean AV = 0.034 ± 0.030 (Ferrari et al. 1999), where the standard de-<br />
98
04:55<br />
-5:05:00<br />
05<br />
-5:05:10<br />
15<br />
-5:05:20<br />
25 10"<br />
4:31:41 41<br />
4:31:40 4:31:40 4:31:40<br />
39 4:31:39<br />
Fig. 3.10.— Left: Adaptively smoothed gray-scale image <strong>of</strong> unresolved X-ray emission<br />
(40 ′′ ×40 ′′ ) with the best-fit beta+power-law SBP removed. Contours are radio (4.885<br />
GHz: 1, 2, 3, 4, 5, and 6 mJy) with the beam in the lower-right corner (Birkinshaw &<br />
Davies 1985). The cross indicates the center <strong>of</strong> the galaxy. Right: Gray-scale image<br />
<strong>of</strong> V − R (0.625, 0.63, 0.635, 0.64); the darker (redder in color) values in correspond<br />
to larger AV (Ferrari et al. 1999).<br />
viation is due to non-uniform extinction over the area <strong>of</strong> measurement. The op-<br />
tical extinction can be converted into a hydrogen column density assuming NH =<br />
5.9 × 10 21 AV /Rv cm −2 (Spitzer 1978). Taking RV ≡ AV /(B − V ) = 3.2, there is an<br />
excess NH <strong>of</strong> (0.63 ± 0.55) × 10 20 cm −2 beyond the Galactic value <strong>of</strong> 4.86 × 10 20 cm −2 .<br />
If one assumes that the X-ray emission <strong>of</strong> a MEKAL model with T = 0.85 keV and<br />
solar abundance is absorbed by this extra column, the surface brightness would be re-<br />
duced by only ∼2% compared to that expected with no excess absorption. Of course,<br />
we actually observe an excess in the X-ray emission in this region <strong>of</strong> slightly larger<br />
extinction. The excess emission to the west <strong>of</strong> the galaxy is ∼1.5–2.5 times the values<br />
expected from the SBP model.<br />
Both the dust lanes and emission line filament appear to be cospatial in projection<br />
with the enhanced X-ray emission. There are several possible explanations for such<br />
99
a correlation. It might be that the hot and cool gas are in thermal contact and that<br />
heat is being conducted from the hot gas to the cool gas (Sparks 1992). This might<br />
cool the X-ray gas; if it remained at nearly the same pressure because <strong>of</strong> the weight<br />
and pressure <strong>of</strong> the surrounding hot gas, the density and X-ray emissivity <strong>of</strong> the X-ray<br />
gas would increase. Mixing between the hot and cool gas could have a similar effect,<br />
as long as the X-ray gas did not mix to a cool temperature out <strong>of</strong> the X-ray band.<br />
Third, the cool gas might result from radiative cooling <strong>of</strong> the X-ray gas. The cooling<br />
timescale at the center <strong>of</strong> NGC 1600 is on the order <strong>of</strong> 300 Myr, which is consistent<br />
with this explanation. On the other hand, it might be difficult to understand the<br />
presence <strong>of</strong> dust grains in cooled X-ray gas.<br />
3.6 Spectral Analysis<br />
We extracted spectra <strong>of</strong> the resolved sources and diffuse emission in NGC 1600,<br />
restricting analysis to the 0.7–9 keV range. The lower limit was taken to avoid<br />
calibration uncertainties, while there are few non-background counts beyond 9 keV.<br />
Since the telescope collecting area changes very rapidly near 2 keV and calibration<br />
problems led to poor fits in that spectral region, we chose to excise the 1.9–2.1 keV<br />
band when we fitted line models (MEKAL). We do not find that this edge significantly<br />
affected fits <strong>of</strong> continuum models. All the spectra were grouped to have at least<br />
25 counts per spectral bin prior to background correction to enable our use <strong>of</strong> χ 2<br />
statistics. In some cases, the fitted range <strong>of</strong> the spectra did not extend up to 9 keV<br />
because there were too few counts to form a bin up to this limiting energy.<br />
The results <strong>of</strong> the spectral fits are summarized in Table 3.2. Spectra were ex-<br />
tracted for the resolved point sources (“Sources”) and the unresolved diffuse emission<br />
excluding the point sources (“Unresolved”). Column (3) gives the geometric region<br />
100
for the spectrum: “Field” implies the entire S3 chip. The value <strong>of</strong> the absorbing<br />
column density (NH) applied to all components <strong>of</strong> the model emission spectrum is<br />
given in column (4). In this and other columns, values in parentheses are fixed (not<br />
allowed to vary). The fixed value <strong>of</strong> NH is the Galactic value from Dickey & Lockman<br />
(1990). To correct for the QE degradation, we used the XSPEC acisabs model. Other<br />
elliptical galaxies are known to have both hard (point source) and s<strong>of</strong>t (diffuse gas)<br />
components (Sarazin et al. 2001). For the hard component, we fitted three different<br />
models, thermal bremsstrahlung (“bremss”), power law (“power”), and disk black-<br />
body (“diskbb”). We always used the MEKAL model for the emission spectrum from<br />
hot diffuse gas. For the hard component, columns (5)–(7) give the spectral model(s),<br />
the temperature Th (for bremsstrahlung or disk blackbody) or photon number spectral<br />
index Γ, and the unabsorbed flux <strong>of</strong> the hard component(s), F h X<br />
101<br />
(0.3–10 keV). Sim-<br />
ilarly, columns (8)–(10) give the temperature Ts, overall heavy-element abundance<br />
relative to solar, and flux for the s<strong>of</strong>t MEKAL component(s). For the unresolved<br />
emission, the spectra exclude regions around each <strong>of</strong> the resolved sources with more<br />
than 3 σ flux. Columns (11) and (12) give the number <strong>of</strong> net counts in each spectrum<br />
and χ 2 per d<strong>of</strong> for the best-fit model. All errors reported in the spectral analysis are
Table 3.2. X-ray Spectral Fits <strong>of</strong> NGC 1600<br />
Hard Component S<strong>of</strong>t Component (MEKAL)<br />
Region NH kTh or Γ kTs Abundance<br />
Row Origin (arcsec) (10 20 cm −2 ) Model (keV) F h X a<br />
(keV) (solar) F s X )a Counts χ 2 /d<strong>of</strong><br />
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12)<br />
1.......... Sources Field (4.86) Bremss 4.73 +1.24<br />
−0.89<br />
2.78 · · · · · · · · · 1318 52.2/48=1.09<br />
2.......... Sources Field 0.48 [
90% confidence level errors. Brackets are used when either the upper or lower bound<br />
on the confidence interval is unconstrained.<br />
The background spectrum for the resolved sources was determined locally, using<br />
the same nearby regions as discussed in § 3.4. For the spectra <strong>of</strong> the unresolved<br />
emission, we used the deep blank sky backgrounds compiled by M. Markevitch. 16<br />
The spectra <strong>of</strong> several spatial regions were analyzed. We have adopted the ellip-<br />
ticity and P.A. <strong>of</strong> the optical de Vaucouleurs fit. Some <strong>of</strong> the regions are scaled to<br />
the elliptical optical isophote containing one-half <strong>of</strong> the optical light, the “1 effective<br />
radius” region. In NGC 1600 the semimajor axis <strong>of</strong> this isophote, aeff, is 55. ′′ 2. Since<br />
there were few source counts near the center <strong>of</strong> the galaxy, we fitted the sources for<br />
the entire field. We searched for changes in unresolved emission with radius using<br />
annuli containing ∼1000 net counts.<br />
3.6.1 X-ray Spectrum <strong>of</strong> Resolved Sources<br />
All resolved source spectral analysis was performed on sources with determined<br />
fluxes <strong>of</strong> more than 3 σ. Sources 1–3 were excluded because we are unsure that they<br />
are point sources. Sources 23 (NGC 1601), 40 (NGC 1603), and 50 (GSC 04742-<br />
00254) were also excluded because they are clearly not associated with NGC 1600.<br />
Since there are few source counts near the galaxy’s center, we first extracted the<br />
cumulative spectrum <strong>of</strong> resolved sources within 3 effective radii, yielding only 372 net<br />
counts. This was insufficient to produce a well-constrained fit, so we chose to fit the<br />
sources in the entire field. The observed spectrum, containing 1318 net counts, is<br />
shown in Figure 3.11.<br />
The combined spectrum <strong>of</strong> the sources was reasonably well fitted by either a<br />
16 See footnote 2.<br />
103
Fig. 3.11.— Top: Cumulative X-ray spectrum <strong>of</strong> the resolved sources with more than<br />
3 σ detected flux in the entire field <strong>of</strong> NGC 1600. The spectrum has 1 σ error bars<br />
and is overlaid by the solid histogram <strong>of</strong> the best-fit model spectrum (Table 3.2).<br />
Bottom: Contribution to χ 2 with the sign indicating the sign <strong>of</strong> the residual.<br />
thermal bremsstrahlung model with kTh = 4.73 keV (Table 3.2, row [1]) or a power-<br />
law model with a photon number spectral index <strong>of</strong> Γ = 1.76 (row [3]). The fits were<br />
not improved significantly when the absorbing column was allowed to vary (rows [2]<br />
and [4]), so we fixed the hydrogen column at the Galactic value, NH = 4.86 × 10 20<br />
cm −2 (Dickey & Lockman 1990). Since the sources were very luminous, we also<br />
attempted a disk blackbody model; however, its χ 2 was worse by ∼ 20 for the same<br />
number <strong>of</strong> d<strong>of</strong>. Finally, we attempted a disk blackbody+power-law spectral model<br />
(kTdisk = 1.44, Γ = 1.95, power-law responsible for ∼70% <strong>of</strong> flux). This model had<br />
a χ 2 lower than our bremsstrahlung or power-law fits by ∼2; however, the d<strong>of</strong> was<br />
also reduced by 2. In addition, this fit had an unconstrained disk temperature and<br />
a poorly constrained power law. We could have adopted either the bremsstrahlung<br />
or the power-law model for our best fit. For comparison with other papers and since<br />
the power law was constrained more tightly than the bremsstrahlung temperature,<br />
104
we adopted the power-law model as our best fit. This model, including Galactic<br />
absorption and QE degradation, is shown in Figure 3.11 with the residuals to the fit.<br />
The power-law index is consistent with what was found from the hardness ratios. It<br />
is s<strong>of</strong>ter than the best-fit value <strong>of</strong> the sources simultaneously fitted in a survey <strong>of</strong> 15<br />
early-type galaxies (Irwin et al. 2003); however, it is consistent with both the spread<br />
<strong>of</strong> indices found when the galaxies are fitted separately and the s<strong>of</strong>ter indices <strong>of</strong> the<br />
higher luminosity subsamples.<br />
Approximately half <strong>of</strong> the sources in the entire field are expected to be fore-<br />
ground/background sources. On the other hand, only about one is expected to be<br />
a foreground/background source within 3 effective radii. To ensure that unrelated<br />
sources do not heavily bias the spectral fits, we compared fits to the less constrained<br />
3 effective radii spectrum with the fits to the entire field spectrum. Since all the fits<br />
were consistent within the errors <strong>of</strong> the entire field spectrum fits, we do not believe<br />
the foreground/background sources heavily bias the spectral fits.<br />
3.6.2 X-ray Spectra <strong>of</strong> Unresolved Emission<br />
Projected Spectra<br />
For the unresolved emission, the spectrum <strong>of</strong> the inner effective radius had 3662<br />
net counts. This spectrum is shown in Figure 3.12. First, we attempted to model<br />
the unresolved emission with a s<strong>of</strong>t MEKAL component representing the emission<br />
by diffuse interstellar gas (Table 3.2, row [11]). The χ 2 was large, 168.6 for 87 d<strong>of</strong>.<br />
Since the unresolved emission includes unresolved point sources, as well as diffuse<br />
gas, we added the adopted best-fit spectrum <strong>of</strong> the resolved sources to model the<br />
unresolved sources. The fit was much improved, χ 2 = 110.0 for 86 d<strong>of</strong>; however, it<br />
was still rejected at the more than 95% level. We allowed the absorbing column to<br />
105
Fig. 3.12.— Top: Cumulative X-ray spectrum <strong>of</strong> the unresolved emission within 1aeff<br />
<strong>of</strong> NGC 1600. The notation is the same as in Fig. 3.11.<br />
vary, but this did not significantly improve the fit and was still consistent with the<br />
Galactic value. Therefore, we have assumed Galactic absorption for the remaining<br />
fits. Since the hardness ratios <strong>of</strong> the unresolved emission indicated spectral evolution<br />
at a ∼ 25 ′′ , we attempted a two-temperature gas solution (row [9]). We found a good<br />
fit, χ 2 = 78.7 for 83 d<strong>of</strong>; however, the abundance <strong>of</strong> the low-temperature gas was<br />
unconstrained. Therefore, we tried a two-temperature gas model with the abundances<br />
tied together. This fit, with a low MEKAL temperature <strong>of</strong> 0.85 ± 0.04 keV, a high<br />
MEKAL temperature <strong>of</strong> 2.55 +0.52<br />
−0.86 keV, and an abundance <strong>of</strong> 1.07 +1.00<br />
−0.40 solar, was almost<br />
as good as when both abundances were free. We also attempted a MEKAL cooling<br />
flow model; however, its fit, χ 2 = 94.4 for 85 d<strong>of</strong>, was worse than the two-temperature<br />
model. Therefore, we adopted the two-temperature gas model (row [10]) as our<br />
best-fit model for unresolved emission (Fig. 3.12). Although the best-fit flux <strong>of</strong> this<br />
model from the unresolved point sources was not large, the upper limit on the flux<br />
<strong>of</strong> 1.41 × 10 −13 ergs cm −2 s −1 in the 0.3–10 keV band still indicates that unresolved<br />
106
sources could be a non-trivial source <strong>of</strong> emission in the inner effective radius.<br />
Since this galaxy was bright enough to fit multiple annuli <strong>of</strong> unresolved emission<br />
and there were indications <strong>of</strong> multiple temperatures <strong>of</strong> the diffuse gas, we attempted<br />
to determine the radial dependence <strong>of</strong> gas temperature and abundance. We used eight<br />
annuli, each with approximately 1000 net counts, out to a = 180 ′′ . In Table 3.2 rows<br />
(11)–(18), we show the results <strong>of</strong> assuming the model was the sum <strong>of</strong> the resolved<br />
point source model with its normalization free and a single-temperature gas MEKAL<br />
model. Most <strong>of</strong> the fits produced reasonable χ 2 . Any radial changes in the abundance<br />
are dwarfed by the errors <strong>of</strong> the fits, although the best-fit abundances were mainly<br />
subsolar. On the other hand, it is clear that the first two annuli have a much lower<br />
temperature, ∼0.85 keV, than the outer five annuli, ∼1.5 keV. The temperature <strong>of</strong><br />
the third annulus is between the two temperatures. These fits are in rough agreement<br />
with the two-temperature model found within 1 effective radius, a < 55. ′′ 2; however,<br />
the flux <strong>of</strong> the unresolved sources is smaller, and the temperature fit for the hotter<br />
gas is larger when fitting the inner effective radius at once, as opposed to in multiple<br />
annuli. The best-fit normalization <strong>of</strong> the power-law and MEKAL model suggest that<br />
for a < 180 ′′ they both contribute approximately equally to the flux. Within 1aeff,<br />
the diffuse gas is dominant by at least 2:1. From the best-fit fluxes <strong>of</strong> the annular<br />
fits, we can estimate the X-ray luminosity (0.3–10 keV) to be ∼2.9 × 10 41 ergs s −1 in<br />
gas and ∼2.4 × 10 41 ergs s −1 in unresolved sources for a < 180 ′′ . Around 30%–40%<br />
<strong>of</strong> the gaseous luminosity comes from the cooler gas. The resolved 3 σ sources in the<br />
entire field have an X-ray luminosity <strong>of</strong> ∼1.4 × 10 41 ergs s −1 . In a < 180 ′′ , this scales<br />
to ∼0.4×10 41 ergs s −1 . Bolometric corrections increase the source luminosity by 44%<br />
and the total gaseous luminosity by 28%.<br />
107<br />
Using the RC3 optical pr<strong>of</strong>ile, a < 180 ′′ corresponds to ∼80% <strong>of</strong> the total optical
light, LB,80% = 8.5 × 10 10 LB⊙ (O’Sullivan et al. 2001). The source X-ray to optical<br />
ratio is 3.3 × 1030 ergs s−1 L −1<br />
B⊙ , approximately 4 times that found in NGC 4697<br />
(Sarazin et al. 2001) or NGC 1553 (Blanton et al. 2001). It is more than 10 times the<br />
expected contribution from discrete sources reported in O’Sullivan et al. (2001). Since<br />
the unresolved sources dominate the total source luminosity, there is an excess in the<br />
flux <strong>of</strong> faint sources in addition to the excess in the number <strong>of</strong> detected sources. It is<br />
unlikely that cosmic variance would lead to an excess number <strong>of</strong> sources at all fluxes.<br />
This suggests that the number <strong>of</strong> LMXBs found in NGC 1600 is not proportional to<br />
the number <strong>of</strong> stars as estimated by the optical light or that the unresolved source<br />
flux is overestimated. The most likely solution is that NGC1600 has a high specific<br />
frequency <strong>of</strong> GCs; this is discussed in more detail later in the chapter (see § 3.8).<br />
The large unresolved hard component flux in the spectral models suggests that<br />
there are many unresolved point sources. This is also roughly consistent with the<br />
observed LF for resolved sources (§ 3.4.3). If we extend the best-fit LF down to<br />
10 36 ergs s −1 and adjust the normalizations to account for the observed sources within<br />
3aeff, we expect an unresolved flux <strong>of</strong> ∼2.2 × 10 −13 ergs cm −2 s −1 in the 0.3–10 keV<br />
band. Although this is approximately half the flux estimated by the spectral fits, it is<br />
within the errors <strong>of</strong> the spectral fit flux. This agreement between the LF and spectral<br />
fits could point to a large number <strong>of</strong> unresolved point sources. It might also suggest<br />
that there is no strong break in the LF at lower X-ray luminosities than observed.<br />
Deprojected Spectra<br />
We also fitted deprojected spectra. We did the deprojections by fitting the spectra<br />
from the outside annulus to the inside. Each annulus was fitted assuming the best-fit<br />
model for the emission in each <strong>of</strong> the outer annuli and assuming simple geometric pro-<br />
108
jection to include the emission from outer annuli in the inner ones. First, we allowed<br />
the power-law normalization and MEKAL model to vary within each annulus. The<br />
outer four annuli had unphysically large abundances, and in general the abundances<br />
were poorly constrained. The temperature results were similar to those for the pro-<br />
jected fits. Next, we fitted the deprojected spectra assuming a solar abundance in all<br />
annuli to ensure that the abundance problems in the previous deprojection did not<br />
cause problems in the temperature determination. This deprojection also produced<br />
results similar to the projected fits, except that the jump between the low tempera-<br />
ture gas and high temperature gas moved inward. Since these results are qualitatively<br />
the same as the projected fit, but we had to assume a constant abundance, we choose<br />
not to present the details <strong>of</strong> these results.<br />
Galaxy and Group Gas<br />
Both the unresolved emission within 1 effective radius and the unresolved emis-<br />
sion in annuli out to 180 ′′ point to a model involving two components <strong>of</strong> hot gas. In<br />
the inner 25 ′′ –40 ′′ region, there is gas with kT ∼ 0.85 keV. With a stellar velocity<br />
dispersion <strong>of</strong> 321 km s −1 (Faber et al. 1989), NGC 1600 has a stellar kinetic tem-<br />
perature <strong>of</strong> ∼0.65 keV, predicting an X-ray temperature <strong>of</strong> ∼1 ± 0.2 keV based on<br />
Davis & White (1996) and Brown & Bregman (1998). This prediction is consistent<br />
with the measured X-ray temperature. At semimajor distances beyond 40 ′′ , the gas is<br />
hotter, kT ∼ 1.5 keV. This temperature is more consistent with the gas temperature<br />
<strong>of</strong> X-ray–bright groups (Helsdon & Ponman 2000) than <strong>of</strong> X-ray–luminous early-type<br />
galaxies (O’Sullivan et al. 2003). Since the abundances are poorly constrained, we<br />
cannot tell if there is any gradient in the abundance or if the average abundance is<br />
higher or lower than solar.<br />
109
Near the same radius at which there is a transition in spectrum, we saw transitions<br />
in the behavior <strong>of</strong> the SBP and the hardness ratios. This break in behavior <strong>of</strong> the<br />
surface brightness, hardness ratio, and spectrum at a ∼ 25 ′′ –40 ′′ (7.3–11.7 kpc in<br />
projection) might be explained if emission from a lower temperature diffuse gas from<br />
the interstellar medium (ISM) <strong>of</strong> NGC 1600 dominates in the inner regions and a<br />
higher temperature diffuse gas from the intergalactic medium <strong>of</strong> the NGC 1600 group<br />
provides the emission at larger radii.<br />
110<br />
The total gas X-ray to optical ratio is 3.4 × 1030 ergs s−1 L −1<br />
B⊙ ; the galaxy gas<br />
luminosity is ∼30%–40% <strong>of</strong> the total gas luminosity. Compared with the LX,bol–<br />
LB relationships from O’Sullivan et al. (2001), the galaxy and the total gaseous<br />
luminosity are consistent with the standard deviation around the best-fit relationship<br />
to the early-type galaxies, excluding AGNs, brightest cluster galaxies, and dwarfs.<br />
The total emission is consistent with the best-fit relationship for the brightest group<br />
galaxies.<br />
3.7 Mass Determination<br />
By combining the SBP model and the spectral fits <strong>of</strong> the diffuse gas, we estimated<br />
the gas and gravitational mass around NGC 1600. In equation (3.3), the SBP is<br />
represented as the sum <strong>of</strong> two functions. Because the X-ray emissivity is a quadratic<br />
function <strong>of</strong> the density, equation (3.3) does not lead to a simple expression for the gas<br />
density as the sum <strong>of</strong> two terms. Thus, we assumed that the two terms in the SBP<br />
represented two cospatial phases <strong>of</strong> gas, a 0.85 keV gas following the inner beta model<br />
pr<strong>of</strong>ile and a 1.5 keV gas following the outer beta model pr<strong>of</strong>ile. To remove the ∼30%<br />
contribution to the counts by unresolved point sources (see § 3.5), we multiplied the<br />
SBP by 0.7. We integrated the sum <strong>of</strong> the physical densities over volume to determine
Fig. 3.13.— Estimated gas and gravitational mass pr<strong>of</strong>iles around NGC 1600. The<br />
dotted line and right axis display the gas mass pr<strong>of</strong>ile, while the solid line and left<br />
axis display the gravitational mass pr<strong>of</strong>ile.<br />
the gas mass, and we used hydrostatic equilibrium to estimate the gravitational mass.<br />
For both estimates, we assumed the galaxy was shaped as an oblate spheroid.<br />
In Figure 3.13 we display the resulting gravitational and gas mass pr<strong>of</strong>iles. At<br />
a ∼ 20 ′′ , there is a slope change in the gravitational mass pr<strong>of</strong>ile. This indicates the<br />
likely presence <strong>of</strong> two gravitational potentials, supporting the view that the exterior<br />
gas is group gas and the interior gas is galaxy gas. On the other hand, the total<br />
gravitational mass within a < 180 ′′ is only (2.0 ± 0.5) × 10 12 M⊙ with errors in the hot<br />
gas temperature dominating the error budget. The mass-to-light ratio for a < 180 ′′<br />
is M/LB = (24 ± 6) M⊙L −1<br />
B⊙ . Within 1 effective radius, the mass-to-light ratio is<br />
(10 ± 3) M⊙L −1<br />
B⊙ . The total mass is not that much larger than might be expected<br />
for NGC 1600 alone, which may not be consistent with the suggestion that the outer<br />
component is due to a group dark matter potential.<br />
111<br />
The total gas mass within a < 180 ′′ is (1.14 ± 0.06) × 10 10 M⊙, with errors in
the surface brightness dominating the error budget. Assuming a normal elliptical<br />
galaxy stellar mass loss rate per stellar luminosity <strong>of</strong> 1.3 ×10−11M⊙L −1<br />
B⊙ (Mathews &<br />
Brighenti 2003), the rate <strong>of</strong> stellar mass loss for the entire galaxy is about 1.4 M⊙ yr −1 .<br />
Almost all <strong>of</strong> the gas mass around NGC 1600 can be attributed to stellar mass loss<br />
in NGC 1600, assuming an age <strong>of</strong> 7.3 Gyr (Terlevich & Forbes 2002). This is not<br />
surprising since NGC 1600 dominates the stellar population <strong>of</strong> the NGC 1600 group.<br />
On the other hand, it is not consistent with there being a large amount <strong>of</strong> intergalactic<br />
group gas in the system.<br />
3.8 Conclusions<br />
We have used Chandra observations to study the X-ray emission from the point<br />
sources and unresolved emission <strong>of</strong> NGC 1600. Since NGC 1600 is ∼60 Mpc away,<br />
we could only resolve the very brightest point sources. We detected 71 total point<br />
sources, <strong>of</strong> which 45 were bright enough to have fluxes determined at ≥3 σ. We<br />
identified two <strong>of</strong> the sources with foreground stars, two with known galaxy members<br />
<strong>of</strong> the NGC 1600 group, and three with nonstellar objects, presumably galaxies.<br />
We did not clearly detect a point source at the center <strong>of</strong> NGC 1600, and we put a<br />
conservative 0.3–10 keV upper flux limit <strong>of</strong> 6.7 × 10 39 ergs s −1 on the luminosity <strong>of</strong><br />
the central AGN.<br />
Twenty-one <strong>of</strong> the sources without clear associations to objects besides NGC 1600<br />
are brighter than 2×10 39 ergs s −1 (0.3–10 keV); approximately 11±2 <strong>of</strong> those sources<br />
are expected to be unrelated foreground/background sources. The excess is strongest<br />
within 2D25, where we observe a source density <strong>of</strong> 2250 ± 796 deg −2 compared to<br />
the expected 600 ± 100 deg −2 . NGC 1600 may have the largest number <strong>of</strong> ULX<br />
candidates observed to date in an early-type galaxy, although cosmic variance in the<br />
112
ackground source population cannot be completely ruled out. A combination <strong>of</strong><br />
cosmic variance for the high-flux sources and a distance overestimate <strong>of</strong> ∼ 40% could<br />
also reduce the number <strong>of</strong> ULX candidates; however, this model requires NGC 1600<br />
to have a peculiar velocity <strong>of</strong> ∼ +1300km s −1 . As found in Irwin et al. (2003), the<br />
bright LMXBs have s<strong>of</strong>ter spectra than is typical for fainter LMXBs in early-types<br />
galaxies. The spectrum <strong>of</strong> sources in NGC 1600, Γ = 1.76 +0.10<br />
−0.09, and the LF slope,<br />
α = 2.00 +1.14<br />
−0.35, both suggest that these sources are different from the ULX candidates<br />
observed in star-forming galaxies. The age <strong>of</strong> the galaxy and the X-ray spectra <strong>of</strong> the<br />
sources argue against these sources being HMXBs.<br />
Since this galaxy is X-ray bright, we expected the unresolved emission to domi-<br />
nate the flux. Although this is true, the contribution from unresolved point sources<br />
is nearly as large as that due to the diffuse gas in the best-fit models. Even if one<br />
uses the lower limit on the unresolved point source flux, unresolved point sources are<br />
responsible for 25% <strong>of</strong> the unresolved flux. Combined with the large normalization<br />
<strong>of</strong> the X-ray LF, this suggests that NGC 1600 has a larger population <strong>of</strong> LMXBs than<br />
found in most previously observed galaxies (Sarazin et al. 2001; Blanton et al. 2001;<br />
Finoguenov & Jones 2002; Zezas & Fabbiano 2002; Jeltema et al. 2003; Chapter 2;<br />
Randall et al. 2004). When normalized to the optical luminosity <strong>of</strong> the galaxy, the<br />
source X-ray to optical ratio is also very high, LX/LB = 3.3 × 10 30 ergs s −1 L −1<br />
B⊙ .<br />
This ratio is a factor <strong>of</strong> 2 larger than found in most early-type galaxies. Recently, Gil-<br />
fanov (2004) suggested that total X-ray source luminosities correlate better with near-<br />
infrared luminosities than with optical luminosities. From the extrapolated 2MASS<br />
Ks magnitude (8.04), MKs,⊙ = 3.39, and the distance <strong>of</strong> NGC 1600, we find that the<br />
source X-ray to near-infrared ratio is almost an order <strong>of</strong> magnitude higher than the<br />
average found in Gilfanov (2004). Gilfanov (2004) limited the sources he considered<br />
113
in his total X-ray luminosities to LX > 10 37 ergs s −1 , so part <strong>of</strong> the difference might<br />
be explained if NGC 1600 has a very large number <strong>of</strong> fainter sources.<br />
Previous studies have shown that a large fraction <strong>of</strong> LMXBs in elliptical galaxies<br />
are located in GCs (Sarazin et al. 2000, 2001; Angelini et al. 2001; Kundu et al.<br />
2003; Sarazin et al. 2003), and that the luminosity <strong>of</strong> LMXBs may correlate better<br />
with the GC population than the optical luminosity (White et al. 2002; Sarazin et al.<br />
2003). Unfortunately, we were unable to find a determination <strong>of</strong> the GC population<br />
in NGC 1600, which is more distant than most galaxies that have GC observations.<br />
However, one explanation for the large number <strong>of</strong> LMXBs in NGC 1600 would be<br />
that this galaxy has a large GC specific frequency. Thus, we predict that NGC 1600<br />
will be found to have large numbers <strong>of</strong> GCs. Observations <strong>of</strong> the GC population in<br />
NGC 1600 would be very useful to test this prediction. Such a large population <strong>of</strong><br />
GCs might be connected to NGC 1600’s position as the central elliptical galaxy in<br />
a group with a significant potential; it may be more closely related to cD galaxies,<br />
which have larger GC populations (e.g., Harris 1991) than normal ellipticals.<br />
We note that many <strong>of</strong> the bright X-ray sources associated with NGC 1600 are at<br />
large distances from the galaxy center. One possibility is that these sources are due<br />
to cosmic variance in the background source population. For the sources within 2D25,<br />
the variance would have to be much larger than the ∼8% cosmic variance between the<br />
Chandra Deep Fields found by (Rosati et al. 2002). Another possibility is that these<br />
sources are actually located in intergalactic GCs in the NGC 1600 group, rather than<br />
being directly associated with NGC 1600. Recently, intergalactic GCs have probably<br />
been detected in nearby groups and clusters (e.g., Bassino et al. 2003).<br />
The X-ray image, SBP, and spatially resolved spectra suggest that there are<br />
two components to the gas around NGC 1600. There is a component centered on<br />
114
NGC 1600 that has a small spatial scale (25 ′′ ) and a lower temperature (0.85 keV),<br />
which we propose is gas that is bound to NGC 1600. A second component is centered<br />
to the northeast <strong>of</strong> NGC 1600, has a larger spatial scale, and is hotter (1.5 keV); we<br />
argue that this gas is bound to the dark matter potential <strong>of</strong> the NGC 1600 group.<br />
The X-ray image suggests that the center <strong>of</strong> the potential <strong>of</strong> the group is slightly<br />
displaced from the center <strong>of</strong> NGC 1600. One would expect that NGC 1600 would be<br />
moving in the group potential, and this motion could affect the distribution <strong>of</strong> the<br />
galaxy and group gas.<br />
We also observe structure in the diffuse emission on small scales. Excess emission is<br />
seen west <strong>of</strong> the center <strong>of</strong> NGC 1600 in the inner 35 ′′ . This excess emission is partially<br />
cospatial with Hα and dust filaments. Possible models to explain this correlation <strong>of</strong><br />
hot and cooler gas include thermal conduction between the two phases, radiative<br />
cooling <strong>of</strong> the hot X-ray gas to form the cooler gas, and mixing <strong>of</strong> the hot and cool<br />
gas. Directly to the north and south <strong>of</strong> the galaxy center, there are holes in the X-<br />
ray emission. These holes are roughly coincident with the lobes <strong>of</strong> the radio source,<br />
suggesting that there may be two radio bubbles being blown in the hot gas. Finally,<br />
we see that NGC 1603, a galaxy east <strong>of</strong> NGC 1600, has a tail <strong>of</strong> s<strong>of</strong>t X-ray emission<br />
to its west. Calculations indicate that this is likely to be a ram pressure-stripped tail<br />
<strong>of</strong> ISM from NGC 1603, removed as a result <strong>of</strong> motions <strong>of</strong> this galaxy through the<br />
surrounding group gas.<br />
115
Chapter 4<br />
Luminous X-Ray Flares from<br />
Low-Mass X-Ray Binary<br />
Candidates in the Early-Type<br />
Galaxy NGC 4697<br />
4.1 Introduction<br />
Galactic X-ray binaries (XRBs) exhibit a wide-range <strong>of</strong> short-timescale variability.<br />
X-ray bursts from XRBs were first studied in the mid-1970s (e.g., Grindlay et al. 1976;<br />
Belian et al. 1976). Type I bursts, found in low-mass X-ray binaries (LMXBs), are due<br />
to thermonuclear flashes on the neutron star (NS) surface with luminosities peaking<br />
at the Eddington limit. Eight bursts lasting several hours, but otherwise like type<br />
I bursts, have been observed (Kuulkers 2004). These superbursts are relatively rare<br />
and appear to recur on year timescales.<br />
116<br />
Short-timescale variability has also been seen in high-mass X-ray binaries
(HMXBs). LMC X-4, an HMXB pulsar, has a persistent luminosity <strong>of</strong><br />
∼2 × 10 38 ergs s −1 and super-Eddington flares (up to ∼2 × 10 39 ergs s −1 ) with du-<br />
rations <strong>of</strong> ∼70 s (Moon et al. 2003).<br />
Since black holes (BHs) lack a surface, type I bursts do not occur. Typical short<br />
flares observed in BH XRBs tend to last on the order <strong>of</strong> days (McClintock & Remillard<br />
2005) as opposed to minutes, as in NS XRBs; however, rapid flares have been seen<br />
(e.g., Greiner et al. 1996; Wijnands & van der Klis 2000). In GRS 1915+105, which<br />
has been relatively luminous (∼3 × 10 38 ergs s −1 ) since its discovery, these rapid flares<br />
typically last for minutes or less, have peak-to-persistent flux ratios 10, and <strong>of</strong>ten<br />
recur on both regular and irregular intervals <strong>of</strong> minutes or less (Yadav et al. 1999).<br />
V4641 Sgr, an HMXB, showed variations <strong>of</strong> a factor up to 500 on the timescale <strong>of</strong><br />
minutes (Wijnands & van der Klis 2000).<br />
In this chapter, we perform the first search specifically targeting short-timescale<br />
flares from LMXBs in an early-type galaxy. Since nearby early-type galaxies have<br />
many bright LMXBs (>10 37 ergs s −1 ; e.g., Sarazin et al. 2000), they have a high<br />
potential for having sources with interesting flare behaviors. We targeted NGC 4697,<br />
the nearest (11.7 Mpc; Tonry et al. 2001) optically luminous (MB < −20) elliptical<br />
galaxy. As an X-ray–faint galaxy (low LX/LB), most <strong>of</strong> its X-ray emission is resolved<br />
into 158 point sources (G. R. Sivak<strong>of</strong>f et al. 2005, in preparation, hereafter Paper IV).<br />
Five Chandra observations <strong>of</strong> NGC 4697 give extended time coverage for searching for<br />
variability. We discuss a new method for detecting flares in the low count regime and<br />
characterize short-timescale flares in three LMXBs. All errors refer to 90% confidence<br />
intervals. Count rates and fluxes are in the 0.3–10 keV band.<br />
117
4.2 Observations and Data Reduction<br />
Chandra has observed NGC 4697 five times (observations 0784, 4727, 4728, 4729,<br />
and 4730), 2000 January 15, 2003 December 26, 2004 January 6, February 2, and<br />
August 18, using the Advanced CCD Imaging Spectrometer S3 detector. After re-<br />
moval <strong>of</strong> background flares, ONTIME values were 37651, 40447, 36072, 32462, and<br />
40574 s. All observations were analyzed under CIAO 3.1 with CALDB 2.28. We de-<br />
tected 158 sources using the wavelet detection algorithm (CIAO wavdetect). Optical<br />
identifications were used to refine the coordinates to 0. ′′ 4 accuracy, with larger errors<br />
for fainter sources away from the chip center. We give details concerning the X-ray<br />
observations, data analysis, and source properties in Paper IV.<br />
We observed the center <strong>of</strong> NGC 4697 with the Hubble Space Telescope Advance<br />
Camera for Surveys (HST ACS), acquiring two 375 s exposures in the F475W (g475)<br />
band, two 560 s exposures in the F850LP (z850) band, and one 90 s F850LP expo-<br />
sure. Source detection and characterization were performed similarly to Jordán et al.<br />
(2004a), leading to a list <strong>of</strong> globular clusters (GCs) and other optical sources. Details<br />
concerning the HST ACS observation, data analysis, and optical source properties<br />
will be given in A. Jordán et al. (2005, in preparation).<br />
4.3 Detection <strong>of</strong> Flaring Sources<br />
A bright LMXB (10 38 ergs s −1 ) will have only ∼25 counts in an ∼40 ks Chandra<br />
observation <strong>of</strong> NGC 4697, making it difficult to search for intraobservation variability.<br />
Tests that require binning the events and the Kolmogorov-Smirnov test are not useful<br />
for detecting flares with small numbers <strong>of</strong> events. Instead, we consider arrival times<br />
<strong>of</strong> individual events and compare them to a constant rate Poisson distribution. We<br />
118
searched for the shortest time tn over which n consecutive photons (hereafter an n-<br />
tuple) arrived. Assuming there are N photons in the entire ONTIME (texp), the<br />
probability that at least n photons are seen in tn due to Poisson fluctuations is given<br />
by the incomplete gamma function,<br />
P (n in tn given N in texp) =<br />
119<br />
Ntn/texp<br />
1<br />
e<br />
Γ(n − 1) 0<br />
−a a n−2 da . (4.1)<br />
Since we search N − n + 1 n-tuples, the probability that the n observed photons that<br />
are seen in tn are not due to random fluctuations is given by<br />
Pflare(n) = [1 − P (n in tn given N in tN)] N−n+1 , (4.2)<br />
assuming the n-tuples are independent. The probability that the flare resulted from<br />
a statistical fluctuation is Pconstant(n) = 1 − Pflare(n).<br />
With each observation, we search through N − 1 different sets <strong>of</strong> n-tuples; i.e.,<br />
n = 2 . . . N. Thus, eq. 4.2 overestimates the probability a detected flare <strong>of</strong> n photons<br />
is real. However, the N − 1 sets <strong>of</strong> n-tuples are not independent. To derive accurate<br />
probabilities, we determined the number <strong>of</strong> false flares detected by our algorithm<br />
due to statistical fluctuations by running sets <strong>of</strong> >200, 000 Monte Carlo simulations,<br />
assuming the source emitted at a constant rate. From the simulations, which were<br />
analyzed identically to the actual observations and included the effects <strong>of</strong> finite frame<br />
times, readout time, and background, we derived a correction factor to eq. (4.2) to<br />
give the correct probability that a flare was real, P ′ flare . We determined the ratio be-<br />
tween P ′ constant and Pconstant when Pconstant < 5%; this ratio A(N) ≡ P ′ constant/Pconstant<br />
depended only on the mean number <strong>of</strong> counts N for a set <strong>of</strong> simulations and was<br />
typically 2–3. We linearly interpolated between simulation sets with different N to
find P ′ constant for each flare. For each flaring source, we checked all n−tuples for other<br />
less probable but still significant flares within the same observation. We did not find<br />
multiple flares in the same observation. As a caveat, note that the use <strong>of</strong> the total<br />
observed counts in eq. (4.1) creates a bias against detecting multiple intraobservation<br />
flares.<br />
We found that several <strong>of</strong> the sources showed flares in different observations with<br />
similar properties. Detecting multiple flares from a source makes it even less likely<br />
that the flares are due to statistical fluctuations. Let P ′ constant,i be the probability<br />
that the most significant flare within a given observation i is due to a statistical<br />
fluctuation. When Pconstant,i > 5%, we conservatively set P ′ constant,i = 1. We only<br />
consider sequences <strong>of</strong> flares with properties that are all identical within the errors.<br />
With five observations, the joint probability that the flare sequence is a statistical<br />
fluctuation is,<br />
Pconstant,joint =<br />
where k is the number <strong>of</strong> observations with Pconstant,i < 5%.<br />
120<br />
<br />
5 5<br />
P<br />
k<br />
i=1<br />
′ constant,i , (4.3)<br />
Whenever Pconstant,joint < 0.32%, we considered a source to be a flaring source.<br />
At this level, we expect
with NGC 4697. Columns (1)–(4) list the source name, position, and observation<br />
number in which the flare occurred. Columns (5)–(8) list the total number <strong>of</strong> events<br />
N from the source during this observation, the number <strong>of</strong> events in the flare n, the flare<br />
duration ∆t, and the Modified Julian Day (MJD) <strong>of</strong> the first event, t0. Column (9)<br />
lists the probability that a given n-tuple is a statistical fluctuation, and column (10)<br />
gives the probability, including all <strong>of</strong> the n-tuples that were searched. Column (11)<br />
gives the joint probability that sequences <strong>of</strong> similar flares during several observations<br />
are all just statistical fluctuations.<br />
For each event in a flaring source, we examined the chip coordinates and ASCA<br />
grades to eliminate previously unknown flickering pixels as possible false positive<br />
flares. Although the four flare events in Obs. 0784 <strong>of</strong> source C occur at only two<br />
chip positions, their ASCA grades (2 and 0, 6 and 2) indicate they are unlikely to be<br />
due to flickering pixels. We note that the time intervals between events at the same<br />
chip positions in Obs. 0784 <strong>of</strong> source C are 6.4 s and 12.8 s, much less than the aspect<br />
motion periods. Thus, it is likely that subsequent events from the same source can<br />
occur at the same detector position. The other sources, which all had longer flare<br />
durations, did not have duplicate chip positions in their flares.<br />
It is likely that the observed flare duration underestimates the actual duration<br />
because <strong>of</strong> the small number <strong>of</strong> photons detected and that other properties may be<br />
biased by the flare detection algorithm. On the other hand, if a photon due to emission<br />
outside <strong>of</strong> the flare duration arrives just before or after a flare, this could lead to an<br />
overestimate <strong>of</strong> the flare properties. To assess these effects, we adopted a simple<br />
model for the temporal development <strong>of</strong> the flare and used Monte Carlo simulations<br />
to derive the best-fit model flare parameters and their uncertainties. For the flare,<br />
we adopted a top-hat model, characterized by a constant flare rate, rflat, over a burst<br />
121
Table 4.1. Observed Properties <strong>of</strong> Short-Timescale Flares in NGC 4697<br />
∆t t0 Pconstant P ′ constant Pconstant,joint Source Name R.A. Decl. Obs. N n (s) (MJD) (%) (%) (%)<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11)<br />
CXOU J124837.8−054652 (source A) ..... 12 48 37.86 −05 46 52.9 0784 14 5 1047 51558.79424 0.700 1.787<br />
4727 16 4 628 52999.75883 2.729 7.006<br />
4728 14 4 509 53010.70296 1.212 3.096<br />
0784,4727,4728 0.039<br />
CXOU J124831.0−054828 (source B) ..... 12 48 31.04 −05 48 28.8 4727 9 5 1329 53000.04327 0.224 0.552<br />
4728 9 4 1420 53010.72445 3.368 7.982<br />
4729 6 5 5654 53047.59917 4.327 9.007<br />
4727,4728 0.441<br />
4727–4729 0.040<br />
CXOU J124839.0−054750 (source C) ..... 12 48 39.03 −05 47 50.2 0784 20 4 68 51558.95771 0.013 0.034<br />
4727 20 3 50 53000.05857 0.547 1.420<br />
0784,4727 0.005<br />
NOTE.—Units <strong>of</strong> right ascension are hours, minutes, and seconds, and units <strong>of</strong> declination are degrees, arcminutes, and arcseconds.<br />
Table 4.2. Inferred Properties <strong>of</strong> Short-Timescale Flares in NGC 4697<br />
rflat ∆tflat Lflare Eflare<br />
Source Name Obs. nflat (10−3 s−1 ) (s) rflat/rpersistent (1038 ergs s−1 ) (1041 ergs)<br />
(1) (2) (3) (4) (5) (6) (7) (8)<br />
CXOU J124837.8−054652 (source A) .... 0784 3.7 +4.1 + 17.4<br />
−2.2 3.2 − 1.2 1168 +1418<br />
+ 99<br />
+ 23.2<br />
−1038 14 − 2 4.2 − 1.5 4.9 +5.4<br />
−3.0<br />
4727 2.6 +3.4 + 36.5<br />
−1.7 3.5 − 2.3 754 +3573<br />
+ 161<br />
+ 60.7<br />
− 701 12 − 6 5.8 − 3.9 4.4 +5.6<br />
−2.9<br />
4728 2.3 +3.0 + 24.8<br />
−1.5 4.5 − 2.6 609 +1681<br />
+ 117<br />
+ 39.8<br />
− 534 17 − 6 7.3 − 4.2 3.7 +4.8<br />
−2.4<br />
0784,4727,4728 844 +1399<br />
+ 74<br />
+ 25.4<br />
− 454 14 − 3 5.8 − 2.0 4.3 +3.0<br />
−1.6<br />
CXOU J124831.0−054828 (source B) ..... 4728 4.2 +4.6 + 11.7<br />
+ 789<br />
+ 234<br />
+ 19.5<br />
−2.6 2.8 − 0.5 1483 −1244 26 − 2 4.7 − 0.9 7.0 +7.7<br />
−4.2<br />
4729 3.0 +3.9 + 43.5<br />
−2.2 1.8 − 0.8 1662 +2739<br />
−1621 13 +1274<br />
+ 69.7<br />
− 2 2.9 − 0.8 4.8 +6.2<br />
−3.5<br />
4730 3.8 +4.2 + 19.0<br />
−2.3 0.6 − 0.1 6320 +1067<br />
+ ∞<br />
+ 31.1<br />
−6235 22 − 1 1.0 − 0.1 6.2 +6.8<br />
−3.8<br />
4727,4728 1573 +1425<br />
+ 649<br />
+ 18.4<br />
−1022 20 − 1 3.8 − 0.9 5.9 +4.9<br />
−2.7<br />
4727–4729 3155 +1015<br />
+ ∞<br />
+ 26.3<br />
−2187 20 − 1 2.9 − 0.5 6.0 +4.0<br />
−2.2<br />
CXOU J124839.0−054750 (source C) ..... 0784 2.8 +3.7 + 85.4<br />
+ 74<br />
+ 220<br />
−1.9 36.5 −10.9 78 − 52 76 − 20 48.5 +113.5<br />
− 14.5 3.8 +4.9<br />
−2.5<br />
4727 2.1 +3.3<br />
−1.5 37.1 +116.3<br />
+ 226<br />
+ 382<br />
−26.0 57 − 42 96 − 63 61.8 +193.5<br />
− 43.3 3.5 +5.5<br />
−2.5<br />
+ 119<br />
+ 220<br />
0784,4727 68 − 33 86 − 33 55.2 +112.2<br />
− 22.8 3.7 +3.7<br />
−1.8<br />
122
duration, ∆tflat, beginning at a given time, t0,flat. Outside <strong>of</strong> the flare duration, we<br />
assumed a constant persistent source rate rpersistent. For a given model flare rate<br />
rflat, duration ∆tflat, and beginning time t0,flat, we performed 200,000 Monte Carlo<br />
simulations. We varied the model parameters until we found the model that was<br />
most likely to have reproduced the observed flare properties. For this best-fit model,<br />
the symmetric 90% confidence region for each model parameter was determined from<br />
the simulations. The rates and durations were used to calculate X-ray luminosities<br />
and fluences for each observation using conversion factors based on the best-fit model<br />
for the cumulative X-ray spectrum <strong>of</strong> all the sources (a power-law with Γ = 1.47;<br />
Paper IV). The spectral model was corrected for Galactic absorption and the quantum<br />
efficiency degradation for each observation.<br />
In Table 4.2, we list the best-fit model properties <strong>of</strong> the flaring sources. Columns<br />
(1) and (2) list the source name and observation number. Columns (3)–(8) list the<br />
best-fit flare properties: number <strong>of</strong> flare photons (nflat), flare rate (rflat), flare dura-<br />
tion (∆tflat), ratio <strong>of</strong> flare rate to persistent rate, flare luminosity (Lflat), and flare<br />
fluence (Eflat). Rows with multiple observations listed display the averages <strong>of</strong> the<br />
flare duration, ratio <strong>of</strong> flare rate to persistent rate, flare luminosity, and flare fluence<br />
<strong>of</strong> the matching flares.<br />
Given our limited temporal coverage, it is difficult to place strong limits on the<br />
recurrence timescale (∆T ) <strong>of</strong> the flares. Our simulations show that the probability<br />
that our algorithm will detect a flare is only ∼50%. However, the fact that two<br />
flares were not seen in any single observation and that there are observations without<br />
observed flares for each <strong>of</strong> the sources implies that ∆T 5 hr. One upper limit on<br />
∆T is given by the shortest observed time between observations with flares; this is 11<br />
days for sources A and B, and 1441 days for source C. However, detections <strong>of</strong> flares in<br />
123
two or three out <strong>of</strong> five observations lasting ∼10 hr suggest that the recurrence time<br />
is much shorter than this, ∆T ≈ 10 hr. One caveat is that it is possible that most <strong>of</strong><br />
the LMXBs in NGC 4697 are undergoing flares with a longer recurrence timescale,<br />
and we have just selected the three sources where flares occurred within several <strong>of</strong><br />
our observing windows.<br />
4.4 Discussion<br />
4.4.1 CXOU J124837.8−054652 (Source A) and<br />
124<br />
CXOU J124831.0−054828 (Source B): Type-I X-ray<br />
Superbursts?<br />
Sources A and B both show similar flares, with average durations <strong>of</strong> 844 +1399<br />
− 454 s<br />
and 3155 +1015<br />
−2187 s, respectively. In source B, the longer flare in observation 4729 is less<br />
probable; however, the error bars <strong>of</strong> all its inferred properties overlap with the error<br />
bars <strong>of</strong> the other flares in source B. If one removed the observation 4729 flare, the<br />
average flare duration decreases to 1573 +1425<br />
−1022 s. Although the durations are larger<br />
than typical type I bursts, they are consistent within the uncertainties with type<br />
I superbursts. Since type I bursts are Eddington-limited, observations <strong>of</strong> distant<br />
galaxies may select for longer bursts, given the small numbers <strong>of</strong> photons in each<br />
burst. Thus, we may be observing relatively rare, extreme forms <strong>of</strong> type I superbursts.<br />
The average luminosities for the flares in sources A and are 5.8 +25.4<br />
− 2.0 and 2.9 +26.3<br />
− 0.5 ×<br />
10 38 ergs s −1 , respectively, higher than the Eddington luminosity <strong>of</strong> a 1.4 M⊙ NS ac-<br />
creting hydrogen. If one removed the Obs. 4729 flare from source B, the average flare<br />
luminosity increases to 3.8 +18.4<br />
− 0.9 × 10 38 ergs s −1 . The reported luminosities are for the<br />
0.3–10 keV band, and the bolometric luminosities would be even higher. Furthermore,
the uncertainties quoted do not include the systematic uncertainty in the distance to<br />
NGC 4697 (although this is smaller than the statistical uncertainties) or in the spec-<br />
tral model for the source. Typically, Galactic type I bursts can be modeled as ∼2<br />
keV blackbodies; if this model were used the observed luminosities would increase by<br />
a factor <strong>of</strong> ∼2.7.<br />
125<br />
The average fluences <strong>of</strong> the flares in these two sources are 4.3 +3.0<br />
−1.6 and 6.0 +4.0<br />
−2.2 ×<br />
10 41 ergs, respectively. Assuming the flares are powered by fusion <strong>of</strong> hydrogen and<br />
that the thermonuclear efficiency to the iron-peak elements is 0.007c 2 (Lewin et al.<br />
1995), this requires the accretion <strong>of</strong> ∼4 × 10 −11 M⊙. For accretion <strong>of</strong> helium and an<br />
efficiency <strong>of</strong> 0.002c 2 , the mass is ∼ 1 × 10 −10 M⊙. The persistent luminosities <strong>of</strong> the<br />
sources are ∼4 and ∼1×10 37 ergs s −1 implying accretion rates <strong>of</strong> ∼4 and ∼1×10 −9 M⊙<br />
yr −1 for an NS. Thus, it would require days to weeks to build up a layer sufficient to<br />
produce the observed flares as thermonuclear flashes. As noted above, the recurrence<br />
time for the flares is probably shorter than this, ∆T ≈ 10 hr. However, if most <strong>of</strong> the<br />
LMXBs in NGC 4697 produce similar flares, then the only limit is ∆T 11 days.<br />
The durations and fluences are similar to superbursts; however, the intervals between<br />
Galactic superbursts are much longer, on order <strong>of</strong> a year.<br />
Both sources are close to GCs in NGC 4697; thus, it is unlikely these sources are<br />
background active galactic nuclei (AGNs). Source A is 0. ′′ 1 from an HST ACS GC<br />
with g − z = 0.89 and z = 20.91. This source is a highly probable match. Source B<br />
is 0. ′′ 8 from an HST ACS GC with g − z = 1.32 and z = 19.15. Within 0. ′′ 8 at this<br />
projected position in the galaxy, the probability <strong>of</strong> a match occurring at random is<br />
1%. Thus, both <strong>of</strong> these flaring sources are probably located in GCs.
4.4.2 CXOU J124839.0−054750 (Source C)<br />
By itself, the flare in observation 0784 <strong>of</strong> source C is highly significant. The com-<br />
bination <strong>of</strong> a similar flare in observation 4727 makes it the most probable (99.995%)<br />
flaring source in this chapter.<br />
There is no clear optical counterpart for source C. The nearest globular cluster is<br />
1. ′′ 8 away. Given the rms <strong>of</strong> 0. ′′ 4 for X-ray/optical matches, we do not think this is a<br />
likely match. At this source’s radius from the center <strong>of</strong> NGC 4697 (48 ′′ ), one only<br />
expects ∼0.3 background sources at this flux level. There are 18 other sources as<br />
bright as source C and interior to it. Therefore, there is only a 1.6% probability the<br />
source is a background AGN from the X-ray data alone. The source is even less likely<br />
to be an AGN given the lack <strong>of</strong> an optical detection. We have estimated the 50%<br />
completeness limit near the source to be 24.9 in the z-band. Since, the X-ray flux in<br />
the 0.5–8.0 keV band is 4.2 × 10 −15 ergs s −1 cm −2 , log(FX/Fopt) is greater than 0.5. If<br />
we relax this to log(FX/Fopt) > 0.25 (z > 24.3), and look at GOODS X-ray selected<br />
sources (Treister et al. 2004), only 9.6% <strong>of</strong> the sources have log(FX/Fopt) > 0.25.<br />
Combining the expected X-ray background with the results for obscured AGN in the<br />
GOODS fields, we estimate that there is a 0.15% probability source C is an AGN.<br />
The flare behavior <strong>of</strong> source C has no clear analog in our own Galaxy. Its peak<br />
luminosity <strong>of</strong> 5.5 +11.2<br />
− 2.3 × 10 39 ergs s −1 (8 times the Eddington luminosity <strong>of</strong> a helium-<br />
burning NS) is clearly super-Eddington for an NS. These flares are not type I X-ray<br />
bursts. Since NGC 4697 is an elliptical galaxy, this source is unlikely to be an HMXB<br />
like LMC X−4 or V4641 Sgr.<br />
The outburst need not exceed the Eddington limit by much if the compact object<br />
is a 10 M⊙ BH. The flare timescale is similar to rapid transients seen in the BH XRBs,<br />
GRS1915+105 and V4641 Sgr. Compared to GRS1915+105, the ratio <strong>of</strong> flare rate<br />
126
to persistent rate for short flares is too high, and the recurrence timescale too long,<br />
arguing against accretion behavior like that in GRS1915+105. The rapid transient<br />
in V4641 Sgr, seen at the tail <strong>of</strong> a flare event with the Rossi X-Ray Timing Explorer<br />
(RXTE; Wijnands & van der Klis 2000), has the correct duration and peak luminosity<br />
(assuming a distance <strong>of</strong> ∼10 kpc, Orosz et al. 2001); however, its quiescent luminosity<br />
is too low compared to source C by more than a factor <strong>of</strong> 10. The activity in V4641<br />
Sgr has been attributed to super-Eddington accretion onto a black hole with the<br />
formation <strong>of</strong> an extended envelope (Revnivtsev et al. 2002). This variability might<br />
look like source C if it occurred during a long-term luminous stage, as has been seen<br />
in GRS1915+105.<br />
Since its behavior is most like LMC X−4, one might suggest that they have a<br />
similar phenomenology. That is, the flare might be due to density inhomogeneities in<br />
the accretion columns on a neutron star polar caps (Moon et al. 2003). This would<br />
require that source C have a large magnetic field. Since most Galactic LMXBs do<br />
not appear to have strong fields, it is thought that magnetic fields in NS binaries<br />
decay with time or as a result <strong>of</strong> accretion (Bhattacharya & Srinivasan 1995). Since<br />
an NS in NGC 4697 is unlikely to be newly formed, a strong magnetic field in an NS<br />
binary could only occur if accretion causes the magnetic field decay in LMXBs and<br />
millisecond pulsars, and if the neutron star in this binary has only recently begun to<br />
accrete from its donor.<br />
One possibility is that source C (and possibly sources A and B as well) are related<br />
to Galactic microquasar sources. Microquasars are XRBs with accreting BHs that<br />
produce relativistic jets (e.g., Mirabel & Rodríguez 1999). In most <strong>of</strong> the known<br />
Galactic examples, we are observing the sources at a large angle from the jet axis<br />
(see, however, Orosz et al. 2001). The very high luminosity <strong>of</strong> source C might be<br />
127
explained if we are seeing this source along the jet axis. In analogy to their AGN<br />
counterparts, microquasars observed along the jet axis are referred to as microblazars<br />
(Mirabel & Rodríguez 1999). Blazars are known to undergo relatively short timescale<br />
outbursts; the same phenomena, scaled to microblazars, might account for the X-ray<br />
flares in source C.<br />
4.5 Conclusions<br />
In this chapter, we have presented a new technique to detect short-timescale flares,<br />
both for individual and multiple observations <strong>of</strong> a given target. We also describe<br />
simulations used to estimate the intrinsic properties <strong>of</strong> the detected flares. Although<br />
these technique were used to perform the first search specifically targeting short-<br />
timescale flares from LMXBs in an early-type galaxy, they can be applied to other<br />
astrophysical sources whose X-ray data is count-limited.<br />
We detect three LMXB candidates that exhibit short-timescale flares. Two sources<br />
(A and B) appear to be in GCs and exhibit flares with average X-ray luminosities<br />
(0.3–10 keV) <strong>of</strong> 5.8 +25.4<br />
− 2.0 and 2.9 +26.3<br />
− 0.5 × 10 38 ergs s −1 over 844 +1399<br />
− 454 s and 3155 +1015<br />
−2187 s,<br />
respectively. Although the durations and fluences <strong>of</strong> the flares are similar to Galactic<br />
type I superbursts, the flares recur too <strong>of</strong>ten. Since their bolometric luminosities will<br />
be larger, these flares are likely to be super-Eddington for a 1.4 M⊙ NS accreting<br />
hydrogen. Thus, it is unlikely that these sources are undergoing type I superbursts.<br />
128<br />
The flare behavior <strong>of</strong> source C is more extreme. Its peak luminosity <strong>of</strong> 5.5 +11.2<br />
− 2.3 ×<br />
10 39 ergs s −1 (8 times the Eddington luminosity <strong>of</strong> a helium-burning NS) is clearly<br />
super-Eddington for an NS, while its duration is 68 +119<br />
− 33 s. Source C has no clear<br />
analog in our own Galaxy. One explanation for its X-ray flares, as well as those in<br />
sources A and B, may be that these sources are microblazars.
Chapter 5<br />
Multi-Epoch Chandra X-ray<br />
Observations <strong>of</strong> Low Mass X-ray<br />
Binary Candidates in the<br />
Early-Type Galaxy NGC 4697<br />
5.1 Introduction<br />
Although early-type galaxies have been known to be luminous X-ray sources since<br />
the time <strong>of</strong> the Einstein Observatory (Forman et al. 1985), it is only with the Chandra<br />
X-ray Observatory that the nature <strong>of</strong> their X-ray emission can be studied in detail.<br />
Prior to Chandra, observations <strong>of</strong> X-ray faint galaxies, galaxies with relatively low<br />
X-ray-to-optical luminosity ratios, indicated the presence <strong>of</strong> two distinct spectral<br />
components: a s<strong>of</strong>t (∼ 0.2 keV) component (Fabbiano et al. 1994; Pellegrini 1994;<br />
Kim et al. 1996) and a hard (∼ 5–10 keV) component (Matsumoto et al. 1997). While<br />
the s<strong>of</strong>t component was attributed to hot interstellar gas and the hard component<br />
129
was attributed to low-mass X-ray binaries (LMXBs; Kim et al. 1992), it is only with<br />
Chandra’s sub-arcsecond resolution that this picture could be verified.<br />
Starting with the Chandra observation <strong>of</strong> the X-ray faint elliptical, NGC 4697<br />
(Sarazin et al. 2000, 2001, hereafter Paper I; Paper II), the majority <strong>of</strong> X-ray emis-<br />
sion in X-ray faint early-type galaxies has been resolved into X-ray point sources,<br />
whose properties are consistent with LMXBs. With its ability to resolve LMXBs and<br />
accurately measure their positions, Chandra has raised at least two major issues re-<br />
garding the behavior <strong>of</strong> the LMXBs as a population, namely the connection between<br />
LMXBs and globular clusters (GCs) and the nature <strong>of</strong> the LMXB luminosity function<br />
(LF).<br />
From Chandra, a high percentage (∼ 20 − 70%) <strong>of</strong> LMXBs have positions coin-<br />
cident with globular clusters (GCs, Angelini et al. 2001; Sarazin et al. 2003); only<br />
∼ 10% <strong>of</strong> Milky Way LMXBs are found in GCs. This raised the question as to where<br />
LMXBs in early-type galaxies formed. One early suggestion was that all LMXBs in<br />
early-type galaxies formed in GCs, with LMXBs observed to be in the field <strong>of</strong> the<br />
galaxy (Field-LMXBs) having escaped from GCs through supernovae kick velocities,<br />
stellar dynamical processes, or the dissolution <strong>of</strong> the GC due to tidal effects (White<br />
et al. 2002). Later analyses have suggested that a significant fraction <strong>of</strong> Field-LMXBs<br />
were formed in situ (Juett 2005; Irwin 2005), although there is evidence that more<br />
Field-LMXBs in lenticular galaxies, as opposed to elliptical galaxies, may have orig-<br />
inated in GCs that have since escaped into the field (Irwin 2005). The extent to<br />
which LMXBs can be used to probe GC formation and evolution, as well as LMXB<br />
formation, depends critically on understanding the GC/LMXB connection. Given<br />
that the primary binary formation scenario in GCs is thought to involve dynamical<br />
interactions, as opposed to the predominantly primordial nature <strong>of</strong> binaries formed in<br />
130
the field, these different populations should trace different LMXB formation histories<br />
and may trace different star formation histories in early-type galaxies.<br />
Chandra has also explored the LF <strong>of</strong> LMXBs. At the bright end <strong>of</strong> the LF <strong>of</strong><br />
NGC 4697, a possible break in the LF near the Eddington limit <strong>of</strong> a 1.4 M⊙ neutron<br />
star (NS) was found in Paper I. This break was argued to be due to the presence<br />
<strong>of</strong> two LMXB populations, a black hole (BH) population at the bright end, and a<br />
NS population at the faint end. Bildsten & Deloye (2004) argued that such a break<br />
may be due to ultracompact binaries. Although Kim & Fabbiano (2003) argue that<br />
no break was required in NGC 4697 after correcting for incompleteness, they do<br />
find that a break near 5 × 10 38 ergs s −1 gives an improved fit compared to a single<br />
power-law for a uniformly selected, incompleteness corrected sample <strong>of</strong> 14 early-type<br />
galaxies. At the faint end, Voss & Gilfanov (2006) found that the LF in Cen A<br />
flattens significantly below 5 × 10 37 ergs s −1 and follows the dN/dL ∝ L −1 law in<br />
agreement with the behavior found for LMXBs in the Milky Way and the bulge <strong>of</strong><br />
M31. One interpretation <strong>of</strong> this break in the Milky Way LF is that there are two<br />
populations <strong>of</strong> short ( 20 hr) period LMXBs: those where magnetized stellar winds<br />
dominate mass transfer, and those where gravitational radiation drives the accretion<br />
(Postnov & Kuranov 2005). Measuring and understanding the LF <strong>of</strong> LMXBs in early-<br />
type galaxies has clear implications in our understanding <strong>of</strong> the number and type <strong>of</strong><br />
binary systems that make up the zoo <strong>of</strong> LMXBs.<br />
Examples <strong>of</strong> extragalactic LMXB candidates with extreme behaviors, such as<br />
supers<strong>of</strong>t sources (SSs), ultraluminous X-ray sources (ULXs), and flaring sources,<br />
have also been examined with Chandra in greater detail. The SSs have very s<strong>of</strong>t<br />
X-ray spectra ( 75 eV) similar to SSs in our Galaxy and M31 that are generally<br />
believed to be accreting white dwarfs (WDs); however, the bolometric luminosities<br />
131
<strong>of</strong> extragalactic SSs can exceed the Eddington luminosity for a Chandrasekhar mass<br />
WD. One hypothesis is that these sources contain intermediate-mass (∼ 10 2 –10 3 M⊙)<br />
accreting BHs (Swartz et al. 2002). Due to the degradation <strong>of</strong> the s<strong>of</strong>t response<br />
<strong>of</strong> the Advanced CCD Imaging Spectrometer (ACIS) on Chandra, the study <strong>of</strong> SSs<br />
have been limited. A great deal <strong>of</strong> attention has been spent on ULXs, which we<br />
define as LX > 2 × 10 39 ergs s −1 (0.3–10.0 keV). However, except possibly for LMXB<br />
candidates in NGC 720 (Jeltema et al. 2003), NGC 1399 (Angelini et al. 2001), NGC<br />
1600 (Sivak<strong>of</strong>f et al. 2004), and NGC 4552 (Xu et al. 2005), ULXs are generally not<br />
found within old stellar systems (Irwin et al. 2004) beyond the number expected from<br />
unrelated foreground or background sources. Recently, XMM-Newton detected type<br />
I X-ray bursts in M31 (Pietsch & Haberl 2005) and we reported a more extreme<br />
example <strong>of</strong> flares in NGC 4697 (Sivak<strong>of</strong>f et al. 2005, hereafter Chapter 5).<br />
By stacking multi-epoch Chandra observations <strong>of</strong> an early-type galaxy, more,<br />
fainter LMXB candidates can be studied, and brighter LMXB candidates can be<br />
studied in greater detail. Moreover, such observations open up an important regime<br />
<strong>of</strong> behavior — interobservation variability. Low mass X-ray binaries exhibit a wide<br />
range <strong>of</strong> variability, including transient outbursts, type I bursts, and milder fluc-<br />
tuations. Our understanding <strong>of</strong> LMXB variability in the Galaxy drives models for<br />
accretion and LMXB evolution. However, there are several limitations in studying<br />
Galactic LMXBs: source distances are known for only a small subset, it is difficult to<br />
observe the whole Galaxy at once, and the size <strong>of</strong> the observed sample is very limited.<br />
Observations <strong>of</strong> nearby early-type galaxies can overcome these limitations <strong>of</strong> Galactic<br />
studies.<br />
In this chapter, we report on multi-epoch Chandra X-ray observations <strong>of</strong><br />
NGC 4697, the nearest (11.3 Mpc 1 ; S. Mei 2005, private communication), optically<br />
132<br />
1 The distance calibration (Mei et al. 2005) uses Hubble Key Project distances from Freedman
luminous (MB < −20) elliptical (E6) galaxy 2 . We adopted the 2MASS Point Source<br />
Catalog 3 position <strong>of</strong> R.A. = 12 h 48 m 35. s 90 and Dec. = −5 ◦ 48 ′ 02. ′′ 6 as the location<br />
<strong>of</strong> the center <strong>of</strong> NGC 4697 and the Third Reference Catalogue <strong>of</strong> Bright Galaxies<br />
(RC3) values for the optical photometry’s effective radius (reff = 72. ′′ 0), position an-<br />
gle (P A = 70 ◦ , measured from north to east), and ellipticity (e = 0.354), which<br />
assumes a de Vaucouleurs pr<strong>of</strong>ile (de Vaucouleurs et al. 1992). From these values, we<br />
calculate the optical photometry’s effective semi-major distance (aeff = 89. ′′ 6). This<br />
galaxy lies ∼ 5 Mpc in front <strong>of</strong> the bulk <strong>of</strong> the galaxies in the Virgo cluster, and<br />
18. ◦ 7 south <strong>of</strong> M87, the central galaxy <strong>of</strong> the Virgo cluster. We also report on the<br />
GC/LMXB connection as determined from a joint observation <strong>of</strong> the central region<br />
by the Hubble Space Telescope Advance Camera for Surveys (HST-ACS).<br />
In § 5.2, we discuss the observations and data reduction <strong>of</strong> NGC 4697. The X-ray<br />
image and the detection <strong>of</strong> X-ray sources are discussed in § 5.3 and § 5.4. In § 5.5,<br />
we discuss the optical counterparts from ground-based and HST observations. We<br />
examine the GC/LMXB connection in detail in § 5.6. The analyses <strong>of</strong> luminosity,<br />
hardness ratios, and spectra are considered in §§ 5.7–5.9. We concentrate on the<br />
variability <strong>of</strong> the X-ray sources in § 5.10. Finally, we summarize our conclusions in<br />
§ 5.11. Unless otherwise noted, all errors refer to 1σ confidence intervals, count rates<br />
are in the 0.3–6 keV band, and fluxes and luminosities are in the 0.3–10 keV band.<br />
et al. (2001).<br />
2There is a weak disk; however, it not comparable to those seen in lenticular galaxies (Peletier<br />
et al. 1990).<br />
3See http://www.ipac.caltech.edu/2mass/releases/allsky/doc/explsup.html.<br />
133
5.2 Observations and Data Reduction<br />
5.2.1 Chandra X-ray Observatory<br />
Chandra has observed NGC 4697 five times, 2000 January 15, 2003 December<br />
26, 2004 January 06, February 02, and August 18, using the ACIS detector for live<br />
exposures <strong>of</strong> 39260, 39920, 35683, 38103, and 40046 s (Observations 0784, 4727, 4728,<br />
4729, and 4730). Observation 0784 was operated at −110 deg C with a frame time <strong>of</strong><br />
3.2 s, and the ACIS-23678 chips were telemetered and cleaned in Faint mode. Obser-<br />
vations 4727, 4728, 4729, 4730 (hereafter the Cycle-5 observations) were operated at<br />
−120 deg C with frame times <strong>of</strong> 3.1 s, and the ACIS-35678 chips were telemetered and<br />
cleaned in Very-Faint mode. Since the X-ray point spread function (PSF) increases<br />
as the distance between point sources and the optical axis <strong>of</strong> Chandra, the Cycle-5<br />
pointings were determined to maximize field-<strong>of</strong>-view (FOV) while placing the galaxy<br />
center close to the optical axis and away from node boundaries on the S3 chip. The<br />
analysis in this chapter is based on data from the S3 chip alone, although a number<br />
<strong>of</strong> serendipitous sources were seen on the other chips. The elliptical area common to<br />
all five observations on the S3 chip (a < 220 ′′ ) corresponds to 74% <strong>of</strong> the integrated<br />
light for a de Vaucouleurs pr<strong>of</strong>ile. Known aspect <strong>of</strong>fsets were applied for each ob-<br />
servation. Our analysis includes only events with ASCA grades <strong>of</strong> 0, 2, 3, 4, and 6.<br />
Photon energies were determined using the gain files acisD1999-09-16gainN0005.fits<br />
(Observation 0784) and acisD2000-01-29gain ctiN0001.fits (Cycle-5 observations). In<br />
the latter cases, we corrected for time dependence <strong>of</strong> the gain and the charge-transfer<br />
inefficiency. All five observations were corrected for quantum efficiency (QE) degra-<br />
dation and had exposure maps determined at 750 eV. We excluded bad pixels, bad<br />
columns, and columns adjacent to bad columns or chip node boundaries.<br />
134
Although Chandra is known to encounter periods <strong>of</strong> high background (“back-<br />
ground flares”), which especially affect the backside-illuminated S1 and S3 chips 4 ,<br />
the use <strong>of</strong> local backgrounds in point source analysis mitigates the effect <strong>of</strong> flaring.<br />
To avoid periods with extreme flaring we only included times where the blank-sky<br />
rate was less than three times the expected blank-sky rate derived from calibrated<br />
blank-sky backgrounds. For Observation 0784, the S3 chip itself, excluding regions<br />
<strong>of</strong> emission, was used as the observed blank-sky and checked against Maxim Marke-<br />
vitch’s aciss B 7 bg evt 271103.fits blank-sky background 4 using 0.3–10.0 keV count<br />
rates. For the Cycle-5 observations, the S1 chip was used, excluding regions <strong>of</strong> emis-<br />
sion, and compared to the blank-sky background in CALDB using 2.6–6.0 keV count<br />
rates. Minimal time was lost in all observations due to the binning used to check the<br />
rates; more extensive time was lost in Observation 4729 due to a large background<br />
flare. No periods <strong>of</strong> data dropout were observed. Final flare-filtered live exposure<br />
times for the five observations were 37174, 39919, 35601, 32038, and 40044 s.<br />
We registered the Cycle-5 observations astrometry against the Observation 0784<br />
astrometry (see § 5.4). No absolute astrometric correction was necessary (See § 5.5.1.).<br />
For imaging and source detection only, we created a merged events file and exposure<br />
map with a live exposure time <strong>of</strong> 184775 s. In this chapter, we analyze the 158 sources<br />
detected from the merged events file.<br />
All Chandra observations were analyzed using ciao 3.1 5 with caldb 2.28 and<br />
NASA’s ftools 5.3 6 . Source positions and extraction regions were refined using<br />
ACIS Extract 3.34 7 . All spectra were fit using xspec 6 .<br />
4 See http://cxc.harvard.edu/contrib/maxim/acisbg/.<br />
5 See http://asc.harvard.edu/ciao/.<br />
6 See http://heasarc.gsfc.nasa.gov/docs/s<strong>of</strong>tware/lheas<strong>of</strong>t/.<br />
7 See http://www.astro.psu.edu/xray/docs/TARA/ae users guide.html.<br />
135
5.2.2 Hubble Space Telescope<br />
We observed the center <strong>of</strong> NGC 4697 with the Hubble Space Telescope Advance<br />
Camera for Surveys (HST-ACS), acquiring two 375 s exposures in the F475W (g475)<br />
band, two 560 s exposures in the F850LP (z850) band, and one 90 s F850LP expo-<br />
sure. Source detection and characterization were performed similarly to Jordán et al.<br />
(2004a), leading to a list <strong>of</strong> globular clusters (GCs) and other optical sources. Details<br />
concerning the HST-ACS observation, data analysis, and optical source properties<br />
are given in Jordán et al. (2006, in preparation).<br />
5.3 X-ray Image<br />
In Paper I and Paper II, it was shown that most <strong>of</strong> the X-ray emission in NGC 4697<br />
is resolved into point sources. We display the raw Chandra image from the combi-<br />
nation <strong>of</strong> all five observations in the 0.3–6 keV band in Figures 5.1 and 5.2. These<br />
images are roughly consistent with the previously published data; new sources have<br />
been detected due to greater sensitivity, source variability, and increased FOV. The<br />
FOV <strong>of</strong> the five observations, as well as a finding chart for the X-ray sources, are<br />
overlaid on the raw images.<br />
To contrast the detected sources with the diffuse emission, we adaptively smoothed<br />
the Chandra S3 X-ray raw image using a minimum signal-to-noise ratio (S/N) per<br />
smoothing beam <strong>of</strong> 3. We then applied these smoothing scales to background-<br />
subtracted, exposure-corrected images in the s<strong>of</strong>t (0.3–1 keV), medium (1–2 keV),<br />
and hard (2–6 keV) bands. The background includes the readout artifact in ACIS<br />
and the deep blank-sky backgrounds compiled by Maxim Markevitch 4 . We combined<br />
these three bands to create a logarithmically scaled image between 5 × 10 −7 and<br />
136
42:00.0<br />
44:00.0<br />
46:00.0<br />
48:00.0<br />
-5:50:00.0<br />
52:00.0<br />
54:00.0<br />
150<br />
149<br />
154<br />
148<br />
139<br />
140<br />
Obs. 4730<br />
143<br />
128<br />
158<br />
136<br />
156<br />
12:49:00.0 50.0 40.0 30.0 20.0 48:10.0<br />
157<br />
127 106<br />
98 90<br />
87<br />
131<br />
97<br />
134 146<br />
116<br />
96<br />
126<br />
113<br />
92 103 133<br />
125<br />
108 107 109<br />
115 89<br />
OC<br />
88<br />
91<br />
111<br />
130<br />
93 121<br />
144<br />
117<br />
104<br />
132<br />
110<br />
94<br />
95<br />
101<br />
99<br />
114<br />
100<br />
123 135<br />
124<br />
141<br />
137<br />
112<br />
102 105 122<br />
147<br />
119<br />
120<br />
118<br />
142<br />
153<br />
152<br />
129<br />
145<br />
138<br />
155<br />
Obs. 4727-4729<br />
Obs. 0784<br />
Fig. 5.1.— Chandra S3 image (0.3–6 keV) <strong>of</strong> NGC 4697 from all five observations<br />
combined. This image has not been corrected for background or exposure, and has<br />
not been smoothed. The gray scale varies with the logarithm <strong>of</strong> the X-ray surface<br />
brightness, which ranges from 1 to 25 count pixel −1 . (The ACIS pixels are 0. ′′ 492<br />
square.) The optical center <strong>of</strong> NGC 4697 is marked by “OC”. The positions <strong>of</strong><br />
detected sources outside <strong>of</strong> the central 3 ′ × 3 ′ in the image are indicated by their<br />
source numbers in Table 5.1; the source numbers are ordered by increasing distance<br />
from the center <strong>of</strong> the galaxy. The FOV <strong>of</strong> each observation is indicated by a labeled<br />
black square and the D25 ellipse is shown. (D25 is the elliptical isophote with a<br />
surface brightness <strong>of</strong> 25 mag per arcsec in the B-band.)<br />
151<br />
137
86<br />
47:00.0<br />
30.0<br />
83<br />
-5:48:00.0<br />
78<br />
30.0<br />
49:00.0<br />
30.0<br />
76<br />
74<br />
65<br />
66<br />
64<br />
85<br />
82<br />
68 67<br />
63<br />
58<br />
57<br />
52<br />
56<br />
46<br />
71<br />
50<br />
49<br />
28<br />
29<br />
31<br />
19<br />
41<br />
26<br />
20<br />
16<br />
40<br />
15<br />
23<br />
39<br />
53<br />
9<br />
12<br />
8 7<br />
55<br />
14<br />
30<br />
34<br />
79<br />
21<br />
18<br />
10<br />
5<br />
2 1 4<br />
35<br />
62<br />
33<br />
59<br />
61<br />
138<br />
40.0 38.0 36.0 34.0 32.0 12:48:30.0<br />
Fig. 5.2.— Chandra S3 image (0.3–6 keV) <strong>of</strong> the central 3 ′ × 3 ′ <strong>of</strong> NGC 4697 from all<br />
five observations. The optical center <strong>of</strong> NGC 4697 lies within the circle for Source 1.<br />
The gray scale is the same as in Figure 5.1. The positions <strong>of</strong> detected sources in the<br />
image are indicated by their source numbers in Table 5.1<br />
11<br />
6<br />
3<br />
13<br />
24<br />
47<br />
32<br />
25<br />
17<br />
27<br />
42<br />
43<br />
22<br />
84<br />
36<br />
37<br />
51<br />
38<br />
44<br />
60<br />
45<br />
48<br />
54<br />
77<br />
81<br />
69<br />
70<br />
73<br />
72<br />
75<br />
80
Fig. 5.3.— Adaptively smoothed Chandra true-color S3 image (with red = 0.3–<br />
1 keV, green = 1–2 keV, and blue = 2–6 keV) <strong>of</strong> NGC 4697 (all five observations),<br />
corrected for exposure and blank-sky background. The intensity scale for the colors<br />
is logarithmic and ranges from 5 × 10 −7 to 1 × 10 −5 count s −1 arcsec −2 in total surface<br />
brightness. The D25 ellipse is shown.<br />
139
Fig. 5.4.— Adaptively smoothed Chandra true-color S3 image (with red = 0.3–1 keV,<br />
green = 1–2 keV, and blue = 2–6 keV) <strong>of</strong> the central 3 ′ × 3 ′ <strong>of</strong> NGC 4697 (all five<br />
observations), corrected for exposure and blank-sky background. The color scaling is<br />
the same as in Figure 5.3.<br />
140
1 × 10 −5 count s −1 arcsec −2 in total surface brightness. The resulting true-color im-<br />
ages <strong>of</strong> the entire galaxy and <strong>of</strong> the central 3 ′ × 3 ′ region are shown in Figures 5.3<br />
& 5.4. There is clearly s<strong>of</strong>t (red) diffuse emission near the center <strong>of</strong> NGC 4697. The<br />
majority <strong>of</strong> the sources stand out clearly in color from the s<strong>of</strong>t diffuse gas, appearing<br />
yellow to green. There are some s<strong>of</strong>t sources which appear to be associated with<br />
NGC 4697 based on their concentration towards the center <strong>of</strong> the galaxy, while most<br />
<strong>of</strong> the hardest (blue) sources, which are likely to be absorbed AGNs (see § 5.8), tend<br />
to lie in the outer regions <strong>of</strong> the image.<br />
5.4 X-ray Source Detection<br />
In Table 5.1, we list all discrete sources detected by wavdetect over the 0.3–<br />
6 keV range. We ordered the sources by increasing projected radial distance from the<br />
center <strong>of</strong> the galaxy, d. Columns 1–8 provide the source number, IAU name, source<br />
position (J2000), projected radial distance, projected semi-major distance from the<br />
center <strong>of</strong> NGC 4697, a, photometric count rate with its 1σ error, and S/N for the count<br />
rate. Photon errors were calculated using the upper Gehrels error approximation <strong>of</strong><br />
1 + √ N + 0.75 (Gehrels 1986). For comparison with Paper II, column 10 lists the<br />
source number used there. Notes for each source are listed in column 11. The derived<br />
parameters and notes are expanded upon in the text below.<br />
To identify the discrete X-ray source population, we applied the wavelet detection<br />
algorithm (ciao wavdetect program) with √ 2 scales ranging from 1 to 32 pixels<br />
with a source detection threshold <strong>of</strong> 10 −6 . Source detection was not done in regions<br />
with an exposure <strong>of</strong> less then 10% <strong>of</strong> the total for the observation. We expect 1<br />
false source (due to a statistical fluctuation in the background) for each S3 image.<br />
The sources detections were first done on each observation separately to create a<br />
141
Table 5.1. Discrete X-ray Sources in NGC 4697<br />
Source R.A. Dec. d a Count Rate Paper II<br />
No. Name (h m s) ( ◦ ′ ′′ ) ( ′′ ) ( ′′ ) (10−4 s−1 ) S/N csim Source Notes<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11)<br />
1 CXOU J124835.8−054802 12 48 35.86 −05 48 02.7 0.45 0.46 25.57±1.26 20.24 1.00 1 c<br />
2 CXOU J124836.0−054803 12 48 36.03 −05 48 03.3 2.26 2.84 5.58±0.63 8.86 1.00 2 a<br />
3 CXOU J124835.8−054759 12 48 35.81 −05 47 59.9 2.89 4.47 2.77±0.50 5.57 1.00 · · · · · ·<br />
4 CXOU J124835.6−054804 12 48 35.68 −05 48 04.1 3.53 3.56 7.60±0.75 10.16 1.00 3 · · ·<br />
5 CXOU J124836.1−054802 12 48 36.15 −05 48 02.1 3.96 4.12 6.73±0.68 9.91 1.00 4 a<br />
6 CXOU J124835.6−054757 12 48 35.65 −05 47 57.8 5.88 8.87 2.95±0.50 5.93 1.00 5 · · ·<br />
7 CXOU J124835.9−054756 12 48 35.96 −05 47 56.5 6.07 8.69 13.34±0.93 14.40 1.00 6 · · ·<br />
8 CXOU J124836.2−054758 12 48 36.29 −05 47 58.7 7.07 7.29 1.39±0.40 3.53 1.04 · · · b,f<br />
9 CXOU J124836.5−054801 12 48 36.56 −05 48 01.8 10.06 10.59 2.66±0.49 5.47 1.00 7?,10? · · ·<br />
10 CXOU J124835.9−054752 12 48 35.90 −05 47 52.3 10.19 15.18 13.08±0.94 13.98 1.00 8 · · ·<br />
11 CXOU J124835.3−054754 12 48 35.37 −05 47 54.6 11.16 16.37 7.09±0.70 10.09 1.00 9 · · ·<br />
12 CXOU J124836.3−054812 12 48 36.30 −05 48 12.0 11.36 17.33 2.93±0.50 5.91 1.00 11 · · ·<br />
13 CXOU J124835.1−054811 12 48 35.14 −05 48 11.2 14.26 15.16 3.04±0.50 6.04 1.00 12 · · ·<br />
14 CXOU J124836.2−054816 12 48 36.22 −05 48 16.1 14.49 22.43 3.52±0.52 6.71 1.00 13 · · ·<br />
15 CXOU J124836.9−054801 12 48 36.95 −05 48 01.1 15.84 16.55 10.62±0.84 12.71 1.00 14 d<br />
16 CXOU J124836.9−054810 12 48 36.92 −05 48 10.8 17.49 23.34 2.37±0.47 5.01 1.00 15 · · ·<br />
17 CXOU J124834.7−054806 12 48 34.74 −05 48 06.6 17.60 17.75 0.94±0.33 2.84 1.16 · · · · · ·<br />
18 CXOU J124835.4−054745 12 48 35.47 −05 47 45.2 18.40 28.48 0.59±0.27 2.19 2.74 · · · · · ·<br />
19 CXOU J124837.1−054759 12 48 37.15 −05 47 59.1 19.14 19.52 6.62±0.68 9.77 1.00 16 · · ·<br />
20 CXOU J124837.0−054753 12 48 37.03 −05 47 53.6 19.14 19.38 2.33±0.45 5.19 1.00 17 · · ·<br />
21 CXOU J124835.7−054742 12 48 35.77 −05 47 42.1 20.50 31.12 0.59±0.29 2.05 2.34 · · · · · ·<br />
22 CXOU J124834.5−054759 12 48 34.51 −05 47 59.4 20.84 23.96 1.89±0.42 4.53 1.00 18 b<br />
23 CXOU J124836.8−054817 12 48 36.89 −05 48 17.2 20.92 30.57 0.65±0.29 2.20 2.11 · · · · · ·<br />
24 CXOU J124834.6−054814 12 48 34.67 −05 48 14.8 21.91 22.79 0.78±0.33 2.35 1.37 · · · · · ·<br />
Continued on Next Page. . .<br />
142
Table 5.1—Continued<br />
Source R.A. Dec. d a Count Rate Paper II<br />
No. Name (h m s) ( ◦ ′ ′′ ) ( ′′ ) ( ′′ ) (10−4 s−1 ) S/N csim Source Notes<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11)<br />
25 CXOU J124834.5−054749 12 48 34.52 −05 47 49.5 24.18 33.14 5.44±0.62 8.83 1.00 19 · · ·<br />
26 CXOU J124837.3−054749 12 48 37.36 −05 47 49.7 25.36 25.91 0.55±0.31 1.76 3.20 · · · · · ·<br />
27 CXOU J124834.4−054820 12 48 34.48 −05 48 20.3 27.57 29.79 2.18±0.44 4.98 1.00 · · · · · ·<br />
28 CXOU J124837.7−054801 12 48 37.79 −05 48 01.8 28.31 30.25 1.31±0.37 3.50 1.01 21 · · ·<br />
29 CXOU J124837.7−054806 12 48 37.77 −05 48 06.5 28.38 32.50 8.76±0.77 11.42 1.00 20 · · ·<br />
30 CXOU J124836.0−054732 12 48 36.07 −05 47 32.4 30.24 44.27 2.36±0.44 5.41 1.00 23 · · ·<br />
31 CXOU J124837.5−054743 12 48 37.50 −05 47 43.5 30.61 32.68 16.52±1.02 16.21 1.00 24 · · ·<br />
32 CXOU J124834.4−054740 12 48 34.48 −05 47 40.1 30.75 45.38 16.91±1.03 16.44 1.00 22 · · ·<br />
33 CXOU J124835.0−054831 12 48 35.03 −05 48 31.0 31.27 40.96 0.65±0.30 2.13 1.84 · · · · · ·<br />
34 CXOU J124836.0−054833 12 48 36.08 −05 48 33.6 31.28 47.50 4.83±0.61 7.91 1.00 25 · · ·<br />
35 CXOU J124835.3−054732 12 48 35.30 −05 47 32.5 31.30 48.40 7.69±0.71 10.77 1.00 26 · · ·<br />
36 CXOU J124833.9−054815 12 48 33.97 −05 48 15.8 31.62 31.77 0.62±0.28 2.19 1.96 · · · · · ·<br />
37 CXOU J124833.8−054751 12 48 33.87 −05 47 51.4 32.08 40.35 1.47±0.37 3.98 1.00 · · · · · ·<br />
38 CXOU J124833.7−054810 12 48 33.78 −05 48 10.7 32.57 32.78 1.32±0.37 3.58 1.01 · · · · · ·<br />
39 CXOU J124836.7−054731 12 48 36.71 −05 47 31.8 32.98 44.00 16.84±1.02 16.45 1.00 27 · · ·<br />
40 CXOU J124837.1−054830 12 48 37.13 −05 48 30.4 33.48 50.99 1.07±0.33 3.21 1.04 · · · · · ·<br />
41 CXOU J124836.9−054732 12 48 36.95 −05 47 32.7 33.73 43.05 1.92±0.40 4.84 1.00 · · · · · ·<br />
42 CXOU J124834.3−054734 12 48 34.34 −05 47 34.5 36.37 54.44 7.53±0.71 10.64 1.00 28 · · ·<br />
43 CXOU J124834.3−054831 12 48 34.34 −05 48 31.2 36.92 43.24 0.48±0.25 1.89 3.51 · · · · · ·<br />
44 CXOU J124833.7−054820 12 48 33.74 −05 48 20.9 36.96 37.70 1.52±0.37 4.06 1.00 · · · · · ·<br />
45 CXOU J124833.3−054802 12 48 33.33 −05 48 02.3 38.22 41.29 1.23±0.34 3.60 1.00 29 · · ·<br />
46 CXOU J124838.2−054747 12 48 38.28 −05 47 47.5 38.64 38.71 6.14±0.66 9.33 1.00 30 · · ·<br />
47 CXOU J124834.6−054727 12 48 34.64 −05 47 27.3 39.87 61.37 0.83±0.30 2.73 1.17 · · · · · ·<br />
48 CXOU J124833.3−054816 12 48 33.31 −05 48 16.4 41.01 41.02 4.19±0.57 7.30 1.00 31 · · ·<br />
Continued on Next Page. . .<br />
143
Table 5.1—Continued<br />
Source R.A. Dec. d a Count Rate Paper II<br />
No. Name (h m s) ( ◦ ′ ′′ ) ( ′′ ) ( ′′ ) (10−4 s−1 ) S/N csim Source Notes<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11)<br />
49 CXOU J124837.7−054731 12 48 37.78 −05 47 31.7 41.74 47.56 7.63±0.71 10.73 1.00 32 a<br />
50 CXOU J124837.7−054729 12 48 37.70 −05 47 29.3 42.79 50.04 1.69±0.38 4.48 1.04 34 a<br />
51 CXOU J124833.9−054834 12 48 33.93 −05 48 34.6 43.45 49.54 2.37±0.46 5.22 1.00 33 · · ·<br />
52 CXOU J124838.6−054746 12 48 38.65 −05 47 46.9 44.09 44.10 8.19±0.73 11.14 1.00 35 · · ·<br />
53 CXOU J124836.6−054846 12 48 36.67 −05 48 46.2 45.21 69.83 1.74±0.39 4.45 1.01 · · · · · ·<br />
54 CXOU J124833.1−054741 12 48 33.19 −05 47 41.9 45.29 59.87 41.02±1.57 26.18 1.00 36 · · ·<br />
55 CXOU J124836.4−054847 12 48 36.47 −05 48 47.4 45.77 70.33 6.82±0.68 9.99 1.00 37 f<br />
56 CXOU J124838.1−054728 12 48 38.18 −05 47 28.9 47.92 53.35 2.51±0.45 5.55 1.00 38 · · ·<br />
57 CXOU J124839.0−054750 12 48 39.02 −05 47 50.1 48.36 48.63 4.91±0.60 8.24 1.00 39 · · ·<br />
58 CXOU J124839.3−054807 12 48 39.31 −05 48 07.3 51.18 57.36 42.63±1.59 26.79 1.00 40 · · ·<br />
59 CXOU J124835.0−054856 12 48 35.06 −05 48 56.0 54.89 77.25 1.15±0.34 3.45 1.08 · · · · · ·<br />
60 CXOU J124833.6−054849 12 48 33.60 −05 48 49.4 58.05 69.50 0.41±0.26 1.58 5.41 · · · · · ·<br />
61 CXOU J124834.9−054859 12 48 34.91 −05 48 59.4 58.75 82.02 12.41±0.90 13.78 1.00 41 · · ·<br />
62 CXOU J124835.0−054704 12 48 35.00 −05 47 04.7 59.35 91.47 0.69±0.28 2.48 1.27 · · · · · ·<br />
63 CXOU J124839.3−054730 12 48 39.33 −05 47 30.5 60.47 62.26 19.81±1.12 17.62 1.00 42 · · ·<br />
64 CXOU J124839.7−054741 12 48 39.75 −05 47 41.2 61.33 61.33 0.77±0.30 2.54 1.98 · · · · · ·<br />
65 CXOU J124840.0−054800 12 48 40.06 −05 48 00.2 62.29 66.25 0.79±0.29 2.75 1.22 · · · · · ·<br />
66 CXOU J124839.9−054738 12 48 39.90 −05 47 38.3 64.56 64.62 7.05±0.70 10.10 1.00 43 · · ·<br />
67 CXOU J124838.8−054714 12 48 38.82 −05 47 14.5 64.93 74.08 4.41±0.57 7.78 1.00 · · · · · ·<br />
68 CXOU J124839.0−054714 12 48 39.01 −05 47 14.5 66.84 75.22 7.63±0.73 10.52 1.00 44 · · ·<br />
69 CXOU J124832.6−054851 12 48 32.63 −05 48 51.2 68.83 76.93 10.08±0.83 12.12 1.00 45 · · ·<br />
70 CXOU J124831.8−054838 12 48 31.83 −05 48 38.6 70.59 72.28 1.57±0.39 4.07 1.00 46 · · ·<br />
71 CXOU J124837.8−054652 12 48 37.85 −05 46 52.9 75.55 99.97 3.64±0.53 6.90 1.00 48 · · ·<br />
72 CXOU J124831.6−054844 12 48 31.66 −05 48 44.4 75.79 78.65 1.36±0.34 4.03 1.95 · · · a<br />
Continued on Next Page. . .<br />
144
Table 5.1—Continued<br />
Source R.A. Dec. d a Count Rate Paper II<br />
No. Name (h m s) ( ◦ ′ ′′ ) ( ′′ ) ( ′′ ) (10−4 s−1 ) S/N csim Source Notes<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11)<br />
73 CXOU J124831.7−054846 12 48 31.71 −05 48 46.7 76.49 80.13 4.77±0.57 8.30 1.00 47 a<br />
74 CXOU J124840.8−054823 12 48 40.86 −05 48 23.1 76.93 93.31 1.30±0.34 3.84 1.00 50 · · ·<br />
75 CXOU J124831.0−054828 12 48 31.03 −05 48 28.7 77.14 77.14 3.78±0.53 7.19 1.00 49 · · ·<br />
76 CXOU J124840.9−054731 12 48 40.91 −05 47 31.5 81.04 81.15 3.99±0.56 7.13 1.00 51 · · ·<br />
77 CXOU J124833.1−054913 12 48 33.17 −05 49 13.1 81.48 102.38 3.34±0.51 6.56 1.00 · · · · · ·<br />
78 CXOU J124841.2−054819 12 48 41.25 −05 48 19.7 81.79 96.62 4.21±0.54 7.79 1.00 52 · · ·<br />
79 CXOU J124835.7−054640 12 48 35.78 −05 46 40.6 81.87 122.80 1.61±0.39 4.14 1.00 · · · d<br />
80 CXOU J124830.8−054837 12 48 30.81 −05 48 37.0 83.36 83.71 24.61±1.23 19.95 1.00 53 d<br />
81 CXOU J124832.8−054913 12 48 32.85 −05 49 13.6 84.40 103.92 1.06±0.34 3.09 1.05 · · · · · ·<br />
82 CXOU J124838.9−054650 12 48 38.91 −05 46 50.2 85.13 105.34 0.81±0.29 2.84 1.09 · · · · · ·<br />
83 CXOU J124841.4−054737 12 48 41.49 −05 47 37.2 87.28 87.47 3.95±0.55 7.13 1.00 55 d<br />
84 CXOU J124834.1−054926 12 48 34.17 −05 49 26.4 87.75 120.66 2.17±0.43 5.08 1.00 54 f<br />
85 CXOU J124839.2−054645 12 48 39.21 −05 46 45.6 91.48 112.44 3.46±0.51 6.75 1.00 56 · · ·<br />
86 CXOU J124841.6−054847 12 48 41.64 −05 48 47.1 96.70 128.24 0.92±0.32 2.91 1.06 · · · d<br />
87 CXOU J124833.2−054628 12 48 33.22 −05 46 28.2 102.43 158.44 6.48±0.68 9.53 1.00 57 · · ·<br />
88 CXOU J124829.1−054822 12 48 29.10 −05 48 22.0 103.14 104.93 0.82±0.30 2.74 1.14 · · · d<br />
89 CXOU J124843.2−054808 12 48 43.20 −05 48 08.9 109.28 120.68 4.20±0.55 7.68 1.00 58 · · ·<br />
90 CXOU J124832.9−054614 12 48 32.99 −05 46 14.7 116.14 179.73 4.46±0.58 7.68 1.00 59 · · ·<br />
91 CXOU J124828.4−054837 12 48 28.44 −05 48 37.7 116.58 116.72 0.93±0.34 2.71 1.09 · · · · · ·<br />
92 CXOU J124829.0−054704 12 48 29.08 −05 47 04.7 116.92 157.35 1.52±0.38 4.02 1.00 60 · · ·<br />
93 CXOU J124828.0−054832 12 48 28.01 −05 48 32.6 121.40 122.21 1.08±0.35 3.13 1.04 · · · d<br />
94 CXOU J124837.5−055001 12 48 37.56 −05 50 01.9 122.02 187.75 1.55±0.37 4.13 1.00 · · · · · ·<br />
95 CXOU J124836.3−055008 12 48 36.30 −05 50 08.5 126.12 190.19 1.00±0.33 3.02 1.06 · · · · · ·<br />
96 CXOU J124829.6−054635 12 48 29.66 −05 46 35.3 127.44 185.20 1.10±0.36 3.07 1.01 · · · · · ·<br />
Continued on Next Page. . .<br />
145
Table 5.1—Continued<br />
Source R.A. Dec. d a Count Rate Paper II<br />
No. Name (h m s) ( ◦ ′ ′′ ) ( ′′ ) ( ′′ ) (10−4 s−1 ) S/N csim Source Notes<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11)<br />
97 CXOU J124830.6−054618 12 48 30.60 −05 46 18.5 130.63 196.97 0.90±0.30 2.95 1.08 · · · · · ·<br />
98 CXOU J124835.9−054551 12 48 35.93 −05 45 51.7 130.76 195.20 8.85±0.76 11.59 1.00 61 d<br />
99 CXOU J124832.4−055004 12 48 32.42 −05 50 04.7 132.75 175.51 6.16±0.66 9.33 1.00 62 · · ·<br />
100 CXOU J124828.7−054922 12 48 28.71 −05 49 22.1 133.52 140.91 6.17±0.66 9.36 1.00 63 · · ·<br />
101 CXOU J124834.3−055014 12 48 34.39 −05 50 14.2 133.62 191.51 13.38±0.93 14.32 1.00 64 d<br />
102 CXOU J124834.7−055019 12 48 34.79 −05 50 19.5 137.96 200.48 1.09±0.35 3.12 1.12 · · · · · ·<br />
103 CXOU J124827.3−054707 12 48 27.34 −05 47 07.8 138.87 178.58 24.24±1.23 19.72 1.00 65 · · ·<br />
104 CXOU J124827.4−054901 12 48 27.44 −05 49 01.0 138.98 139.69 0.67±0.31 2.14 1.72 · · · · · ·<br />
105 CXOU J124832.7−055018 12 48 32.77 −05 50 18.0 143.30 194.59 1.42±0.38 3.76 1.00 · · · · · ·<br />
106 CXOU J124841.4−054603 12 48 41.42 −05 46 03.2 145.01 175.66 4.73±0.58 8.11 1.00 66 · · ·<br />
107 CXOU J124826.4−054725 12 48 26.49 −05 47 25.2 145.19 175.23 0.61±0.29 2.12 1.93 · · · · · ·<br />
108 CXOU J124845.0−054711 12 48 45.09 −05 47 11.5 146.45 146.45 0.74±0.29 2.54 1.20 · · · · · ·<br />
109 CXOU J124826.1−054729 12 48 26.14 −05 47 29.5 149.27 177.21 2.09±0.43 4.91 1.00 67 · · ·<br />
110 CXOU J124840.4−055020 12 48 40.47 −05 50 20.7 154.20 237.85 4.69±0.60 7.80 1.00 · · · · · ·<br />
111 CXOU J124825.5−054808 12 48 25.50 −05 48 08.6 155.22 164.99 3.95±0.54 7.27 1.00 68 · · ·<br />
112 CXOU J124839.7−055026 12 48 39.79 −05 50 26.4 155.24 240.23 1.27±0.37 3.45 1.01 · · · · · ·<br />
113 CXOU J124827.3−054634 12 48 27.30 −05 46 34.1 155.74 216.19 0.77±0.30 2.53 1.23 · · · · · ·<br />
114 CXOU J124827.0−054925 12 48 27.01 −05 49 25.5 156.38 161.08 16.47±1.03 15.95 1.00 69 · · ·<br />
115 CXOU J124846.5−054812 12 48 46.54 −05 48 12.3 159.21 176.02 5.58±0.64 8.74 1.00 70 · · ·<br />
116 CXOU J124827.3−054624 12 48 27.35 −05 46 24.9 160.57 226.61 1.94±0.42 4.61 1.00 · · · · · ·<br />
117 CXOU J124846.8−054853 12 48 46.83 −05 48 53.2 170.91 210.15 67.37±2.00 33.66 1.00 72 e<br />
118 CXOU J124834.3−055052 12 48 34.30 −05 50 52.0 171.15 247.36 13.18±0.95 13.94 1.00 71 f<br />
119 CXOU J124840.1−055044 12 48 40.17 −05 50 44.4 174.09 269.43 0.73±0.31 2.33 1.67 · · · · · ·<br />
120 CXOU J124835.6−055057 12 48 35.67 −05 50 57.5 175.04 260.53 0.76±0.33 2.28 1.74 · · · · · ·<br />
Continued on Next Page. . .<br />
146
Table 5.1—Continued<br />
Source R.A. Dec. d a Count Rate Paper II<br />
No. Name (h m s) ( ◦ ′ ′′ ) ( ′′ ) ( ′′ ) (10−4 s−1 ) S/N csim Source Notes<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11)<br />
121 CXOU J124824.1−054817 12 48 24.16 −05 48 17.3 175.66 183.87 1.16±0.37 3.18 1.03 73 · · ·<br />
122 CXOU J124828.7−055026 12 48 28.73 −05 50 26.1 179.00 213.42 4.77±0.65 7.33 1.00 74 · · ·<br />
123 CXOU J124826.2−054955 12 48 26.25 −05 49 55.5 182.96 194.93 1.63±0.43 3.76 1.03 · · · b<br />
124 CXOU J124826.0−055002 12 48 26.02 −05 50 02.4 189.91 203.66 6.89±0.74 9.27 1.00 75 · · ·<br />
125 CXOU J124823.7−054659 12 48 23.73 −05 46 59.7 192.02 239.48 11.18±0.86 12.94 1.00 76 · · ·<br />
126 CXOU J124824.7−054625 12 48 24.77 −05 46 25.1 192.49 260.34 1.47±0.38 3.87 1.00 · · · · · ·<br />
127 CXOU J124846.3−054607 12 48 46.34 −05 46 07.8 193.54 203.96 0.86±0.30 2.89 1.10 · · · · · ·<br />
128 CXOU J124845.4−054542 12 48 45.43 −05 45 42.5 199.71 222.43 25.34±1.97 12.83 1.00 77 · · ·<br />
129 CXOU J124827.7−054523 12 48 27.73 −05 45 23.7 200.12 301.51 2.09±0.42 4.95 1.00 · · · · · ·<br />
130 CXOU J124822.4−054815 12 48 22.46 −05 48 15.9 200.87 211.47 13.81±0.96 14.43 1.00 78 · · ·<br />
131 CXOU J124825.4−054552 12 48 25.43 −05 45 52.2 203.34 290.69 3.94±0.56 7.01 1.00 80 · · ·<br />
132 CXOU J124822.4−054840 12 48 22.47 −05 48 40.0 203.72 207.48 1.83±0.41 4.42 1.00 79 · · ·<br />
133 CXOU J124822.8−054653 12 48 22.82 −05 46 53.1 207.01 259.15 3.56±0.53 6.74 1.00 81 · · ·<br />
134 CXOU J124824.4−054558 12 48 24.44 −05 45 58.1 211.36 295.99 122.27±2.73 44.71 1.00 82 · · ·<br />
135 CXOU J124823.8−054954 12 48 23.81 −05 49 54.0 211.98 218.02 0.72±0.36 2.01 3.51 · · · · · ·<br />
136 CXOU J124837.5−054431 12 48 37.53 −05 44 31.1 212.84 309.62 2.21±0.75 2.95 1.06 83 · · ·<br />
137 CXOU J124847.2−055014 12 48 47.27 −05 50 14.6 215.10 304.34 6.65±0.70 9.54 1.00 84 · · ·<br />
138 CXOU J124825.4−054533 12 48 25.43 −05 45 33.1 216.14 314.90 0.81±0.34 2.40 1.26 · · · · · ·<br />
139 CXOU J124850.4−054825 12 48 50.44 −05 48 25.3 218.24 245.77 1.73±0.41 4.21 1.00 · · · · · ·<br />
140 CXOU J124850.8−054848 12 48 50.85 −05 48 48.8 227.92 268.36 1.44±0.42 3.46 1.03 · · · · · ·<br />
141 CXOU J124821.5−054926 12 48 21.52 −05 49 26.6 230.35 230.45 2.27±0.48 4.68 1.00 · · · · · ·<br />
142 CXOU J124827.5−055116 12 48 27.52 −05 51 16.8 231.02 284.06 2.01±0.53 3.83 1.03 · · · · · ·<br />
143 CXOU J124847.4−054513 12 48 47.45 −05 45 13.0 241.87 269.34 47.12±3.64 12.93 1.00 85 · · ·<br />
144 CXOU J124819.5−054733 12 48 19.59 −05 47 33.9 245.00 277.40 3.63±0.57 6.34 1.00 86 · · ·<br />
Continued on Next Page. . .<br />
147
Table 5.1—Continued<br />
Source R.A. Dec. d a Count Rate Paper II<br />
No. Name (h m s) ( ◦ ′ ′′ ) ( ′′ ) ( ′′ ) (10−4 s−1 ) S/N csim Source Notes<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11)<br />
145 CXOU J124826.9−054433 12 48 26.97 −05 44 33.1 248.12 378.84 0.46±0.30 1.51 5.71 · · · · · ·<br />
146 CXOU J124821.4−054552 12 48 21.49 −05 45 52.2 251.36 341.78 2.46±0.62 3.94 1.00 · · · · · ·<br />
147 CXOU J124848.2−055058 12 48 48.23 −05 50 58.5 254.68 371.02 4.39±0.71 6.17 1.00 · · · · · ·<br />
148 CXOU J124849.2−054513 12 48 49.27 −05 45 13.1 261.91 283.08 5.60±1.60 3.51 1.04 · · · · · ·<br />
149 CXOU J124851.1−054548 12 48 51.12 −05 45 48.6 263.80 269.84 6.01±1.28 4.69 1.00 88 f<br />
150 CXOU J124852.9−054647 12 48 52.95 −05 46 47.1 265.50 266.19 1.61±0.43 3.76 1.01 · · · · · ·<br />
151 CXOU J124817.6−054726 12 48 17.64 −05 47 26.0 274.78 313.34 9.24±1.70 5.43 1.00 89 · · ·<br />
152 CXOU J124827.8−055214 12 48 27.85 −05 52 14.0 278.73 361.87 1.70±0.59 2.91 1.49 · · · · · ·<br />
153 CXOU J124828.4−054326 12 48 28.43 −05 43 26.6 297.57 460.47 7.81±1.41 5.56 1.00 90 · · ·<br />
154 CXOU J124850.0−054420 12 48 50.09 −05 44 20.5 306.91 346.50 24.90±2.96 8.41 1.00 · · · · · ·<br />
155 CXOU J124820.2−055153 12 48 20.26 −05 51 53.8 328.52 366.56 68.67±2.80 24.54 1.00 · · · f<br />
156 CXOU J124836.3−055333 12 48 36.38 −05 53 33.2 330.81 496.45 60.69±2.66 22.85 1.00 · · · e<br />
157 CXOU J124833.8−054206 12 48 33.87 −05 42 06.3 357.43 542.16 3.00±1.46 2.06 3.36 · · · · · ·<br />
158 CXOU J124843.8−055416 12 48 43.81 −05 54 16.1 391.81 606.20 4.05±1.13 3.59 1.12 · · · b<br />
NOTE.—The simulated completeness correction factor, csim, is accurate to 5% for the majority <strong>of</strong> sources.<br />
a Source may be confused with nearby sources, making its position, flux, and extent uncertain.<br />
b Source region noticeably more extended than PSF.<br />
c Possible cataloged optical counterpart may be the central AGN.<br />
d Possible cataloged optical counterpart appears to be a globular cluster.<br />
e Possible cataloged optical counterpart is known to not be a globular cluster.<br />
f Possible cataloged optical counterpart does not appear to be a globular cluster.<br />
g Possible uncataloged optical counterpart on DSS.<br />
h Possible radio counterpart.<br />
i Source may exhibit variability.<br />
148
source list against which to register the astrometry. We detected 97, 78, 87, 77, and<br />
98 sources in Observations 0784, 4727, 4728, 4729, and 4730. We then registered the<br />
astrometry <strong>of</strong> each Cycle-5 observation against Observation 0784. Using 55, 56, 51,<br />
and 55 sources matched to within 0. ′′ 5, the relative astrometry corrections were 0. ′′ 31,<br />
0. ′′ 38, 0. ′′ 31, and 0. ′′ 48.<br />
To maximize S/N, we analyzed the wavelet detection results from the combination<br />
<strong>of</strong> the five observations (Figure 5.1). Since there were five approximately equally sen-<br />
sitive observations, we reduced the exposure threshold <strong>of</strong> this merged source detection<br />
to 2% <strong>of</strong> the total. There was a 50% increase in the FOV compared to a single S3<br />
chip, so we expect 1.5 false source. We detected 158 sources. All <strong>of</strong> the detections<br />
in Observation 0784 were in the merged detection list. In the Cycle-5 observations,<br />
a few weak detections were not found in the merged detection list. None <strong>of</strong> these de-<br />
tections would have fluxes determined at the ≥ 3σ level; detections not in the merged<br />
detection list are not discussed further in this chapter.<br />
We used the coordinate list generated by wavdetect in ACIS Extract to create<br />
source extraction and masking regions, as well as refine the source positions. For<br />
each observation, we created a source extraction region consistent with the X-ray<br />
PSF at the source position. Most <strong>of</strong> the regions encircled 90% <strong>of</strong> the X-ray PSF at<br />
≈ 1.5 keV. For sources whose median photon energy over all five observations was<br />
not ∼ 0.6–2.6 keV, we determined the PSF at either ≈ 0.3 keV (Sources 19, 23, 25,<br />
62, and 78) or ≈ 4.5 keV (Sources 96, 119, and 138). We used a lower percentage <strong>of</strong><br />
the PSF in the case <strong>of</strong> few sources whose regions would otherwise have overlapped in<br />
one <strong>of</strong> the observations (85% for Sources 2/5; 80% for Sources 49/50; 50% for Sources<br />
72/73). The wavdetect regions were compared to the PSF sizes at the locations <strong>of</strong><br />
the sources; all were consistent except those for Sources 8, 22, 123, and 158. Thus,<br />
149
these sources may be extended or multiple, and are marked with a note in Table 5.1.<br />
Masking circular regions around the source at a radius encircling > 97% <strong>of</strong> the PSF<br />
were created for every source.<br />
The refined source positions for a majority <strong>of</strong> the sources came from the average<br />
position <strong>of</strong> 0.3–6 keV photons in the source extraction regions. For Sources 142, 148,<br />
152, and 154–158, whose average positional <strong>of</strong>fset from the optical axis is more than<br />
5 ′ , we correlated the 0.3–6 keV photons near the wavdetect coordinates against the<br />
average X-ray PSF <strong>of</strong> each source to refine their positions.<br />
To subtract out overlapping diffuse gas and blank-sky background we used a local<br />
background with an area approximately three times that <strong>of</strong> each source’s extraction<br />
region. The background region excluded photons in the masking region. In cases<br />
where background regions overlapped or fell along node/chip boundaries, we slightly<br />
altered these overlapping regions, preserving the ratio <strong>of</strong> source to background ar-<br />
eas and ensuring that the source region and background region had similar mean<br />
exposures.<br />
The observed net count rates, their errors, and S/N were calculated by stacking<br />
the observations, correcting for background photons, and dividing by the sum <strong>of</strong> the<br />
mean exposures over each source region.<br />
We list the results <strong>of</strong> all analyses for all sources in this chapter’s tables; however, we<br />
restrict discussion <strong>of</strong> sources, except for identification <strong>of</strong> possible optical counterparts,<br />
to the 126 that have photometric count rates determined at the ≥ 3σ level. These<br />
significantly detected sources, hereafter the Analysis Sample, all have at least 18 net<br />
counts.<br />
The minimum detected count rate in the 0.3–6 keV band for our Analysis Sample<br />
sources is 1.0 × 10 −4 counts s −1 . This count rate is 2.6 times as deep as the count<br />
150
ate from Observation 0784 alone (Paper II). Three sources below the Analysis limit<br />
(136, 152, 157) but with count rates above 10 −4 counts s −1 are not covered by all five<br />
observations. The other sources below the Analysis limit reach count rates as low as<br />
∼ 5 × 10 −5 counts s −1 .<br />
We estimated the completeness <strong>of</strong> all sources through simulations using marx<br />
4.0.8 8 . We used the normalized background generated by wavdetect and the pho-<br />
tometrically determined counts (after PSF corrections) to perform 400 simulated runs<br />
<strong>of</strong> our five observations <strong>of</strong> NGC 4697. The resulting completeness correction factor,<br />
csim = Nsim/Ndet , is accurate to ∼ 5% for the majority <strong>of</strong> sources; however, the<br />
accuracy increases to ∼ 12% for the largest correction factors. All sources with ob-<br />
served count rates > 10 −4 counts s −1 had correction factors < 1.1 except for Sources<br />
72, 102, and 158. In the simulations, Sources 72 and 73 were <strong>of</strong>ten confused as one<br />
source with a position closer to Source 73. Sources 102 and 158 had csim = 1.12. The<br />
average completeness correction factor in the Analysis Sample is ∼ 1.01. For sources<br />
not in the Analysis Sample, csim averaged ∼ 1.99, and reached as high as 5.71 for<br />
the weakest sources. Our completeness results are roughly consistent with Kim &<br />
Fabbiano (2003).<br />
There are objects unrelated to NGC 4697 among the detected sources. Since the<br />
FOV sampled by Kim et al. (2004) are larger than the Chandra deep fields, the source<br />
counts from the former should be less susceptible to cosmic variance. Therefore, we<br />
chose to use their s<strong>of</strong>t band source counts to estimate the number <strong>of</strong> foreground or<br />
background objects at different flux levels. At the flux limit <strong>of</strong> our Analysis Sample,<br />
∼ 9×10 −16 erg cm −2 s −1 , we expect ≈ 29 foreground or background objects, including<br />
corrections for exposure and completeness. We estimate ≈ 7 <strong>of</strong> the sources outside<br />
<strong>of</strong> the Analysis Sample are also unrelated to NGC 4697. Since these sources should<br />
8 See http://space.mit.edu/CXC/MARX/.<br />
151
e fairly uniform over the FOV, sources close to NGC 4697 are more likely to be<br />
associated with the galaxy than sources farther out.<br />
5.5 Optical Counterpart Identification<br />
5.5.1 Existing Catalog Identifications<br />
The refined source positions <strong>of</strong> seven X-ray sources from the combined S3 image<br />
agreed with positions from the Tycho-2 Catalog (Høg et al. 2000), the 2MASS Point<br />
Source and Extended Source Catalogs, and/or the USNO-B Catalog (Monet et al.<br />
2003). (When a source appeared in both 2MASS catalogs, the Point Source Catalog<br />
positions were used.) In cases where there are counterparts in multiple catalogs, we<br />
adopt the positions in the order <strong>of</strong> the catalogs listed above. These seven sources (15,<br />
55, 84, 117, 149, 155, and 156) were used to check the absolute astrometry. Since<br />
the mean positional <strong>of</strong>fset <strong>of</strong> the sources was 0. ′′ 07 ± 0. ′′ 30 in R.A. and 0. ′′ 10 ± 0. ′′ 27 in<br />
Dec., the ACIS Extract positions are consistent with no required absolute astrometric<br />
change. The overall absolute astrometric errors are probably ∼ 0. ′′ 4 near the field<br />
center, with larger errors for weaker sources with extended PSFs.<br />
Having established the absolute astrometry, we conservatively considered all op-<br />
tical sources within 2 ′′ as potential optical counterparts. We summarize their optical<br />
properties in Table 5.2. The first three columns list the X-ray source number, desig-<br />
nation <strong>of</strong> the optical counterpart, and positional <strong>of</strong>fset between the X-ray and optical<br />
catalogs. In the fourth column, we list the photometric properties <strong>of</strong> the optical<br />
counterpart, while we list notes about the optical properties in the fifth column. We<br />
classify the counterpart as optically extended or an optical point source. For 2MASS<br />
objects, we use its values <strong>of</strong> the reduced χ 2 for fitting PSFs to each source in each<br />
152
Table 5.2. : Optical Properties <strong>of</strong> Ground-Based Optical Sources Matched to X-ray Sources in NGC 4697<br />
X-ray Source Offset<br />
No. Optical Source ( ′′ ) Photometry Optical Notes<br />
(1) (2) (3) (4) (5)<br />
1 Center <strong>of</strong> NGC 4697 0.5<br />
8 2MASS J12483635-0547577 1.4 J = 13.1, H > 10.9, Ks > 10.7 Galaxy light may contaminate photometry and PSF-fitting<br />
Optically extended?<br />
15 2MASS J12483692-0548007 0.6 J = 14.4, H = 13.7, Ks > 11.7 Galaxy light may contaminate photometry and PSF-fitting<br />
Optically extended?<br />
55 2MASS J12483648-0548475 0.2 J = 16.6, H = 16.2, Ks > 14.5 Galaxy light may contaminate photometry<br />
Optical point source<br />
84 2MASS J12483420-0549261 0.5 J = 16.0, H = 15.5, Ks = 15.1 Optical point source<br />
USNO-B1 0841-0238559 1.0 Bpg ∼ 20.2, Rpg ∼ 19.4, Ipg ∼ 17.9 Optical point source?<br />
117 USNO-B1 0841-0238601 0.4 Bpg ∼ 19.1, Rpg ∼ 19.1 Optically extended?<br />
Known AGN (z = 0.696; Paper II)<br />
118 USNO-B1 0841-0238561 1.1 Bpg ∼ 20.1, Rpg ∼ 19.5 Optically extended<br />
149 USNO-B1 0842-0237849 0.1 Bpg ∼ 20.7, Rpg ∼ 19.6 Optical point source<br />
155 USNO-B1 0841-0238528 0.1 Bpg ∼ 20.5, Rpg ∼ 19.0 Optically extended?<br />
156 Tycho-2 4955-1175-1 0.5 B = 11.0, V = 10.2 Foreground star (BD-05 3573)<br />
2MASS J12483640-0553335 0.5 J = 9.0, H = 8.7, Ks = 8.6<br />
USNO-B1 0841-0238574 0.5 Bpg ∼ 10.9, Rpg ∼ 9.8, Ipg ∼ 9.4<br />
153
and (a reduced χ 2 > 2 indicates the optical counterpart is extended, and may be a<br />
galaxy). For the USNO-B1 objects, we use their star-galaxy separation class (objects<br />
in the lower half <strong>of</strong> classes are classified as optically extended). We add a question-<br />
mark when we are unsure <strong>of</strong> the classification. Typically this occurs because galaxy<br />
light may have contaminated the analysis or because the classification in at least one<br />
color differs significantly from the other colors.<br />
In addition to the sources used to check astrometry, Sources 1, 8, and 118 have<br />
potential optical counterparts. Since Source 1 is 0. ′′ 5 away from the adopted center <strong>of</strong><br />
NGC 4697, it may be a central AGN. Since this source could also be an LMXB (or<br />
several confused LMXBs) near the center <strong>of</strong> the galaxy, we did not use this match to<br />
check the astrometry. The optical counterparts <strong>of</strong> Sources 8, 15, 117, 118, and 155<br />
appear to be optically extended. We note that Source 117 is a known AGN Paper II.<br />
Although Source 118 is associated with 2MASX J12483504-0550473 in NED, that<br />
source is actually 12 ′′ away and its counterpart, USNO-B1 0841-0238567, is clearly<br />
different on Digital Sky Survey (DSS) images. Since the extrapolated fiducial ra-<br />
dius <strong>of</strong> 2MASX J12483504-0550473 is 6. ′′ 2, it is unlikely that Source 118 is associated<br />
with that galaxy. Sources 55, 84, 149, and 156 appear point-like from the ground;<br />
Source 156 is clearly the bright foreground star BD-05 3573. Finally, we note that<br />
Sources 103, 123, 132, 143 may have uncatalogued counterparts on DSS second gen-<br />
eration images. Footnotes in Table 5.1 indicate X-ray sources with possible optical<br />
counterparts.<br />
In Sarazin et al. (2001), associations with GCs in lists <strong>of</strong> Hanes (1977) and Kave-<br />
laars (2000, private communication) were made. Sources 101 and 117 were previously<br />
identified with Hanes (1977) GC candidates; we find no new GC-LMXB candidates<br />
among the Hanes (1977) sources and note that Source 117 has already been shown to<br />
154
actually be an AGN. Sources 79, 80, 83, 84, 86, 88, 93, 98, 101, 109, 113, and 114 are<br />
associated with GC candidates in the Kavelaars data, with Sources 79, 86, 88, 93, and<br />
113 representing new detections. Some <strong>of</strong> the Kavelaars GC candidates with potential<br />
X-ray counterparts are also in the HST-ACS FOV discussed in § 5.5.2 (Sources 79,<br />
80, 83, 84, 86). The measured colors and sizes from the HST-ACS observations allow<br />
us to more accurately identify GC candidates. The colors <strong>of</strong> Source 84 suggest it is<br />
not a GC, while the other sources have colors and sizes consistent with GCs. Since<br />
the Hanes and Kavelaars GC datasets do not have the same sensitivity or measured<br />
properties <strong>of</strong> the HST-ACS dataset, and the flanking field ACS observations occur-<br />
ring during AO14 do, we will not make further use <strong>of</strong> GC counterparts outside <strong>of</strong> the<br />
HST-ACS FOV here.<br />
We matched the X-ray sources with a previous ROSAT-HRI X-ray observation<br />
<strong>of</strong> NGC 4697 (Irwin et al. 2000, hereafter ISB2000). Twelve sources within 4 ′ <strong>of</strong><br />
NGC 4697 were detected by ROSAT-HRI with LX 2.6×10 38 erg s −1 , after correcting<br />
for the distance and spectra we use in this chapter. We match ISB2000 Sources 1, 2,<br />
4, 5, 6, 9, 10, 11, and 12 with this chapter’s Sources 103, 80, 69, 54, 118, 58, 128, 117,<br />
143. Confusion in the center <strong>of</strong> NGC 4697 limits matching ISB2000 Source 7 with this<br />
chapter’s Sources 1, 3, 4, and 6; although it is likely matched to this chapter’s Source<br />
1, which is the brightest <strong>of</strong> the four sources. Similarly, confusion limits matching<br />
ISB2000 Source 8 with this chapter’s Sources 6, 7, 10, and 11. We clearly do not<br />
detect ISB2000 Source 3.<br />
We also matched sources with Paper II, whose data (Observation 0784) is a subset<br />
<strong>of</strong> the data in this chapter. We list those matches in Table 5.1. Only two Paper II<br />
sources (7 and 87) are undetected in the larger dataset. Paper II Sources 7 and 10 are<br />
separated by only 1. ′′ 1. It is unclear whether they are a single source. Paper II Source<br />
155
87 was near the limit <strong>of</strong> the S/N in Paper II. It was not detected in the individual<br />
reanalysis <strong>of</strong> Observation 0784, even when detections were made in the 0.3–10 keV<br />
range to match Paper II.<br />
5.5.2 HST-ACS Identifications<br />
In our HST-ACS observation, we placed the center <strong>of</strong> NGC 4697 ∼ 20 ′′ from the<br />
center <strong>of</strong> the ACS FOV to avoid a chip boundary. Within this FOV, we can identify<br />
optical sources and separate out the GCs using a combination <strong>of</strong> magnitude, color,<br />
and spatial extent. This method is discussed in detail in Jordán et al. (2004a) and<br />
Jordán et al. (2006, in preparation). Out <strong>of</strong> 703 optical sources, there are 298 GCs.<br />
We registered the HST observation to the Chandra observation using all 703 op-<br />
tical sources detected by KINGPHOT. Through cross-correlation techniques, we<br />
determined that the HST coordinates required astrometric shifts <strong>of</strong> −0. ′′ 27 in R.A.<br />
and −0. ′′ 42 in Dec. Based on singly matched sources within 1 ′′ , we estimate a rel-<br />
ative astrometric error <strong>of</strong> 0. ′′ 21 and 0. ′′ 25 in R.A. and Dec., respectively, or 0. ′′ 32 in<br />
quadrature. Since most <strong>of</strong> these matches occur close to the X-ray pointing center,<br />
it is not surprising that this astrometric error is slightly smaller than the astromet-<br />
ric error derived from ground-based catalogs. After correcting the astrometry, we<br />
determined that the ACS FOV covers X-ray Sources 1–67, 69–87, 89, 94, and 108.<br />
Due to a prominent elliptical dust feature (≈ 7.0 ′′ × 1.7 ′′ or ≈ 384 pc × 93 pc), we<br />
did not attempt to detect optical sources in the region <strong>of</strong> X-ray Sources 1–5 and 8.<br />
X-ray Source 68 falls in the chip boundary. Adopting a search radius <strong>of</strong> 1 ′′ , we find<br />
42 optical counterparts to 39 X-ray sources; three X-ray sources have two candidate<br />
optical counterparts within 1 ′′ . Thirty-three <strong>of</strong> the X-ray sources are associated with<br />
a single GC counterpart, while one X-ray source is likely to be associated with one <strong>of</strong><br />
156
two potential GC counterparts. We list the optical properties <strong>of</strong> the matched sources<br />
in Table 5.3.<br />
By randomizing the P.A. <strong>of</strong> a source list, assuming both a circular pr<strong>of</strong>ile and a<br />
pr<strong>of</strong>ile matching the galaxy’s elliptical isophotes, we have determined the percentage<br />
<strong>of</strong> false matches within a given radius. Randomizing the optical source list, we find<br />
that ≈ 6.8% <strong>of</strong> X-ray sources without a physically associated optical source will have<br />
a false optical match within 1 ′′ . This is consistent with only 3/39 <strong>of</strong> the X-ray/optical<br />
matches being false. If one considers only the GCs, ≈ 4.2% <strong>of</strong> X-ray sources will have<br />
a false match. This is consistent with only 2/34 <strong>of</strong> the X-ray/GC matches being<br />
false. Finally, comparing the optical source list to itself suggests that ≈ 1.8 X-ray<br />
sources will be matched to two optical sources within 1 ′′ by chance; we find three<br />
such matches.<br />
157
Table 5.3. : Optical Properties <strong>of</strong> HST Sources Matched to X-ray Sources in NGC 4697<br />
X-ray Source Offset rh g475 z850 G475 − Z850<br />
No. ( ′′ ) (pc) (AB mag) (AB mag) (AB mag) Notes<br />
(1) (2) (3) (4) (5) (6) (7)<br />
7 0.05 2.37 ± 0.13 21.49 ± 0.05 20.43 ± 0.03 1.06 ± 0.06 a<br />
15 0.11 2.12 ± 0.08 19.30 ± 0.04 17.95 ± 0.02 1.35 ± 0.04 b<br />
16 0.06 1.43 ± 0.10 23.10 ± 0.05 21.64 ± 0.04 1.47 ± 0.06 b<br />
18 0.80 1.48 ± 0.14 24.58 ± 0.07 23.18 ± 0.03 1.40 ± 0.08 b<br />
21 0.44 2.08 ± 0.08 20.95 ± 0.04 19.68 ± 0.01 1.27 ± 0.04 b<br />
22 0.06 · · · · · · · · · · · · f<br />
0.25 · · · · · · · · · · · · f<br />
24 0.10 1.43 ± 0.16 22.89 ± 0.04 21.56 ± 0.04 1.33 ± 0.06 b<br />
25 0.95 3.79 ± 15.53 26.08 ± 1.92 24.11 ± 0.17 1.97 ± 1.93 d,e<br />
26 0.34 1.47 ± 0.14 23.22 ± 0.06 21.92 ± 0.03 1.29 ± 0.07 b<br />
31 0.09 1.42 ± 0.11 22.32 ± 0.06 20.99 ± 0.02 1.33 ± 0.06 b<br />
34 0.04 1.07 ± 0.07 20.94 ± 0.03 19.57 ± 0.01 1.37 ± 0.03 b<br />
39 0.06 1.97 ± 0.13 22.47 ± 0.06 21.09 ± 0.03 1.38 ± 0.07 b<br />
40 0.30 1.25 ± 0.06 22.78 ± 0.03 21.34 ± 0.02 1.45 ± 0.04 b<br />
41 0.09 1.58 ± 0.09 21.88 ± 0.03 20.80 ± 0.01 1.08 ± 0.03 a<br />
0.69 1.80 ± 0.17 23.31 ± 0.04 22.47 ± 0.07 0.84 ± 0.08 a<br />
45 0.87 0.30 ± 0.12 23.00 ± 0.04 19.12 ± 0.85 3.89 ± 0.85 d<br />
47 0.09 1.98 ± 0.10 22.98 ± 0.03 21.50 ± 0.03 1.48 ± 0.05 b<br />
50 0.03 2.01 ± 0.08 20.54 ± 0.04 19.28 ± 0.02 1.26 ± 0.04 b<br />
51 0.03 1.37 ± 0.11 21.61 ± 0.04 20.25 ± 0.02 1.36 ± 0.05 b<br />
52 0.02 2.17 ± 0.10 22.53 ± 0.05 21.32 ± 0.03 1.21 ± 0.06 b<br />
54 0.09 1.05 ± 0.22 25.25 ± 0.10 23.77 ± 0.11 1.48 ± 0.15 b<br />
55 0.12 3.74 ± 0.49 18.01 ± 0.07 17.76 ± 0.13 0.25 ± 0.15 c<br />
58 0.02 1.16 ± 0.07 22.08 ± 0.03 20.78 ± 0.02 1.29 ± 0.03 b<br />
60 0.29 1.73 ± 0.08 22.80 ± 0.03 21.66 ± 0.03 1.15 ± 0.04 b<br />
Continued on Next Page. . .<br />
158
Table 5.3—Continued<br />
X-ray Source Offset rh g475 z850 G475 − Z850<br />
No. ( ′′ ) (pc) (AB) (AB) (AB) Notes<br />
(1) (2) (3) (4) (5) (6) (7)<br />
63 0.35 1.73 ± 0.06 21.24 ± 0.03 19.81 ± 0.02 1.43 ± 0.03 b<br />
0.71 1.52 ± 0.08 22.50 ± 0.03 21.26 ± 0.03 1.25 ± 0.04 b<br />
65 0.40 2.56 ± 0.15 20.71 ± 0.05 19.31 ± 0.02 1.40 ± 0.06 b<br />
66 0.98 1.79 ± 0.05 21.51 ± 0.03 20.49 ± 0.01 1.02 ± 0.03 a<br />
69 0.12 2.18 ± 0.06 21.63 ± 0.02 20.64 ± 0.02 0.99 ± 0.03 a<br />
70 0.08 1.77 ± 0.06 21.76 ± 0.04 20.81 ± 0.01 0.95 ± 0.04 a<br />
71 0.06 1.39 ± 0.08 21.71 ± 0.04 20.75 ± 0.01 0.96 ± 0.04 a<br />
73 0.05 2.35 ± 0.42 23.90 ± 0.06 22.51 ± 0.09 1.39 ± 0.11 b<br />
74 0.19 1.88 ± 0.13 20.87 ± 0.03 19.88 ± 0.02 0.99 ± 0.04 a<br />
75 0.75 2.51 ± 0.07 20.39 ± 0.03 18.99 ± 0.02 1.40 ± 0.03 b<br />
76 0.02 1.54 ± 0.17 20.19 ± 0.04 18.84 ± 0.29 1.35 ± 0.29 b<br />
77 0.06 2.30 ± 0.12 21.55 ± 0.05 20.25 ± 0.02 1.30 ± 0.06 b<br />
79 0.11 1.56 ± 0.05 20.68 ± 0.03 19.33 ± 0.01 1.35 ± 0.03 b<br />
80 0.04 0.81 ± 0.10 23.44 ± 0.03 22.16 ± 0.41 1.27 ± 0.41 b<br />
83 0.11 1.39 ± 0.08 22.54 ± 0.03 21.23 ± 0.02 1.31 ± 0.03 b<br />
84 0.06 0.70 ± 0.14 19.87 ± 0.04 17.36 ± 0.07 2.52 ± 0.08 d<br />
86 0.19 1.33 ± 0.05 22.14 ± 0.03 20.95 ± 0.01 1.18 ± 0.03 b<br />
a Optical counterpart is a blue GC.<br />
b Optical counterpart is a red GC.<br />
c Optical counterpart rejected as GC since G475 − Z850 < 0.5.<br />
d Optical counterpart rejected as GC since G475 − Z850 > 1.9.<br />
e Optical counterpart G − Z is poorly constrained and could be a GC.<br />
f Multiple nearby optical counterparts prevented kingphot analysis.<br />
159
Fig. 5.5.— Percentage <strong>of</strong> GCs with an LMXB within 1 ′′ , corrected for random associations,<br />
as a function <strong>of</strong> the limiting X-ray luminosity (LX,37 ≡ LX/10 37 ergs s −1 ).<br />
The detection limits for all sources and for the Analysis Sample (3σ) are indicated.<br />
5.6 GC/LMXB Connection<br />
Having identified the LMXBs associated with GCs and determined the percentage<br />
<strong>of</strong> falsely matched sources, we now explore the GC/LMXB connection. The broadest<br />
measures <strong>of</strong> the GC/LMXB connection are the fraction <strong>of</strong> LMXBs associated with<br />
GCs and the fraction <strong>of</strong> GCs associated with LMXBs. The fraction <strong>of</strong> LMXBs associ-<br />
ated with GCs, fX,GC, is 38.4 +6.1<br />
−5.7% and does not appear to depend on X-ray luminos-<br />
ity. On the other hand, the fraction <strong>of</strong> GCs with an LMXB, PX, naturally depends<br />
on the limiting X-ray luminosity. The result is shown in Figure 5.5. In NGC 4697,<br />
and other early-type galaxies (Sarazin et al. 2003), PX ≈ 4% above 10 38 ergs s −1 . At<br />
the limit <strong>of</strong> our Analysis Sample, 1.4 × 10 37 ergs s −1 , PX has increased to 8.1 +1.9<br />
−1.6%<br />
(∼ 2.7 × 10 −7 LMXBs per L⊙,Z normalizing LMXB detection to GC luminosity in<br />
160
Fig. 5.6.— Color (G475−Z850) - magnitude (Z850) diagram (left) and color - encounter<br />
rate (Γh ∝ M 3/2 r −5/2<br />
h ) diagram (right) for GCs in HST-ACS. The larger symbols<br />
indicate GCs containing LMXBs. The vertical line indicates the separation <strong>of</strong> GCs<br />
into blue and red GC populations following Peng et al. (2006a). LMXBs reside more<br />
<strong>of</strong>ten in GCs with larger optically luminosity, larger encounter rates, and redder<br />
colors.<br />
the Z850 band). Among all detected sources (LX > 0.6 × 10 37 ergs s −1 ), PX rises to<br />
10.7 +2.1<br />
−1.8% (∼ 3.5 × 10 −7 LMXBs per L⊙,Z). Since we are incomplete below the limit<br />
<strong>of</strong> our Analysis Sample and active LMXBs can have LX 10 36 ergs s −1 , it is likely<br />
that the percentage <strong>of</strong> GCs with an active LMXB is even higher.<br />
The optical properties <strong>of</strong> GCs are known to effect the GC/LMXB connection;<br />
LMXBs are found more <strong>of</strong>ten in optically bright GCs and in red GCs (e.g., Kundu<br />
et al. 2003; Sarazin et al. 2003). The GC/LMXB connection in the center <strong>of</strong> NGC 4697<br />
clearly follows this now familiar pattern (Figure 5.6, left). Following Sarazin et al.<br />
(2003), we have compared the distributions <strong>of</strong> GCs with and without LMXBs using<br />
the two-sample Kolmogorov-Smirnov test (PKS), which measures the probability that<br />
two populations sampled from the same distribution have a maximum difference at<br />
least as large as is observed, and the non-parametric Wilcoxon rank-sum test (σWRS,<br />
equivalent to the Mann-Whitney rank-sum test; Mann & Whitney 1947), which mea-<br />
sures the probability that a random sampling <strong>of</strong> two distributions with the same<br />
median would produce at least the observed difference in the sum <strong>of</strong> the ranks <strong>of</strong> the<br />
161
two distributions.<br />
First, we compared optical luminosity <strong>of</strong> GCs (represented by their Z850 band<br />
magnitudes) with and without LMXBs. We found PKS = 2.6 × 10 −4 and σWRS = 4.5.<br />
That is, LMXBs are preferentially associated with optically luminous GCs. Next,<br />
we compared the G475 − Z850 color distributions <strong>of</strong> GCs with and without LMXBs.<br />
The distributions are clearly different (PKS = 3.6 × 10 −4 and σWRS = 3.0). That<br />
is, LMXBs are more likely to be found in red GCs. These results are illustrated<br />
in Figure 5.6 (left). Quantifying the probabilities that GC contain LMXBs, we find<br />
LMXBs in 4.8 +2.7<br />
−1.9% <strong>of</strong> the blue GCs (∼ 2.1 × 10 −7 LMXBs per L⊙,Z) and 15.1 +3.2<br />
−2.8%<br />
<strong>of</strong> the red GCs (∼ 4.9 × 10 −7 LMXBs per L⊙,Z).<br />
Jordán et al. (2004b) used HST-ACS data from M87 to compare the GC/LMXB<br />
connection with the encounter rates due to tidal capture and exchange interactions,<br />
Γ ≡ ρ 1.5<br />
0 r 2 c, where ρ0, the central density, and rc, the core radii, were estimated from<br />
fitting King pr<strong>of</strong>iles and the Virial Theorem is assumed to relate the velocity <strong>of</strong> stars<br />
to the core radius. They found a strong indication that dynamical processes play a key<br />
role; however, poorly constrained concentrations led to a poorly constrained estimate<br />
<strong>of</strong> Γ. Since the half-mass radii, r ′ h , and surface brightnesses <strong>of</strong> GCs, σh ∝ M (r ′ h )−2 ,<br />
are better constrained, we choose to use an alternate measure <strong>of</strong> the encounter rate.<br />
Using the z-band magnitude <strong>of</strong> GCs, we estimate their masses,<br />
162<br />
M = ΥZ 10 −0.4∗(Z850−Z⊙) M⊙, (5.1)<br />
where a mass-to-light ratio <strong>of</strong> ΥZ ≡ 1.45 M⊙/L⊙,Z is predicted by PÉGASE, Version 2<br />
(Fioc & Rocca-Volmerange 1997), and Z⊙ = 4.512 is the absolute Z-band magnitude<br />
<strong>of</strong> the Sun from calcphot in IRAF. Assuming that the correlation typically observed<br />
between half-light radius, rh, and color (e.g., Kundu & Whitmore 2001) is due to
mass segregation <strong>of</strong> GCs with the same half-light mass (Jordán 2004), we apply the<br />
color-size relation found in the ACS Virgo Cluster Survey (Peng et al. 2006a),<br />
163<br />
r ′ h ≡ rh 10 0.17[(G475−Z850)−1.2] . (5.2)<br />
We then calculate the proxy for encounter rates (See Appendix A),<br />
Γh ≡ σ 3/2<br />
h (r ′ h) 1/2 ∝ M 3/2 (r ′ h) −5/2 . (5.3)<br />
A similar proxy was used recently for the Galactic GC/LMXB connection (Bregman<br />
et al. 2006) without correcting for possible mass segregation effects.<br />
In Figure 5.6 (right), we display the color - encounter rate diagram. Globular<br />
clusters with larger encounter rates are more likely to contain LMXBs; the hypothesis<br />
that the distributions <strong>of</strong> encounter rates are the same for GCs with and without<br />
LMXBs is rejected (PKS = 5.8 × 10 −7 and σWRS = 5.5). (If LMXBs are preferentially<br />
found in core-collapse GCs, the difference between the actual encounter rates <strong>of</strong> GCs<br />
with and without LMXBs will be larger than what we measured.) This correlation<br />
is actually stronger than that found for the optical luminosity, apparently because<br />
smaller GCs appear (marginally) more likely to contain GCs. When we compare the<br />
distributions <strong>of</strong> r ′ h<br />
for GCs with and without LMXBs, the hypothesis that they are<br />
the same is rejected, although rather weakly (PKS = 2.2 × 10 −2 and σWRS = 2.6).<br />
Our correction for the half-mass radius actually reduces the apparent preference for<br />
LMXBs to be in smaller GCs; if the distributions <strong>of</strong> rh are compared instead, the<br />
hypothesis that they are the same is more strongly rejected (PKS = 7.3 × 10 −3 and<br />
σWRS = 3.6). However, part <strong>of</strong> this correlation is due to the fact that redder GCs are<br />
both more likely to contain LMXBs due to their color, and are also smaller for the
same mass.<br />
Recently, Kim et al. (2006b) suggested that PX may have a spatial dependence<br />
due to higher encounter rates in GCs near the centers <strong>of</strong> their host galaxies. Although<br />
our comparison <strong>of</strong> the projected galactocentric distances d <strong>of</strong> GCs with and without<br />
LMXBs do not indicate that they are drawn from two separate populations at a sig-<br />
nificant level (PKS = 0.21 and σWRS = 1.6), we do note that the median galactocentric<br />
distance <strong>of</strong> GCs with LMXBs is smaller than those without. This question will be<br />
best addressed with our ongoing HST-ACS observations <strong>of</strong> the entire galaxy.<br />
We have attempted to fit the expected number <strong>of</strong> LMXBs in a GC (λ) with<br />
power-law dependences on the GC mass M, metallicity Z, radius r ′ h , or encounter<br />
rate parameter Γh. We considered the forms:<br />
and<br />
164<br />
λ = A M α (Z/Z⊙) β (r ′ h) δ , (5.4)<br />
λ = A (Z/Z⊙) β Γ ɛ h . (5.5)<br />
We converted color to metallicity following equation (2) <strong>of</strong> Peng et al. (2006a),<br />
log Z<br />
Z⊙<br />
⎧<br />
⎪⎨<br />
=<br />
⎪⎩ −2.75 + (1.83 ± 0.23)(G475 − Z850) otherwise.<br />
−6.21 + (5.14 ± 0.67)(G475 − Z850) if G475 − Z850 ≤ 1.05;<br />
(5.6)<br />
The expected number <strong>of</strong> LMXBs in a GC can be converted to a probability that there<br />
are no LMXBs, PnX,i = e −λi , and the probability that there is at least one LMXB,<br />
PX,i = 1 − e−λi . One can then maximize the log likelihood for a given form <strong>of</strong> λ,<br />
ψ = ln[( <br />
PnX) ( <br />
PX)], where the products are taken over the lists <strong>of</strong> GCs with no<br />
nX<br />
X<br />
LMXBs and GCs with LMXBs (Table 5.4).
Table 5.4. Fits to the Expected Number <strong>of</strong> LMXBs per GC (λ)<br />
λ = A M α (Z/Z⊙) β (r ′ h )δ or λ = A Γɛ β<br />
h (Z/Z⊙)<br />
Row α β δ ɛ ψ ∆ d<strong>of</strong><br />
1 [0] [0] [0] [0] -101.16 0<br />
2 0.90 +0.18<br />
−0.18 [0] [0] [0] -87.66 1<br />
3 [0] 0.38 +0.13<br />
−0.13 [0] [0] -95.74 1<br />
4 [0] [0] −1.49 +0.53<br />
−0.54 [0] -97.81 1<br />
5 [0] [0] [0] 0.78 +0.32<br />
−0.28 -80.25 1<br />
6 1.16 +0.22<br />
−0.20 [0] −2.84 +0.74<br />
−0.76 [0] -79.35 2<br />
7 0.91 +0.18<br />
−0.17<br />
8 [0] 0.47 +0.16<br />
−0.13<br />
0.48 +0.16<br />
−0.15 [0] [0] -81.62 2<br />
−1.73 +0.53<br />
−0.52 [0] -90.13 2<br />
9 [0] 0.50 +0.18<br />
−0.16 [0] 0.74 +0.14<br />
−0.13 -74.53 2<br />
10 1.27 +0.20<br />
−0.18<br />
11 1.08 +0.22<br />
−0.21<br />
0.51 +0.18<br />
−0.16 [2 − 3α] [0] -75.38 2<br />
0.50 +1.18<br />
−0.16<br />
−2.58 +0.68<br />
−0.72 [0] -73.85 3<br />
Although the general maximum likelihood statistic does not provide a measure<br />
<strong>of</strong> goodness-<strong>of</strong>-fit, relative improvements (∆ψ = −∆χ 2 /2) can be used to determine<br />
whether a given fit is a statistical improvement over a previous fit given the change<br />
in the number <strong>of</strong> degrees <strong>of</strong> freedom (d<strong>of</strong>). The change in the log-likelihood can also<br />
be used to provide errors on the fitted power-law indices. Here, we assumed that the<br />
errors in the fitting parameters in equations (5.4) & (5.5) are are much larger than the<br />
uncertainties in the GC parameters (M, Z, and r ′ h ) due to either measurement errors<br />
or systematic errors in the conversions. Given the derived sizes <strong>of</strong> our errors, this is<br />
justified. To use the relative change in the log-likelihood (∆ψ), we first established<br />
165
a baseline value <strong>of</strong> the log-likelihood (ψ0) for the case where the expected number <strong>of</strong><br />
LMXBs λ was constant and did not depend on any GC properties (Table 5.4, row 1).<br />
We then fit various combinations <strong>of</strong> dependencies <strong>of</strong> λ on GC properties, and<br />
determined the values <strong>of</strong> ψ for the best-fit values. In rows 2–4 <strong>of</strong> Table 5.4, the<br />
expected number <strong>of</strong> GCs λ is assumed to depend on only a single GC property (the<br />
mass, metallicity, or radius). Each fit is significantly better (∆χ 2 = −27.0, −10.8,<br />
and −6.7 for one less d<strong>of</strong>) than the baseline fit, suggesting that all three properties<br />
affect λ, with mass having the strongest effect.<br />
In the next row (5), the expected number <strong>of</strong> LMXBs is assumed to depend only<br />
on the encounter rate parameter Γh. This fit was considerably better than those for<br />
any other single parameter. Thus, it appears that the most important single factor<br />
determining the occurrence <strong>of</strong> LMXBs in GCs is the dynamical encounter rate.<br />
In the next 4 rows (6-9), the expected number <strong>of</strong> LMXBs is assumed to depend on<br />
pairs <strong>of</strong> the GC properties. It is particularly interesting to compare row 6 with row<br />
5. The encounter rate parameter Γh is calculated from the mass M and the radius<br />
r ′ h<br />
(eq. 5.3). Thus, rows 6 and 5 compare a general dependence on mass and radius<br />
with the specific form expected if LMXBs are formed dynamically in GCs. Allowing<br />
the separate mass and radius dependences does not produce a significantly better fit<br />
(i.e., ∆χ 2 < 2.706, which implies < 90% significance) than just the Γh dependence.<br />
However, both are significantly better fits than just the GC mass, metallicity, or size<br />
dependence alone. In row 6, note that the best-fit exponent for the mass (α = 1.16) is<br />
very close to the value predicted by the dependence on Γh in row 5 (α = 1.5 × 0.78 =<br />
1.17), although the dependence on radius is steeper (δ = −2.84) than predicted by<br />
row 5 (δ = −2.5 ∗ 0.78 = −1.95).<br />
166<br />
In the next set <strong>of</strong> (rows 7–8), the metallicity dependence and either mass or radius
dependence are allowed to vary. Varying mass and metallicity dependences have<br />
the strongest effect; however, neither effect is as strong as varying the dynamical<br />
dependences (combination <strong>of</strong> mass and radius).<br />
In the final set <strong>of</strong> rows, we combine dynamical dependence and metallicity de-<br />
pendence variations, providing the best fits to the data. Our best fit (row 9) is<br />
λ ∝ Γ 0.74+0.14<br />
−0.13<br />
h (Z/Z⊙) 0.50+0.18<br />
−0.16. The dependence on interaction rate matches well with<br />
the Galactic value found by Pooley et al. (2003) <strong>of</strong> λ ∝ Γ 0.74±0.36<br />
h . For comparison<br />
with Jordán et al. (2004b), we fit λ ∝ ρ 1.27+0.20<br />
−0.18<br />
0 r2 c (Z/Z⊙) 0.51+0.18<br />
−0.16 (row 10); our results<br />
agree. We note that allowing mass, metallicity, and size to vary all at once does not<br />
significantly improve the fit compared to allowing encounter rate and metallicity to<br />
vary (row 11).<br />
For our best fit, we find<br />
167<br />
λ = 3.6 × 10 −6 Γ 0.74+0.14<br />
−0.13<br />
h (Z/Z⊙) 0.50+0.18<br />
−0.16 . (5.7)<br />
Since our analysis includes matches below the completeness limit, the measured nor-<br />
malization is intermediate between the true normalizations at the detection limit and<br />
the completeness limit. Nevertheless, we can use the normalization to estimate the<br />
number <strong>of</strong> GCs that might contain multiple LMXBs. By summing 1 − exp −λ (1 + λ)<br />
over all the GCs, we calculate that ∼ 7 GCs contain multiple LMXBs. The majority<br />
<strong>of</strong> GCs we detect are likely to contain only one LMXB.<br />
5.7 X-ray Luminosities and Luminosity Functions<br />
We used the best-fit Chandra X-ray spectrum <strong>of</strong> the inner resolved sources (a <<br />
aeff: Table 5.5, row 3) and the assumption that each source was at the distance <strong>of</strong>
Table 5.5. X-ray Spectral Fits for Point Sources in NGC 4697<br />
NH Row Group a<br />
Model (10 20 cm −2 ) kT /1keV or Γ F0784 b F4727 b F4728 b F4729 b F4730 b Counts χ 2 /d<strong>of</strong><br />
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12)<br />
1 a < aeff Power (2.14) 1.505 +0.048<br />
−0.032<br />
3.77 3.71 3.87 3.79 3.59 7190.3 294.26/245=1.20<br />
2 a < aeff Power 7.0 +2.5<br />
−2.4<br />
1.605 +0.061<br />
−0.060<br />
3.82 3.74 3.88 3.82 3.64 7190.3 283.16/244=1.16<br />
3 c<br />
a < aeff Bremss (2.14) 9.1 +1.3<br />
−1.1<br />
3.42 3.34 3.46 3.41 3.26 7190.3 270.49/245=1.10<br />
4 a < aeff Bremss 1.8 +1.9<br />
−1.8<br />
9.3 +1.9<br />
−1.5<br />
3.42 3.34 3.46 3.41 3.26 7190.3 270.41/244=1.11<br />
5 aeff < a < 2aeff Bremss (2.14) 7.8 +3.3<br />
−2.5<br />
0.82 0.84 0.82 0.90 0.78 1587.4 60.39/57=1.06<br />
6 2aeff < a < 3aeff Bremss (2.14) 5.7 +1.6<br />
−1.1<br />
0.91 0.53 0.62 0.76 0.72 1652.9 68.07/64=1.06<br />
7 2aeff < a < 3aeff Power (2.14) 1.649 +0.079<br />
−0.077<br />
1.00 0.58 0.71 0.86 0.79 1652.9 63.80/64=1.00<br />
d<br />
8 a < 2aeff Bremss (2.14) 8.9 +1.2<br />
−1.0<br />
4.18 4.12 4.22 4.24 3.99 8777.7 331.35/303=1.09<br />
d<br />
9 a < 3aeff Bremss (2.14) 8.3 +1.0<br />
−0.8<br />
5.12 4.65 4.84 5.02 4.72 10430.6 406.00/368=1.10<br />
10 ACS FOV: GC-LMXBs Bremss (2.14) 12.3 +3.6<br />
−2.2<br />
2.17 2.22 2.13 2.24 2.19 4271.8 149.18/152=0.98<br />
11 ACS FOV: GC-LMXBs Bremss 4.7 +2.6<br />
−2.5<br />
10.3 +3.7<br />
−2.2<br />
2.17 2.21 2.10 2.23 2.18 4271.8 146.41/151=0.97<br />
12 ACS FOV: Field-LMXBs Bremss (2.14) 7.3 +1.8<br />
−1.3<br />
1.19 1.11 1.24 1.25 1.16 2614.8 92.38/98=0.94<br />
13 ACS FOV: Field-LMXBs Bremss 0.0 [< 2.1] 8.2 +2.2<br />
−1.6<br />
1.19 1.11 1.25 1.25 1.16 2614.8 89.57/97=0.92<br />
14 ACS FOV: GC-LMXBs + Field-LMXBs d<br />
Bremss (2.14) 10.0 +1.7<br />
−1.3<br />
3.35 3.30 3.37 3.49 3.35 6886.6 250.15/251=1.00<br />
15 ACS FOV: GC-LMXBs + Field-LMXBs d<br />
Bremss 2.6 +2.1<br />
−2.0<br />
9.7 +2.3<br />
−1.7<br />
3.35 3.30 3.37 3.48 3.34 6886.6 250.01/250=1.00<br />
16 ACS FOV: Blue-GC-LMXBs Bremss 0.0 [< 5.5] 99.7 [> 16.6] 0.44 0.53 0.33 0.42 0.39 553.1 13.87/15=0.92<br />
17 ACS FOV: Red-GC-LMXBs Bremss 5.2 +2.8<br />
−2.7<br />
9.1 +3.0<br />
−2.0<br />
1.80 1.78 1.84 1.83 1.79 3643.6 128.77/129=1.00<br />
18 ACS FOV: Red-GC-LMXBs + Blue GC-LMXBs d Bremss 4.5 +2.7<br />
−2.6<br />
10.1 +3.9<br />
−2.2<br />
2.17 2.23 2.12 2.18 2.11 4196.7 148.29/146=1.02<br />
19 a < 2aeff ,L38 < 2 Bremss (2.14) 7.2 +1.1<br />
−0.9<br />
2.26 2.27 2.30 2.21 2.20 5008.8 175.71/182=0.97<br />
20 a < 2aeff ,L38 < 2 Bremss 0.4 [< 2.6] 7.9 +1.5<br />
−1.3<br />
2.26 2.27 2.31 2.22 2.20 5008.8 173.98/181=0.96<br />
21 a < 2aeff ,2 < L38 Bremss (2.14) 10.7 +3.0<br />
−1.9<br />
1.82 1.85 1.82 2.05 1.73 3709.4 120.28/132=0.91<br />
22 a < 2aeff ,2 < L38 Bremss 5.9 +2.9<br />
−2.8<br />
8.3 +2.5<br />
−1.7<br />
1.82 1.83 1.80 2.03 1.72 3709.4 115.13/131=0.91<br />
23 a < 2aeff ,L38 < 2 + 2 < L38 d<br />
Bremss (2.14) 8.4 +1.1<br />
−0.9<br />
4.07 4.11 4.11 4.25 3.92 8718.2 303.73/315=0.96<br />
24 a < 2aeff ,L38 < 2 + 2 < L38 d<br />
Bremss 2.8 +1.8<br />
−1.7<br />
8.1 +0.9<br />
−0.8<br />
4.07 4.10 4.10 4.24 3.92 8718.2 303.36/314=0.97<br />
a<br />
We abbreviate LX /10 38 ergs s −1 in the 0.3–10 keV band as L38.<br />
b −13 −2 −1<br />
Units are 10 ergs cm s in the 0.3–10 keV band.<br />
c<br />
The adopted best-fit model for LMXBs.<br />
d<br />
The group fitted is the simultaneous fit <strong>of</strong> two (or three) other rows. See the note in § 5.9 to understand the implications <strong>of</strong> this.<br />
168
NGC 4697 to convert the observed source count rates into unabsorbed X-ray<br />
(0.3–10 keV) luminosities (LX). The fluxes were corrected for exposure (including<br />
vignetting), the time dependent QE degradation <strong>of</strong> the ACIS-S3 chip, and the PSF<br />
fraction <strong>of</strong> source counts within the region used to extract the counts. The indi-<br />
vidual conversion factors from observed count rates were 1.18, 1.50, 1.46, 1.46, and<br />
1.47 × 10 41 ergs count −1 for a typical source. We list the individual luminosities <strong>of</strong><br />
Observations 0784 (A), 4727 (B), 4728 (C), 4729 (D), and 4730 (E) in columns 2–6<br />
<strong>of</strong> Table 5.6.<br />
In Figure 5.7, we display the individual observation LFs <strong>of</strong> the sources in the<br />
Analysis Sample within a < 220 ′′ . We calculate the probability the LFs <strong>of</strong> each pair<br />
<strong>of</strong> observations are drawn from the same population using the two-sample K-S test.<br />
Since PKS range from 0.33 (0784 versus 4727) to 0.94 (4729 versus 4730), we believe<br />
that the LFs do not change significantly on our inter-observation timescales, which<br />
vary from 11 d to 4.6 yr.<br />
We combined the luminosities from all <strong>of</strong> the different observations; as before, we<br />
included the effects <strong>of</strong> varying exposure (including vignetting), the time dependent<br />
QE degradation <strong>of</strong> the ACIS-S3 chip, and the PSF fraction <strong>of</strong> source counts within<br />
the region used to extract the counts. We give this luminosity, combining all five<br />
observations, as Lall in Table 5.7 (column 4).<br />
One can compare Lall to the individual luminosities using χ 2 to test if the indi-<br />
vidual values are all consistent with a constant luminosity. In Figure 5.8, we display<br />
the LF <strong>of</strong> sources with a < 220 ′′ and a < 90% probability <strong>of</strong> being variable. We fit<br />
this LF (for the 68 sources in the Analysis Sample, Lall > 1.4 × 10 37 ergs s −1 ) using<br />
the same techniques we have used previously (Paper I; Paper II; Blanton et al. 2001;<br />
Irwin et al. 2002). Since the average completeness correction factor in the Analysis<br />
169
Table 5.6. Instantaneous Luminosities <strong>of</strong> X-ray Sources<br />
Source LA LB LC LD LE<br />
(1) (2) (3) (4) (5) (6)<br />
1 40.3± 4.1 32.6±4.0 34.1±4.2 36.2± 4.6 35.3±4.0<br />
2 6.6± 2.0 10.7±2.6 8.9±2.5 10.4± 2.8 5.8±2.0<br />
3 2.5± 1.6 3.6±1.7 3.5±1.8 6.4± 2.3 3.9±1.8<br />
4 11.6± 2.5 7.4±2.2 11.8±2.8 9.7± 2.8 12.5±2.6<br />
5 7.1± 2.1 9.4±2.4 13.6±3.0 10.4± 2.8 10.6±2.5<br />
6 3.4± 1.5 5.9±2.0 6.3±2.2 4.7± 2.1 0.9±1.2<br />
7 21.5± 3.1 22.3±3.3 12.6±2.8 21.8± 3.7 15.0±2.8<br />
8 1.8± 1.4 2.1±1.6 3.5±1.7 1.1± 1.7 1.2±1.3<br />
9 5.7± 1.9 1.1±1.3 1.4±1.6 3.5± 1.9 6.5±2.0<br />
10 20.3± 3.1 18.0±3.1 23.5±3.7 14.7± 3.1 14.7±2.8<br />
11 t 10.7± 2.4 12.1±2.6 11.6±2.7 12.9± 3.0 3.2±1.5<br />
12 5.5± 1.9 1.8±1.4 3.4±1.7 5.6± 2.2 4.3±1.8<br />
13 6.8± 2.0 3.3±1.7 3.5±1.8 4.5± 2.1 2.9±1.5<br />
14 4.9± 1.8 5.2±1.9 6.8±2.1 5.3± 2.2 2.7±1.5<br />
15 18.6± 2.9 15.2±2.8 17.0±3.1 9.2± 2.8 13.2±2.6<br />
16 4.3± 1.7 3.2±1.6 1.6±1.6 4.1± 2.1 3.3±1.7<br />
17 1.5± 1.2 1.6±1.4 0.7±1.1 2.1± 1.7 0.7±1.1<br />
18 2.5± 1.4 0.4±0.9 0.0±1.0 0.3± 1.1 0.6±1.0<br />
19 13.6± 2.6 7.2±2.2 5.5±2.0 12.1± 2.9 8.1±2.2<br />
20 5.1± 1.8 2.2±1.5 3.3±1.6 2.0± 1.6 3.3±1.7<br />
21 0.1± 0.8 1.1±1.2 1.9±1.4 0.6± 1.4 0.5±1.0<br />
22 3.0± 1.5 2.0±1.4 2.6±1.6 1.4± 1.5 4.0±1.8<br />
23 −0.2± 0.9 −0.3±0.8 −0.3±0.9 0.2± 1.1 4.9±1.8<br />
24 1.5± 1.3 1.2±1.3 0.1±1.2 2.0± 1.7 0.9±1.2<br />
25 16.9± 2.8 3.0±1.6 2.8±1.6 6.5± 2.3 7.5±2.1<br />
26 0.3± 1.2 3.5±1.6 −0.7±0.9 0.9± 1.4 −0.3±1.0<br />
27 2.3± 1.5 2.3±1.5 3.3±1.8 3.6± 1.9 4.0±1.7<br />
28 3.7± 1.7 1.5±1.3 −0.3±1.0 2.1± 1.6 1.9±1.4<br />
29 10.7± 2.3 14.2±2.8 13.6±2.8 13.6± 3.0 9.9±2.4<br />
30 4.9± 1.7 2.0±1.4 2.7±1.6 3.9± 2.0 2.9±1.5<br />
31 18.8± 2.9 22.0±3.3 28.1±3.8 29.8± 4.2 19.1±3.1<br />
32 24.3± 3.3 26.4±3.6 20.8±3.3 22.4± 3.7 23.7±3.4<br />
33 1.6± 1.5 1.1±1.1 1.5±1.4 0.5± 1.3 −0.1±0.9<br />
34 8.2± 2.4 6.5±2.0 3.5±1.8 9.9± 2.8 6.7±2.1<br />
35 10.5± 2.2 11.8±2.5 12.6±2.7 12.4± 2.9 6.8±2.1<br />
36 0.3± 1.1 1.4±1.3 1.1±1.3 0.8± 1.3 0.9±1.1<br />
37 t 0.0± 0.7 0.3±0.9 0.0±1.0 1.1± 1.4 8.6±2.3<br />
38 0.8± 1.3 1.2±1.3 1.5±1.4 2.8± 1.8 3.0±1.5<br />
39 38.9± 4.0 18.3±3.0 17.0±3.1 20.1± 3.5 20.5±3.2<br />
40 2.7± 1.5 0.9±1.2 1.9±1.4 0.2± 1.1 1.7±1.3<br />
41 t 0.2± 0.8 4.9±1.8 3.7±1.7 2.6± 1.7 2.5±1.5<br />
42 10.8± 2.3 9.6±2.3 10.5±2.5 11.6± 2.8 10.2±2.4<br />
43 0.7± 1.2 0.3±0.9 0.8±1.1 0.9± 1.4 0.7±1.0<br />
44 1.0± 1.3 2.5±1.5 3.2±1.7 2.3± 1.6 1.8±1.4<br />
Continued on Next Page. . .<br />
170
Table 5.6—Continued<br />
Source LA LB LC LD LE<br />
(1) (2) (3) (4) (5) (6)<br />
45 7.4± 2.0 0.1±1.0 0.1±1.0 0.3± 1.1 −0.1±0.7<br />
46 8.0± 2.1 6.6±2.1 10.3±2.5 8.1± 2.4 10.1±2.5<br />
47 1.6± 1.2 1.5±1.3 0.7±1.1 1.4± 1.5 0.6±1.0<br />
48 8.5± 2.4 4.2±1.8 5.4±2.1 4.8± 2.2 6.8±2.0<br />
49 16.1± 2.9 9.8±2.5 9.2±2.6 12.6± 3.1 11.9±2.7<br />
50 4.9± 1.8 1.0±1.4 2.8±1.7 2.6± 2.0 1.7±1.4<br />
51 t 3.4± 1.6 5.2±1.9 7.6±2.3 0.3± 1.3 −0.1±0.8<br />
52 10.8± 2.3 13.7±2.7 14.1±2.9 6.0± 2.2 12.1±2.6<br />
53 1.7± 1.4 4.8±1.8 0.3±1.0 3.7± 2.0 1.8±1.3<br />
54 62.3± 5.0 61.4±5.3 55.4±5.3 61.3± 5.8 48.8±4.6<br />
55 8.9± 2.2 8.1±2.2 10.7±2.6 8.0± 2.5 12.3±2.5<br />
56 4.7± 1.7 4.0±1.7 5.2±2.1 1.3± 1.5 2.1±1.4<br />
57 6.1± 1.9 7.0±2.1 6.6±2.1 7.4± 2.4 7.5±2.1<br />
58 58.9± 4.8 53.0±4.9 59.1±5.3 62.2± 5.8 66.3±5.4<br />
59 0.5± 1.1 1.4±1.3 2.5±1.5 4.2± 1.9 0.3±0.9<br />
60 −0.2± 0.7 0.5±1.1 −0.1±1.1 −0.5± 1.0 3.2±1.6<br />
61 14.0± 2.6 18.1±3.1 18.9±3.4 20.2± 3.6 17.1±2.9<br />
62 1.6± 1.2 1.0±1.2 0.4±1.0 0.2± 1.2 1.4±1.2<br />
63 20.4± 3.0 33.2±4.0 29.5±4.0 30.2± 4.3 27.0±3.6<br />
64 0.1± 0.8 2.9±1.6 1.4±1.4 0.2± 1.3 0.9±1.1<br />
65 1.2± 1.2 1.5±1.2 0.4±1.0 0.9± 1.2 1.4±1.2<br />
66 9.2± 2.2 10.7±2.5 9.5±2.5 11.4± 2.8 8.8±2.2<br />
67 t −0.3± 0.7 6.0±1.9 12.2±2.7 8.6± 2.6 6.1±2.1<br />
68 t 10.4± 2.3 13.8±2.7 23.1±3.5 −0.1± 0.9 4.5±2.0<br />
69 15.1± 2.6 19.0±3.3 10.1±2.7 12.1± 3.1 13.8±2.7<br />
70 3.4± 1.5 3.6±1.8 0.4±1.0 0.8± 1.3 2.4±1.5<br />
71 4.3± 1.6 5.8±1.9 5.6±2.0 5.0± 2.0 4.8±2.1<br />
72 6.1± 2.6 1.4±1.9 4.3±2.8 4.3± 2.9 1.3±1.8<br />
73 12.3± 3.5 11.2±3.6 10.0±3.6 9.4± 3.8 17.2±4.1<br />
74 3.6± 1.5 1.5±1.2 1.1±1.2 1.7± 1.5 1.0±1.1<br />
75 5.4± 1.7 3.6±1.7 3.6±1.8 2.6± 1.7 10.7±2.4<br />
76 6.3± 1.9 5.1±1.9 8.6±2.5 4.4± 2.0 3.7±1.7<br />
77 t −0.3± 0.7 0.7±1.1 9.2±2.6 5.4± 2.2 9.8±2.3<br />
78 14.9± 2.6 3.4±1.6 2.5±1.5 3.2± 1.8 4.0±1.7<br />
79 1.7± 1.2 5.5±1.9 1.9±1.4 2.0± 1.6 −0.3±1.0<br />
80 30.3± 3.6 39.0±4.3 33.0±4.2 30.4± 4.3 40.3±4.2<br />
81 0.6± 1.1 2.4±1.6 2.7±1.6 1.5± 1.5 0.7±1.1<br />
82 0.9± 1.1 1.9±1.3 0.4±1.0 0.9± 1.2 1.5±1.3<br />
83 3.1± 1.5 7.5±2.2 4.2±1.9 5.8± 2.4 7.3±2.1<br />
84 4.2± 1.6 2.4±1.5 1.3±1.4 4.2± 2.0 2.9±1.5<br />
85 4.4± 1.7 6.3±2.0 4.0±1.8 2.7± 1.8 6.5±2.0<br />
86 1.5± 1.2 0.5±1.2 1.9±1.4 1.1± 1.4 1.5±1.2<br />
87 12.3± 2.4 7.2±2.1 7.1±2.2 9.5± 2.6 8.4±2.5<br />
88 0.7± 0.9 1.8±1.5 0.1±1.0 1.3± 1.4 1.9±1.3<br />
Continued on Next Page. . .<br />
171
Table 5.6—Continued<br />
Source LA LB LC LD LE<br />
(1) (2) (3) (4) (5) (6)<br />
89 6.2± 1.9 5.1±1.8 5.7±2.0 4.4± 2.0 7.8±2.1<br />
90 4.5± 1.8 4.5±1.8 8.1±2.3 10.2± 2.7 4.7±1.9<br />
91 1.8± 1.3 1.1±1.2 0.9±1.4 1.1± 1.7 1.5±1.3<br />
92 3.3± 1.5 2.2±1.4 2.0±1.6 2.3± 1.6 0.9±1.1<br />
93 0.3± 1.0 1.1±1.2 2.1±1.5 3.9± 2.1 1.0±1.1<br />
94 t 0.7± 1.0 0.3±0.9 −0.1±0.8 3.7± 2.0 6.5±2.0<br />
95 1.3± 1.2 1.0±1.2 2.4±1.7 1.6± 1.6 0.9±1.1<br />
96 1.4± 1.2 1.5±1.3 2.0±1.6 1.2± 1.7 1.8±1.4<br />
97 3.0± 1.4 1.2±1.2 −0.1±0.8 0.2± 1.2 1.7±1.4<br />
98 17.4± 2.7 6.6±2.0 10.2±2.5 9.6± 2.6 16.8±3.0<br />
99 8.6± 2.1 12.5±2.7 4.7±2.0 7.9± 2.5 9.1±2.3<br />
100 8.1± 2.1 8.6±2.3 6.9±2.3 9.9± 2.8 9.9±2.3<br />
101 18.8± 2.9 15.0±2.9 17.0±3.2 29.0± 4.3 15.5±2.8<br />
102 1.1± 1.3 1.2±1.3 2.8±1.6 1.3± 1.6 1.5±1.2<br />
103 31.4± 3.6 34.1±4.1 39.6±4.6 41.3± 5.0 27.0±3.6<br />
104 −0.2± 0.8 0.0±1.0 −0.3±1.1 −0.3± 1.0 5.2±1.9<br />
105 1.9± 1.3 0.8±1.2 1.4±1.4 2.7± 1.9 3.2±1.6<br />
106 9.8± 2.2 7.1±2.1 5.7±2.0 4.0± 1.9 5.5±2.0<br />
107 0.6± 0.9 1.2±1.3 1.6±1.4 −0.2± 1.2 1.1±1.2<br />
108 0.0± 0.7 0.8±1.0 0.7±1.1 0.6± 1.3 3.1±1.7<br />
109 2.9± 1.5 3.1±1.6 3.0±1.6 4.6± 2.1 1.6±1.3<br />
110 t −0.2± 1.0 −0.4±0.8 0.0±1.2 0.2± 1.2 32.5±4.0<br />
111 4.9± 1.7 4.3±1.8 4.0±1.8 5.3± 2.2 9.0±2.2<br />
112 2.1± 1.4 1.9±1.4 1.7±1.5 2.5± 1.7 0.8±1.0<br />
113 1.6± 1.3 0.8±1.1 1.1±1.3 0.9± 1.5 0.9±1.1<br />
114 26.7± 3.4 25.1±3.6 19.7±3.4 29.4± 4.3 15.6±2.8<br />
115 3.8± 1.7 11.2±2.5 9.2±2.5 6.5± 2.3 8.6±2.3<br />
116 2.9± 1.4 1.2±1.4 4.8±2.0 2.2± 1.8 2.5±1.5<br />
117 96.3± 6.1 127.4±7.4 81.7±6.3 40.0± 4.8 117.9±7.1<br />
118 22.3± 3.3 15.5±2.9 14.3±3.0 20.1± 3.7 19.8±3.2<br />
119 1.5± 1.3 2.1±1.4 −0.3±1.1 0.9± 1.5 0.8±1.0<br />
120 −0.1± 1.0 2.3±1.5 2.1±1.6 1.6± 1.7 −0.2±0.8<br />
121 t 6.5± 1.8 −0.3±1.1 0.9±1.3 −1.0± 1.4 0.4±0.9<br />
122 11.2± 2.4 2.3±1.7 6.5±2.2 5.7± 2.4 6.6±3.0<br />
123 1.5± 1.3 2.6±1.7 3.0±1.9 2.5± 1.9 2.0±1.5<br />
124 12.6± 2.6 12.0±2.7 7.1±2.5 9.4± 2.7 5.8±2.2<br />
125 16.3± 2.7 15.2±2.9 15.0±3.0 22.4± 3.8 10.8±2.4<br />
126 2.2± 1.3 2.0±1.5 1.6±1.4 4.1± 2.1 0.8±1.2<br />
127 0.7± 0.9 1.0±1.2 0.4±1.0 1.0± 1.4 2.8±1.6<br />
128 34.5± 3.7 · · · · · · · · · 35.3±4.2<br />
129 2.7± 1.4 3.7±1.7 1.5±1.4 3.8± 1.9 2.9±1.6<br />
130 27.3± 3.4 21.2±3.3 13.5±2.9 20.0± 3.6 12.9±2.7<br />
131 3.5± 1.6 2.0±1.5 5.6±2.1 5.4± 2.3 11.3±2.6<br />
132 5.1± 1.8 1.8±1.4 0.4±1.2 1.7± 1.7 2.9±1.5<br />
Continued on Next Page. . .<br />
172
Table 5.6—Continued<br />
Source LA LB LC LD LE<br />
(1) (2) (3) (4) (5) (6)<br />
133 7.2± 2.0 2.4±1.5 5.0±2.0 7.3± 2.5 3.1±1.6<br />
134 154.0± 7.6 195.0±9.4 171.0±9.3 181.2±10.1 163.3±8.3<br />
135 0.4± 1.2 0.5±1.1 1.1±1.4 0.0± 1.4 4.2±2.6<br />
136 3.2± 1.5 · · · · · · · · · 2.6±1.6<br />
137 9.8± 2.3 10.4±2.5 7.6±2.3 8.3± 2.6 10.3±2.5<br />
138 1.0± 1.0 2.6±1.6 0.4±1.2 0.8± 1.5 0.6±1.5<br />
139 3.5± 1.5 1.1±1.3 3.9±1.8 2.5± 1.8 1.0±1.3<br />
140 5.2± 2.8 0.6±1.2 3.0±1.8 2.1± 1.9 0.8±1.2<br />
141 4.6± 1.9 1.7±1.6 3.2±1.8 2.0± 2.1 4.1±1.7<br />
142 5.4± 1.9 1.4±1.4 2.9±1.9 0.8± 1.5 · · ·<br />
143 71.2±17.5 · · · · · · · · · 66.6±5.5<br />
144 3.9± 1.7 2.0±1.7 7.9±2.7 2.0± 2.0 8.7±2.2<br />
145 0.8± 1.0 1.9±1.4 −0.6±1.1 0.2± 1.2 0.8±1.4<br />
146 3.9± 1.6 5.2±4.2 3.9±3.9 1.5± 3.7 2.4±1.6<br />
147 · · · 2.4±1.6 4.4±2.0 13.7± 3.2 6.3±2.7<br />
148 · · · · · · · · · · · · 8.2±2.3<br />
149 7.6± 2.8 · · · · · · · · · 8.5±2.5<br />
150 3.5± 1.6 1.3±1.3 1.7±1.5 1.8± 2.0 2.4±1.7<br />
151 11.5± 2.4 · · · · · · · · · 11.6±5.4<br />
152 0.4± 1.7 1.9±1.7 1.9±1.8 5.7± 2.5 · · ·<br />
153 14.8± 3.3 · · · · · · · · · 7.0±2.4<br />
154 · · · · · · · · · · · · 36.5±4.3<br />
155 · · · 89.1±6.6 95.8±7.1 121.6± 8.4 · · ·<br />
156 · · · 117.1±7.5 66.9±6.2 82.9± 7.2 · · ·<br />
157 · · · · · · · · · · · · 4.5±2.2<br />
158 · · · 5.9±3.0 8.5±3.4 3.0± 3.4 · · ·<br />
NOTE.—Individual luminosities (in units <strong>of</strong> 10 37 ergs s −1 ) <strong>of</strong> Observations 0784<br />
4727, 4728, 4729, 4730 are indicated by LA, LB, LC, LD, and LE, respectively.<br />
t Source is a transient candidate.<br />
173
Fig. 5.7.— Cumulative luminosity functions for each <strong>of</strong> the five observations <strong>of</strong> the<br />
sources detected at the > 3σ level within a < 220 ′′ . The two-sample K-S tests do not<br />
indicate that any two <strong>of</strong> the observations are drawn from different populations.<br />
174
Table 5.7. Combined Luminosities & Hardness Ratios <strong>of</strong> X-ray Sources<br />
Source Not Detected Not in FOV Lall H21 0 all H31 0 all H32 0 all<br />
(1) (2) (3) (4) (5) (6) (7)<br />
1 · · · · · · 35.8±1.8 −0.16 +0.05<br />
−0.05<br />
2 ABCDE · · · 8.4±0.9 −0.13 +0.12<br />
−0.11<br />
3 ABCDE · · · 3.9±0.7 −0.18 +0.18<br />
−0.16<br />
4 B · · · 10.6±1.0 −0.33 +0.09<br />
−0.08<br />
5 · · · · · · 10.1±1.0 −0.17 +0.11<br />
−0.10<br />
6 AE · · · 4.1±0.7 −0.29 +0.16<br />
−0.14<br />
7 · · · · · · 18.7±1.3 −0.24 +0.07<br />
−0.07<br />
8 ABCDE · · · 2.0±0.6 −0.31 +0.29<br />
−0.21<br />
9 BCD · · · 3.7±0.7 −0.17 +0.18<br />
−0.16<br />
10 · · · · · · 18.3±1.3 −0.11 +0.08<br />
−0.08<br />
11 t · · · · · · 9.9±1.0 −0.37 +0.08<br />
−0.08<br />
12 B · · · 4.1±0.7 −0.31 +0.16<br />
−0.14<br />
13 E · · · 4.3±0.7 −0.13 +0.18<br />
−0.16<br />
14 E · · · 4.9±0.7 −0.41 +0.12<br />
−0.12<br />
15 · · · · · · 14.9±1.2 −0.17 +0.08<br />
−0.08<br />
16 · · · · · · 3.3±0.7 +0.12 +0.25<br />
−0.23<br />
17 ABCDE · · · 1.3±0.5 −0.35 +0.34<br />
−0.27<br />
18 BCDE · · · 0.8±0.4 −0.41 +0.36<br />
−0.29<br />
19 · · · · · · 9.4±1.0 −0.98 +0.02<br />
−0.01<br />
20 BD · · · 3.3±0.6 −0.21 +0.18<br />
−0.16<br />
21 ABCDE · · · 0.8±0.4 −0.09 +0.62<br />
−0.38<br />
22 BCD · · · 2.6±0.6 −0.23 +0.25<br />
−0.21<br />
23 ABCD · · · 0.9±0.4 −1.00 +0.13<br />
−0.00<br />
24 ABCDE · · · 1.1±0.5 −0.40 +0.40<br />
−0.29<br />
25 · · · · · · 7.7±0.9 −0.95 +0.03<br />
−0.03<br />
26 ACDE · · · 0.8±0.4 −0.85 +0.33<br />
−0.15<br />
27 ABD · · · 3.1±0.6 −0.32 +0.19<br />
−0.17<br />
28 BCDE · · · 1.8±0.5 −0.32 +0.28<br />
−0.24<br />
29 · · · · · · 12.3±1.1 −0.17 +0.10<br />
−0.09<br />
30 B · · · 3.3±0.6 −0.01 +0.19<br />
−0.18<br />
31 · · · · · · 23.1±1.4 −0.18 +0.07<br />
−0.07<br />
32 · · · · · · 23.6±1.4 −0.03 +0.07<br />
−0.07<br />
33 ABCDE · · · 0.9±0.4 −0.46 +0.43<br />
−0.26<br />
34 · · · · · · 6.9±0.9 −0.00 +0.14<br />
−0.14<br />
35 · · · · · · 10.8±1.0 −0.07 +0.10<br />
−0.10<br />
36 ABCDE · · · 0.9±0.4 −0.07 +0.53<br />
−0.37<br />
37 t ABCD · · · 2.1±0.5 −0.16 +0.24<br />
−0.21<br />
38 ABC · · · 1.9±0.5 +0.06 +0.30<br />
−0.26<br />
39 · · · · · · 23.6±1.4 +0.02 +0.07<br />
−0.07<br />
40 ABCDE · · · 1.5±0.5 −0.61 +0.30<br />
−0.24<br />
41 t ADE · · · 2.7±0.6 −0.21 +0.23<br />
−0.21<br />
42 · · · · · · 10.5±1.0 −0.21 +0.10<br />
−0.10<br />
43 ABCDE · · · 0.7±0.4 −0.10 +0.61<br />
−0.44<br />
44 ADE · · · 2.2±0.5 −0.12 +0.36<br />
−0.29<br />
Continued on Next Page. . .<br />
−0.44+0.05<br />
−0.05<br />
−0.53+0.11<br />
−0.10<br />
−0.64+0.16<br />
−0.12<br />
−0.78+0.07<br />
−0.06<br />
−0.39+0.11<br />
−0.10<br />
−0.76+0.12<br />
−0.10<br />
−0.42+0.07<br />
−0.07<br />
−0.65+0.24<br />
−0.19<br />
−0.79+0.14<br />
−0.11<br />
−0.37+0.08<br />
−0.07<br />
−0.94+0.04<br />
−0.03<br />
−0.50+0.16<br />
−0.13<br />
−0.38+0.18<br />
−0.16<br />
−0.71+0.11<br />
−0.09<br />
−0.48+0.08<br />
−0.07<br />
+0.03+0.27<br />
−0.24<br />
−0.57+0.30<br />
−0.22<br />
−0.75+0.36<br />
−0.25<br />
−0.99+0.02<br />
−0.01<br />
−0.69+0.17<br />
−0.13<br />
−0.63+0.63<br />
−0.28<br />
−0.26+0.24<br />
−0.20<br />
−1.00+0.11<br />
−0.00<br />
−0.69+0.37<br />
−0.21<br />
−1.00+0.01<br />
−0.00<br />
−0.87+0.29<br />
−0.13<br />
−0.58+0.18<br />
−0.14<br />
−0.47+0.27<br />
−0.21<br />
−0.41+0.09<br />
−0.09<br />
−0.48+0.21<br />
−0.17<br />
−0.43+0.06<br />
−0.06<br />
−0.33+0.07<br />
−0.07<br />
−0.69+0.40<br />
−0.25<br />
−0.28+0.16<br />
−0.14<br />
−0.34+0.10<br />
−0.10<br />
−0.49+0.56<br />
−0.34<br />
−0.70+0.21<br />
−0.15<br />
−0.58+0.33<br />
−0.23<br />
−0.23+0.07<br />
−0.07<br />
−0.21+0.29<br />
−0.25<br />
−0.13+0.23<br />
−0.21<br />
−0.35+0.10<br />
−0.09<br />
−0.43+0.66<br />
−0.37<br />
+0.11+0.31<br />
−0.28<br />
−0.30 +0.05<br />
−0.06<br />
−0.43 +0.12<br />
−0.11<br />
−0.53 +0.17<br />
−0.16<br />
−0.60 +0.11<br />
−0.10<br />
−0.23 +0.11<br />
−0.11<br />
−0.60 +0.18<br />
−0.15<br />
−0.20 +0.08<br />
−0.08<br />
−0.43 +0.29<br />
−0.27<br />
−0.71 +0.17<br />
−0.15<br />
−0.27 +0.08<br />
−0.07<br />
−0.88 +0.08<br />
−0.06<br />
−0.22 +0.19<br />
−0.18<br />
−0.25 +0.17<br />
−0.17<br />
−0.43 +0.17<br />
−0.16<br />
−0.34 +0.09<br />
−0.08<br />
−0.10 +0.19<br />
−0.19<br />
−0.27 +0.39<br />
−0.33<br />
−0.49 +0.54<br />
−0.51<br />
−0.39 +0.66<br />
−0.61<br />
−0.56 +0.20<br />
−0.18<br />
−0.57 +0.42<br />
−0.32<br />
−0.04 +0.22<br />
−0.23<br />
+0.00 +1.00<br />
−1.00<br />
−0.40 +0.50<br />
−0.37<br />
−1.00 +0.51<br />
−0.00<br />
−0.06 +1.06<br />
−0.94<br />
−0.31 +0.22<br />
−0.20<br />
−0.17 +0.32<br />
−0.29<br />
−0.26 +0.09<br />
−0.09<br />
−0.47 +0.18<br />
−0.16<br />
−0.28 +0.07<br />
−0.07<br />
−0.30 +0.06<br />
−0.06<br />
−0.33 +0.51<br />
−0.51<br />
−0.28 +0.13<br />
−0.13<br />
−0.27 +0.10<br />
−0.10<br />
−0.43 +0.38<br />
−0.37<br />
−0.60 +0.23<br />
−0.19<br />
−0.62 +0.24<br />
−0.20<br />
−0.25 +0.07<br />
−0.06<br />
+0.46 +0.31<br />
−0.33<br />
+0.09 +0.21<br />
−0.21<br />
−0.15 +0.11<br />
−0.10<br />
−0.34 +0.49<br />
−0.40<br />
+0.23 +0.22<br />
−0.23<br />
175
Table 5.7—Continued<br />
Source Not Detected Not in FOV Lall H21 0 all H31 0 all H32 0 all<br />
(1) (2) (3) (4) (5) (6) (7)<br />
45 BCDE · · · 1.7±0.5 −0.10 +0.24<br />
−0.22<br />
46 · · · · · · 8.6±0.9 −0.13 +0.12<br />
−0.11<br />
47 ABCDE · · · 1.2±0.4 +0.05 +0.44<br />
−0.39<br />
48 · · · · · · 5.9±0.8 −0.07 +0.14<br />
−0.14<br />
49 · · · · · · 12.1±1.1 −0.10 +0.10<br />
−0.09<br />
50 BDE · · · 2.7±0.6 −0.35 +0.19<br />
−0.16<br />
51 t DE · · · 3.4±0.6 −0.31 +0.17<br />
−0.15<br />
52 · · · · · · 11.5±1.0 −0.15 +0.09<br />
−0.09<br />
53 ACDE · · · 2.5±0.6 −0.02 +0.20<br />
−0.19<br />
54 · · · · · · 57.8±2.2 −0.07 +0.04<br />
−0.04<br />
55 · · · · · · 9.7±1.0 −0.39 +0.09<br />
−0.08<br />
56 DE · · · 3.5±0.6 −0.11 +0.18<br />
−0.18<br />
57 · · · · · · 6.9±0.8 +0.07 +0.14<br />
−0.13<br />
58 · · · · · · 59.8±2.2 −0.06 +0.04<br />
−0.04<br />
59 D · · · 1.6±0.5 −0.27 +0.31<br />
−0.25<br />
60 ABCD · · · 0.6±0.4 −0.03 +0.90<br />
−0.46<br />
61 · · · · · · 17.4±1.3 −0.16 +0.08<br />
−0.08<br />
62 ABCDE · · · 1.0±0.4 −0.97 +0.15<br />
−0.03<br />
63 · · · · · · 27.7±1.6 −0.09 +0.06<br />
−0.06<br />
64 ABCDE · · · 1.1±0.4 −0.65 +0.28<br />
−0.21<br />
65 ABCDE · · · 1.1±0.4 −0.65 +0.23<br />
−0.17<br />
66 · · · · · · 9.8±1.0 −0.07 +0.12<br />
−0.11<br />
67 t A · · · 6.2±0.8 +0.06 +0.16<br />
−0.15<br />
68 t DE · · · 10.7±1.0 −0.32 +0.10<br />
−0.09<br />
69 · · · · · · 14.2±1.2 −0.06 +0.09<br />
−0.09<br />
70 CD · · · 2.2±0.5 +0.12 +0.26<br />
−0.25<br />
71 · · · · · · 5.1±0.7 −0.34 +0.16<br />
−0.14<br />
72 BCDE · · · 3.5±0.9 −0.37 +0.22<br />
−0.19<br />
73 · · · · · · 12.2±1.5 −0.03 +0.14<br />
−0.13<br />
74 BCDE · · · 1.8±0.5 +0.16 +0.27<br />
−0.26<br />
75 · · · · · · 5.3±0.7 +0.08 +0.14<br />
−0.14<br />
76 · · · · · · 5.6±0.8 −0.28 +0.13<br />
−0.12<br />
77 t AB · · · 4.7±0.7 −0.26 +0.14<br />
−0.13<br />
78 · · · · · · 6.0±0.8 −1.00 +0.02<br />
−0.00<br />
79 ACE · · · 2.2±0.5 −0.13 +0.24<br />
−0.22<br />
80 · · · · · · 34.7±1.7 −0.22 +0.05<br />
−0.05<br />
81 ABDE · · · 1.5±0.5 +0.51 +0.49<br />
−0.53<br />
82 ACDE · · · 1.1±0.4 −0.55 +0.27<br />
−0.21<br />
83 · · · · · · 5.5±0.8 +0.02 +0.15<br />
−0.15<br />
84 BC · · · 3.0±0.6 −0.73 +0.11<br />
−0.10<br />
85 · · · · · · 4.8±0.7 −0.00 +0.17<br />
−0.16<br />
86 ABCDE · · · 1.3±0.4 −0.80 +0.22<br />
−0.15<br />
87 · · · · · · 9.0±0.9 −0.20 +0.11<br />
−0.10<br />
88 ABCD · · · 1.2±0.4 −0.05 +0.44<br />
−0.36<br />
Continued on Next Page. . .<br />
−0.86+0.25<br />
−0.14<br />
−0.34+0.12<br />
−0.11<br />
+0.05+0.44<br />
−0.38<br />
−0.47+0.14<br />
−0.13<br />
−0.50+0.10<br />
−0.09<br />
−0.80+0.14<br />
−0.11<br />
−0.77+0.13<br />
−0.10<br />
−0.47+0.09<br />
−0.08<br />
−1.00+0.15<br />
−0.00<br />
−0.35+0.04<br />
−0.04<br />
−0.69+0.07<br />
−0.07<br />
−0.41+0.19<br />
−0.16<br />
−0.34+0.15<br />
−0.13<br />
−0.28+0.04<br />
−0.04<br />
−0.34+0.31<br />
−0.25<br />
−0.65+0.97<br />
−0.35<br />
−0.34+0.08<br />
−0.08<br />
−1.00+0.04<br />
−0.00<br />
−0.40+0.06<br />
−0.06<br />
−0.71+0.25<br />
−0.18<br />
−0.93+0.17<br />
−0.07<br />
−0.15+0.11<br />
−0.11<br />
−0.15+0.17<br />
−0.15<br />
−0.40+0.09<br />
−0.09<br />
−0.35+0.09<br />
−0.09<br />
−0.26+0.31<br />
−0.26<br />
−0.29+0.15<br />
−0.13<br />
−0.59+0.21<br />
−0.16<br />
−0.18+0.14<br />
−0.14<br />
−0.31+0.31<br />
−0.27<br />
−0.71+0.13<br />
−0.11<br />
−0.55+0.13<br />
−0.11<br />
−0.79+0.11<br />
−0.08<br />
−1.00+0.02<br />
−0.00<br />
−0.42+0.26<br />
−0.21<br />
−0.62+0.04<br />
−0.04<br />
+0.55+0.45<br />
−0.52<br />
−0.65+0.24<br />
−0.19<br />
−0.41+0.16<br />
−0.14<br />
−0.89+0.09<br />
−0.07<br />
−0.22+0.18<br />
−0.16<br />
−0.50+0.26<br />
−0.21<br />
−0.49+0.10<br />
−0.09<br />
−0.09+0.45<br />
−0.37<br />
−0.84 +0.28<br />
−0.16<br />
−0.23 +0.11<br />
−0.11<br />
−0.00 +0.34<br />
−0.34<br />
−0.41 +0.14<br />
−0.13<br />
−0.42 +0.10<br />
−0.09<br />
−0.62 +0.23<br />
−0.19<br />
−0.61 +0.20<br />
−0.17<br />
−0.35 +0.10<br />
−0.10<br />
−1.00 +0.15<br />
−0.00<br />
−0.29 +0.04<br />
−0.04<br />
−0.41 +0.12<br />
−0.11<br />
−0.31 +0.18<br />
−0.17<br />
−0.40 +0.12<br />
−0.11<br />
−0.22 +0.04<br />
−0.04<br />
−0.08 +0.29<br />
−0.28<br />
−0.63 +0.53<br />
−0.37<br />
−0.19 +0.08<br />
−0.08<br />
−1.00 +1.00<br />
−0.00<br />
−0.32 +0.06<br />
−0.06<br />
−0.11 +0.55<br />
−0.47<br />
−0.71 +0.56<br />
−0.29<br />
−0.08 +0.10<br />
−0.11<br />
−0.21 +0.12<br />
−0.12<br />
−0.10 +0.11<br />
−0.11<br />
−0.29 +0.09<br />
−0.08<br />
−0.37 +0.23<br />
−0.22<br />
+0.06 +0.16<br />
−0.16<br />
−0.28 +0.29<br />
−0.26<br />
−0.15 +0.12<br />
−0.12<br />
−0.45 +0.24<br />
−0.20<br />
−0.75 +0.11<br />
−0.09<br />
−0.31 +0.16<br />
−0.15<br />
−0.67 +0.15<br />
−0.13<br />
+0.00 +1.00<br />
−1.00<br />
−0.30 +0.25<br />
−0.24<br />
−0.47 +0.05<br />
−0.05<br />
+0.05 +0.26<br />
−0.26<br />
−0.16 +0.44<br />
−0.40<br />
−0.43 +0.14<br />
−0.13<br />
−0.46 +0.36<br />
−0.32<br />
−0.22 +0.15<br />
−0.14<br />
+0.50 +0.37<br />
−0.46<br />
−0.32 +0.11<br />
−0.11<br />
−0.04 +0.34<br />
−0.33<br />
176
Table 5.7—Continued<br />
Source Not Detected Not in FOV Lall H21 0 all H31 0 all H32 0 all<br />
(1) (2) (3) (4) (5) (6) (7)<br />
89 · · · · · · 5.9±0.8 −0.22 +0.13<br />
−0.12<br />
90 · · · · · · 6.2±0.8 −0.17 +0.13<br />
−0.12<br />
91 ABCDE · · · 1.3±0.5 +0.62 +0.38<br />
−0.45<br />
92 CDE · · · 2.1±0.5 −0.39 +0.22<br />
−0.19<br />
93 ABCE · · · 1.5±0.5 −0.13 +0.37<br />
−0.30<br />
94 t ABC · · · 2.2±0.5 −0.62 +0.16<br />
−0.13<br />
95 ABDE · · · 1.4±0.5 −0.28 +0.28<br />
−0.26<br />
96 ABDE · · · 1.5±0.5 −0.15 +0.64<br />
−0.48<br />
97 BCDE · · · 1.3±0.4 −0.26 +0.34<br />
−0.27<br />
98 · · · · · · 12.4±1.1 −0.27 +0.08<br />
−0.08<br />
99 · · · · · · 8.7±0.9 −0.25 +0.10<br />
−0.09<br />
100 · · · · · · 8.7±0.9 −0.15 +0.12<br />
−0.11<br />
101 · · · · · · 18.7±1.3 −0.25 +0.06<br />
−0.06<br />
102 ABDE · · · 1.5±0.5 +0.25 +0.48<br />
−0.35<br />
103 · · · · · · 34.2±1.7 −0.14 +0.05<br />
−0.05<br />
104 ABCD · · · 0.9±0.4 −0.21 +0.63<br />
−0.40<br />
105 ABCD · · · 2.0±0.5 +1.00 +0.00<br />
−0.35<br />
106 · · · · · · 6.6±0.8 −0.16 +0.12<br />
−0.11<br />
107 ABCDE · · · 0.9±0.4 +0.15 +0.63<br />
−0.46<br />
108 ABCD · · · 1.0±0.4 −0.73 +0.22<br />
−0.16<br />
109 E · · · 2.9±0.6 −0.37 +0.22<br />
−0.19<br />
110 t ABCD · · · 6.6±0.8 −1.00 +0.02<br />
−0.00<br />
111 · · · · · · 5.6±0.8 −0.26 +0.13<br />
−0.12<br />
112 ABCDE · · · 1.8±0.5 +0.68 +0.32<br />
−0.56<br />
113 ABCDE · · · 1.1±0.4 +0.14 +0.53<br />
−0.41<br />
114 · · · · · · 23.2±1.5 −0.22 +0.06<br />
−0.06<br />
115 · · · · · · 7.8±0.9 +0.04 +0.13<br />
−0.13<br />
116 BD · · · 2.7±0.6 −0.16 +0.19<br />
−0.19<br />
117 · · · · · · 94.9±2.8 −0.07 +0.03<br />
−0.03<br />
118 · · · · · · 18.5±1.3 −0.32 +0.07<br />
−0.07<br />
119 ABCDE · · · 1.0±0.4 +1.00 +0.00<br />
−1.00<br />
120 ABCDE · · · 1.1±0.5 +0.05 +0.94<br />
−0.48<br />
121 t BCDE · · · 1.6±0.5 −0.34 +0.24<br />
−0.21<br />
122 B · · · 6.6±0.9 −0.30 +0.12<br />
−0.12<br />
123 ABD · · · 2.3±0.6 +1.00 +0.00<br />
−0.45<br />
124 · · · · · · 9.6±1.0 −0.41 +0.10<br />
−0.09<br />
125 · · · · · · 15.7±1.2 −0.04 +0.09<br />
−0.08<br />
126 BCE · · · 2.1±0.5 +0.37 +0.33<br />
−0.30<br />
127 ABCD · · · 1.2±0.4 −0.25 +0.33<br />
−0.28<br />
128 · · · BCD 34.9±2.7 −0.45 +0.07<br />
−0.06<br />
129 C · · · 2.9±0.6 +0.06 +0.26<br />
−0.23<br />
130 · · · · · · 19.3±1.3 −0.25 +0.07<br />
−0.07<br />
131 B · · · 5.5±0.8 +0.12 +0.17<br />
−0.16<br />
132 BCDE · · · 2.6±0.6 −0.24 +0.21<br />
−0.20<br />
Continued on Next Page. . .<br />
−0.55+0.12<br />
−0.10<br />
−0.51+0.13<br />
−0.11<br />
+0.36+0.64<br />
−0.59<br />
−0.65+0.18<br />
−0.14<br />
−0.24+0.40<br />
−0.30<br />
−0.97+0.10<br />
−0.03<br />
−0.73+0.26<br />
−0.22<br />
+0.45+0.37<br />
−0.33<br />
−0.44+0.33<br />
−0.25<br />
−0.64+0.07<br />
−0.07<br />
−0.57+0.10<br />
−0.09<br />
−0.39+0.12<br />
−0.10<br />
−0.74+0.05<br />
−0.05<br />
−0.01+0.59<br />
−0.41<br />
−0.44+0.05<br />
−0.05<br />
−0.19+0.62<br />
−0.42<br />
+1.00+0.00<br />
−0.20<br />
−0.69+0.11<br />
−0.09<br />
−0.22+0.82<br />
−0.46<br />
−0.87+0.20<br />
−0.13<br />
−0.14+0.20<br />
−0.19<br />
−1.00+0.01<br />
−0.00<br />
−0.60+0.12<br />
−0.11<br />
+0.70+0.30<br />
−0.53<br />
−0.09+0.62<br />
−0.42<br />
−0.60+0.06<br />
−0.05<br />
−0.29+0.14<br />
−0.13<br />
−0.68+0.19<br />
−0.16<br />
−0.32+0.03<br />
−0.03<br />
−0.64+0.06<br />
−0.05<br />
+1.00+0.00<br />
−0.00<br />
+0.15+0.85<br />
−0.48<br />
−1.00+0.24<br />
−0.00<br />
−0.70+0.11<br />
−0.10<br />
+1.00+0.00<br />
−0.56<br />
−0.56+0.09<br />
−0.08<br />
−0.38+0.09<br />
−0.08<br />
+0.06+0.44<br />
−0.36<br />
−0.50+0.34<br />
−0.25<br />
−0.74+0.05<br />
−0.05<br />
+0.01+0.26<br />
−0.23<br />
−0.60+0.06<br />
−0.06<br />
−0.13+0.19<br />
−0.17<br />
−0.50+0.21<br />
−0.18<br />
−0.37 +0.14<br />
−0.13<br />
−0.37 +0.14<br />
−0.13<br />
−0.34 +0.31<br />
−0.28<br />
−0.34 +0.28<br />
−0.25<br />
−0.11 +0.29<br />
−0.31<br />
−0.86 +0.36<br />
−0.14<br />
−0.56 +0.38<br />
−0.35<br />
+0.57 +0.26<br />
−0.29<br />
−0.21 +0.34<br />
−0.32<br />
−0.44 +0.10<br />
−0.09<br />
−0.37 +0.12<br />
−0.12<br />
−0.26 +0.12<br />
−0.11<br />
−0.60 +0.07<br />
−0.07<br />
−0.26 +0.27<br />
−0.27<br />
−0.31 +0.06<br />
−0.05<br />
+0.02 +0.43<br />
−0.44<br />
+0.31 +0.20<br />
−0.22<br />
−0.60 +0.12<br />
−0.11<br />
−0.36 +0.41<br />
−0.36<br />
−0.39 +0.62<br />
−0.61<br />
+0.24 +0.20<br />
−0.22<br />
+0.00 +1.00<br />
−1.00<br />
−0.40 +0.15<br />
−0.14<br />
+0.05 +0.23<br />
−0.23<br />
−0.23 +0.34<br />
−0.32<br />
−0.44 +0.07<br />
−0.07<br />
−0.33 +0.12<br />
−0.11<br />
−0.58 +0.23<br />
−0.20<br />
−0.26 +0.03<br />
−0.03<br />
−0.41 +0.08<br />
−0.08<br />
+0.80 +0.20<br />
−0.25<br />
+0.09 +0.34<br />
−0.37<br />
−1.00 +0.43<br />
−0.00<br />
−0.50 +0.16<br />
−0.15<br />
−0.15 +0.21<br />
−0.22<br />
−0.20 +0.13<br />
−0.13<br />
−0.35 +0.08<br />
−0.08<br />
−0.32 +0.23<br />
−0.22<br />
−0.28 +0.35<br />
−0.32<br />
−0.43 +0.10<br />
−0.09<br />
−0.05 +0.20<br />
−0.19<br />
−0.41 +0.08<br />
−0.07<br />
−0.24 +0.14<br />
−0.14<br />
−0.28 +0.26<br />
−0.24<br />
177
Table 5.7—Continued<br />
Source Not Detected Not in FOV Lall H21 0 all H31 0 all H32 0 all<br />
(1) (2) (3) (4) (5) (6) (7)<br />
133 B · · · 5.0±0.7 +0.14 +0.17<br />
−0.18<br />
134 · · · · · · 171.7±3.8 +0.62 +0.03<br />
−0.03<br />
135 ABCD · · · 1.0±0.5 −0.64 +0.33<br />
−0.28<br />
136 E BCD 2.9±1.0 +0.56 +0.44<br />
−0.98<br />
137 · · · · · · 9.4±1.0 −0.27 +0.11<br />
−0.10<br />
138 ABCDE · · · 1.1±0.5 −0.30 +1.30<br />
−0.70<br />
139 BDE · · · 2.4±0.6 −0.13 +0.24<br />
−0.21<br />
140 ABCDE · · · 2.1±0.6 −0.23 +0.30<br />
−0.23<br />
141 BCD · · · 3.2±0.7 −0.50 +0.19<br />
−0.16<br />
142 BCD E 2.8±0.7 −0.40 +0.24<br />
−0.21<br />
143 · · · BCD 67.2±5.2 −0.37 +0.07<br />
−0.07<br />
144 BD · · · 5.1±0.8 +0.03 +0.19<br />
−0.17<br />
145 ABCDE · · · 0.6±0.4 +0.13 +0.87<br />
−1.12<br />
146 CDE · · · 3.4±0.9 +0.39 +0.35<br />
−0.32<br />
147 B A 6.5±1.0 −0.10 +0.16<br />
−0.15<br />
148 · · · ABCD 8.2±2.3 +1.00 +0.00<br />
−0.22<br />
149 · · · BCD 8.1±1.7 −0.06 +0.24<br />
−0.21<br />
150 BCDE · · · 2.2±0.6 +0.46 +0.26<br />
−0.25<br />
151 · · · BCD 11.5±2.1 −0.23 +0.16<br />
−0.16<br />
152 ABCD · · · 2.4±0.8 +0.22 +0.48<br />
−0.36<br />
153 · · · BCD 10.5±1.9 +0.60 +0.21<br />
−0.23<br />
154 · · · ABCD 36.5±4.3 −0.15 +0.13<br />
−0.12<br />
155 · · · AE 101.1±4.1 −0.02 +0.05<br />
−0.05<br />
156 · · · AE 90.0±3.9 −0.79 +0.02<br />
−0.02<br />
157 · · · ABCD 4.5±2.2 +0.05 +0.55<br />
−0.45<br />
158 BCD AE 6.0±1.7 +0.99 +0.01<br />
−0.45<br />
−0.06+0.19<br />
−0.18<br />
+0.60+0.03<br />
−0.03<br />
−0.78+0.31<br />
−0.22<br />
+0.90+0.10<br />
−0.41<br />
−0.38+0.11<br />
−0.10<br />
+0.70+0.30<br />
−0.47<br />
−0.42+0.26<br />
−0.22<br />
−0.49+0.29<br />
−0.23<br />
−0.52+0.18<br />
−0.16<br />
−0.47+0.23<br />
−0.22<br />
−0.65+0.06<br />
−0.06<br />
−0.17+0.20<br />
−0.18<br />
+0.58+0.42<br />
−0.64<br />
+0.41+0.34<br />
−0.33<br />
−0.66+0.15<br />
−0.13<br />
+1.00+0.00<br />
−0.09<br />
−0.33+0.26<br />
−0.22<br />
−0.36+0.49<br />
−0.42<br />
−0.65+0.17<br />
−0.14<br />
−0.30+0.67<br />
−0.46<br />
+0.51+0.26<br />
−0.27<br />
−0.37+0.13<br />
−0.12<br />
−0.30+0.05<br />
−0.05<br />
−1.00+0.01<br />
−0.00<br />
−0.13+0.60<br />
−0.51<br />
+0.98+0.02<br />
−0.64<br />
−0.19 +0.15<br />
−0.14<br />
−0.03 +0.02<br />
−0.02<br />
−0.28 +0.79<br />
−0.72<br />
+0.68 +0.21<br />
−0.25<br />
−0.12 +0.12<br />
−0.12<br />
+0.83 +0.17<br />
−0.33<br />
−0.31 +0.25<br />
−0.25<br />
−0.29 +0.30<br />
−0.29<br />
−0.03 +0.27<br />
−0.28<br />
−0.09 +0.30<br />
−0.33<br />
−0.37 +0.09<br />
−0.09<br />
−0.20 +0.16<br />
−0.15<br />
+0.49 +0.51<br />
−0.54<br />
+0.02 +0.22<br />
−0.22<br />
−0.60 +0.15<br />
−0.14<br />
+0.43 +0.20<br />
−0.22<br />
−0.27 +0.21<br />
−0.21<br />
−0.71 +0.22<br />
−0.20<br />
−0.49 +0.20<br />
−0.19<br />
−0.49 +0.31<br />
−0.33<br />
−0.14 +0.16<br />
−0.16<br />
−0.24 +0.13<br />
−0.12<br />
−0.28 +0.04<br />
−0.04<br />
−0.99 +0.06<br />
−0.01<br />
−0.18 +0.45<br />
−0.44<br />
−0.22 +0.22<br />
−0.22<br />
NOTE.—Luminosities are in units <strong>of</strong> 10 37 ergs s −1 . Observations 0784, 4727, 4728, 4729, 4730<br />
are indicated by A, B, C, D, and E, respectively. If an observation is listed in the “Not in FOV”<br />
column, it means the source was not in the S3 FOV for that observation, and thus could not<br />
possibly be detected. If an observation is listed in the “Not Detected” column, it means the<br />
source was in the FOV for that observation, but was not detected by wavdetect in that<br />
individual observation. Sources with ABCDE in the “Not Detected” were not detected in any<br />
individual observation, only in the combined sum <strong>of</strong> the observations.<br />
t Source is a transient candidate.<br />
178
Fig. 5.8.— Cumulative luminosity function <strong>of</strong> the constant sources (LX = Lconstant)<br />
detected within a < 220 ′′ using their cumulative luminosity for all observations. The<br />
continuous curves are the sum <strong>of</strong> the best-fit LMXB luminosity functions (to sources<br />
detected at the 3σ level) and the expected background source counts. The broken<br />
power law is the best fit model; however, a cut<strong>of</strong>f power law is acceptable according<br />
to the K-S test.<br />
179
Sample is only ∼ 1.01, we do not apply completeness corrections for this fit. We<br />
adopted the background LF from Kim et al. (2004); however, we have assumed that<br />
background sources exhibit the same level <strong>of</strong> variability as the LMXBs and reduced<br />
the expected background number from 11.7 to 8.2.<br />
We modeled the LMXB populations with a single power law, a cut<strong>of</strong>f power law,<br />
and a broken power law.<br />
Single :<br />
Cut<strong>of</strong>f :<br />
Broken :<br />
dN<br />
dL37<br />
dN<br />
dL37<br />
dN<br />
dL37<br />
180<br />
= N0,s L −αs<br />
=<br />
37 ;<br />
⎧<br />
−αc ⎪⎨ LX<br />
Lc<br />
N0,c<br />
⎪⎩ 0<br />
if LX ≤ Lc;<br />
otherwise;<br />
(5.8a)<br />
(5.8b)<br />
=<br />
⎧<br />
−αl ⎪⎨ LX<br />
Lb<br />
N0,b −αh ⎪⎩ LX<br />
if LX ≤ Lb;<br />
otherwise,<br />
(5.8c)<br />
where L37 is the X-ray luminosity in units <strong>of</strong> 10 37 ergs s −1 . We used the maximum<br />
likelihood method to determine the best fits to the cumulative LF and Monte Carlo<br />
techniques to determine the errors (90% confidence interval). A K-S test against<br />
the cumulative distribution function <strong>of</strong> our best-fit LF indicated only a 12% chance<br />
that the single power law is a proper fit. Much better fits were achieved for a cut<strong>of</strong>f<br />
power-law (∆χ 2 = −10.6 for one less d<strong>of</strong>) with N0,c = (9.5 +22.5<br />
− 5.6)×10 −2 , αc = 1.48 +0.21<br />
−0.27,<br />
and Lc = (6.0 +3.8<br />
−2.7) × 10 38 ergs s −1 and for a broken power-law (∆χ 2 = −14.3 for two<br />
less d<strong>of</strong>) with N0,b = 2.2 +3.0<br />
−1.2, αl = 1.02 +0.30<br />
−0.55, αh = 2.91 +3.14<br />
−0.59, and Lb = (10.6 +5.8<br />
−4.4) ×<br />
10 37 ergs s −1 . Although the broken power-law is the best fit according to ∆χ 2 , we<br />
note that the one-sided K-S test indicated the cut<strong>of</strong>f power law model was acceptable<br />
(at the 50% confidence level). All three fits are overlaid in Figure 5.8.<br />
Since each <strong>of</strong> the five observations is an independent measure <strong>of</strong> the instantaneous<br />
Lb
LF, there are enough datapoints that one can apply fits <strong>of</strong> equations 5.8a–5.8c to<br />
a binned, differential LF using standard χ 2 techniques. In addition to the five-fold<br />
increase in the number <strong>of</strong> datapoints, this analysis has the advantage <strong>of</strong> including<br />
variable sources and producing a clearer goodness-<strong>of</strong>-fit test than is provided by the<br />
K-S statistic. We chose to combine the luminosities in bins <strong>of</strong> at least 25 instantaneous<br />
luminosities. Since there are five observations, each luminosity added 0.2 to the<br />
instantaneous LF. All fits were done for LX > 4 × 10 37 ergs s −1 to avoid problems<br />
due to incompleteness and less accurate measurements <strong>of</strong> LX; this resulted in 12<br />
bins being used to fit the LFs. For our best fit single, cut<strong>of</strong>f, and broken power law<br />
LFs we found χ 2 = 25.1, 14.0, and 4.9 for 10, 9, and 8 d<strong>of</strong>, which correspond to<br />
rejection probabilities <strong>of</strong> 99.5%, 88%, and 23%. We believe that one <strong>of</strong> the reasons<br />
these rejection probabilities are stronger than for the K-S statistic is that the K-S<br />
test is less sensitive at the ends <strong>of</strong> its distribution. The single power law is strongly<br />
rejected. The broken power-law is clearly the best fit, with N0,b = 3.1 ± 1.5, αl =<br />
0.83 ± 0.52, αh = 2.38 ± 0.33, and Lb = (10.8 ± 2.9) × 10 37 ergs s −1 ; however, we do<br />
not definitively rule out a cut<strong>of</strong>f power law with N0,c = 0.19 ± 0.11, αc = 1.55 ± 0.18,<br />
and Lc = (4.9 ± 1.1) × 10 38 ergs s −1 (90% confidence intervals). We also checked for<br />
effects due to errors in the background LF from Kim et al. (2004) by determining<br />
the best-fit LMXB LFs assuming 100 randomized realizations <strong>of</strong> the background LF.<br />
The single power law was rejected at the 98% confidence level for all realizations. For<br />
90% <strong>of</strong> the realizations, the cut<strong>of</strong>f power law can be rejected at better than the 85%<br />
confidence level (the lowest rejection is at the 70% confidence level). Including these<br />
effects would have little impact on our error budget.<br />
We display the completeness-corrected, instantaneous, differential luminosity func-<br />
tion <strong>of</strong> the five observations for sources detected within a < 220 ′′ in Figure 5.9. The<br />
181
Fig. 5.9.— Completeness-corrected, instantaneous, differential luminosity function<br />
from all five observations for sources detected within a < 220 ′′ . Fits were performed<br />
on the solid data-points, whose incompleteness correction is minimal. The continuous<br />
curves are the sum <strong>of</strong> the best-fit LMXB luminosity function and the expected<br />
background source counts. The broken power law is the best fit; however, a cut<strong>of</strong>f<br />
power law cannot be rejected according to the χ 2 test (at the 85% confidence level<br />
for a majority <strong>of</strong> fits with different realizations <strong>of</strong> the background LF). The reliability<br />
<strong>of</strong> both the best-fit broken power law LF and the incompleteness correction factors<br />
are strengthened by the broken power law LF going through many <strong>of</strong> the dotted<br />
data-points (above 10 37 ergs s −1 ) that were not part <strong>of</strong> the fit.<br />
182
Fig. 5.10.— Cumulative luminosity functions (LX = Lconstant) <strong>of</strong> X-ray sources in the<br />
HST-ACS FOV, excluding sources identified with non-GC optical sources. There are<br />
more bright X-ray sources in GCs; however, this difference is not highly statistically<br />
significant.<br />
best-fit single, cut<strong>of</strong>f, and broken power law LFs derived above are overlaid. The<br />
reliability <strong>of</strong> both the fitted LF and the independent completeness correction factors<br />
(above 10 37 ergs s −1 ) are strengthened by the broken power law LF going through<br />
many <strong>of</strong> the low luminosity data-points that were not included in the fitting process.<br />
In Figure 5.10 we have displayed the LFs (using Lall) <strong>of</strong> X-ray sources in the<br />
HST-ACS FOV that are in GCs (34 GC-LMXBs) and in the field (44 Field-LMXBs).<br />
After proper renormalization, the distributions track each other very well when LX <<br />
3 × 10 37 ergs s −1 . Above 6 × 10 37 ergs s −1 , there are always more GC-LMXBs than<br />
Field-LMXBs. A similar result was found by Angelini et al. (2001) in NGC 1399,<br />
183
ut was not seen clearly in other samples <strong>of</strong> early-type galaxies (Kundu et al. 2002;<br />
Sarazin et al. 2003). Neither the K-S (PKS = 0.33) nor the Wilcoxon rank-sum test<br />
σWRS = 0.8 indicate that the two LFs are drawn from a different distribution. On<br />
the other hand, we can construct 2 × 2 contingency tables, comparing the numbers<br />
<strong>of</strong> Field-LMXBs and GC-LMXBs below and above a given luminosity, and calculate<br />
Fisher’s Exact Test probabilities (PFE; Fisher 1922) that indicate aeff. We display the luminosities <strong>of</strong> Analysis Sample sources<br />
versus galactocentric semimajor axis in the top frame <strong>of</strong> Figure 5.11.<br />
184
Fig. 5.11.— Merged luminosities (LX = Lconstant) and hardness ratios as a function<br />
<strong>of</strong> the projected galactocentric semimajor distance, a, for Analysis Sample sources.<br />
No significant spatial difference in the luminosity function is observed. Correlations<br />
between hardness ratios and position (harder at greater distance) appear to be associated<br />
with sources beyond 220 ′′ , and are likely due to hard background AGNs as<br />
opposed to LMXBs in NGC 4697.<br />
185
5.8 Hardness Ratios<br />
The spectral properties <strong>of</strong> sources can be crudely characterized by hardness ratios<br />
or X-ray colors (e.g., Paper I; Paper II). We defined hardness ratios <strong>of</strong> H21 ≡ (M −<br />
S)/(M + S), H31 ≡ (H − S)/(H + S), and H32 ≡ (H − M)/(H + M), where S,<br />
M, and H are the total counts in the s<strong>of</strong>t (0.3–1 keV), medium (1–2 keV), and<br />
hard (2–6 keV) bands (Sivak<strong>of</strong>f et al. 2004). Hardness ratios without superscripts<br />
are the measured values; we use the superscript 0 to indicate the intrinsic hardness<br />
ratios, correcting for Galactic absorption and QE degradation in the Chandra ACIS<br />
detectors. The counts in each band are corrected assuming the best-fit Chandra X-ray<br />
spectrum <strong>of</strong> the inner resolved sources (a < aeff: Table 5.5, row 3). Since the different<br />
observations had different QE degradations, we adopted the following technique for<br />
correcting the observed counts in a band. Let Ni,j,k be the net counts for source<br />
i in band j during observation k, and let Cj,k be the absorption and degradation<br />
correction to counts for observation k in band j. (The QE degradation was assumed<br />
to be independent <strong>of</strong> position on the detector and thus the same for all sources within<br />
a given observation.) The combined correction for source i in band j is given by<br />
〈Ci,j〉 ≡ <br />
(Cj,kNi,j,k)/ <br />
Ni,j,k, where the sums are only performed over observations<br />
k<br />
k<br />
where Ni,j,k > 0. We require that Ni,j,k > 0 because there is no correction to the source<br />
hardness when a source is not emitting at a detectable level. Having determined the<br />
appropriate correction, the corrected number <strong>of</strong> counts for source i in band j is N 0 i,j =<br />
〈Ci,j〉 <br />
k<br />
Ni,j,k, where the sum is now over all observations. The corrected band counts<br />
are then used to calculate the corrected hardness ratios. We also combined Monte<br />
Carlo simulations <strong>of</strong> the observed counts in the source and background apertures<br />
with the count corrections to calculate the 1σ confidence intervals for the hardness<br />
ratios. (When no counts are observed, we set the expected number <strong>of</strong> counts in the<br />
186
Fig. 5.12.— X-ray color-color diagrams H 0 31 vs. H 0 21 (left) and H 0 32 vs. H 0 21 (right)<br />
for the combined counts from all observations for the Analysis Sample sources. Here,<br />
H 0 21 ≡ (M 0 −S 0 )/(M 0 +S 0 ), H 0 31 ≡ (H 0 −S 0 )/(H 0 +S 0 ), and H 0 32 ≡ (H 0 −M 0 )/(H 0 +<br />
M 0 ), where S 0 , M 0 , and H 0 are the counts in the s<strong>of</strong>t (0.3–1 keV), medium (1–2<br />
keV), and hard (2–6 keV) bands, corrected for the effect <strong>of</strong> Galactic absorption and<br />
QE degradation according to the best-fit spectra <strong>of</strong> resolved sources. The area <strong>of</strong><br />
each circle is proportional to the observed number <strong>of</strong> net counts. The solid curve and<br />
large diamonds show the hardness ratios for power-law spectral models; the diamonds<br />
indicate values <strong>of</strong> the power-law photon number index from Γ = 0 (upper right) to<br />
3.2 (lower left) in increments <strong>of</strong> 0.4. The model underwent the same correction as the<br />
sources. The 1σ error bars at the upper left illustrate the median <strong>of</strong> the uncertainties.<br />
Monte Carlo simulations to 0.653. This is the average expectation for the Poisson<br />
distribution for expected numbers <strong>of</strong> counts between 0 and 1.841, which are the 1σ<br />
confidence intervals on a measurement <strong>of</strong> zero counts.)<br />
X-ray color-color diagrams <strong>of</strong> the combined intrinsic hardness ratios <strong>of</strong> the Analysis<br />
Sample sources are shown in Figure 5.12. The values <strong>of</strong> the hardness ratios and their<br />
1σ errors are listed in columns (5)–(7) <strong>of</strong> Table 5.7. Harder sources tend to lie in the<br />
upper right <strong>of</strong> Figure 5.12a. Extra absorption tends to push objects to the right in<br />
Figure 5.12b.<br />
187<br />
The majority <strong>of</strong> sources have hardness ratios consistent with power-law indices <strong>of</strong>
1.2–2.0. On average, these sources tend to lie to the right <strong>of</strong> the power-law curve,<br />
which might indicate some extra absorption is occurring. A few sources occupy very<br />
different positions in the hardness ratio planes. Sources 81, 96, 105, 112, 123, 134,<br />
146, 148, 153, and 158 are harder than the typical source in NGC 4697. Both their<br />
spectral properties and tendency to occur farther away from the center <strong>of</strong> NGC 4697<br />
suggest that these very hard sources may be unrelated, strongly absorbed AGNs.<br />
Sources 11, 19, 25, 78, 84, 94, 110, 121, and 156 are s<strong>of</strong>ter than the typical source<br />
in NGC 4697. Sources 84 and 156 both have optical counterparts; the former is an<br />
extended object much redder than a typical GC, while the latter is a star. Sources<br />
19, 25, 78, and 110 have little if any emission above 1 keV and are all SSs. Based on<br />
its H32 color, Source 150 may be strongly absorbed or have a very atypical spectrum.<br />
As with luminosity, we used the Spearman’s ρ test to search for a correlation<br />
between merged hardness ratio and galactocentric semimajor distance, a. We display<br />
the hardness ratios <strong>of</strong> Analysis Sample sources versus spatial position in the bottom<br />
frames <strong>of</strong> Figure 5.11. If we use the entire Analysis Sample, we find 1.8σ, 2.2σ,<br />
and 1.8σ significant correlations <strong>of</strong> H 0 21, H 0 31, and H 0 32, respectively, with distance.<br />
In each case, the sense <strong>of</strong> the correlation is that harder sources are found at larger<br />
a. These correlation become insignificant (< 1σ) when only sources with a < 220 ′′<br />
are considered. The Wilcoxon rank-sum comparison <strong>of</strong> a < 220 ′′ and a > 220 ′′<br />
significantly detected sources reproduces the effects seen by the Spearman’s ρ test.<br />
However, we believe that the correlation at larger distances is due to the increasing<br />
dominance <strong>of</strong> hard background AGNs, as opposed to LMXBs intrinsic to NGC 4697.<br />
Scaling the expected number <strong>of</strong> sources unrelated to NGC 4697 with the area in<br />
each region, we expect ∼12/97 and ∼17/29 Analysis Sample sources are unrelated to<br />
NGC 4697 for a < 220 ′′ and a > 220 ′′ , respectively.<br />
188
5.9 Spectral Analysis<br />
We performed an analysis <strong>of</strong> the spectra <strong>of</strong> sources in the 0.5–10.0 keV band,<br />
extracting the spectra and response files separately for each observation <strong>of</strong> each source.<br />
The background spectra for each source were determined locally, using the same<br />
nearby regions as discussed in § 5.4. Note that the response files for each separate<br />
observation and source include the varying effects <strong>of</strong> absorption by the contaminant<br />
which produces the QE degradation in the ACIS detectors. Since the majority <strong>of</strong><br />
our sources are too faint for spectral analysis, we co-added the spectra and responses<br />
<strong>of</strong> groups <strong>of</strong> sources for each observation. We only included sources whose total<br />
count rate was determined at the 3σ level. We also excluded the sources discussed<br />
individually in § 5.9.5 and 5.10.2. All <strong>of</strong> the spectra were grouped to have at least<br />
25 counts per spectral bin prior to background correction to enable our use <strong>of</strong> χ 2<br />
statistics. The use <strong>of</strong> a minimum number <strong>of</strong> counts per spectral bin and the restricted<br />
energy range in the spectrum can result in some excluded bins, although those bins<br />
have some photons in the allowed energy range. Unless otherwise noted, the individual<br />
observations were required to have the same spectral shape, but their normalizations<br />
were allowed to vary.<br />
The spectra <strong>of</strong> Galactic LMXBs can be complex. High luminosity LMXBs, like<br />
those seen in NGC 4697, have <strong>of</strong>ten been modeled with multi-component models that<br />
may include combinations <strong>of</strong> an isothermal blackbody, a multi-color disk blackbody,<br />
a Comptonized power-law, or more complicated models (White et al. 1995). For<br />
our observations, there are two complicating factors. First, we are looking at a<br />
collection <strong>of</strong> sources, each <strong>of</strong> which is likely to have a slightly different spectrum.<br />
Second, our spectra, even when co-added, have a much lower signal-to-noise ratio<br />
than that for a Galactic LMXB. Therefore, we have only attempted to fit simple<br />
189
power-law or bremsstrahlung models to our spectra. We summarize the results <strong>of</strong><br />
the spectral fits in Table 5.5. In each row, we list how the sources were grouped<br />
together in the second column. In the third column we list the model we used to fit<br />
the spectra. In addition to the input model, we accounted for an absorption column<br />
(NH) using the Tuebingen-Boulder absorption (tbabs) model assuming abundances<br />
from Wilms et al. (2000) and photoelectric absorption cross-sections from Verner<br />
et al. (1996). The absorbing column will typically be fixed at the Galactic absorption<br />
column (2.14 × 10 20 cm 2 ; Dickey & Lockman 1990); however, some fits require non-<br />
Galactic absorption. Absorption columns below the Galactic value may indicate a<br />
problem with the chosen model at low energies, while absorption columns above<br />
the Galactic value may indicate the presence <strong>of</strong> a local absorber. The value <strong>of</strong> the<br />
absorbing column density (NH) is given in the fourth column. In the fifth column, we<br />
list either the temperature kT (for bremsstrahlung) or photon number spectral index<br />
Γ (for a power-law). The sixth through tenth column list the unabsorbed fluxes F<br />
(0.3–10 keV) <strong>of</strong> observations 0784, 4727, 4728, 4729, and 4730 respectively. The last<br />
two columns give the total number <strong>of</strong> net counts in each set <strong>of</strong> spectra and χ 2 per d<strong>of</strong><br />
for the best-fit model. All errors reported in the spectral analysis are 90% confidence<br />
level errors. Parentheses are used to indicate a frozen parameter, and square brackets<br />
are used when an error is unconstrained on one side.<br />
We emphasize that some <strong>of</strong> the groups <strong>of</strong> spectra fitted in Table 5.5 are the<br />
simultaneous fit <strong>of</strong> two (or three) other rows. The data bins fit in such a row will<br />
differ from the data bins one would fit if they first extracted the spectra <strong>of</strong> all sources in<br />
the group and then binned them. The difference is two-fold, first the bins themselves<br />
will differ because <strong>of</strong> the minimum grouping requirement. Second the number <strong>of</strong> bins<br />
excluded at the edges <strong>of</strong> the spectra will differ. Although this approach results in<br />
190
some data loss, it allows for direct comparison <strong>of</strong> the fits <strong>of</strong> the other rows that make<br />
up the group.<br />
5.9.1 Best-Fit Spectra <strong>of</strong> LMXBs<br />
To determine the best-fit spectra for all LMXBs, we considered the spectrum <strong>of</strong> all<br />
significantly detected sources within the elliptical isophote that contains half <strong>of</strong> the<br />
optical light (a < 1aeff; Table 5.5 rows 1–4). Of the four fits to this spectrum, those<br />
with bremsstrahlung models (bremss, rows 3 and 4) were significantly better than<br />
those with power-law models (power, rows 1 and 2). For one d<strong>of</strong>, the ∆χ 2 > 12.8.<br />
We note that the derived power-law photon indices, Γ = 1.47–1.66 are consistent with<br />
Γ = 1.56 ± 0.02 found by Irwin et al. (2003) for LMXBs in a sample <strong>of</strong> early-type<br />
galaxies. The better fit to a bremsstrahlung model compared to a power-law model<br />
has important implications for estimating the unabsorbed flux <strong>of</strong> a source; the flux<br />
conversion for the Galactic-absorbed bremsstrahlung model is ∼ 10% lower than that<br />
for the Galactic-absorbed power-law model. There is no evidence for a non-Galactic<br />
absorbing column in the bremsstrahlung models (∆χ 2 = 0.08 between row 3 and 4).<br />
We adopt row 3 (NH = 2.14 × 10 20 cm 2 , kT = 9.1 +1.3<br />
−1.1 keV) as our best-fit spectra.<br />
We believe that calibration changes may account for our spectra being slightly harder<br />
than that found by Irwin et al. (2003) (kT = 7.3 ± 0.3 keV). We display the observed<br />
spectra overlaid by the best-fit spectral model in Figure 5.13. Hereafter, we present<br />
results for a bremsstrahlung model with Galactic absorption in different selections <strong>of</strong><br />
sources. We also present other models (power-law or non-Galactic absorption) when<br />
they are statistically better fits.<br />
191
Fig. 5.13.— Top panel: Cumulative X-ray spectra <strong>of</strong> the resolved sources in the inner<br />
effective elliptical isophote <strong>of</strong> NGC 4697 overlayed by the solid histograms <strong>of</strong> the<br />
best-fit model spectra (Table 5.5, row 3). The different observations are shown in<br />
different colors. Bottom panel: Contribution to χ 2 with the sign indicating the sign<br />
<strong>of</strong> the residual.<br />
5.9.2 Spectra Grouped by Position<br />
In Table 5.5, rows 3, 4–6, 8 and 9, we compare bremsstrahlung models with<br />
Galactic absorption for different collections <strong>of</strong> sources grouped by position. When we<br />
compare the independent fits <strong>of</strong> sources within a < aeff (row 3) and in the annulus<br />
aeff < a < 2aeff (row 5) to the fit when their temperatures are tied together (row 8),<br />
we find a ∆χ 2 = 0.5 for 1 d<strong>of</strong>. There is no evidence for any spectral variation with<br />
galactocentric distance within 2aeff.<br />
On the other hand, there is evidence for a spectral change in sources within<br />
2aeff < a < 3aeff. First, comparing the fit to the spectra when the temperatures<br />
within 3aeff are grouped together (row 9) to the fits when the temperatures can vary<br />
(rows 3, 5, and 6) indicates a slightly significant statistical difference (∆χ 2 = 7.0<br />
192
for 2 d<strong>of</strong> and the f-test indicates the probability that the free temperature model<br />
comes from the tied temperature model is 4.0%). Furthermore, a power-law fit (row<br />
7) for 2aeff < a < 3aeff sources is a statistically better fit (∆χ 2 = 4.3 for 0 d<strong>of</strong>)<br />
than a bremsstrahlung fit (row 6). The increasing dominance <strong>of</strong> background AGN in<br />
the spectra <strong>of</strong> regions further afield from the galaxy center is a likely cause for the<br />
apparent spatial evolution <strong>of</strong> the spectra. Our flanking-field HST observations will<br />
allow us to better address this issue.<br />
5.9.3 Spectra Grouped by GC Association<br />
We compare bremsstrahlung models in Table 5.5 rows 10–18 for different collec-<br />
tions <strong>of</strong> sources grouped by their association with GCs in the HST-ACS FOV. Our<br />
comparisons <strong>of</strong> GC-LMXBs, Field-LMXBs, and their combination (rows 10, 12, and<br />
14; rows 11, 13, and 15) indicate that the GC-LMXBs and Field-LMXBs are unlikely<br />
to be fit by the same spectrum. When a Galactic absorbing column is used, the<br />
∆χ 2 = 8.6 for 1 d<strong>of</strong> and the probability both populations have the same temperature<br />
and absorption is 3.1 × 10 −3 . The disparity is even larger if we allow a non-Galactic<br />
absorbing column; ∆χ 2 = 14.0 for 2 d<strong>of</strong> and the probability they have the same<br />
temperature and absorption is 7.7 × 10 −4 .<br />
The best overall fit comes from allowing both GC-LMXBs and field-LMXBs have<br />
independent absorbing columns and temperatures (rows 11 and 13). The GC-LMXBs<br />
are better fit with a harder spectrum and larger absorbing column compared to the<br />
field-LMXBs. Although a larger absorbing column in GC-LMXBs might explain this<br />
discrepancy, we note that the absorption column <strong>of</strong> field-LMXBs tends be pushed<br />
towards sub-Galactic columns. This suggests that the bremsstrahlung model un-<br />
derpredicts the low-energy end <strong>of</strong> their spectra. A more accurate model and better<br />
193
understanding <strong>of</strong> low energy calibration issues is required to better probe the cause<br />
<strong>of</strong> the discrepancy in spectra between GC-LMXBs and field-LMXBs.<br />
In Maccarone et al. (2003), the summed spectra <strong>of</strong> LMXBs in blue-GCs are found<br />
to be harder than the summed spectra for LMXBs in red-GCs. This appears to be<br />
best explained by an additional absorbing column in blue-GCs. This is attributed to<br />
irradiation induced winds. While extra absorption due to winds might explain why<br />
our GC-LMXBs have a larger column than field-LMXBs, we note that our data is<br />
not entirely consistent with this scenario. When we compare the fits to spectra red-<br />
GC-LMXBs and blue-GC-LMXBs where they share an absorbing column and tem-<br />
perature to fits where they have independent absorbing columns and temperatures,<br />
we find the ∆χ 2 = 5.6 for 2 d<strong>of</strong> and the probability they have the same temperature<br />
and absorption is 6.1%. There differences are only marginal at best. Although the<br />
blue-GC LMXBs have a harder temperature than red-GC LMXBs, they also have a<br />
lower absorbing column that tends towards being sub-Galactic. Our understanding<br />
<strong>of</strong> the spectra <strong>of</strong> the blue-GC-LMXBs is limited by their relatively small numbers. In<br />
addition to a more accurate model and better understanding <strong>of</strong> low energy calibra-<br />
tion issues, the spectra <strong>of</strong> blue-GC-LMXBs from other galaxies must be included to<br />
improve our statistics.<br />
5.9.4 Spectra Grouped by Luminosity<br />
In our final grouped spectral fits, we examine the different spectra in two lumi-<br />
nosity bins, L38 < 2 and 2 < L38, where L38 = LX/10 38 ergs s −1 . Since the brighter<br />
sources are above the Eddington limit for a hydrogen accreting 1.4 M⊙ NS, they are<br />
likely to be either super-Eddington accreting NS-LMXBs or BH-LMXBs. Since we<br />
believe AGN may be contaminating the spectra outside <strong>of</strong> 2aeff, we restrict our sam-<br />
194
ple to LMXBs interior to that semi-major distance. We note that the brightest X-ray<br />
source in this spatial region (Source 58) has L38 ≈ 6.<br />
Comparing the fainter LMXBs, the brighter LMXBs, and their combination (rows<br />
19, 21, and 23; rows 20, 22, and 24) indicates that the fainter and brighter LMXBs are<br />
unlikely to be fit by the same spectrum. Separate spectra improve the fit by ∆χ 2 =<br />
7.7, and the probability both populations have the same temperature and Galactic<br />
absorption is 4.4 × 10 −3 . Again, the disparity is larger if the groups are allowed to<br />
have different absorbing columns; the ∆χ 2 = 14.2 for 2 d<strong>of</strong> and the probability both<br />
populations have the same temperature and absorption is 5.5 × 10 −4 . The best-fit<br />
comes from allowing faint LMXBs and bright LMXBs to have different temperatures<br />
and absorbing columns. Both populations tend to have the same temperature (∼<br />
8 keV). The fainter LMXBs tend to have smaller (mostly sub-Galactic) absorbing<br />
columns, while the brighter LMXBs tend to have a small excess (local?) absorption<br />
column (∆NH = 3.8 +2.9<br />
−2.8 × 10 20 cm 2 ). The extra rate <strong>of</strong> accretion in brighter sources<br />
might account for the extra absorption column.<br />
5.9.5 Individual Source Spectra<br />
We can also explore the individual spectra <strong>of</strong> several sources. Although we mainly<br />
consider sources with Lall > 6 × 10 38 ergs s −1 , we also discuss the spectrum <strong>of</strong> the<br />
central source (Source 1). The spectra were extracted in the identical manner as the<br />
grouped spectra above. For these fits, the errors in fluxes and luminosities are only<br />
the scaled errors in the count rates from the spectral fitting process. Since Source<br />
110 is also a variable, transient source, we discuss its spectrum below in § 5.10.2 after<br />
describing tests for variability in sources.<br />
195
Source 1: The central source in NGC 4697 could be a central AGN, a LMXB,<br />
or a collection <strong>of</strong> confused LMXBs. Although the source is not particularly bright<br />
(spectral fits made to 343.9 total net counts), we extracted its individual spectra. The<br />
source is best fit by a power-law Γ = 1.40 +0.23<br />
−0.22 with Galactic absorption (χ 2 = 11.6 for<br />
8 d<strong>of</strong>). The weighted unabsorbed luminosity at NGC 4697 for this spectral model,<br />
Lall = (4.00 ± 0.20) × 10 38 ergs s −1 , is 12% higher than the best-fit spectra for the<br />
sources within a < aeff, which is consistent with the difference between power-law<br />
and bremsstrahlung models. As this spectral fit is completely consistent with either<br />
a central AGN having a low absorbing column or an LMXB (or several LMXBs), the<br />
nature <strong>of</strong> Source 1 is still unknown.<br />
Source 117: This source is known to be an AGN at z = 0.696 (Paper II). The<br />
total net counts fit by spectra for this source was 993.3, but there was a large variance<br />
between observations. (We fit to 49.3 net counts in Observation 4729 and 280.0 in<br />
Observation 4730.) As we discuss later (§ 5.10.2), the spectral state <strong>of</strong> this source in<br />
Observation 4729 appears to differ from that in the other observations. We accounted<br />
for this by allowing Observation 4729 to have a different absorption than the other<br />
observations. The best-fit spectra (χ 2 = 30.1 for 31 d<strong>of</strong>) involved absorbed power-<br />
law (Γ = 1.55 +0.24<br />
−0.23) models. Observation 4729 had a much larger absorbing column<br />
(NH = 3.4 +1.9<br />
−1.6×10 22 cm 2 ) than the other observations (NH = 2.3 +1.1<br />
−1.0×10 21 cm 2 ). This<br />
fits implies absorbed 0.5–8.0 keV X-ray luminosities <strong>of</strong> (1.18±0.08, 1.48±0.09, 1.00±<br />
0.08, 1.12 ± 0.16, and 1.43 ± 0.09) × 10 44 ergs s −1 , respectively, for Observations 0784,<br />
and 4727-4730.<br />
Source 134: Source 134 is the brightest X-ray source in our observations and<br />
has 1973.3 net counts in its spectrum. Its hardness ratios, which vary between<br />
observations (§ 5.10.2) indicate it is harder than a typical LMXB. Its spectra is<br />
196
est-fit (χ 2 = 56.4 for 65 d<strong>of</strong>) by a power-law model (Γ = 1.79 +0.18<br />
−0.18). Each obser-<br />
vation has a different absorbing column: (1.35 +0.30<br />
−0.27, 1.59 +0.33<br />
−0.30, 0.85 +0.30<br />
−0.27, 1.10 +0.30<br />
−0.26, and<br />
1.30 +0.38<br />
−0.35) × 10 22 cm 2 , respectively, for Observations 0784, and 4727-4730. If Source<br />
134 is at the distance <strong>of</strong> NGC 4697, its unabsorbed 0.3–10.0 keV X-ray luminosities are<br />
then (4.21±0.20, 4.92±0.23, 3.25±0.17, 3.77±0.21, and 4.42±0.22)×10 39 ergs s −1 . In<br />
this case, Source 134 would be a heavily absorbed ULX. However, we believe it is more<br />
likely that this source is a background AGN with absorbed 0.5–8.0 keV X-ray fluxes <strong>of</strong><br />
(1.36±0.07, 1.54±0.07, 1.16±0.06, 1.28±0.07, and 1.44±0.07, )×10 −13 ergs cm −2 s −1 .<br />
Source 143: This source appears to have an uncatalogued DSS counterpart. Al-<br />
though the X-ray source is bright, Source 143 only has enough counts for spectral<br />
fitting in Observation 4730 (150.4 net counts). The best-fit model (χ 2 = 4.1 for 4 d<strong>of</strong>)<br />
is a Galactic-absorbed power-law (Γ = 1.92 +0.35<br />
−0.32). Its absorbed 0.5–8.0 keV X-ray flux<br />
is (2.59 ± 0.21) × 10 −14 ergs cm −2 s −1 . Its unabsorbed 0.3–10.0 keV X-ray luminosity<br />
at the distance <strong>of</strong> NGC 4697 is (5.1 ± 0.4) × 10 38 ergs s −1 for this spectral model.<br />
Source 155: Like Source 143, Source 155 appears to have an uncatalogued DSS<br />
counterpart. We fit spectra to 621.8 net X-ray counts from Observations 4727-<br />
4729. Although we tried power-law, bremsstrahlung, disk blackbody, and gas models<br />
(apec), none <strong>of</strong> these spectra gave a good fit. The Galactic-absorbed power-law<br />
(Γ = 1.26 +0.12<br />
−0.12) was the best fit we found (χ 2 = 34.5 for 21 d<strong>of</strong>). This spectral<br />
model implies absorbed 0.5–8.0 keV X-ray fluxes <strong>of</strong> (5.48 ± 0.40, 6.17 ± 0.44, 7.46 ±<br />
0.50) × 10 −14 ergs cm −2 s −1 , respectively for Observations 4727-4729. The unabsorbed<br />
0.3–10.0 keV X-ray luminosities at the distance <strong>of</strong> NGC 4697 are (1.07 ± 0.08, 1.20 ±<br />
0.09, 1.45 ± 0.10) × 10 39 ergs s −1 , respectively.<br />
Source 156: This source is clearly associated with the bright foreground star<br />
BD-05 3573, whose optical colors are roughly consistent with an early to middle G<br />
197
type star (Binney & Merrifield 1998). Its effective temperature is Teff ∼ 5300 K<br />
(Gondoin 1999). Based on its optical magnitude, the distance to the star is likely<br />
to be ∼ 7 – 700 pc, for dwarf to giant luminosity classes, respectively. In the three<br />
observations during which it is in our FOV (Observations 4727-4729), the spectrum<br />
contains 563.5 net counts. Among likely, simple stellar models <strong>of</strong> X-ray emission,<br />
we find the emission spectrum from collisionally-ionized diffuse gas (apec) model<br />
that has kT = 440 +56<br />
−47 eV and a heavy element abundance <strong>of</strong> 1.18[> 0.32] solar fits<br />
best. (The upper limit to the abundance is unconstrained. This may also affect<br />
the accuracy <strong>of</strong> the lower limit <strong>of</strong> the temperature.) The temperature, ∼ 5 × 10 6 K,<br />
is reasonable for that <strong>of</strong> an X-ray corona. While the 0.3–10.0 keV X-ray fluxes are<br />
(2.89 ± 0.17, 1.68 ± 0.15, and 1.88 ± 0.15, ) × 10 −14 ergs cm −2 s −1 , its bolometric flux<br />
from the source <strong>of</strong> the X-ray emission is ∼ 60% higher. We note that the X-ray<br />
luminosities expected at the distance <strong>of</strong> a giant G star are consistent with those <strong>of</strong><br />
other K and G giant stars with Teff ∼ 5300 K (Gondoin 1999). One type <strong>of</strong> giant stars,<br />
FK Comae stars, are rapidly rotating chromospherically active stars. Such activity<br />
might explain the X-ray flaring (§ 5.10.1) observed in this source. Follow-up optical<br />
spectroscopy is necessary to determine the spectral type and rotation speed <strong>of</strong> BD-05<br />
3573 and to test whether it is an FK Comae star.<br />
5.10 X-ray Source Variability<br />
Our observations <strong>of</strong> NGC 4697 provide for five approximately equal chances to<br />
detect variability within a given ∼ 40 ks observation, as well variability between<br />
different observations on timescales <strong>of</strong> 11 d to 4.6 yr.<br />
198
5.10.1 Intraobservation Variability<br />
After applying barycentric corrections to the times in event files, we applied three<br />
techniques to search for intraobservation variability: the Rayleigh statistic (e.g., Muno<br />
et al. 2003), the K-S test (e.g., Paper II), and a newly developed flare detection<br />
technique (Chapter 5). These three techniques consider all photons in the source<br />
apertures, and thus are likely to include some background photons.<br />
We used the Rayleigh statistic to search for periodic signals with frequencies<br />
between 5.0 × 10 −5 Hz and 1.0 × 10 −1 Hz (periods <strong>of</strong> 10–20, 000 s), testing every<br />
2.5 × 10 −5 Hz. Table 5.8 summarizes the results for > 2σ level variable sources<br />
(i.e., the chance the observed source variability is due to a statistical fluctuation is<br />
< 4.6%), listing the observation, probability detected periodicity is due to a statisti-<br />
cal fluctuation, PR, and detected period, τR. Between zero and two sources appear<br />
periodic at the > 2σ level in any given observation. Since the expected number <strong>of</strong><br />
false detected sources at this level is ∼ 7, we concentrate our discussion on the one<br />
periodic source detected at the > 3σ level (probability that the variability is due to<br />
a fluctuation is < 0.27%). The probability that the apparent periodicity among the<br />
26 counts <strong>of</strong> Source 143 in Observation 0784 is due to a statistical fluctuation is only<br />
4.6 × 10 −8 . Unfortunately, this source is located near an edge <strong>of</strong> the S3 chip, and the<br />
period <strong>of</strong> ∼ 1000 s is consistent with a periodicity induced by the yaw <strong>of</strong> the satellite<br />
aspect motion. Thus, it is likely that this periodicity is instrumental, and we have no<br />
cases <strong>of</strong> detected periodic variations for sources in NGC 4697.<br />
By comparing the cumulative fraction <strong>of</strong> events received from a source to a con-<br />
stant rate, the K-S test can identify intraobservation variability. This method has<br />
been applied to LMXB candidates in previous papers (e.g., Paper II). We summa-<br />
rize the results in Table 5.9 for sources which are variable at the > 2σ level. We list the<br />
199
Table 5.8. Possible Periodically Variable Sources<br />
Period τR<br />
Source Observation Probability Constant PR (sec)<br />
(1) (2) (3) (4)<br />
1 0784 1.1E-02 21.93<br />
101 4727 6.7E-03 14.98<br />
103 4728 4.4E-02 20.02<br />
143 0785 4.6E-08 1000.00<br />
155 4728 8.1E-03 16.99<br />
NOTE.—The value <strong>of</strong> PR indicates the probability that the<br />
observed periodicity is due to a statistical fluctuation. All periods,<br />
τR, are measured in seconds. No periodic variable sources were<br />
detected in Observations 4729 and 4730.<br />
Table 5.9. KS Test for Intraobservation Variability<br />
Source Observation PKS<br />
(1) (2) (3)<br />
2 0784 2.4E-02<br />
10 4727 4.6E-02<br />
11 0784 1.4E-02<br />
12 4728 1.2E-02<br />
40 0784 2.9E-02<br />
42 4730 3.0E-02<br />
54 4729 1.2E-02<br />
65 4727 1.6E-02<br />
71 4728 5.0E-03<br />
75 4727 2.0E-02<br />
76 4729 4.3E-02<br />
78 0784 1.5E-02<br />
79 0784 1.5E-02<br />
83 0784 2.6E-02<br />
96 0784 3.5E-02<br />
100 4729 1.6E-02<br />
115 4728 3.9E-02<br />
130 0784 2.0E-02<br />
137 0784 3.7E-02<br />
4727 2.0E-02<br />
156 4727 6.9E-07<br />
NOTE.—The value <strong>of</strong> PKS<br />
indicates the probability that the<br />
observed variability is due to a<br />
statistical fluctuation.<br />
200
Fig. 5.14.— Binned lightcurve using 1350 s bins <strong>of</strong> Source 156 (the foreground star<br />
BD-05 3573) in Observation 4727. Both the K-S test and our flare detection technique<br />
classify this source as variable within this observation. This star flared shortly after<br />
the observation began. The average count rate during the observations is indicated<br />
with the dotted line. The count rate during the flare determined by our flare detection<br />
algorithm is indicated by the red dashed line.<br />
probability the detected variability is due to a statistical fluctuation for each obser-<br />
vation, PKS. Between one and nine sources appear variable in any given observation.<br />
Again, we concentrate on the one variable source detected at the > 3σ level. Source<br />
156 is the foreground star BD-05 3573 which undergoes a clear flare (PKS = 6.9×10 −7 )<br />
soon after Observation 4727 begins. We display the binned lightcurve <strong>of</strong> this source<br />
in Figure 5.14. We note that source 137 appears as a 2σ variable source in both<br />
Observations 0784 and 4727. Following equation 3 <strong>of</strong> Chapter 5, the joint probability<br />
that this source is constant is 4.6 × 10 −3 , which is still less than 3σ significant.<br />
201
Finally, we applied a new method developed to search for flaring sources. This<br />
technique is based on the arrival times <strong>of</strong> individual events compared to the Poisson<br />
distribution at a constant rate, and was presented previously in (Chapter 5). This<br />
flare detection uses the ONTIME values (37651, 40447, 36072, 32462, and 40574 s,<br />
respectively for observations 0784 and 4727–4730) as opposed to the live exposure<br />
times. That paper gave the results for the most significantly flaring sources; note<br />
that Sources A, B, and C in (Chapter 5) correspond to Sources 71, 75, and 57 here,<br />
respectively. We summarize the results <strong>of</strong> these tests in Table 5.10 for sources which<br />
are variable at the > 2σ level in at least one observation. For each observation <strong>of</strong> a<br />
flare-candidate source, we list the observation number, the total number <strong>of</strong> photons<br />
in the observation, N, the number <strong>of</strong> photons in the flare, n, the duration <strong>of</strong> the flare,<br />
δt, and the Modified Julian Date (MJD) <strong>of</strong> the arrival time <strong>of</strong> the first photon in the<br />
flare, t0. The value <strong>of</strong> Pconstant indicates the mathematical probability <strong>of</strong> the given<br />
flare occurring due to a statistical fluctuation in a constant rate source; however, we<br />
must take account for the number <strong>of</strong> non-independent flare searches undertaken. After<br />
applying corrections to Pconstant based on the number <strong>of</strong> photons in the observation,<br />
P ′ constant is the probability a flare in a given observation is not real. The number <strong>of</strong><br />
sources with a statistically significant flare ranges from one to seven in the different<br />
observations.<br />
Given the number <strong>of</strong> sources expected to show a flare from a statistical fluctuation,<br />
we only consider the flaring sources in individual observations detected at the > 3σ<br />
level, which are Sources 57, 155, and 156. These sources have flares ranging from a few<br />
photons over tens <strong>of</strong> seconds to nearly a hundred photons over thousands <strong>of</strong> seconds.<br />
Source 57 was discussed earlier in Chapter 5 as Source C; note that the luminosity<br />
conversion used in this chapter is about 10% smaller than in Chapter 5. We display an<br />
202
Table 5.10. Possible Flaring Sources in NGC 4697<br />
Source Observation N n ∆t t0 Pconstant P ′ constant Pconstant,joint<br />
(s) (MJD)<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
25 4730 21 9 2952 53235.81643 2.5E-03 6.5E-03 3.2E-02<br />
42 4728 26 3 25 53010.59465 3.9E-03 1.0E-02 5.2E-02<br />
56 4727 10 5 1919 52999.89337 8.7E-03 2.1E-02 1.1E-01<br />
57 0784 20 4 68 51558.95770 1.3E-04 3.4E-04 · · ·<br />
4727 20 3 50 53000.06223 5.5E-03 1.4E-02 · · ·<br />
0784, 4727 · · · · · · · · · · · · · · · · · · 4.8E-05<br />
71 0784 14 5 1047 51558.79423 7.0E-03 1.8E-02 · · ·<br />
4727 16 4 628 52999.75882 2.7E-02 7.0E-02 · · ·<br />
4728 14 4 509 53010.70295 1.2E-02 3.1E-02 · · ·<br />
0784, 4727, 4728 · · · · · · · · · · · · · · · · · · 3.9E-04<br />
75 4727 10 5 1329 53000.04326 2.2E-03 5.5E-03 · · ·<br />
4728 9 4 1420 53010.72444 3.4E-02 8.0E-02 · · ·<br />
4729 6 5 5654 53047.59915 4.3E-02 9.0E-02 · · ·<br />
4727, 4728 · · · · · · · · · · · · · · · · · · 4.4E-03<br />
4727–4729 · · · · · · · · · · · · · · · · · · 4.0E-04<br />
78 0784 44 4 52 51558.84209 1.5E-03 4.1E-03 2.0E-02<br />
83 0784 10 8 6910 51558.83658 8.5E-03 2.1E-02 1.1E-01<br />
90 4727 13 3 116 52999.82502 7.5E-03 1.9E-02 9.5E-02<br />
107 0784 2 2 480 51559.09218 2.5E-02 5.2E-02 · · ·<br />
4728 4 2 63 53010.69939 2.1E-02 4.2E-02 · · ·<br />
0784, 4728 · · · · · · · · · · · · · · · · · · 2.2E-02<br />
115 4728 22 8 1857 53010.37696 2.7E-03 6.9E-03 3.5E-02<br />
118 4728 35 11 2667 53010.42386 9.0E-03 2.5E-02 1.2E-02<br />
124 4728 20 4 270 53010.38518 8.5E-03 2.2E-02 1.1E-01<br />
135 0784 4 2 78 51558.70911 2.4E-02 5.0E-02 · · ·<br />
4730 6 2 57 53235.77593 4.1E-02 8.5E-02 · · ·<br />
0784, 4730 · · · · · · · · · · · · · · · · · · 4.3E-02<br />
137 4727 27 12 5529 53000.01065 2.4E-02 6.5E-02 · · ·<br />
4729 18 6 1034 53047.40640 4.2E-03 1.1E-02 · · ·<br />
4727, 4729 · · · · · · · · · · · · · · · · · · 6.9E-03<br />
146 0784 13 4 697 51559.01802 1.9E-02 4.9E-02 · · ·<br />
4727 4 2 22 52999.76129 6.5E-03 1.3E-02 · · ·<br />
0784, 4727 · · · · · · · · · · · · · · · · · · 6.6E-03<br />
155 4728 219 17 584 53010.48733 2.2E-04 7.5E-04 3.7E-03<br />
156 4727 289 99 7423 52999.64230 4.0E-06 1.3E-05 6.7E-05<br />
NOTE.—This table follows the nomenclature <strong>of</strong> Chapter 5: N is the total number <strong>of</strong> photons during an<br />
observation. A flare candidate with n photons <strong>of</strong> observed duration δt begins at t0, where we list the time<br />
measured prior to barycentric corrections. The value <strong>of</strong> Pconstant indicates the mathematical probability <strong>of</strong><br />
the given flare occurring due to a statistical fluctuation; P ′ constant is the same probability after accounting<br />
for the number <strong>of</strong> non-independent flare searches the technique examines. If the same type <strong>of</strong> flare occurs in<br />
multiple observations, one can calculate the joint probability the flare is not real, Pconstant,joint.<br />
203
Fig. 5.15.— Impulse diagram indicating the time <strong>of</strong> arrival <strong>of</strong> photons in Source 57<br />
(Observation 0784). This LMXB candidate undergoes short, bright flares in multiple<br />
observations (Chapter 5), which were detected only with our new flare detection<br />
technique.<br />
impulse diagram <strong>of</strong> the photon arrival times for Observation 0784 <strong>of</strong> Source 57 in<br />
Figure 5.15. The observed count rate <strong>of</strong> the flare is over 100 times the average count<br />
rate. Source 57 has no optical counterpart in the HST-ACS image, suggesting it is<br />
most likely a flaring field-LMXB.<br />
A flare <strong>of</strong> several hundred seconds with 17 counts is detected in Source 155, but<br />
was missed by the K-S test. The observed count rate <strong>of</strong> the flare is about five times<br />
the average. As shown in Figure 5.16, the flare is marked by a clearly increased rate<br />
(larger slope in the cumulative light curve) that straddles the cumulative light curve<br />
for a constant rate source. Since the K-S test looks for the largest deviation from a<br />
204
Fig. 5.16.— Cumulative lightcurve <strong>of</strong> Source 155 (Observation 4727) overlaid by<br />
the expected distribution for a constant source (dotted line). Our flare detection<br />
technique classifies this source as variable within this observation; however, the K-S<br />
test misses this source. The flare interval, which lies between the dashed lines, has a<br />
clearly increased rate (larger slope).<br />
constant rate, it is not surprising that the K-S test fails to detect this type <strong>of</strong> flare.<br />
Follow-up <strong>of</strong> the optical counterpart to Source 155 is necessary to determine if this<br />
source is an flaring LMXB in a GC or a source unrelated to NGC 4697. As discussed<br />
earlier, Source 156 is the foreground star BD-05 3573 that undergoes a clear flare<br />
with 99 counts. In Figure 5.14, we overlay the flare count rate determined by the<br />
flare detection algorithm for Source 156, which is about twice the average rate.<br />
If we consider searching for flares over multiple observations, one can calculate<br />
the joint probability the flares are real, Pconstant,joint. Thirteen sources in the Analysis<br />
205
Sample have a Pconstant,joint that indicate a > 2σ detection <strong>of</strong> flaring across multiple<br />
observations; however, the detected flares in two <strong>of</strong> those sources (137 and 146) have<br />
disparate enough durations that their separate flare detections probably should not<br />
be combined. Only 4 sources (57, 71, 75, and 156) have flaring which is significant<br />
at the > 3σ level across multiple observations; these are the sources discussed in<br />
(Chapter 5), plus the foreground star BD-05 3573. After correcting for the number <strong>of</strong><br />
sources expected from statistical fluctuations, we find that 4.2 +3.3<br />
−2.5% <strong>of</strong> the Analysis<br />
Sample sources exhibit flaring which is detectable at the > 2σ level with our new<br />
algorithm.<br />
5.10.2 Interobservation Variability<br />
Our observations <strong>of</strong> NGC 4697 are among the first designed to measure interob-<br />
servation variability with strong coverage over a wide time baseline; some variability<br />
results have been presented before using fewer observations (e.g., Centaurus A: Kraft<br />
et al. 2001 and NGC 4636: Posson-Brown et al. 2006) by others. We searched for<br />
luminosity variability between any two observations, as well as luminosity or spectral<br />
variability over the entire set <strong>of</strong> observations.<br />
Luminosity Variability Between Two Observations<br />
We first searched for variability between pairs <strong>of</strong> observations by comparing the<br />
value <strong>of</strong> χ 2 assuming the fluxes were different with the value assuming they are con-<br />
stant. Sources were considered possibly variable if χ 2 > 4, i.e., a 2σ detection <strong>of</strong><br />
variability. This method differs slightly from Posson-Brown et al. (2006), which com-<br />
pares the individual luminosities to each other. The probability that the variability is<br />
due to a statistical fluctuation is listed in columns (2)–(11) <strong>of</strong> Table 5.11 for the ten<br />
206
pairs <strong>of</strong> observations. In Figure 5.17, we display the percentage <strong>of</strong> variable sources<br />
as a function <strong>of</strong> the timescale between two observations for all <strong>of</strong> the Analysis Sam-<br />
ple sources that are in the FOV for both observations in each pair. We also display<br />
the percentage <strong>of</strong> variable sources expected due to statistical fluctuations at the 2σ<br />
level. There is a slight tendency for a higher percentage <strong>of</strong> variable sources at longer<br />
timescales; however, this is not statistically significant, based on a χ 2 test. (There are<br />
two caveats with this: the error bars in Figure 5.17 are not independent, and there<br />
may be a slight excess variability on the four longest timescales due to the improper<br />
correction <strong>of</strong> QE degradation for SSs. This latter effect is well within the displayed<br />
errors.) If we treat the error bars as independent, we find that 11.3 ± 1.0% <strong>of</strong> the<br />
Analysis Sample sources are variable on average. (If we only consider sources variable<br />
at the 3σ level, the fraction <strong>of</strong> variable sources is 6.0 ± 0.7%.) Given the expected<br />
number <strong>of</strong> falsely identified variable sources, 6.7±1.0% <strong>of</strong> the Analysis Sample sources<br />
are intrinsically variable between any pair <strong>of</strong> observations. This number is roughly<br />
consistent with that found for Centaurus A (9.8 +4.5<br />
−3.3%) for a variability timescale<br />
<strong>of</strong> 164 d (Kraft et al. 2001); although they derive a much higher percentage when<br />
they include a generous definition <strong>of</strong> transient candidates (14.2 +2.6<br />
−2.3%). Our derived<br />
variability percentage is lower than that found for a 1115 d timescale in NGC 4636<br />
(23.8 +3.3<br />
−3.0%; Posson-Brown et al. 2006); however, it is consistent with the variability<br />
for a day timescale (4.6 +3.5<br />
−2.2%).<br />
Long-Term Luminosity Variability<br />
207<br />
We can apply a similar χ 2 technique to search for sources that show any luminosity
Table 5.11. Sources Which Vary between Pairs <strong>of</strong> Observations<br />
Source PL,AB PL,AC PL,AD PL,AE PL,BC PL,BD PL,BE PL,CD PL,CE PL,DE PL,All PH21,All PH31,All PH32,All<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13) (14) (15)<br />
6 · · · · · · · · · · · · · · · · · · 1.7E-02 · · · 1.4E-02 · · · · · · · · · · · · · · ·<br />
7 · · · 3.0E-02 · · · · · · 2.1E-02 · · · · · · 4.1E-02 · · · · · · · · · · · · · · · · · ·<br />
8 · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · ·<br />
9 3.4E-02 · · · · · · · · · · · · · · · 1.6E-02 · · · 3.5E-02 · · · · · · · · · · · · · · ·<br />
10 · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · 5.1E-04 2.4E-02<br />
11a · · · · · · · · · 3.0E-03 · · · · · · 7.9E-04 · · · 2.1E-03 8.5E-04 2.4E-04 3.0E-02 · · · · · ·<br />
15 · · · · · · 1.8E-02 · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · ·<br />
19b · · · 8.9E-03 · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · ·<br />
23 · · · · · · · · · 1.5E-03 · · · · · · 2.7E-04 · · · 4.7E-04 9.4E-03 2.5E-02 · · · · · · · · ·<br />
25b 3.1E-07 7.9E-08 1.9E-03 5.1E-03 · · · · · · · · · · · · · · · · · · 7.8E-06 · · · · · · · · ·<br />
26 · · · · · · · · · · · · 6.3E-03 · · · 2.5E-02 · · · · · · · · · · · · · · · · · · · · ·<br />
28 · · · 2.1E-02 · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · ·<br />
31 · · · · · · 2.9E-02 · · · · · · · · · · · · · · · · · · 3.7E-02 · · · · · · · · · · · ·<br />
34 · · · · · · · · · · · · · · · · · · · · · 4.0E-02 · · · · · · · · · · · · · · · · · ·<br />
37a · · · · · · · · · 6.8E-11 · · · · · · 6.1E-07 · · · 1.9E-06 7.6E-04 2.8E-05 · · · · · · · · ·<br />
39 1.3E-05 3.7E-06 2.5E-04 1.7E-04 · · · · · · · · · · · · · · · · · · 6.8E-05 · · · · · · · · ·<br />
41a 2.6E-03 2.8E-02 · · · · · · · · · · · · · · · · · · · · · · · · 2.7E-02 · · · · · · · · ·<br />
45 1.4E-05 3.4E-05 1.1E-04 3.3E-08 · · · · · · · · · · · · · · · · · · 3.0E-04 · · · · · · · · ·<br />
48 · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · 6.5E-04 · · ·<br />
51a · · · · · · · · · 1.1E-02 · · · 2.0E-02 2.5E-04 1.0E-03 4.7E-07 · · · 9.2E-06 · · · · · · · · ·<br />
52 · · · · · · · · · · · · · · · 2.3E-02 · · · 2.0E-02 · · · · · · · · · · · · · · · · · ·<br />
53 · · · · · · · · · · · · 8.7E-03 · · · · · · · · · · · · · · · · · · · · · · · · · · ·<br />
58 · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · 1.5E-02 · · ·<br />
59 · · · · · · · · · · · · · · · · · · · · · · · · · · · 2.9E-02 · · · · · · · · · · · ·<br />
60 · · · · · · · · · 1.2E-02 · · · · · · · · · · · · · · · 2.3E-02 · · · · · · · · · · · ·<br />
63 8.8E-03 · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · 2.9E-02 · · · · · ·<br />
66 · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · 1.5E-02 2.5E-03<br />
67a 3.9E-06
Table 5.11—Continued<br />
Source PL,AB PL,AC PL,AD PL,AE PL,BC PL,BD PL,BE PL,CD PL,CE PL,DE PL,All PH21,All PH31,All PH32,All<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13) (14) (15)<br />
69 · · · · · · · · · · · · 3.1E-02 · · · · · · · · · · · · · · · · · · · · · · · · · · ·<br />
75 · · · · · · · · · · · · · · · · · · 1.0E-02 · · · 1.2E-02 2.9E-03 · · · · · · · · · · · ·<br />
77a · · · 7.0E-10 2.4E-04 3.6E-13 6.8E-05 2.5E-02 3.3E-06 · · · · · · · · · 4.3E-15 · · · · · · · · ·<br />
78b 1.3E-05 5.9E-07 2.1E-05 8.5E-05 · · · · · · · · · · · · · · · · · · 1.1E-04 · · · · · · · · ·<br />
79 · · · · · · · · · · · · · · · · · · 2.8E-04 · · · · · · · · · 3.4E-02 · · · · · · · · ·<br />
81 · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · 3.5E-02<br />
94a · · · · · · · · · 1.6E-03 · · · · · · 1.9E-04 1.6E-02 7.6E-06 · · · 6.9E-04 · · · · · · · · ·<br />
97 · · · 2.5E-02 · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · ·<br />
98 7.1E-04 · · · 3.6E-02 · · · · · · · · · 2.5E-03 · · · · · · · · · 3.8E-03 · · · · · · · · ·<br />
99 · · · · · · · · · · · · 1.4E-02 · · · · · · · · · · · · · · · · · · · · · · · · · · ·<br />
100 · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · ·<br />
101 · · · · · · 4.3E-02 · · · · · · 4.5E-03 · · · 1.9E-02 · · · 5.8E-03 · · · · · · · · · · · ·<br />
102 · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · 4.1E-02 2.4E-02<br />
103 · · · · · · · · · · · · · · · · · · · · · · · · 2.9E-02 1.8E-02 · · · 2.7E-04 · · · · · ·<br />
104 · · · · · · · · · 8.1E-04 · · · · · · 2.4E-03 · · · 2.7E-03 6.2E-04 2.9E-02 · · · · · · · · ·<br />
106 · · · · · · 3.6E-02 · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · ·<br />
108 · · · · · · · · · 1.4E-02 · · · · · · · · · · · · · · · · · · · · · · · · · · · · · ·<br />
110a · · · · · · · · ·
Table 5.11—Continued<br />
Source PL,AB PL,AC PL,AD PL,AE PL,BC PL,BD PL,BE PL,CD PL,CE PL,DE PL,All PH21,All PH31,All PH32,All<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13) (14) (15)<br />
134 6.0E-04 · · · 3.0E-02 · · · · · · · · · 1.1E-02 · · · · · · · · · 8.9E-03 9.9E-03 1.0E-03 2.0E-02<br />
140 · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · 3.5E-02 · · · · · ·<br />
142 · · · · · · 3.8E-02 · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · ·<br />
144 · · · · · · · · · · · · 4.0E-02 · · · 9.6E-03 · · · · · · 1.9E-02 4.2E-02 · · · · · · · · ·<br />
147 · · · · · · · · · · · · · · · 1.3E-04 · · · 7.8E-03 · · · · · · 4.8E-03 · · · · · · · · ·<br />
151 · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · 1.4E-02<br />
152 · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · 3.9E-03 · · · · · ·<br />
155 · · · · · · · · · · · · · · · 2.2E-03 · · · 1.9E-02 · · · · · · 7.7E-03 · · · · · · · · ·<br />
156 · · · · · · · · · · · · 1.1E-07 9.0E-04 · · · · · · · · · · · · 8.5E-07 4.2E-02 · · · · · ·<br />
NOTE.—Observations 0784, 4727, 4728, 4729, 4730 are indicated by A, B, C, D, and E, respectively. The subscripts to the probability,<br />
P , indicate the parameter (luminosity L or hardness ratio) and the observations a source is variable over, while the value <strong>of</strong> P indicates the<br />
probability that the observed variability is due to a statistical fluctuation.<br />
a Source is a transient candidate.<br />
b Variations in the QE degradation may be misinterpreted as variability when comparing Observation 0784 to Cycle 5 observations for this<br />
supers<strong>of</strong>t source.<br />
210
Fig. 5.17.— Percentage <strong>of</strong> Analysis Sample sources that appear variable (at the<br />
> 2σ level) between two observations against the time period between the observations.<br />
Note that the error bars are not independent as the pairs contain the same<br />
five observations. The dotted horizontal line represents the percentage <strong>of</strong> sources<br />
that would appear variable just due to statistical fluctuations. Although there is a<br />
rough tendency for more variable sources on longer timescales, a constant variability<br />
percentage <strong>of</strong> 11.3% is statistically consistent with the data. Although very s<strong>of</strong>t<br />
sources may be misidentified as variable sources at the four longest timescales due to<br />
improper correction <strong>of</strong> QE degradation, this effect is well within the displayed errors.<br />
variability over the entire period <strong>of</strong> five observations. We refer to these sources as<br />
Long-Term Luminosity Variables (LTLVs), and the probability PL,All that the vari-<br />
ability arises from statistical fluctuations is given in column 12 <strong>of</strong> Table 5.11. The χ 2 ,<br />
when compared to a single merged luminosity and combined with the appropriate de-<br />
grees <strong>of</strong> freedom (one less than the number <strong>of</strong> observations a source is in the FOV), is<br />
211
used to calculate the probability an observed LTLV is due to a statistical fluctuation.<br />
Sources 148, 154, and 157 are excluded from these calculations as they are only in<br />
the FOV <strong>of</strong> one observation. From the Analysis Sample, 26/124 sources (21.0 +4.3<br />
−3.8%)<br />
are LTLVs at the 2σ significance level, while 11.3 +3.6<br />
−2.9% <strong>of</strong> Analysis Sample sources<br />
are LTLVs at the > 3σ significance level. Statistically correcting for falsely identified<br />
LTLVs, we find 16.4 +4.3<br />
−3.8% <strong>of</strong> the significantly detected sources show LTLV behavior.<br />
Three <strong>of</strong> these sources are not associated with NGC 4697: Source 45 has an optical<br />
ID that is not a GC and thus is probably due to a background AGN, Source 117 is<br />
a known background AGN, and Source 156 is a known foreground star. Two sources<br />
(25 and 155) are associated with optical counterparts that may or may not be GCs<br />
in NGC 4697. Sources 39, 41, 51, 77, and 79 are GC-LMXBs that exhibit LTLV<br />
behavior. (Sources 98 and 114 are associated with Kavelaars GC candidates; new<br />
HST-ACS data will be used to test whether these sources are really GC-LMXBs.)<br />
After correcting for the likely percentage <strong>of</strong> falsely identified LTLVs, 10.1 +8.7<br />
−6.2% <strong>of</strong><br />
GC-LMXBs and < 8.5% <strong>of</strong> Field-LMXBs exhibit LTLV behavior.<br />
Since some Galactic LMXBs are known to undergo transitions between distinct<br />
luminosity states, we developed a method that groups observations together into pos-<br />
sible luminosity states. For every LTLV, we first considered all possible combinations<br />
<strong>of</strong> observation groupings that divide into two separate states. That is, we assumed<br />
that the luminosity had two distinct values, and that one or the other <strong>of</strong> the two<br />
values applied to each observation <strong>of</strong> that source. The two luminosity values were<br />
allowed to vary, and each observation was assigned to one <strong>of</strong> the two luminosity states<br />
so as to minimize χ 2 . Some sources still had a much larger χ 2 than the number <strong>of</strong><br />
d<strong>of</strong>s. Given the new χ 2 , we could calculate the probability that any deviations from<br />
our two-state hypothesis were due to statistical fluctuations, given the new number <strong>of</strong><br />
212
d<strong>of</strong>s and the number <strong>of</strong> combinations <strong>of</strong> states. If this probability was low (< 4.6%),<br />
then we tried to divide the observations into three luminosity states. No source re-<br />
quired more than three states to be fit acceptably. We list the states in Table 5.12.<br />
For each state, we list the observations included in a state (column 2), and the com-<br />
bined luminosity and hardness ratios <strong>of</strong> the state (columns 3–6). Unless otherwise<br />
noted, we placed no requirement on the temporal pattern <strong>of</strong> the states; LTLVs whose<br />
states are interspersed temporally may be switching between those states or the in-<br />
trinsic variability may be poorly characterized by a simple transition between states.<br />
There are several categories <strong>of</strong> luminosity state transitions that indicate potentially<br />
interesting transitions and a few sources that bear individual scrutiny.<br />
Sources 25, 78, and 110 are SSs that exhibit LTLV. As such, they are more affected<br />
by QE degradation than the typical source. Among these sources, the first two<br />
have a luminosity that drops precipitously in the last four observations compared<br />
to the first observation. Since the last four observations all have a similar amount<br />
<strong>of</strong> QE degradation, we reran the LTLV detection method only considering the last<br />
four observations; neither <strong>of</strong> the sources remained LTLVs. Therefore, we do not<br />
consider Sources 25 and 78 as LTLVs. Since Source 110 does not turn on until the<br />
last observation, the QE degradation does not complicate its identification as a LTLV.<br />
Sources 68 and 117 were the only sources broken into three luminosity states. The<br />
individual luminosities <strong>of</strong> Source 68 are qualitatively described by an increase over<br />
the first three observations, followed by the source turning <strong>of</strong>f, and perhaps beginning<br />
to turn on again in the last observation. Its two-state mode is consistent with this<br />
qualitative picture, containing a higher-luminosity state <strong>of</strong> the first three observations<br />
and a state where the source is not significantly detected in the last two observations;<br />
however, the probability the two-state description is correct is 6.1 × 10 −3 . In its best<br />
213
Table 5.12. States <strong>of</strong> Variable X-ray Sources<br />
Source Obs.State LState H21 0 State H31 0 State H32 0 State<br />
(1) (2) (3) (4) (5) (6)<br />
States Determined by Luminosity Selection<br />
11 ABCD 11.7 ± 1.2 −0.32 +0.09<br />
−0.08<br />
E 3.2 ± 1.5 −0.91 +0.15<br />
−0.09<br />
23 ABCD −0.2 ± 0.3 +0.00 +1.00<br />
−1.00<br />
E 4.9 ± 1.8 −1.00 +0.09<br />
−0.00<br />
25 A 16.9 ± 2.8 −0.94 +0.04<br />
−0.05<br />
BCDE 4.9 ± 0.8 −0.95 +0.03<br />
−0.04<br />
37 ABCD 0.3 ± 0.4 −0.56 +1.54<br />
−0.44<br />
E 8.6 ± 2.3 −0.12 +0.24<br />
−0.21<br />
39 A 38.9 ± 4.0 +0.10 +0.11<br />
−0.11<br />
BCDE 19.0 ± 1.5 −0.01 +0.09<br />
−0.09<br />
41 A 0.2 ± 0.8 +1.00 +0.00<br />
−2.00<br />
BCDE 3.4 ± 0.7 −0.25 +0.23<br />
−0.22<br />
45 A 7.4 ± 2.0 −0.29 +0.21<br />
−0.22<br />
BCDE 0.1 ± 0.3 +1.00 +0.00<br />
−0.52<br />
51 ABC 5.3 ± 1.0 −0.33 +0.17<br />
−0.15<br />
DE 0.1 ± 0.6 +0.98 +0.02<br />
−1.98<br />
67 A −0.3 ± 0.7 +0.00 +1.00<br />
−1.00<br />
BCDE 8.2 ± 1.0 +0.05 +0.16<br />
−0.14<br />
68 AE 7.8 ± 1.5 −0.24 +0.18<br />
−0.18<br />
BC 18.3 ± 2.1 −0.35 +0.11<br />
−0.11<br />
D −0.1 ± 0.9 +1.00 +0.00<br />
−2.00<br />
77 AB 0.1 ± 0.5 +0.96 +0.04<br />
−1.96<br />
CDE 8.3 ± 1.3 −0.28 +0.14<br />
−0.13<br />
78 A 14.9 ± 2.6 −1.00 +0.04<br />
−0.00<br />
BCDE 3.3 ± 0.7 −1.00 +0.03<br />
−0.00<br />
79 ACDE 1.4 ± 0.5 −0.39 +0.33<br />
−0.26<br />
B 5.5 ± 1.9 +0.19 +0.42<br />
−0.37<br />
94 ABC 0.3 ± 0.4 −0.84 +0.59<br />
−0.16<br />
DE 5.3 ± 1.3 −0.59 +0.16<br />
−0.14<br />
98 AE 17.1 ± 1.9 −0.37 +0.10<br />
−0.09<br />
BCD 8.7 ± 1.3 −0.12 +0.14<br />
−0.14<br />
104 ABCD −0.2 ± 0.3 +1.00 +0.00<br />
−1.00<br />
E 5.2 ± 1.9 −0.44 +0.30<br />
−0.28<br />
110 ABCD −0.1 ± 0.4 −1.00 +1.00<br />
−0.00<br />
E 32.5 ± 4.0 −0.99 +0.01<br />
−0.01<br />
114 ABD 26.9 ± 2.0 −0.23 +0.08<br />
−0.07<br />
CE 17.5 ± 2.1 −0.19 +0.12<br />
−0.11<br />
117 AC 89.8 ± 4.3 −0.06 +0.05<br />
−0.05<br />
BE 122.6 ± 5.0 −0.09 +0.05<br />
−0.05<br />
D 40.0 ± 4.8 −0.01 +0.18<br />
−0.17<br />
121 A 6.5 ± 1.8 −0.55 +0.18<br />
−0.20<br />
BCDE 0.0 ± 0.4 +1.00 +0.00<br />
−0.33<br />
122 A 11.2 ± 2.4 −0.43 +0.16<br />
−0.16<br />
BCDE 5.0 ± 1.0 −0.21 +0.19<br />
−0.17<br />
Continued on Next Page. . .<br />
−0.94+0.03<br />
−0.03<br />
−1.00+0.16<br />
−0.00<br />
+1.00+0.00<br />
−1.59<br />
−1.00+0.08<br />
−0.00<br />
−1.00+0.04<br />
−0.00<br />
−1.00+0.02<br />
−0.00<br />
−0.46+1.44<br />
−0.54<br />
−0.74+0.18<br />
−0.17<br />
−0.15+0.12<br />
−0.12<br />
−0.26+0.09<br />
−0.09<br />
−1.00+2.00<br />
−0.00<br />
−0.11+0.24<br />
−0.20<br />
−0.80+0.17<br />
−0.17<br />
+0.00+1.00<br />
−1.00<br />
−0.76+0.11<br />
−0.12<br />
−1.00+2.00<br />
−0.00<br />
+1.00+0.00<br />
−2.00<br />
−0.17+0.16<br />
−0.15<br />
−0.36+0.18<br />
−0.17<br />
−0.42+0.11<br />
−0.10<br />
+1.00+0.00<br />
−2.00<br />
−1.00+2.00<br />
−0.00<br />
−0.78+0.09<br />
−0.09<br />
−1.00+0.04<br />
−0.00<br />
−1.00+0.04<br />
−0.00<br />
−0.71+0.28<br />
−0.26<br />
−0.04+0.50<br />
−0.39<br />
−1.00+0.51<br />
−0.00<br />
−0.92+0.08<br />
−0.08<br />
−0.67+0.09<br />
−0.08<br />
−0.57+0.13<br />
−0.12<br />
+1.00+0.00<br />
−1.00<br />
−0.46+0.32<br />
−0.26<br />
−1.00+1.00<br />
−0.00<br />
−0.99+0.01<br />
−0.01<br />
−0.58+0.07<br />
−0.07<br />
−0.64+0.10<br />
−0.09<br />
−0.41+0.05<br />
−0.05<br />
−0.34+0.05<br />
−0.05<br />
+0.27+0.15<br />
−0.14<br />
−0.89+0.09<br />
−0.11<br />
+0.00+1.00<br />
−1.00<br />
−0.91+0.10<br />
−0.09<br />
−0.55+0.18<br />
−0.16<br />
−0.88+0.06<br />
−0.06<br />
−1.00+2.00<br />
−0.00<br />
+1.00+0.00<br />
−2.00<br />
−1.00+2.00<br />
−0.00<br />
−1.00+1.00<br />
−0.00<br />
−1.00+1.00<br />
−0.00<br />
+0.14+0.86<br />
−1.14<br />
−0.68+0.20<br />
−0.21<br />
−0.25+0.10<br />
−0.11<br />
−0.25+0.08<br />
−0.08<br />
−1.00+2.00<br />
−0.00<br />
+0.14+0.22<br />
−0.19<br />
−0.67+0.28<br />
−0.29<br />
−1.00+0.67<br />
−0.00<br />
−0.57+0.17<br />
−0.19<br />
−1.00+2.00<br />
−0.00<br />
+1.00+0.00<br />
−2.00<br />
−0.21+0.12<br />
−0.13<br />
−0.13+0.20<br />
−0.20<br />
−0.08+0.13<br />
−0.13<br />
+0.00+1.00<br />
−1.00<br />
−1.00+2.00<br />
−0.00<br />
−0.64+0.14<br />
−0.13<br />
+0.00+1.00<br />
−1.00<br />
+1.00+0.00<br />
−2.00<br />
−0.44+0.44<br />
−0.48<br />
−0.22+0.31<br />
−0.31<br />
−1.00+2.00<br />
−0.00<br />
−0.73+0.27<br />
−0.27<br />
−0.40+0.14<br />
−0.14<br />
−0.49+0.14<br />
−0.13<br />
+0.95+0.05<br />
−1.95<br />
−0.02+0.43<br />
−0.38<br />
+0.00+1.00<br />
−1.00<br />
−0.26+1.26<br />
−0.74<br />
−0.41+0.08<br />
−0.08<br />
−0.52+0.11<br />
−0.11<br />
−0.36+0.05<br />
−0.05<br />
−0.26+0.04<br />
−0.05<br />
+0.28+0.13<br />
−0.11<br />
−0.68+0.30<br />
−0.32<br />
−1.00+0.32<br />
−0.00<br />
−0.78+0.23<br />
−0.22<br />
−0.39+0.20<br />
−0.20<br />
214
Table 5.12—Continued<br />
Source Obs.State LState H21 0 State H31 0 State H32 0 State<br />
(1) (2) (3) (4) (5) (6)<br />
130 ABD 23.3 ± 1.9 −0.18 +0.08<br />
−0.08<br />
CE 13.2 ± 1.9 −0.40 +0.12<br />
−0.11<br />
131 ABCD 4.0 ± 0.8 +0.10 +0.24<br />
−0.21<br />
E 11.3 ± 2.6 +0.14 +0.28<br />
−0.24<br />
134 ACE 161.9 ± 4.7 +0.67 +0.03<br />
−0.03<br />
BD 188.8 ± 6.8 +0.54 +0.05<br />
−0.05<br />
144 ABD 2.9 ± 0.9 −0.03 +0.35<br />
−0.30<br />
CE 8.4 ± 1.6 +0.06 +0.23<br />
−0.22<br />
147 BCE 4.1 ± 1.0 +0.07 +0.28<br />
−0.23<br />
D 13.7 ± 3.2 −0.24 +0.22<br />
−0.18<br />
155 BC 92.3 ± 4.8 −0.04 +0.06<br />
−0.06<br />
D 121.6 ± 8.4 −0.00 +0.08<br />
−0.08<br />
156 B 117.1 ± 7.5 −0.74 +0.03<br />
−0.03<br />
CD 74.5 ± 4.6 −0.84 +0.03<br />
−0.02<br />
States Determined by H 0 21 Selection<br />
11 ABE 8.7 ± 1.2 −0.56 +0.09<br />
−0.09<br />
CD 12.2 ± 1.9 −0.14 +0.14<br />
−0.13<br />
63 ACD 26.1 ± 2.0 +0.09 +0.09<br />
−0.09<br />
BE 30.0 ± 2.6 −0.28 +0.09<br />
−0.09<br />
103 AC 35.0 ± 2.8 +0.14 +0.09<br />
−0.09<br />
BDE 33.6 ± 2.3 −0.33 +0.07<br />
−0.07<br />
134 AE 158.3 ± 5.5 +0.73 +0.04<br />
−0.04<br />
BCD 182.8 ± 5.4 +0.55 +0.04<br />
−0.04<br />
140 AD 3.4 ± 1.4 +0.83 +0.17<br />
−0.45<br />
BCE 1.4 ± 0.7 −0.74 +0.24<br />
−0.24<br />
152 AC 1.2 ± 1.1 +1.00 +0.00<br />
−0.00<br />
BD 3.6 ± 1.4 −0.28 +0.34<br />
−0.28<br />
156 B 117.1 ± 7.5 −0.74 +0.04<br />
−0.03<br />
CD 74.5 ± 4.6 −0.84 +0.03<br />
−0.02<br />
States Determined by H 0 31 Selection<br />
10 ABCE 19.1 ± 1.5 −0.08 +0.09<br />
−0.09<br />
D 14.7 ± 3.1 −0.23 +0.18<br />
−0.17<br />
48 ACDE 6.4 ± 1.0 −0.02 +0.17<br />
−0.15<br />
B 4.2 ± 1.8 −0.26 +0.31<br />
−0.29<br />
58 ABCE 59.3 ± 2.4 −0.10 +0.05<br />
−0.05<br />
D 62.2 ± 5.8 +0.19 +0.12<br />
−0.12<br />
66 ABCE 9.5 ± 1.1 −0.09 +0.12<br />
−0.12<br />
D 11.4 ± 2.8 +0.16 +0.61<br />
−0.38<br />
102 ABCE 1.6 ± 0.5 +0.15 +0.39<br />
−0.30<br />
D 1.3 ± 1.6 +0.00 +1.00<br />
−1.00<br />
117 ABCE 106.1 ± 3.3 −0.08 +0.04<br />
−0.03<br />
D 40.0 ± 4.8 −0.01 +0.18<br />
−0.17<br />
Continued on Next Page. . .<br />
−0.56+0.07<br />
−0.07<br />
−0.68+0.11<br />
−0.10<br />
−0.18+0.26<br />
−0.23<br />
−0.06+0.31<br />
−0.26<br />
+0.64+0.04<br />
−0.04<br />
+0.55+0.05<br />
−0.05<br />
−0.26+0.39<br />
−0.32<br />
−0.12+0.26<br />
−0.22<br />
−0.52+0.30<br />
−0.24<br />
−0.76+0.17<br />
−0.14<br />
−0.33+0.06<br />
−0.06<br />
−0.26+0.08<br />
−0.08<br />
−0.99+0.01<br />
−0.01<br />
−1.00+0.01<br />
−0.00<br />
−0.95+0.03<br />
−0.04<br />
−0.93+0.06<br />
−0.07<br />
−0.27+0.10<br />
−0.09<br />
−0.50+0.08<br />
−0.08<br />
−0.36+0.10<br />
−0.09<br />
−0.47+0.07<br />
−0.06<br />
+0.72+0.04<br />
−0.04<br />
+0.52+0.04<br />
−0.04<br />
+0.75+0.25<br />
−0.64<br />
−0.91+0.14<br />
−0.09<br />
+1.00+0.00<br />
−1.00<br />
−0.55+0.36<br />
−0.32<br />
−0.99+0.01<br />
−0.01<br />
−1.00+0.01<br />
−0.00<br />
−0.28+0.09<br />
−0.08<br />
−0.87+0.09<br />
−0.11<br />
−0.32+0.18<br />
−0.15<br />
−1.00+0.16<br />
−0.00<br />
−0.34+0.05<br />
−0.05<br />
+0.05+0.13<br />
−0.12<br />
−0.35+0.12<br />
−0.12<br />
+0.62+0.30<br />
−0.20<br />
−0.56+0.48<br />
−0.38<br />
+1.00+0.00<br />
−0.33<br />
−0.37+0.04<br />
−0.03<br />
+0.27+0.15<br />
−0.14<br />
−0.42+0.09<br />
−0.09<br />
−0.39+0.16<br />
−0.16<br />
−0.28+0.19<br />
−0.19<br />
−0.20+0.21<br />
−0.20<br />
−0.07+0.03<br />
−0.03<br />
+0.02+0.04<br />
−0.04<br />
−0.23+0.32<br />
−0.31<br />
−0.18+0.19<br />
−0.17<br />
−0.57+0.21<br />
−0.22<br />
−0.64+0.21<br />
−0.21<br />
−0.29+0.05<br />
−0.05<br />
−0.26+0.07<br />
−0.07<br />
−0.95+0.06<br />
−0.05<br />
−1.00+0.06<br />
−0.00<br />
−0.84+0.09<br />
−0.13<br />
−0.91+0.08<br />
−0.09<br />
−0.35+0.08<br />
−0.08<br />
−0.26+0.10<br />
−0.10<br />
−0.47+0.08<br />
−0.08<br />
−0.18+0.08<br />
−0.08<br />
−0.02+0.03<br />
−0.03<br />
−0.04+0.03<br />
−0.03<br />
−0.23+0.34<br />
−0.34<br />
−0.54+0.82<br />
−0.46<br />
−0.74+0.46<br />
−0.26<br />
−0.32+0.41<br />
−0.47<br />
−0.95+0.06<br />
−0.05<br />
−1.00+0.06<br />
−0.00<br />
−0.20+0.08<br />
−0.08<br />
−0.80+0.12<br />
−0.16<br />
−0.31+0.15<br />
−0.14<br />
−1.00+0.26<br />
−0.00<br />
−0.24+0.05<br />
−0.05<br />
−0.15+0.09<br />
−0.09<br />
−0.26+0.11<br />
−0.12<br />
+0.50+0.21<br />
−0.19<br />
−0.65+0.27<br />
−0.30<br />
+1.00+0.00<br />
−0.57<br />
−0.30+0.03<br />
−0.03<br />
+0.28+0.12<br />
−0.11<br />
215
Table 5.12—Continued<br />
Source Obs.State LState H21 0 State H31 0 State H32 0 State<br />
(1) (2) (3) (4) (5) (6)<br />
134 ABE 169.6 ± 4.7 +0.68 +0.03<br />
−0.03<br />
CD 175.8 ± 6.7 +0.53 +0.05<br />
−0.05<br />
States Determined by H 0 32 Selection<br />
10 ABCE 19.1 ± 1.5 −0.08 +0.09<br />
−0.09<br />
D 14.7 ± 3.1 −0.23 +0.18<br />
−0.18<br />
66 AD 10.1 ± 1.6 −0.24 +0.19<br />
−0.19<br />
BCE 9.7 ± 1.3 −0.00 +0.15<br />
−0.14<br />
81 ABD 1.4 ± 0.7 +0.21 +0.68<br />
−0.41<br />
CE 1.6 ± 0.9 +1.00 +0.00<br />
−1.27<br />
102 ACE 1.7 ± 0.7 +0.14 +0.38<br />
−0.32<br />
BD 1.2 ± 0.9 +1.00 +0.00<br />
−1.41<br />
117 ABCE 106.1 ± 3.3 −0.08 +0.04<br />
−0.03<br />
D 40.0 ± 4.8 −0.01 +0.18<br />
−0.17<br />
134 ABDE 171.9 ± 4.3 +0.63 +0.03<br />
−0.03<br />
C 171.0 ± 9.3 +0.57 +0.07<br />
−0.06<br />
151 A 11.5 ± 2.4 −0.10 +0.19<br />
−0.19<br />
E 11.6 ± 5.4 −0.76 +0.29<br />
−0.24<br />
+0.69+0.03<br />
−0.03<br />
+0.44+0.06<br />
−0.05<br />
−0.28+0.09<br />
−0.09<br />
−0.87+0.09<br />
−0.11<br />
+0.10+0.17<br />
−0.17<br />
−0.35+0.15<br />
−0.15<br />
−0.56+0.88<br />
−0.44<br />
+1.00+0.00<br />
−0.15<br />
−0.84+0.43<br />
−0.16<br />
+1.00+0.00<br />
−0.34<br />
−0.37+0.04<br />
−0.03<br />
+0.27+0.15<br />
−0.14<br />
+0.63+0.03<br />
−0.03<br />
+0.44+0.08<br />
−0.08<br />
−0.82+0.16<br />
−0.16<br />
−0.34+0.41<br />
−0.31<br />
+0.01+0.03<br />
−0.03<br />
−0.11+0.04<br />
−0.04<br />
−0.20+0.08<br />
−0.08<br />
−0.80+0.13<br />
−0.16<br />
+0.33+0.16<br />
−0.17<br />
−0.35+0.12<br />
−0.13<br />
−0.69+0.32<br />
−0.31<br />
+0.75+0.25<br />
−0.21<br />
−0.88+0.27<br />
−0.12<br />
+0.77+0.23<br />
−0.34<br />
−0.30+0.03<br />
−0.03<br />
+0.28+0.12<br />
−0.11<br />
−0.00+0.03<br />
−0.02<br />
−0.17+0.05<br />
−0.05<br />
−0.78+0.19<br />
−0.18<br />
+0.56+0.44<br />
−0.42<br />
three-state mode, Observations 0784 and 4730 are grouped together in a lower-<br />
luminosity state that is still significantly detected; we note that the three-state set<br />
where the first two observations share a lower-luminosity state, the third observation<br />
is the higher-luminosity state, and the last two observations are a state where the<br />
source is not significantly detected has a χ 2 only 0.46 higher than the best three-<br />
state set. The individual luminosities <strong>of</strong> Source 117 vary significantly with no clear<br />
temporal pattern. In its two-state set, Observation 4729 is in the lower-luminosity<br />
state and the rest <strong>of</strong> the observations are in the higher-luminosity state; however, the<br />
probability the two-state description is correct is 4.2 × 10 −5<br />
Some sources had a lower-luminosity state that was consistent with no emission<br />
at the 3σ level, and a higher-luminosity state, whose observations were sequential and<br />
had emission detected at the > 3σ level. We labeled sources following this pattern<br />
216
<strong>of</strong> states as transient candidates. For Sources 68 and 117, we considered their two-<br />
state properties for discussions <strong>of</strong> transience. Eleven <strong>of</strong> the Analysis Sample sources<br />
(8.9 +3.3<br />
−2.6%) are transient candidates (Sources 11, 37, 41, 45, 51, 67, 68, 77, 94, 110,<br />
and 121). For the eleven transient candidate sources we also calculated the minimum<br />
ratio <strong>of</strong> fluxes at the 3σ level. Only the flux ratio <strong>of</strong> source 110 is above 10. We believe<br />
source 110 is a truly transient source and we discuss it in § 5.10.2. The other transient<br />
candidates are either transient sources or LTLVs that have a lower luminosity state<br />
that is below the detection limit. All eleven transient candidates appeared to turn<br />
either on or turn <strong>of</strong>f during the 4.6 yr over which we observed; no source turned on<br />
and then <strong>of</strong>f, or <strong>of</strong>f and then came back on again. If we assume all the LMXBs in<br />
NGC 4697 are long-term transients, and that our detected transient sources are just<br />
those which turned <strong>of</strong>f or on during our observation period, then the mean outburst<br />
time for LMXBs in NGC 4697 is 103 +42<br />
−28 yr. Under this hypothesis, the duty cycle<br />
<strong>of</strong> LMXBs would also depend on their recurrence timescale. Since our observations<br />
find no recurring transients, we have adopted the crustal heating recurrence timescale<br />
for the Galactic NS-LMXB K-S 1731−260 <strong>of</strong> ∼ 1500 yr (Rutledge et al. 2002). (The<br />
adoption <strong>of</strong> a crustal reheating timescale also implies that we are assuming all the<br />
LMXBs in NGC 4697 are NS-LMXBs. While this is not necessarily true, we note that<br />
the recurrence timescale <strong>of</strong> Galactic long-term transient BH-LMXBs is unknown.<br />
As such, we present this calculation for illustrative purposes only.) We note that<br />
this implies a duty cycle <strong>of</strong> ∼ 7%, which is comparable to the duty cycle obtained<br />
comparing active and quiescent LMXBs in Galactic GCs (∼ 12%; Heinke et al. 2003).<br />
Six <strong>of</strong> the LTLVs have a > 2σ difference for are least one <strong>of</strong> their hardness ratios<br />
between their states (Sources 11, 45, 117, 121, 134, and 156; Table 5.12, columns 4–<br />
6). These sources appear to exhibit luminosity/spectral state transitions. Since the<br />
217
lower-luminosity state in Sources 45 and 121 is not even a 1σ significant detection,<br />
we exclude these sources from this discussion. Although Source 11 is a Field-LMXB<br />
that is a transient candidate, it may also be a luminosity/spectral state transition<br />
source. The luminosity <strong>of</strong> the lower-luminosity state (Observation 4730) is more<br />
than 2σ significant and appears to be 3.4σ s<strong>of</strong>ter in H21, than the higher-luminosity<br />
state. Although this s<strong>of</strong>ter/fainter to harder/brighter transition is opposite <strong>of</strong> the<br />
conventional relationship in BH state transitions, it is possible that this discrepancy<br />
results from the s<strong>of</strong>ter bands used to calculate the hardness with Chandra (Juett<br />
et al. 2006 in preparation). Alternatively, this source may be transitioning from the<br />
thermal state (formerly called high/s<strong>of</strong>t) to the steep power law state (formerly called<br />
very high). For example, in its 1996–1997 outburst, the Galactic LMXB GRO J1655-<br />
40 is s<strong>of</strong>ter and fainter in its thermal state compared to its steep power law state<br />
(Remillard & McClintock 2006). Source 117, a known AGN, appears to display the<br />
more typical harder/fainter to s<strong>of</strong>ter/brighter transition (e.g., the spectral correlation<br />
<strong>of</strong> Seyfert galaxy NGC 4151 in Perola et al. 1986); Observation 4729 is ∼ 4–5σ harder<br />
in H31 and H32 than the two higher luminosity states. Its spectrum seems to change<br />
most in the 2–6 keV band. Source 134, a suspected AGN based on its hardness<br />
ratios, appears to undergo a change in its 1–2 keV band. The lower-luminosity state<br />
is 2.2σ harder in H21, but 2.0σ s<strong>of</strong>ter in H32 than its higher-luminosity state. Finally,<br />
source 156, a known foreground star, undergoes a transition similar to source 11. The<br />
lower-luminosity state <strong>of</strong> source 156 is 2.4σ s<strong>of</strong>ter in H21 than its higher-luminosity<br />
state.<br />
218
Long-Term Hardness Ratio Variability<br />
Our method for identifying LTLV can also be applied to hardness ratios; we<br />
term sources whose hardness ratios vary as Long Term Hardness Variables (LTHVs).<br />
Sources that have variations in the hardnesses ratios that are significant at the 2σ level<br />
have the probabilities that their variations are due to statistical fluctuations listed in<br />
Table 5.11, columns 13–15. We identify fewer LTHVs than LTLVs because the errors<br />
in hardness ratios are larger than in luminosities. Therefore, we only summarize the<br />
results for the 83 sources in multiple observations and with luminosities detected at<br />
the 5σ level. We detect 6.0 +3.9<br />
−2.6%, 7.3 +4.1<br />
−2.9%, and 6.1 +3.9<br />
−2.6% sources that exhibit H21,<br />
H31, and H32 variability at the > 2σ significance level, respectively. Corrections for<br />
falsely identified variable sources reduce the percentages <strong>of</strong> hardness variable sources<br />
to < 5.3%, < 6.9%, and < 5.5%. That is, the numbers <strong>of</strong> sources selected purely<br />
based on hardness ratio variations could result from statistical fluctuations.<br />
We also applied the same grouping <strong>of</strong> observations into states, selecting on the<br />
individual hardness ratios (Table 5.12, lower portions). Here we discuss sources that<br />
were identified as LTHVs in at least two hardness ratios, or identified as LTHVs<br />
in at least one hardness ratio and also as LTLVs. Sources 10, 66, and 102 are in<br />
the first category, while Sources 11, 117, 134, and 156 are in the the second. We<br />
discuss attempts to resolve the difference in their states, and the implications <strong>of</strong><br />
those attempts.<br />
For Source 10, the selections by H31 and H32 agree, pointing to a probable decrease<br />
in the 2–6 keV count fraction for Observation 4729. Although the best-fit states<br />
disagree for Source 66, matching the H32 selected state to the H31 selected state leads<br />
to a χ 2 that is only 0.7 higher than the best H32 selected state. The fraction <strong>of</strong><br />
2–6 keV counts is higher for Observation 4729. Similarly, matching the H31 selected<br />
219
state to the H32 selected state leads to a χ 2 that is only 0.2 higher than the best H31<br />
selected state for Source 102; the 2–6 keV count fraction is higher for Observations<br />
4727 and 4729.<br />
Sources 11, 117, 134, and 156 were all identified as luminosity/spectral state<br />
transitions using the LTLV selection. The hardness ratio two-state sets in Source<br />
117 are consistent with the two-state luminosity set; the 2–6 keV count fraction is<br />
higher in the lower-luminosity state (Observation 4729). The H21 and luminosity<br />
states match for Source 156, where the lower-luminosity state is s<strong>of</strong>ter in H21 than<br />
the higher-luminosity state. Sources 11 and 134 are more difficult to resolve. If we<br />
match the H21 selected state to the luminosity selected state for Source 11, the χ 2<br />
is 4.1 higher; one cannot easily resolve this difference for Source 11. Nevertheless,<br />
both sets <strong>of</strong> states are consistent with the lower-luminosity state being s<strong>of</strong>ter in H21.<br />
The resolution for Source 134 is even more problematic. This source appears best<br />
described by a non-monotonic evolution <strong>of</strong> hardness with luminosity. As the source<br />
luminosity increases, it first becomes s<strong>of</strong>ter and then becomes harder in all three<br />
hardness ratio bands; however, the s<strong>of</strong>test observation changes between 4728 or 4729<br />
depending on the hardness ratio.<br />
Source 110: A Transient Supers<strong>of</strong>t Source<br />
We consider Source 110 to be a clear transient source. In the first four observa-<br />
tions, there were 5 counts in the source aperture and 19 counts in the (three times)<br />
larger background aperture. After correcting for QE degradation <strong>of</strong> a typical source<br />
in NGC 4697, the corresponding rate is (−1.3±3.8)×10 −5 cnt s −1 ; the source is clearly<br />
undetected. We also calculated the corrected rate including observations 4727-4729,<br />
which have a similar level <strong>of</strong> QE degradation, to be (−1.0 ± 4.6) × 10 −5 cnt s −1 .<br />
220
In the final observation, there were 87 counts in the source aperture and 4 counts<br />
in the background aperture, corresponding to a QE degradation corrected rate <strong>of</strong><br />
(32.6 ± 4.0) × 10 −4 cnt s −1 . The ratio <strong>of</strong> the count rate in Observation 4730 to the<br />
other observations is > 27 at the 3σ level. Therefore, we only consider data from<br />
Observation 4730 hereafter. Within the 0.3–6.0 keV band, only two <strong>of</strong> the source<br />
aperture photons were above 1 keV (1.03 and 3.9 keV). Source 110 is clearly super-<br />
s<strong>of</strong>t. Its 3σ limits on observed hardness ratios are H21 < −0.89 and H31 < −0.88.<br />
Preliminary analysis <strong>of</strong> our flanking-field HST-ACS observations indicates Source 110<br />
is not associated with an optical source, although it is about 1. ′′ 9 away from a GC<br />
candidate. From simulated point sources at the location <strong>of</strong> Source 110 we placed 90%<br />
confidence limits for a single HST-ACS image <strong>of</strong> g475 > 26.3 and z850 > 25.3 in AB<br />
mag. Since Source 110 is in an overlapping region <strong>of</strong> two fields, these magnitudes<br />
correspond to the 99% confidence limit on an optical counterpart to Source 110.<br />
Since Source 110 is both transient and SS, we explored its spectrum in greater<br />
detail. We examined both the raw spectrum and a binned spectrum. Since Source<br />
110 has only 87 gross counts in Observation 4730, we created five bins with at least<br />
16 counts in the 0.3–1 keV range and a bin with two counts from 1–6 keV. These bins<br />
were weighted by Gehrels errors.<br />
Luminous SSs in our Galaxy and M31 are generally believed to be accreting WDs.<br />
Such sources are <strong>of</strong>ten fit by a blackbody (bb) model. Compared to the best-fit for<br />
this model, the spectrum appears to rise too quickly within the 0.3–1 keV band to be<br />
consistent with Galactic absorption in the raw spectrum. In the binned spectrum,<br />
the best-fit model with Galactic absorption was strongly rejected, χ 2 = 16.78 for 4<br />
d<strong>of</strong> (kTbb = 129 ± 16 eV). This model is also hotter than typical fits to SS-WDs<br />
(15–80 eV; Kahabka & van den Heuvel 1997). If we allow the absorption to vary,<br />
221
we do get a high absorbing column and lower temperature, NH = 1.2 +1.0<br />
−0.6 × 10 22 cm 2<br />
and kTbb = 55 +26<br />
−19 eV (90% individual confidence limits), for an acceptable fit with<br />
χ 2 = 2.04 for 3 d<strong>of</strong>. However, the implied X-ray luminosity in the 0.3–10 keV, LX =<br />
3.0 × 10 41 ergs s −1 , is much too large for a WD at the distance <strong>of</strong> NGC 4697. Even<br />
the lowest luminosity allowed by the uncertainties at 90% confidence for varying<br />
absorption and temperature, 1.6 × 10 39 ergs s −1 , is much too luminous for a SS-WD<br />
in NGC 4697. On the other hand, our optical limit suggests that it unlikely Source<br />
110 is a SS-WD within the Milky Way. Of the likely companions for a SS-WD,<br />
main sequence stars earlier than F5, red giants overflowing their Roche lobe, and<br />
asymptotic giant branch stars with winds (Kahabka & van den Heuvel 1997), an F5<br />
main-sequence star is the faintest with MV ∼ 3.5 (Binney & Merrifield 1998). We<br />
would detect such a source out to ∼ 300 kpc in our HST images. Thus, Source 110<br />
is unlikely to be a SS-WD, either as a foreground Galactic source or a source in<br />
NGC 4697.<br />
A very s<strong>of</strong>t, luminous X-ray transient with an excess absorption column has been<br />
observed in M101 (M101 ULX-1; Kong & Di Stefano 2005). The combination <strong>of</strong><br />
spectra, outburst luminosity, and transience was used to suggest that source is an<br />
intermediate-mass BH (IMBH). The disk blackbody model (hereafter diskbb, Mitsuda<br />
et al. 1984) is a multi-color blackbody model that is <strong>of</strong>ten used to represent BH s<strong>of</strong>t<br />
X-ray transients (SXTs), which have kTdiskbb < 1.2 keV (Tanaka & Shibazaki 1996).<br />
As with the simple blackbody model, the spectrum is poorly fit by a model with<br />
Galactic absorption; kTdiskbb = 163 ± 27 eV yields χ 2 = 20.05 for 4 d<strong>of</strong>. If we allow<br />
the absorption to vary, the absorption and temperature are strongly correlated and<br />
span a fairly large range, but the fit is much improved with a χ 2 = 2.02 for 3 d<strong>of</strong>.<br />
We find NH = 1.2 +1.0<br />
−0.6 × 10 22 cm 2 and kTdiskbb = 59 +28<br />
−22 eV (90% individual confidence<br />
222
limits). The 0.3–10 keV X-ray luminosity <strong>of</strong> acceptable spectral models (within the<br />
90% two-dimensional confidence interval for varying absorption and temperature)<br />
ranges from 3.5 × 10 39 – 6.8 × 10 46 ergs s −1 . The bolometric luminosity range is<br />
even larger, 1.4 × 10 40 < Lbol < 4.8 × 10 48 ergs s −1 . We use the normalization <strong>of</strong><br />
the diskbb model to estimate a BH mass following equation (3) in Fabian et al.<br />
(2004). We have assumed a correction factor <strong>of</strong> f0 = 1.35, an inclination angle <strong>of</strong><br />
i = 60 ◦ , and an innermost disk radius <strong>of</strong> 6 G MBH/c 2 , where MBH is the BH mass.<br />
Dividing our derived bolometric luminosity by the Eddington luminosity, LEdd =<br />
1.26 × 10 38 (MBH/M⊙) ergs s −1 , gives the Eddington efficiency <strong>of</strong> the accretion disk,<br />
which we use later in evaluating the plausibility <strong>of</strong> the model. The value <strong>of</strong> the disk<br />
blackbody temperature also provides a second estimate <strong>of</strong> the black hole mass, which<br />
is roughly MBH/M⊙ ∼ (kTdiskbb/1 keV) −4 . Considering models within the 90% two-<br />
dimensional confidence interval for varying absorption and temperature, these two<br />
estimates <strong>of</strong> BH mass agree to within a factor <strong>of</strong> two for absorption columns between<br />
0.5 and 1 × 10 22 cm 2 . Within this region, our source is consistent with BH masses <strong>of</strong><br />
∼ (7.2 × 10 3 –1.1 × 10 6 ) M⊙ accreting at ∼ 1.6–4.7% <strong>of</strong> the Eddington limit. Thus,<br />
this source is consistent with a rather massive IMBH or a small supermassive black<br />
hole about a factor <strong>of</strong> 2–3 smaller in mass than the one at the center <strong>of</strong> the Milky<br />
Way (Ghez et al. 2000). Understanding the origin <strong>of</strong> such a large BH outside <strong>of</strong> the<br />
center <strong>of</strong> a galaxy or <strong>of</strong> a GC is a formidable challenge to our current theories <strong>of</strong> BH<br />
formation.<br />
Some AGNs have ultras<strong>of</strong>t spectra. For example, Puchnarewicz et al. (1992)<br />
identified 53 ultras<strong>of</strong>t AGN candidates with Einstein Observatory. These sources<br />
had 0.16–0.56 keV count rates nearly three times that <strong>of</strong> their 0.56–1.08 keV count<br />
rates. This corresponds to steep power-law photon indices, Γ 3, with Galactic<br />
223
absorption. In a study <strong>of</strong> variability in s<strong>of</strong>t X-ray selected AGNs, Grupe et al. (2001)<br />
found that AGNs with steeper X-ray spectra had larger short-term variability than<br />
those with flatter spectra. Two <strong>of</strong> the transient sources, IC 3599 and HE 0036-5133<br />
(also called WPVS 007) were transient sources that were also previously reported as<br />
ultras<strong>of</strong>t. These sources may be analogs to Source 110. A variety <strong>of</strong> complicated<br />
models have been used to explain the spectra <strong>of</strong> AGNs with excess s<strong>of</strong>t emission<br />
compared to the power-law models derived from harder bands (e.g., Gierliński &<br />
Done 2004). Given the relative paucity <strong>of</strong> our data on Source 110, we chose to only<br />
consider simple power-law and blackbody models. The power-law model with Galactic<br />
absorption, Γ = 4.23 +0.86<br />
−0.58, is an exceptionally poor fit, χ 2 = 30.20 for 4 d<strong>of</strong>. Even<br />
with a free absorption, power-law models with reasonable photon indices, Γ < 10,<br />
did not fit our data well, χ 2 > 12.25 for 3 d<strong>of</strong>. From above, we know that the disk<br />
blackbody model is a good statistical representation <strong>of</strong> the spectra. However, our<br />
derivation <strong>of</strong> the BH masses in the above paragraph was predicated on the source<br />
being at the distance <strong>of</strong> NGC 4697. As we allow the source to lie farther behind<br />
NGC 4697, the agreement between the mass derived from the normalization and<br />
the mass derived from the temperature begins to break down. Thus, it is unlikely<br />
that the disk blackbody model fully represents the physical mechanism behind the<br />
emission. Regardless <strong>of</strong> the model we choose to represent the emission, we measure<br />
an absorbed X-ray flux (0.5–8.0 keV) <strong>of</strong> FX ∼ 7 × 10 −15 ergs s −1 cm −2 . At that flux<br />
level, we only expect ∼ 3.6 sources unrelated to NGC 4697 for galactocentric radii<br />
interior to that <strong>of</strong> Source 110. Thus, the probability Source 110 is a background AGN<br />
is ∼ 3.3% from the X-ray data alone. Based on our non-detection <strong>of</strong> a counterpart<br />
to Source 110, its X-ray–to–optical flux, log(FX/Fopt), is greater than 0.9 at the<br />
99% confidence level, where Fopt is the optical flux in the z850 band. Such a large<br />
224
atio is expected only from the most obscured AGNs. There are two problems with<br />
suggesting Source 110 is an obscured AGN. First, the most obscured AGNs can have<br />
columns one to two orders <strong>of</strong> magnitude larger than the estimated column for Source<br />
110. In fact, its column is actually near the division point typically used for obscured<br />
and unobscured AGN (10 22 cm 2 Treister et al. 2004). Second, very few sources are<br />
predicted to have such high X-ray–to–optical flux ratios. In Treister et al. (2004),<br />
a model based on the AGN unification paradigm predicts only ∼ 13% <strong>of</strong> AGNs will<br />
have log(FX/Fopt) > 0.8. In summary, although some <strong>of</strong> its X-ray properties may be<br />
consistent with transient ultras<strong>of</strong>t AGN behavior, the combination <strong>of</strong> the expected<br />
number <strong>of</strong> background AGNs with the high X-ray–to–optical flux ratios makes it<br />
unlikely (probability ∼ 0.4%) that Source 110 is a transient ultras<strong>of</strong>t AGN.<br />
5.11 Conclusions<br />
Multi-epoch Chandra observations reveal a wealth <strong>of</strong> information on LMXBs in<br />
NGC 4697, the nearest, optically luminous, elliptical galaxy. We detect 158 sources,<br />
126 <strong>of</strong> which have their count rates determined at ≥ 3σ. Ten sources have optical<br />
counterparts in ground-based catalogs, including a known AGN (Source 117) and the<br />
foreground star BD-05 3573 (Source 156). With our Hubble observations <strong>of</strong> the galaxy<br />
center, we find 36 additional optical counterparts. Most importantly, we identify 34<br />
LMXBs clearly associated with GCs.<br />
We detect sources with X-ray luminosities > 6 × 10 36 ergs s −1 . The fraction <strong>of</strong><br />
LMXBs associated with GCs, fX,GC, is 38.4 +6.1<br />
−5.7% and does not appear to depend on<br />
X-ray luminosity. We find 10.7 +2.1<br />
−1.8% <strong>of</strong> GCs contain an LMXB at the detection limit,<br />
although we note that it is likely that the percentage <strong>of</strong> GCs with an active LMXB is<br />
even higher due to the X-ray flux limit <strong>of</strong> the current observations. Furthermore, our<br />
225
X-ray detections are not complete at the detection limit. At the luminosity limit <strong>of</strong><br />
our Analysis Sample (1.4 × 10 37 ergs s −1 ), which is > 89% complete, 8.1 +1.9<br />
−1.6% <strong>of</strong> GCs<br />
contain an LMXB. This is the second deepest probe <strong>of</strong> the GC/LMXB connection<br />
in an early-type galaxy to date. [At 3.4 Mpc, fainter luminosities can be more easily<br />
reached with Cen A; however, studies <strong>of</strong> the GC-LMXB connection in Cen A are<br />
made more difficult by its larger angular extent on the sky and recent star-formation<br />
(Israel 1998)]. We confirm that GCs that are optically brighter (4.5σ) and redder<br />
(3.0σ) are more likely to contain GCs. We find that GCs with larger encounter rates<br />
are also more likely to contain GCs (5.5σ). When we fit the expected number <strong>of</strong><br />
LMXBs in a GC (λ), we find λ ∝ Γ 0.74+0.14<br />
−0.13<br />
h (Z/Z⊙) 0.50+0.18<br />
−0.16, where Γh is the encounter<br />
rate and Z/Z⊙ is the metallicity <strong>of</strong> a GC. Our results agree well with those found<br />
for fainter X-ray sources in Galactic GCs (Pooley et al. 2003) and LMXBs in M87<br />
(Jordán et al. 2004b).<br />
We have determined the X-ray luminosity functions for each individual observa-<br />
tion, from the combination <strong>of</strong> our five observations, and the LF <strong>of</strong> the non-variable<br />
sources. There is no statistically significant difference in the LFs <strong>of</strong> the different<br />
observations. This result is critical because it validates using single-epoch observa-<br />
tions to measure LFs. While we clearly rule out a single power-law LF, we can not<br />
definitively rule out cut<strong>of</strong>f power-law models with slopes <strong>of</strong> α ≈ 1.5 ± 0.2 and cut<strong>of</strong>f<br />
luminosities <strong>of</strong> ≈(6 +4<br />
−3) × 10 38 erg s −1 . Broken power-law models (eq. [5.8c]) provide<br />
the best fits to our LFs. We adopt our fit <strong>of</strong> the instantaneous LF as our best-fit, with<br />
N0,b = 3.1±1.5, αl = 0.83±0.52, αh = 2.38±0.33, and Lb = (10.8±2.9)×10 37 ergs s −1 .<br />
We note that Kim & Fabbiano (2004) found evidence for a possible break in the LF<br />
<strong>of</strong> LMXBs in early-type galaxies at slightly larger luminosities; however recent deep<br />
observations <strong>of</strong> NGC 3379 and NGC 4278 have not found strong evidence for such a<br />
226
eak (Kim et al. 2006a).<br />
We find marginal evidence (significant at the 2.1σ level) that a larger number <strong>of</strong><br />
LMXBs above the Eddington limit for a hydrogen accreting 1.4 M⊙ NS tend to be<br />
found in GCs than in the field. Although this is consistent with results in Angelini<br />
et al. (2001) in NGC 1399, we believe this results needs to be tested with a larger<br />
sample. One possibility is that multiple LMXBs might exist in a given GC. We predict<br />
that this effect is small, only ∼ 7 <strong>of</strong> the GCs are expected to have multiple LMXBs.<br />
Our spectral analysis <strong>of</strong> sources in the inner effective semi-major axis is best-<br />
fit by a bremsstrahlung spectra with Galactic absorption (kT = 9.1 +1.3<br />
−1.1 keV, NH =<br />
2.14 × 10 20 cm 2 ). Both hardness ratios and spectral analysis indicate that the spectra<br />
<strong>of</strong> X-ray sources at large radii (a 180 ′′ ) differ from those at small radii. We be-<br />
lieve that this effect is due to an increasing dominance <strong>of</strong> unrelated foreground and<br />
background sources, particularly background AGNs. The spectra <strong>of</strong> GC-LMXBs and<br />
field-LMXBS appear to differ (significant at the 3.3σ level). The GC-LMXBs are<br />
better fit with higher temperatures and greater absorbing columns compared to the<br />
field-LMXBs. Similarly, we find a difference (significant at the 3.5σ level) between<br />
X-ray fainter and brighter LMXBs. The fainter LMXBs tend to have smaller absorb-<br />
ing columns, while the brighter LMXBs tend to have a small excess in absorption,<br />
which may be due to accreting material. In both cases, the sources with a smaller<br />
absorption column tend to be fit with sub-Galactic absorbing columns. This indicates<br />
that the spectral model (folded in with the calibration) is not reproducing the spectra<br />
properly. To probe the cause <strong>of</strong> the spectral differences, we require a more physically<br />
accurate model and better understanding <strong>of</strong> the calibration at low energies.<br />
Among the spectral fits to individual bright sources, Source 117 (a known AGN)<br />
and Source 134 had spectral fits with large absorbing columns. We predict Source 134<br />
227
is likely to be an AGN. The spectral fit and variability in Source 156 (the foreground<br />
star BD-05 3573) are consistent with it being an FK Comae star, a chromospherically<br />
active giant.<br />
Our observations were planned to shed light on LMXB variability in elliptical<br />
galaxies. We measure variability on timescales <strong>of</strong> seconds to years. Although we<br />
do not detect any periodic LMXBs at significant levels, we detect five sources with<br />
significant variability on short timescales (Source 57, 71, 75, 155, and 156).<br />
When we compare the luminosity <strong>of</strong> sources between every pair <strong>of</strong> observations,<br />
we determine that 6.7 ± 1.0% <strong>of</strong> the Analysis Sample sources are variable. There is a<br />
slight increase in the fraction <strong>of</strong> variable sources with the variability timescale, but it<br />
is not found to be statistically significant. Our number is roughly consistent with that<br />
found for Centaurus A for a variability timescale <strong>of</strong> 164 d (Kraft et al. 2001) and for<br />
NGC 4636 for a day timescale, but is lower than that found for a 1115 d timescale in<br />
NGC 4636 (Posson-Brown et al. 2006). Multi-epoch observation <strong>of</strong> NGC 3379, 4278,<br />
and 4365 will help fill in more variability timescales. As this phase space is populated,<br />
we will be able to test if more sources are variable on longer timescales than shorter<br />
timescales. Increased knowledge <strong>of</strong> the temporal evolution <strong>of</strong> variability will impact<br />
models that explore the nature <strong>of</strong> the observed LMXBs (e.g., Piro & Bildsten 2002).<br />
We are more sensitive to variability when we consider all five observations simul-<br />
taneously. We find that ≈ 16±4% <strong>of</strong> Analysis Sample sources do not have a constant<br />
luminosity over all five observations. For these sources we group observations into sets<br />
<strong>of</strong> luminosity and hardness ratio states. Among these variable sources, we identify<br />
eleven transient candidates. If we assume all the LMXBs in NGC 4697 are long-term<br />
transients, we estimate that they are on for ∼ 100 yr and have a 7% duty cycle.<br />
The latter is comparable to the duty cycle obtained comparing active and quiescent<br />
228
LMXBs in Galactic GCs (Heinke et al. 2003).<br />
Source 110 is clearly a supers<strong>of</strong>t transient source with no detected counterpart<br />
in HST observations. Although it only has ≈ 85 X-ray counts, our spectral analysis<br />
rules out the possibility that this source is a luminous WD supers<strong>of</strong>t. The high X-<br />
ray–to–optical flux ratio and relative small number <strong>of</strong> expected background AGNs<br />
argue against the source being a transient ultras<strong>of</strong>t AGN. Our spectral fit could be<br />
consistent with an accreting BH with a mass in the range <strong>of</strong> ∼(7 × 10 3 –10 6 ) M⊙;<br />
however, the origin <strong>of</strong> such a large BH outside <strong>of</strong> the center <strong>of</strong> a galaxy or <strong>of</strong> a GC is<br />
a formidable challenge to our current theories <strong>of</strong> BH formation. Further observations<br />
<strong>of</strong> NGC 4697 could increase the information we can extract from the spectra <strong>of</strong> Source<br />
110; however, more work must also be done to increase our understanding <strong>of</strong> the X-ray<br />
spectra <strong>of</strong> non-stellar-mass black holes.<br />
229
Chapter 6<br />
The Low-Mass X-ray Binary and<br />
Globular Cluster Connection in<br />
Virgo Cluster Early-type Galaxies:<br />
Optical Properties<br />
6.1 Introduction<br />
A low-mass X-ray binary (LMXB) consists <strong>of</strong> a compact stellar remnant, a neutron<br />
star (NS) or black hole (BH), that accretes the stellar envelope <strong>of</strong> a low-mass (later<br />
than type A) stellar companion 1 . Roche-lobe overflow is the major method <strong>of</strong> mass<br />
transfer in these systems, which in the Milky Way have orbital periods <strong>of</strong> 0.19–<br />
398 hr (White et al. 1995). When actively accreting, LMXBs are bright X-ray sources<br />
(∼ 10 35 –10 39 erg s −1 ; hereafter, the use <strong>of</strong> “LMXBs” refers only to active LMXBs).<br />
The Milky Way contains ≈ 150 LMXBs (Liu et al. 2001). Most <strong>of</strong> these LMXBs are<br />
1 In some cases, the stellar companion may be a white dwarf.<br />
230
in the field <strong>of</strong> the Milky Way and are likely to have been the result <strong>of</strong> the stellar<br />
evolution <strong>of</strong> a primordial binary (Verbunt & van den Heuvel 1995). This primordial<br />
formation <strong>of</strong> an LMXB cannot be particularly efficient as the binary must survive the<br />
supernova that forms the NS/BH, yet remain in a tight enough orbit that Roche-lobe<br />
overflow eventually occurs.<br />
On the other hand, gravitational interactions in dense stellar systems, particularly<br />
globular clusters (GCs), could lead to more efficient formation <strong>of</strong> binaries in general,<br />
and LMXBs in particular. Over the history <strong>of</strong> X-ray astronomy, 13 Galactic LMXBs<br />
have been detected in 12 GCs. Since GCs account for ∼ 0.1% <strong>of</strong> the Galactic light,<br />
but ∼ 10% <strong>of</strong> the Galactic LMXBs, formation <strong>of</strong> LMXBs in GCs must be hundreds<br />
<strong>of</strong> times more efficient than in the field (e.g., Clark 1975; Katz 1975). The increased<br />
efficiency may be due to a combination <strong>of</strong> two effects: (1) LMXB formation through<br />
tidal capture or exchange interactions after the supernova <strong>of</strong> the NS/BH; and (2)<br />
tighter binary orbits (binary hardening) in GCs due to exchange interactions. The<br />
optical properties <strong>of</strong> GCs containing LMXBs provide a platform to test the dynamical<br />
formation <strong>of</strong> LMXBs in GCs. Furthermore, the metallicities <strong>of</strong> GCs can be measured,<br />
allowing one to probe for metallicity dependent evolution or formation <strong>of</strong> LMXBs in<br />
GCs. Although some patterns can be seen in the limited Galactic data (e.g., Bellazzini<br />
et al. 1995; Bregman et al. 2006, hereafter BIS+2006), a larger sample is necessary<br />
to probe LMXB formation and evolution in GCs.<br />
With the launch <strong>of</strong> the Chandra X-ray Observatory (CXO), it is now possible to<br />
examine large samples <strong>of</strong> LMXBs. In particular, X-ray observations <strong>of</strong> nearby early-<br />
type galaxies can identify tens to hundreds <strong>of</strong> bright X-ray sources, most <strong>of</strong> which are<br />
likely to be LMXBs (e.g., Sarazin et al. 2000). In these galaxies, (∼ 20%–70%) <strong>of</strong> the<br />
LMXBs appear to be associated with GCs (e.g., Sarazin et al. 2000, 2001; Angelini<br />
231
et al. 2001; Kundu et al. 2002); early-type galaxies can provide the large number <strong>of</strong><br />
GCs containing LMXBs necessary to probe LMXB formation and evolution in GCs.<br />
Early samples have shown that GCs that are brighter and redder are more likely to<br />
contain LMXBs (e.g. Kundu et al. 2003; Sarazin et al. 2003); however, the use <strong>of</strong><br />
resolution limited ground-based data or field-<strong>of</strong>-view (FOV) limited space-based data<br />
suppressed the numbers <strong>of</strong> GCs that could clearly be identified.<br />
By observing nearby early-type galaxies with the Hubble Space Telescope Ad-<br />
vanced Camera for Surveys (HST-ACS), which has a 3. ′ 2 × 3. ′ 2 FOV and can resolve<br />
GCs in nearby galaxies, one can construct accurate and comprehensive lists <strong>of</strong> GCs.<br />
In particular, the measurement <strong>of</strong> GC size allows better discrimination against un-<br />
resolved background sources with GC colors, while providing a GC property that is<br />
crucially important to probing the structural parameters <strong>of</strong> GCs that contain LMXBs.<br />
The ACS Virgo Cluster Survey (ACSVCS) has observed the centers <strong>of</strong> 100 early-type<br />
galaxies (Côté et al. 2004) and provides excellent GC data. Some <strong>of</strong> its initial work ex-<br />
plored the GC-LMXB connection in NGC 4486 (M87, Jordán et al. 2004b, hereafter<br />
ACSVCS3). In this work, we expand upon this analysis exploring the GC-LMXB<br />
connection in 10 ACSVCS galaxies and an additional galaxy observed following the<br />
ACSVCS observational setup. We identify 270 GCs that contain LMXBs; this is one<br />
<strong>of</strong> the largest such samples to date, and the largest sample that includes information<br />
about GC size.<br />
232
6.2 Sample<br />
6.2.1 Galaxy Sample<br />
Table 6.1. Galaxy Properties <strong>of</strong> Sample<br />
Type reff DSBF MB<br />
Galaxy (RC3) (arcsec) (Mpc) (mag)<br />
(1) (2) (3) (4) (5)<br />
NGC 4365 E3 49.8 23.2 -21.46<br />
NGC 4374 E1 51.0 18.7 -21.45<br />
NGC 4382 S0 54.6 17.9 -21.46<br />
NGC 4406 E3 104.0 18.0 -21.56<br />
NGC 4472 E2 104.0 16.8 -21.98<br />
NGC 4486 E0 94.9 15.7 -21.70<br />
NGC 4526 S0 44.4 16.1 -20.60<br />
NGC 4552 E0 29.3 16.1 -20.55<br />
NGC 4621 E5 40.5 15.0 -20.37<br />
NGC 4649 E2 68.7 16.4 -21.39<br />
NGC 4697 E6 72.0 11.3 -20.29<br />
We selected our sample from early-type Virgo galaxies with central detections <strong>of</strong><br />
LMXBs using CXO and GCs using HST-ACS. Since the most massive galaxies are<br />
the most likely to have large populations <strong>of</strong> both LMXBs and GCs, we concentrated<br />
on galaxies with MB < −20.25. Our sample includes the ten brightest ACSVCS<br />
galaxies (NGC 4472, 4486, 4406, 4365, 4382, 4374, 4649, 4526, 4552, and 4621)<br />
and NGC 4697, a similarly bright galaxy, which we observed with nearly the same<br />
setup as the ACSVCS. Table 6.1 summarizes some properties <strong>of</strong> the galaxies in our<br />
233
sample. The first three columns list the name, Hubble type, and effective radius<br />
reff from de Vaucouleurs et al. (1992). The next columns list the surface brightness<br />
fluctuation distance, DSBF, determined from the HST observations (S. Mei et al.<br />
2006, in preparation) and the total absolute corrected B-magnitude, MB (combining<br />
HyperLeda 2 and DSBF).<br />
6.2.2 X-ray Analysis<br />
These galaxies all had archival or proprietary data from CXO; however, the obser-<br />
vational setup varied widely between galaxies. Table 6.2 summarizes the properties <strong>of</strong><br />
the CXO observations, listing the galaxy name, CXO observation number (OBSID),<br />
detector with data mode (Faint, Graded, or Very-Faint), and the exposure times be-<br />
fore (tobs) and after removing periods <strong>of</strong> high backgrounds (texp). Since the ACIS-I<br />
chips are less sensitive then the ACIS-S3 chip, we only include data from ACIS-I when<br />
its tobs is > 25% the tobs <strong>of</strong> the ACIS-S3. Since the HST-ACS FOV is smaller than<br />
the CXO FOV, we hereafter only discuss detections where they overlap.<br />
All CXO observations were analyzed under ciao 3.1 3 with caldb 2.28 and<br />
NASA’s FTOOLS 5.3 4 . For Observation 0784, the focal plane temperature was<br />
−110 C, while all other observations were taken at −120 C. When Very-Faint mode<br />
telemetry was available, the observations were cleaned using this extra data to reduce<br />
the background level. All other observations were reduced in Faint mode, including<br />
OBSID 0352, which was telemetered in “Graded” mode. Known aspect <strong>of</strong>fsets were<br />
applied for each observation. Our analysis includes only events with ASCA grades<br />
<strong>of</strong> 0, 2, 3, 4, and 6. Photon energies were determined using the gain files acisD2000-<br />
2 See http://leda.univ-lyon1.fr/.<br />
3 See http://asc.harvard.edu/ciao/.<br />
4 See http://heasarc.gsfc.nasa.gov/docs/s<strong>of</strong>tware/lheas<strong>of</strong>t/.<br />
234
Table 6.2. Properties <strong>of</strong> Chandra Observations<br />
tobs texp<br />
Galaxy OBSID Detector (ks) (ks)<br />
(1) (2) (3) (4) (5)<br />
NGC 4365 2015 ACIS-S3/F 40.4 40.4<br />
NGC 4374 0803 ACIS-S3/VF 28.5 28.4<br />
NGC 4382 2016 ACIS-S3/F 39.7 39.7<br />
NGC 4406 0318 ACIS-S3/F 14.6 11.4<br />
· · · 0963 ACIS-S3/F 14.8 12.0<br />
NGC 4472 0321 ACIS-S3/VF 39.6 34.5<br />
· · · 0322 ACIS-I/VF 10.4 7.2<br />
NGC 4486 0352 ACIS-S3/G 37.7 33.6<br />
· · · 2707 ACIS-S3/F 98.7 82.2<br />
· · · 3717 ACIS-S3/F 20.6 9.2<br />
NGC 4526 3925 ACIS-S3/VF 43.5 41.5<br />
NGC 4552 2072 ACIS-S3/VF 54.4 54.4<br />
NGC 4621 2068 ACIS-S3/F 24.8 24.8<br />
NGC 4649 0785 ACIS-S3/VF 36.9 17.0<br />
NGC 4697 0784 ACIS-S3/F 39.3 37.2<br />
· · · 4727 ACIS-S3/VF 39.9 39.9<br />
· · · 4727 ACIS-S3/VF 35.6 35.6<br />
· · · 4729 ACIS-S3/VF 38.1 32.0<br />
· · · 4730 ACIS-S3/VF 40.0 40.0<br />
01-29gain ctiN0001.fits, except for OBSIDs 0352 (acisD2000-07-06gainN0003.fits) and<br />
0784 (acisD1999-09-16gainN0005.fits). When appropriate, we corrected for time de-<br />
pendence <strong>of</strong> the gain and the charge-transfer inefficiency. All observations were cor-<br />
rected for quantum efficiency (QE) degradation and had exposure maps determined at<br />
750 eV. We excluded bad pixels, bad columns, and columns adjacent to bad columns<br />
235
or chip node boundaries.<br />
The use <strong>of</strong> local backgrounds in point source analysis mitigates the effect <strong>of</strong><br />
high background periods (“background flares”), which especially affect the backside-<br />
illuminated S1 and S3 chips 5 . We avoided the periods with the most extreme flares by<br />
only including times where the background rate was below three times the expected<br />
background rate from the blank-sky background fields in the CALDB. When avail-<br />
able, we used the S1 chip to measure the background rate, excluding point sources,<br />
and compared to the blank-sky background count rates in CALDB in the 2.6–6.0 keV<br />
band. If the S1 chip was not available, we used the S3 chip to determine count<br />
rates in the 2.6–7.0 keV band. For Observation 0784, we compared count rates in<br />
the 0.3–10.0 keV band to Maxim Markevitch’s aciss B 7 bg evt 271103.fits blank-sky<br />
background 6 . Only a small amount <strong>of</strong> time was lost in any observation due to the<br />
time binning used to determine the rates. We list the exposure before and after flare<br />
removal in Table 6.2.<br />
To identify the discrete X-ray source population, we applied a wavelet detection<br />
algorithm (the CIAO wavdetect program) with scales increasing by a factor <strong>of</strong> √ 2<br />
from 1 to 32 pixels. We adopted a source detection threshold <strong>of</strong> 10 −6 for both the<br />
ACIS S3 and I chips. Source detection excluded regions with an exposure <strong>of</strong> less then<br />
10% than that <strong>of</strong> the observation (e.g., regions at the edges <strong>of</strong> chips). To maximize<br />
the signal-to-noise (S/N), we analyzed the wavelet detection results from combined<br />
observations when available. We detected 708 X-ray sources that were also in the<br />
FOV <strong>of</strong> the HST-ACS observations. There are regions <strong>of</strong> complex gas emission at<br />
the center <strong>of</strong> NGC 4486. Although detected sources in these region may be LMXBs,<br />
they may also be compact regions <strong>of</strong> enhanced gas emission. To avoid mistaken<br />
5 See http://cxc.harvard.edu/contrib/maxim/acisbg/.<br />
6 See footnote 5.<br />
236
identification <strong>of</strong> point sources, ACSVCS3 excluded all X-ray sources in these regions.<br />
We follow this procedure, excluding 33 X-ray sources.<br />
We used the coordinate list generated by wavdetect in ACIS Extract 3.34 7 to<br />
refine the source positions and determine source extraction regions. This was accom-<br />
plished by determining the mean positions <strong>of</strong> events in source extraction regions con-<br />
sistent with the X-ray point spread functions (PSFs) at the positions <strong>of</strong> the sources.<br />
For most sources the median photon energy was ≈ 0.6–2.6 keV and we required the<br />
extraction region to encircle 90% <strong>of</strong> the X-ray PSF at ≈ 1.5 keV. We determined the<br />
PSF at either ≈ 0.3 keV or ≈ 4.5 keV for the few sources that were either s<strong>of</strong>ter or<br />
harder. In a few sources where the 90% PSF extraction regions overlapped, we used<br />
a lower percentage <strong>of</strong> the PSF to define the extraction region.<br />
When there were multiple observations <strong>of</strong> a galaxy, we matched the positions<br />
<strong>of</strong> detected sources in individual observations to the observation with the largest<br />
exposure. Absolute astrometric corrections were applied for all sources in all galaxies<br />
using a two-dimensional cross-correlation technique to match sources from the Tycho-<br />
2 Catalog (Høg et al. 2000), 2MASS Point Source and Extended Source Catalogs 8 ,<br />
and the USNO-B Catalog (Monet et al. 2003). An astrometric correction (separately<br />
in RA and Dec.) was applied if the <strong>of</strong>fset was statistically significant.<br />
We used a local background from an annular region whose area was approximately<br />
three times that <strong>of</strong> each source’s extraction region; these local backgrounds include<br />
the diffuse emission from the host galaxy. To insure that the local background re-<br />
gions did not contain any significant number <strong>of</strong> source counts, the inner radius <strong>of</strong> the<br />
background region was taken to be the radius encircling 97% <strong>of</strong> the PSF. In cases<br />
where background regions overlapped or fell along node/chip boundaries, we slightly<br />
237<br />
7 See http://www.astro.psu.edu/xray/docs/TARA/ae users guide.html.<br />
8 When a source appeared in both 2MASS catalogs, the Point Source Catalog positions were used.
altered these overlapping regions, preserving the ratio <strong>of</strong> source to background areas<br />
and ensuring that the source region and background region had similar mean expo-<br />
sures. For each <strong>of</strong> the sources, the observed net count rates, their errors, and S/N<br />
were calculated in the 0.3–6.0 keV band by stacking the observations for each galaxy,<br />
correcting for background photons, and dividing by the sum <strong>of</strong> the mean exposure<br />
over each source region. In NGC 4374 and NGC 4486, a few <strong>of</strong> the sources detected<br />
with wavdetect had negative net count rates when determined in this way (two<br />
sources in NGC 4374, five sources in NGC 4486); we excluded these sources from<br />
further discussion.<br />
In order to convert count rates into energy fluxes, we fit a single emission model<br />
to the spectra <strong>of</strong> all <strong>of</strong> the LMXBs in all <strong>of</strong> the galaxies. For each observation <strong>of</strong><br />
each galaxy, we extracted the cumulative spectra <strong>of</strong> essentially all <strong>of</strong> the LMXBs. To<br />
avoid contamination from background AGNs and foreground stars, we excluded all<br />
detected X-ray sources that were located within 1 ′′ <strong>of</strong> a non-GC optical source in the<br />
HST images. We only included LMXBs for which the count rates were determined<br />
with S/N > 3. The source and background regions <strong>of</strong> candidate LMXBs were used to<br />
extract the spectra. We binned the spectra, requiring at least 25 total counts per bin,<br />
and only considered bins completely in the 0.5–10.0 keV band. We simultaneously fit<br />
the spectra <strong>of</strong> all <strong>of</strong> the sources in all <strong>of</strong> the observations <strong>of</strong> all <strong>of</strong> the galaxies to a single<br />
emission model, which was taken to be either a power-law or thermal bremsstrahlung.<br />
However, we accounted for the differing Galactic absorbing columns (NH) to the<br />
different galaxies, using the Tuebingen-Boulder absorption (tbabs) model assuming<br />
abundances from Wilms et al. (2000) and photoelectric absorption cross-sections from<br />
Verner et al. (1996). Note that the response files for each separate observation and<br />
source include the varying effects <strong>of</strong> absorption by the contaminant which produces<br />
238
the QE degradation in the ACIS detectors. The best-fit emission model for all <strong>of</strong> the<br />
sources was found to be a bremsstrahlung model with kT = 9.08 keV. This model,<br />
combined with the individual values <strong>of</strong> NH and distance for each galaxy and the<br />
individual response files for each observation, were used to convert count rates into<br />
unabsorbed X-ray luminosities LX in the 0.3–10.0 keV band.<br />
Due mainly to varying exposure times and distances, the observations <strong>of</strong> differ-<br />
ent galaxies have differing limiting sensitivities. For each galaxy, we summarize the<br />
number <strong>of</strong> X-ray detections and the minimum X-ray luminosity for three sample def-<br />
initions in columns 2 and 3 <strong>of</strong> Table 6.3. The three samples are: all sources with<br />
a positive luminosity (Detected sample); all sources with luminosities determined at<br />
the ≥3σ level (SNR sample); and all sources with LX ≥ 3.2 × 10 38 erg s −1 (Complete<br />
sample). Note that the SNR sample does not include sources that were brighter than<br />
the reported minimum luminosity but not 3σ significant. Since a source with 20 net<br />
counts would be detected at high completeness for most <strong>of</strong> the galaxies, we defined the<br />
Complete sample by the luminosity that a source in NGC 4649 (the galaxy with the<br />
highest minimum luminosity) with 20 net counts would have. We note that detections<br />
at the centers <strong>of</strong> the X-ray brightest galaxies (e.g., NGC 4649) may still be incom-<br />
plete due to contamination from bright gaseous emission; however, we have chosen<br />
this luminosity as a compromise between completeness and a reasonable luminosity<br />
limit.<br />
239
Table 6.3. GC-LMXB Matches by Galaxies<br />
Galaxy NX LX,min a NGCs (G − Z)div NBlue GCs NRed GCs NGCs w LMXBs NBlue GCs w LMXBs NRed GCs w LMXBs NFalse Matches<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11)<br />
Detected: All Sources With Positive Luminosity<br />
NGC 4365 85 0.10 906 1.160 418 [3] 488 [7] 43 (5) 11 (0) 29 (2) 4.36<br />
NGC 4374 49 0.05 506 1.200 310 [0] 196 [0] 18 (0) 9 (0) 9 (0) 1.85<br />
NGC 4382 37 0.52 505 1.230 320 [1] 185 [1] 11 (1) 7 (0) 3 (0) 1.40<br />
NGC 4406 28 0.09 367 1.220 260 [0] 107 [0] 6 (0) 4 (0) 2 (0) 0.75<br />
NGC 4472 86 0.57 764 1.180 306 [0] 458 [4] 40 (2) 4 (0) 36 (2) 2.83<br />
NGC 4486 84 0.14 1639 1.190 690 [4] 949 [10] 49 (6) 12 (0) 34 (3) 6.95<br />
NGC 4526 34 0.31 244 1.170 121 [0] 123 [0] 7 (0) 3 (0) 4 (0) 0.98<br />
NGC 4552 78 0.15 455 1.190 217 [1] 238 [1] 31 (1) 8 (0) 22 (0) 3.00<br />
NGC 4621 44 0.39 306 1.110 121 [0] 185 [2] 17 (1) 1 (0) 16 (1) 1.24<br />
NGC 4649 60 0.65 806 1.200 335 [0] 471 [0] 32 (0) 3 (0) 29 (0) 1.50<br />
NGC 4697 83 0.06 298 1.127 127 [2] 171 [2] 34 (2) 7 (1) 27 (1) 2.15<br />
SNR: All Sources with Luminosities Determined at the 3σ Level<br />
NGC 4365 29 2.26 906 1.160 418 [1] 488 [5] 17 (3) 1 (0) 15 (2) 1.25<br />
NGC 4374 16 2.18 506 1.200 310 [0] 196 [0] 5 (0) 2 (0) 3 (0) 0.62<br />
NGC 4382 21 1.64 505 1.230 320 [0] 185 [0] 5 (0) 4 (0) 1 (0) 0.86<br />
NGC 4406 19 2.65 367 1.220 260 [0] 107 [0] 6 (0) 4 (0) 2 (0) 0.44<br />
NGC 4472 54 1.30 764 1.180 306 [0] 458 [2] 26 (1) 3 (0) 23 (1) 1.72<br />
NGC 4486 61 1.30 1639 1.190 690 [3] 949 [5] 40 (3) 9 (0) 29 (1) 3.65<br />
NGC 4526 12 1.30 244 1.170 121 [0] 123 [0] 3 (0) 1 (0) 2 (0) 0.33<br />
NGC 4552 49 0.80 456 1.190 217 [1] 239 [1] 25 (1) 6 (0) 18 (0) 1.53<br />
NGC 4621 16 1.58 306 1.110 121 [0] 185 [0] 4 (0) 0 (0) 4 (0) 0.55<br />
NGC 4649 21 2.85 807 1.200 335 [0] 472 [0] 13 (0) 2 (0) 11 (0) 0.43<br />
NGC 4697 66 0.15 298 1.127 127 [2] 171 [2] 26 (2) 7 (1) 19 (1) 1.75<br />
Continued on Next Page. . .<br />
240
Table 6.3—Continued<br />
Galaxy NX LX,min a NGCs (g − z)div NBlue GCs NRed GCs NGCs w LMXBs NBlue GCs w LMXBs NRed GCs w LMXBs NFalse Matches<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11)<br />
Complete: All Sources with Luminosities > 3.2 × 1038 erg s−1 NGC 4365 19 3.20 907 1.160 418 [1] 489 [5] 10 (3) 1 (0) 8 (2) 0.93<br />
NGC 4374 12 3.20 506 1.200 310 [0] 196 [0] 4 (0) 2 (0) 2 (0) 0.45<br />
NGC 4382 9 3.20 505 1.230 320 [0] 185 [0] 1 (0) 1 (0) 0 (0) 0.43<br />
NGC 4406 16 3.20 367 1.220 260 [0] 107 [0] 5 (0) 3 (0) 2 (0) 0.38<br />
NGC 4472 19 3.20 764 1.180 306 [0] 458 [2] 9 (1) 0 (0) 9 (1) 0.62<br />
NGC 4486 27 3.20 1639 1.190 690 [3] 949 [5] 14 (3) 2 (0) 10 (1) 2.26<br />
NGC 4526 4 3.20 244 1.170 121 [0] 123 [0] 1 (0) 1 (0) 0 (0) 0.11<br />
NGC 4552 17 3.20 456 1.190 217 [1] 239 [1] 10 (1) 3 (0) 6 (0) 0.45<br />
NGC 4621 7 3.20 308 1.110 121 [0] 187 [0] 2 (0) 0 (0) 2 (0) 0.23<br />
NGC 4649 20 3.20 807 1.200 335 [0] 472 [0] 10 (0) 2 (0) 8 (0) 0.54<br />
NGC 4697 3 3.20 298 1.127 127 [0] 171 [0] 3 (0) 0 (0) 3 (0) 0.00<br />
a Units are 1038 erg s−1 in 0.3–10 keV band.<br />
b If an X-ray source was within 1 ′′ <strong>of</strong> GCs and non-GC sources, it is unclear if the X-ray source is matched to a GC; the possibly matching GCs have<br />
been removed from this sample. Numbers in brackets indicate the number <strong>of</strong> GCs where (only) multiple GCs are within 1 ′′ <strong>of</strong> an X-ray source.<br />
c The number <strong>of</strong> RGC-LMXBs and BGC-LMXBs will not add up to the number <strong>of</strong> GC-LMXBs if an X-ray source is within 1 ′′ <strong>of</strong> both an RGC and a<br />
BGC. Numbers in parenthesis indicate the number <strong>of</strong> X-ray sources where (only) multiple GCs are within 1 ′′ <strong>of</strong> an X-ray source.<br />
241
6.2.3 Optical Analysis<br />
The centers <strong>of</strong> all <strong>of</strong> the galaxies in our sample except NGC 4697 were observed<br />
as part <strong>of</strong> the ACSVCS, which acquired two 360 s exposures in the F475W band,<br />
two 560 s exposures in the F850LP band, and one 90 s F850LP exposure. NGC 4697<br />
was observed separately from the ACSVCS, but in a similar manner; its two F475W<br />
exposures were 15 s longer. We excluded optical sources detected in the central few<br />
arcseconds <strong>of</strong> some galaxies with dusty cores (NGC 4374, NGC 4526, and NGC<br />
4697) and in the region <strong>of</strong> NGC 4649 which overlaps with its nearby spiral neighbor,<br />
NGC 4647.<br />
Observed GC Properties<br />
In our sample, over 10,000 optical sources were characterized by their magnitudes,<br />
g475 and z850, half-light radii, rh, and positions as determined by KINGPHOT (Jordán<br />
et al. 2005). All magnitudes were converted to absolute magnitudes (G475 and Z850)<br />
using the surface brightness fluctuation distances in Table 6.1. We used magnitude,<br />
color (0.5 < G475 − Z850 < 1.9), and size criteria to select 7,084 likely GCs, following<br />
Jordán et al. (2004a). We list the number <strong>of</strong> GCs detected in each galaxy (excluding<br />
GCs whose matching X-ray source may also match to a non-GC optical source and<br />
all optical sources in the X-ray excluded regions <strong>of</strong> NGC 4486) in the fourth column<br />
<strong>of</strong> Table 6.3.<br />
Early-type galaxies <strong>of</strong>ten have a bimodal distribution <strong>of</strong> GC colors. For each<br />
galaxy, we used the division point, (G − Z)div, in the G475 − Z850 color following Peng<br />
et al. (2006a) to divide the GCs into blue-GCs and red-GCs; these division point<br />
ranged from (G − Z)div = 1.11 to 1.23. We list the division points and the number<br />
<strong>of</strong> blue-GCs and red-GCs in columns five, six, and seven <strong>of</strong> Table 6.3.<br />
242
The positions <strong>of</strong> the GCs were used to determine the galactocentric distance, dGC.<br />
These values were then scaled to the effective radii <strong>of</strong> the galaxies. We show scatter<br />
plots and integrated histograms <strong>of</strong> the observed properties <strong>of</strong> the GCs in our sample<br />
in Figures 6.1 and 6.2.<br />
Derived GC Properties<br />
From the magnitude, colors, and radii, we can derive other parameters that might<br />
impact the formation and evolution <strong>of</strong> LMXBs in GCs. We calculate the GC mass<br />
(M) directly from the Z-band magnitude,<br />
243<br />
M = ΥZ 10 −0.4 (Z850−Z850,⊙) M⊙ , (6.1)<br />
where the mass-to-light ratio, ΥZ ≡ 1.45 M⊙/L⊙, is predicted by the synthetic PE-<br />
GASE models (Fioc & Rocca-Volmerange 1997), and Z850,⊙ = 4.512 is the absolute<br />
Z-band magnitude <strong>of</strong> the Sun from calcphot in IRAF. In principle, the values <strong>of</strong> ΥZ<br />
depend slightly on the colors <strong>of</strong> the galaxies, but the variation was less than 1%.<br />
Thus, we chose to use a constant ΥZ for all galaxies, so that GC mass is proportional<br />
to GC luminosity.<br />
There is an observed correlation between rh and G475 − Z850 that may indicate<br />
that the half-mass radius <strong>of</strong> a GC, rh,M, differs from its half-light radius (e.g., Jordán<br />
2004; Jordán et al. 2005). Since rh,M is more physically relevant in discussion <strong>of</strong><br />
Galactic dynamics than rh, we calculated<br />
rh,cor = rh 10 0.17[(G475−Z850)−1.2] , (6.2)<br />
following Jordán et al. (2005), and assumed this was the half-mass radius. We display
Fig. 6.1.— Scatter plot <strong>of</strong> GC magnitudes (Z850) versus GC colors (G475 − Z850),<br />
with integrated histograms <strong>of</strong> the properties above and to the right <strong>of</strong> the scatter<br />
plot. GCs unmatched to LMXBs are indicated by small black dots and unfilled black<br />
histograms (scaled down by a factor <strong>of</strong> 10). Blue GCs with LMXBs are indicated by<br />
filled blue squares and histograms. Red GCs with LMXBs are indicated by filled red<br />
circles and histograms. The histograms <strong>of</strong> the GCs with LMXBs are stacked on each<br />
other. GCs that are redder and brighter are more likely to contain LMXBs.<br />
244
Fig. 6.2.— Scatter plot <strong>of</strong> GC galactocentric distances (dGC) versus observed GC<br />
half-light radii (rh), with integrated histograms <strong>of</strong> the properties above and to the<br />
right <strong>of</strong> the scatter plot. The symbols follow that <strong>of</strong> Figure 6.1. GCs that are smaller<br />
in extent are more likely to contain LMXBs. The galactocentric distance does not<br />
appear to affect whether a GC contains an LMXB.<br />
245
the rh,cor <strong>of</strong> the GCs in our sample in Figure 6.3.<br />
Since BIS+2006 suggested that LMXBs occurred in GCs with ages greater than<br />
five times the relaxation time at the half-mass radius, th,relax, we adopted the Harris<br />
(1996) corrections to Djorgovski (1993) equation (11) and used our corrected half-<br />
mass radius estimate for calculating th,relax,cor:<br />
th,relax,cor = 2.055 × 10 6<br />
1<br />
ln(0.4N∗)<br />
−1 <br />
〈m∗〉 M<br />
M⊙<br />
M⊙<br />
246<br />
1/2 3/2 rh,M<br />
yr , (6.3)<br />
1 pc<br />
where the average stellar mass, 〈m∗〉, is taken to be 1<br />
3 M⊙ and N∗ = M/〈m∗〉.<br />
BIS+2006 suggested that the relaxation time be combined with the number <strong>of</strong> stars<br />
in the globular cluster to give a “stellar interaction rate” <strong>of</strong><br />
S =<br />
N∗<br />
th,relax,cor<br />
yr −1 ∝ M 1/2 r −3/2<br />
h,M . (6.4)<br />
For a system in virial equilibrium, the relaxation time is approximately<br />
(0.1N∗/ ln N∗) tcross, where tcross is the stellar crossing time (roughly the orbital pe-<br />
riod <strong>of</strong> a star within the GC). Thus, S ≈ 10 ln(N∗)/tcross; except for a nearly constant<br />
factor, it is just the inverse <strong>of</strong> the orbital period. We will refer to S as the “stellar<br />
crossing rate.” In Figure 6.4, we plot th,relax,cor versus Z850 for the GCs in our sample,<br />
overlaying lines <strong>of</strong> constant S for comparison with BIS+2006, Figure 5.<br />
The dynamical formation model <strong>of</strong> LMXBs in GCs is the leading explanation for<br />
the larger efficiency <strong>of</strong> LMXB production in GCs compared to the fields <strong>of</strong> galaxies.<br />
In this model, the binary is either formed by tidal capture or through exchange<br />
interactions between a NS/BH and an existing binary. In both cases, the binary<br />
encounter rate (Γ) is thought to depend on the properties <strong>of</strong> GCs at their cores;<br />
Γ ∝ ρ 3/2<br />
0 r 2 c, where ρ0 is the core density, rc is the core radius, and the virial theorem
Fig. 6.3.— Scatter plot <strong>of</strong> estimated GC half-light radii (rh,cor) versus GC colors<br />
(G475 − Z850), with integrated histograms <strong>of</strong> the properties above and to the right <strong>of</strong><br />
the scatter plot. The symbols follow that <strong>of</strong> Figure 6.1. There is no color dependence<br />
<strong>of</strong> rh,cor, indicating we have successfully removed the color dependence <strong>of</strong> half-light<br />
radius rh. GCs that are redder and smaller in extent are more likely to contain<br />
LMXBs.<br />
247
Fig. 6.4.— Scatter plot <strong>of</strong> GC relaxation time (th,relax,cor) at half-mass versus GC<br />
magnitude (Z850), where the symbols follow that <strong>of</strong> Figure 6.1. Overlaid are lines <strong>of</strong><br />
constant stellar crossing rate (S = N∗/th,relax,cor) that decrease by 0.5 dex starting<br />
at log(S [yr −1 ]) = −2.5 (lower left). The Galactic version <strong>of</strong> this plot for V -band<br />
is displayed in BIS+2006, Figure 5. GCs with large relaxation timescales can host<br />
LMXBs, in contrast to the result found in the much smaller sample <strong>of</strong> Galactic GCs<br />
(BIS+2006).<br />
has been assumed to connect core velocities to densities and radii. Although these<br />
parameters are not directly measurable at the distance <strong>of</strong> the Virgo cluster, we can<br />
create a proxy,<br />
Γh ≡<br />
M<br />
2πM⊙<br />
248<br />
3/2 −5/2 rh,M<br />
, (6.5)<br />
1 pc<br />
where we have assumed that the relation between core structural parameters and the<br />
parameters at a half-mass radius (dictated by the concentration, c) is the same for all<br />
GCs. Although the latter assumption is not strictly true, it need only be true that the<br />
distribution <strong>of</strong> c not depend on other parameters. If GCs with higher concentrations
Fig. 6.5.— Scatter plot <strong>of</strong> estimated GC size (rh,cor) versus GC magnitude (Z850),<br />
where the symbols follow that <strong>of</strong> Figure 6.1. Overlaid are lines <strong>of</strong> constant binary<br />
encounter rate that decrease by 0.5 dex starting at log Γh = 9.0 (lower left). The<br />
Galactic version <strong>of</strong> this plot for V -band is displayed in BIS+2006, Figure 3. GCs<br />
with larger encounter rates are more likely to contain LMXBs.<br />
are more likely to contain LMXBs, then the Γh we calculate will underpredict the<br />
binary interaction rate for GCs with LMXBs. We plot rh,cor versus Z850 for GCs<br />
in our sample, overlaying lines <strong>of</strong> constant Γh, in Figure 6.5 for comparison with<br />
BIS+2006, Figure 3.<br />
6.2.4 Matching LMXBs And GCs<br />
To determine the relative astrometry between CXO and HST observations for each<br />
galaxy, we convolved the X-ray and optical positions with a σ = 0. ′′ 5 2-dimensional<br />
Gaussian, and cross-correlated the two images with an <strong>of</strong>fset in RA and Dec. The<br />
249
maximum cross-correlation was used to determine the astrometric <strong>of</strong>fset. After cor-<br />
recting for this <strong>of</strong>fset, X-ray sources within 1 ′′ <strong>of</strong> optical sources were considered to<br />
be matched.<br />
If an X-ray source was matched to both non-GC optical sources and GCs, we<br />
excluded the X-ray source and GCs from our analysis. All remaining 288 X-ray de-<br />
tections in GCs were considered to be GC-LMXBs. For the 18 GC-LMXBs that were<br />
within 1 ′′ <strong>of</strong> multiple GCs, we could not determine which GC contained the LMXB;<br />
however, if the multiple GCs all belonged to the same sub-population (blue-GC vs.<br />
red-GC), we could count the GC-LMXB as belonging to that sub-population. We<br />
indicate the number <strong>of</strong> GCs with LMXBs, and separately list the numbers <strong>of</strong> LMXBs<br />
in blue-GCs and red-GCs, in the eighth, ninth, and tenth columns <strong>of</strong> Table 6.3. In<br />
parenthesis, we indicate the number <strong>of</strong> GC-LMXBs matched to multiple GCs. We<br />
also indicate the corresponding number <strong>of</strong> GCs in the brackets <strong>of</strong> columns four, six,<br />
and seven.<br />
We separated the GCs into two sub-populations, those that clearly contained an<br />
LMXB in our Detected sample (indicated by a subscripted X), and those that clearly<br />
did not (indicated by a subscripted nX). We found 270 GCs that contained an LMXB<br />
at our detection levels and 6,488 GCs that clearly did not. We display the properties<br />
<strong>of</strong> these GCs in Figures 6.1–6.4, indicating blue-GCs with LMXBs using filled blue<br />
squares and red-GCs with LMXBs using filled red circles. Of the 270 GCs clearly<br />
containing an LMXB, 160 contained an LMXB in the SNR sample, and 61 contained<br />
an LMXB in the Complete sample.<br />
We randomized the position angles <strong>of</strong> the GCs around the centers <strong>of</strong> their host<br />
galaxies to estimate the number <strong>of</strong> LMXBs falsely associated with GCs. We either<br />
kept the radius <strong>of</strong> the GC fixed, or assumed that it lay on the sample elliptical<br />
250
isophote from the galaxy optical surface brightness. We redid the matches with the<br />
randomized GC catalogs, and used the number <strong>of</strong> resulting matches to predict the<br />
percentage <strong>of</strong> non-GC X-ray sources falsely matched to a GC, pfalse. Since there<br />
was typically little difference between the two methods, we averaged the two. Given<br />
the typical values <strong>of</strong> these numbers (3.3–14.8%), it is unlikely that any <strong>of</strong> the GC-<br />
LMXBs matched to multiple GCs are not actually associated with a GC; however,<br />
some fraction <strong>of</strong> the GC-LMXBs matched to a single GC will be false matches. The<br />
predicted number <strong>of</strong> falsely matched sources is pfalse/(1 − pfalse) times the number<br />
<strong>of</strong> observed non-GC X-ray sources. The term in the denominator accounts for the<br />
falsely matched sources part <strong>of</strong> the non-GC X-ray sources. The expected number <strong>of</strong><br />
false matches is displayed in the eleventh column <strong>of</strong> Table 6.3. The large GC density<br />
in NGC 4486 leads to a correspondingly larger number <strong>of</strong> false matches; however, the<br />
number <strong>of</strong> false matches still make up less than 15% <strong>of</strong> the identified GC-LMXBs.<br />
With the number <strong>of</strong> false GC-LMXB and total number <strong>of</strong> GCs, we estimate the<br />
expected number <strong>of</strong> false matches per GC, λf, for each galaxy, which range from<br />
about 2 × 10 −3 to 7 × 10 −3 .<br />
6.3 Properties <strong>of</strong> GCs with and without LMXBs<br />
We employ three methods to compare the properties <strong>of</strong> GCs with and without<br />
LMXBs. (Some GCs contain LMXBs that are in the Detected sample, but do not<br />
make it into the SNR or Complete samples. We did not include such GCs as ei-<br />
ther GCs with LMXBs or GC without LMXBs when we compared the properties<br />
<strong>of</strong> the GCs with LMXBs in the SNR sample and Complete sample to GCs without<br />
LMXBs.) First, the binned histograms in Figures 6.1–6.4 display the qualitative dif-<br />
ferences. Second, we calculate the median values <strong>of</strong> the GC properties and use the<br />
251
Fig. 6.6.— The percentage <strong>of</strong> GCs containing an LMXB as a function <strong>of</strong> GC magnitude<br />
(Z850), color (G475 − Z850), half-mass radius (rh,cor), and galactocentric distance<br />
(dGC). GCs that are brighter, are redder, and have smaller half-mass radii are more<br />
likely to contain LMXBs. The uncertainties are at the 1σ confidence level. The bins<br />
were set by requiring 27 GCs with LMXBs per bin.<br />
non-parametric Wilcoxon rank-sum test to quantify the differences. We also used<br />
the Wilcoxon test to compare the properties <strong>of</strong> GCs with LMXBs in the Complete<br />
sample and GCs with LMXBs fainter than the Complete sample limit. Finally, we<br />
bin the GCs by the different parameters and look for non-uniform probabilities <strong>of</strong><br />
GCs containing an LMXB in Figure 6.6. The errors on the fractions in Figure 6.6<br />
are calculated assuming Poisson statistics (i.e., strict 1σ confidence intervals were<br />
calculated as opposed to using the √ N approximation). The fractions in Figure 6.6<br />
were corrected for the rate <strong>of</strong> false matches, λf.<br />
252
6.3.1 Luminosity and Mass<br />
Prior observations have revealed that more luminous GCs appear to preferentially<br />
host LMXBs (e.g.. Angelini et al. 2001; Kundu et al. 2002; Sarazin et al. 2003).<br />
Figure 6.1 confirms that LMXBs are found more <strong>of</strong>ten in brighter GCs. The median<br />
Z850 were −8.5 for GCs without LMXBs, and −9.9 for GCs with LMXBs, which<br />
correspond to differences <strong>of</strong> 15.6σ (Detected sample), 11.8σ (SNR sample), and 6.6σ<br />
(Complete sample). We find no significant difference (0.9σ) in the optical luminosities<br />
<strong>of</strong> GCs in the Complete sample and <strong>of</strong> GCs with fainter LMXBs.<br />
The median mass <strong>of</strong> a GC with an LMXB is 3.6 times that <strong>of</strong> a GC without<br />
an LMXB. Figure 6.6 suggests a power-law dependence <strong>of</strong> the probability <strong>of</strong> a GC<br />
containing an LMXB on the mass <strong>of</strong> the GC.<br />
6.3.2 Color<br />
Prior observations also have revealed that redder GCs appear to preferentially host<br />
LMXBs (e.g., Kundu et al. 2003; Sarazin et al. 2003). Our larger sample (Figure 6.1)<br />
clearly confirms this. The median G475−Z850 color was 1.20 for GCs without LMXBs,<br />
and 1.34 (Detected sample), 1.35 (SNR sample), and 1.38 (Complete sample) for GCs<br />
with LMXBs, which correspond to differences <strong>of</strong> 6.6σ, 5.8σ, and 3.7σ. There were no<br />
significant differences (1.2σ) in the colors <strong>of</strong> GCs in the Complete sample and GCs<br />
with fainter LMXBs.<br />
Many <strong>of</strong> the prior papers have compared the fraction <strong>of</strong> blue-GCs with LMXBs<br />
to the fraction <strong>of</strong> red-GCs with LMXBs, and found that red-GCs are ∼ 3 times as<br />
likely to contain LMXBs. In Figure 6.7, we compare these fractions for the Detected<br />
sample. The cumulative sample suggests that red-GCs are 3.15 ± 0.54 times as likely<br />
to have LMXBs as blue-GCs; however, there are considerable differences between<br />
253
Fig. 6.7.— The percentage <strong>of</strong> red-GCs containing an LMXB versus the percentage<br />
<strong>of</strong> blue-GCs containing an LMXB for the Detected sample. The data points with<br />
1σ confidence limits are the different galaxies in our sample. The line indicates the<br />
cumulative relation that red-GCs contain 3.15 ± 0.54 times as many LMXBs as blue-<br />
GCs. The greyscale indicates the area covered by 1, 2, and 3σ <strong>of</strong>f <strong>of</strong> the best fit.<br />
galaxies.<br />
Figure 6.6 suggests that the probability that a GC contains an LMXB depends<br />
exponentially on the color. If this dependence were due only to a difference between<br />
the red and blue GC populations, but were independent <strong>of</strong> the color <strong>of</strong> a GC within the<br />
two populations, one might expect each population would have a different constant<br />
efficiency. This would appear as a step-function relation in Figure 6.6, except for the<br />
third bluest color bin. This bin contains all but two <strong>of</strong> the different galactic division<br />
points between red-GCs and blue-GCs. As such, its value would be intermediate<br />
between the two efficiencies. Since both interpretations have two constraints, we can<br />
254
compare their χ 2 fits to test which interpretation is more consistent with the data.<br />
For these fits, we always excluded the third bluest color bin and tested the effect <strong>of</strong><br />
excluding zero, one, or two <strong>of</strong> the reddest color bins. Since the step-function model<br />
always had a higher χ 2 (2.5, 6.7, and 3.1 respectively), we do not believe that the<br />
probability a GC contains an LMXB depends on a difference between the red and blue<br />
GC populations that is independent <strong>of</strong> the color <strong>of</strong> a GC within the two populations.<br />
Since color is roughly a logarithm <strong>of</strong> metallicity, we prefer interpreting Figure 6.6 as an<br />
indication that the probability a GC contains an LMXB has a power-law dependence<br />
on GC metallicity.<br />
6.3.3 Size<br />
Although there were indirect indications that the size <strong>of</strong> GCs affect the formation<br />
or evolution <strong>of</strong> LMXBs in ACSVCS3, we present here the first explicit evidence <strong>of</strong><br />
this. We find that LMXBs are found more <strong>of</strong>ten in GCs that have smaller half-light<br />
radii (Figure 6.2). The median rh values were 2.6 pc for GCs without LMXBs, and<br />
2.3 pc (Detected sample), 2.3 pc (SNR sample), and 2.2 pc (Complete sample) for GCs<br />
with LMXBs, which correspond to differences <strong>of</strong> 8.1σ, 7.4σ, and 4.9σ. Although the<br />
differences in the medians are 15%, the distributions are found to be significantly<br />
different for two reasons. First, with the number <strong>of</strong> GCs in our samples, the Wilcoxon<br />
test is sensitive to 10%, 14%, and 22% differences in the medians, respectively, at the<br />
3σ level. Second, the Wilcoxon test samples the entire distribution, not just the<br />
medians. For example, the values <strong>of</strong> the half-light radii that contain 90% <strong>of</strong> the<br />
GCs are 4.3 pc for GCs without LMXBs, and 3.3 pc (Detected sample), 3.0 pc (SNR<br />
sample), and 3.0 pc (Complete sample) for GCs with LMXBs. Kolmogorov-Smirnov<br />
tests indicate that the probability the distributions <strong>of</strong> half-light radii are drawn from<br />
255
the same sample are 5.7 × 10 −13 (Detected sample), 8.1 × 10 −11 (SNR sample), and<br />
9.6 × 10 −6 (Complete sample), consistent with the Wilcoxon tests. Once again, we<br />
found no significant differences (1.2σ) in the half-light radii <strong>of</strong> GCs in the “Complete<br />
sample” and GCs with fainter LMXBs.<br />
Given that redder GCs are more likely to contain LMXBs and have smaller half-<br />
light radii, we also compared the half-mass radii <strong>of</strong> GCs with and without LMXBs<br />
(Figure 6.3). Our adopted half-mass radii should be, by definition, nearly insensitive<br />
to color variations. The median rh,cor <strong>of</strong> GCs with LMXBs were only 0.1 pc more than<br />
their half-light radii. The distributions <strong>of</strong> half-mass radii <strong>of</strong> GCs with and without<br />
LMXBs are different at the 5.9σ (Detected sample), 5.5σ (SNR sample), and 3.7σ<br />
(Complete sample) levels. Thus, GCs that are smaller in extent remain more likely<br />
to contain LMXBs, even if the half-mass radii are used to measure the size.<br />
Figure 6.6 suggests that the probability that a GC has an LMXB may decrease<br />
roughly as a power-law <strong>of</strong> the half-light radius. There is a similar, but slightly flatter<br />
dependence on half-mass radius.<br />
6.3.4 Galactocentric Distance<br />
The effect <strong>of</strong> galactocentric distance on the probability that a GC has a LMXB is<br />
less clear in our data. The values <strong>of</strong> dGC are slightly smaller for GCs with LMXBs in<br />
the Complete sample as compared to GCs with LMXBs not in the Complete sample,<br />
but the difference is not very significant (2.2σ). This could indicate that the values<br />
<strong>of</strong> dGC are affected by incompleteness. Since the incompleteness is more important in<br />
the X-ray brighter, central regions <strong>of</strong> galaxies, and incompleteness affects the fainter<br />
LMXBs more, this effect is not unexpected. There is no significant difference (1.6σ)<br />
in the radial distributions between the Detected sample <strong>of</strong> GCs with LMXBs and<br />
256
GCs without LMXBs; however, there are slightly significant differences when using<br />
the SNR sample (3.1σ) and Complete sample (2.8σ). Figure 6.6 suggest that there<br />
may be a slight decrease with dGC in the probability that a GC contains an LMXB.<br />
However, since red-GCs tend to be closer to the galaxy center and are more likely<br />
to contain LMXBs, it is possible that the lower galactocentric distances <strong>of</strong> GCs with<br />
LMXBs in the SNR and Complete sample can be completely accounted for without<br />
invoking an intrinsic difference in the probability a GC contains an LMXB on dGC.<br />
Given the marginal, if any, strength <strong>of</strong> the dependence on dGC, we do not consider it<br />
further in this chapter.<br />
6.3.5 Relaxation Time<br />
No Galactic GCs with a relaxation timescale 2.5 Gyr contains an active LMXB.<br />
In our much larger sample (Figure 6.4), about 20% <strong>of</strong> the GCs with LMXBs have<br />
relaxation timescales larger than this. The relaxation timescale <strong>of</strong> the GCs with<br />
LMXBs in our sample are larger than GC without LMXBs; the median th,relax,cor<br />
were 1.0 Gyr for GCs without LMXBs, and 1.5 Gyr (Detected sample), 1.4 Gyr (SNR<br />
sample), and 1.3 Gyr (Complete sample) for GCs with LMXBs. This difference is<br />
opposite to that seen in the Galaxy, where the median th,relax are 0.7 Gyr for GCs<br />
with LMXBs and 1.3 Gyr (Harris 1996). In our sample, the relaxation timescale<br />
distributions <strong>of</strong> GCs with LMXBs were different from GCs with LMXBs at the 6.8σ,<br />
4.6σ, and 2.4σ level; the equivalent test on Galactic GCs indicates a difference <strong>of</strong><br />
2.0σ. We found no significant differences (1.3σ) between the half-mass relaxation<br />
timescales <strong>of</strong> GCs in the “Complete sample” and GCs with fainter LMXBs.<br />
257
6.3.6 Dynamical Rates<br />
There are two dynamical rates that could effect formation or evolution <strong>of</strong> LMXBs.<br />
The stellar crossing rate (S ∝ M 1/2 r −3/2 ) and the binary encounter rate (Γh ∝<br />
M 3/2 r −5/2 ). Since GCs that are more massive and smaller in extent are more likely<br />
to contain LMXBs, it is clear that both <strong>of</strong> these rates would be higher in GCs with<br />
LMXBs compared to GCs without LMXBs (Fig. 6.5 and 6.4). The median values <strong>of</strong> S<br />
were 0.74 kyr −1 for GCs without LMXBs and 1.8 kyr −1 (Detected sample), 2.0 kyr −1<br />
(SNR sample), and 1.8 kyr −1 (Complete sample) for GCs with LMXBs, corresponding<br />
to 16.9σ, 13.3σ, and 7.8σ differences. For Γh, the median values were were 6.9 × 10 5<br />
for GCs without LMXBs and 7.3 × 10 6 (Detected sample), 7.9 × 10 6 (SNR sample),<br />
and 6.4×10 6 (Complete sample) for GCs with LMXBs, corresponding to 17.1σ, 13.2σ,<br />
and 7.7σ differences. We found no significant differences (0.1σ) between either <strong>of</strong> the<br />
dynamical rates <strong>of</strong> GCs in the Complete sample and GCs with fainter LMXBs.<br />
6.4 Multi-Variable Relation Between LMXBs and<br />
GCs<br />
6.4.1 Technique<br />
Since several properties appear to affect the probability that a GC contains an<br />
LMXB, it is important to simultaneously account for these properties. Based on<br />
Figure 6.6 and the relatively small percentage <strong>of</strong> GCs falsely matched to LMXBs<br />
λf, we have assumed the expected (true) number <strong>of</strong> LMXBs in a GC (λt) has the<br />
258
following dependence on GC properties:<br />
<br />
M<br />
λt = A<br />
M⊙<br />
β<br />
259<br />
ɛ δ (G475−Z850) r<br />
10 , (6.6)<br />
1 pc<br />
where we fit the normalization (A) and indices (β, δ, and ɛ). Here, r can either be the<br />
measured half-light radius rh or the corrected half-mass radius rh,cor. Our approach<br />
differs from the fitting performed in ACSVCS3; we choose to fit the expected numbers<br />
<strong>of</strong> LMXBs per GC, as opposed to the probability a GC contains an LMXB. The<br />
probability must saturate at unity, whereas the expected number can be unlimited;<br />
this makes it easier to fit simple functions (e.g., power-laws) to the expected number<br />
and compare with Galactic results. The two approaches give the same results when<br />
λt is small. Another difference is that we include a term to account for GCs falsely<br />
matched to LMXBs, λ = λf + λt.<br />
The expected number <strong>of</strong> LMXBs in a GC can be converted to a probability that<br />
there are no LMXBs,<br />
and the probability that there is at least one LMXB,<br />
PnX = exp(−λ) , (6.7)<br />
PX = 1 − exp(−λ) . (6.8)<br />
One can then vary the parameters to maximize the log likelihood,<br />
ψ = ln<br />
<br />
nX<br />
PnX<br />
<br />
X<br />
PX<br />
<br />
, (6.9)<br />
where the products are taken over the lists <strong>of</strong> GCs with no LMXBs and GCs with<br />
LMXBs. Given that we did not find a difference in the masses, colors, or sizes <strong>of</strong> GCs
Table 6.4. Fits <strong>of</strong> the Expected Number λt <strong>of</strong> LMXBs per GC<br />
λt ∝ M β 10 δ (G475−Z850) r ɛ<br />
Row β δ ɛ ψ ∆ d<strong>of</strong><br />
r = rh<br />
1 [0] [0] [0] -1131.1 0<br />
2 1.027 +0.063<br />
−0.061 [0] [0] -986.0 1<br />
3 [0] 0.64 +0.12<br />
−0.11 [0] -1113.5 1<br />
4 1.009 +0.060<br />
−0.059 0.77 +0.13<br />
−0.13 [0] -967.2 2<br />
5 [0] [0] −1.50 +0.20<br />
−0.20 -1101.2 1<br />
6 1.237 +0.076<br />
−0.075<br />
0.52 +0.15<br />
−0.15<br />
−2.22 +0.24<br />
−0.25 -918.4 3<br />
r = rh,cor<br />
7 [0] [0] −1.14 +0.20<br />
−0.21 -1113.6 1<br />
8 1.237 +0.076<br />
−0.075<br />
0.90 +0.15<br />
−0.14<br />
−2.20 +0.31<br />
−0.36 -918.4 3<br />
with LMXBs in the Complete sample as compared to those GCs with fainter LMXBs,<br />
we first choose to use the better statistics provided by the Detected sample to fit the<br />
indices. Given the widely different luminosity limits in the Detected sample, we do<br />
not believe the normalization we fit is physically meaningful. To derive a physically<br />
meaningful normalization, we apply our derived exponents to the Complete sample.<br />
Since the log likelihood can be related to ∆χ 2 , (−2∆ψ = ∆χ 2 ), we use the change<br />
in log likelihood for one degree <strong>of</strong> freedom (d<strong>of</strong>) to determine one-dimensional fitting<br />
errors (1σ) on each varying parameter.<br />
We display the results <strong>of</strong> our fits to the Detected sample in Table 6.4, where<br />
bracketed numbers indicate that an index was frozen to that number. Once a form<br />
for λt as a function <strong>of</strong> mass, color, and radius has been determined, we can use this<br />
expectation to predict the fraction <strong>of</strong> GCs having an LMXB as a function <strong>of</strong> each <strong>of</strong><br />
the GC properties. These predictions can be compared to the plots <strong>of</strong> the variation<br />
260
<strong>of</strong> this probability with individual properties in Figure 6.6. For each <strong>of</strong> the binned<br />
data points in each <strong>of</strong> the panels, we apply the best-fit expectation calculated for<br />
each <strong>of</strong> other properties <strong>of</strong> the GCs in the binned data point, and then compute the<br />
expected fraction integrated over that bin. This is compared to the actual fraction<br />
for the bin, and the contribution to χ 2 from that bin is determined. Since we do<br />
not consider the dependence <strong>of</strong> λt on galactocentric distance, we did not include that<br />
panel’s contribution to χ 2 . Since the χ 2 <strong>of</strong> that panel ranged from 4.2–11.4 for 10<br />
d<strong>of</strong>, this is justified. In this way, we can determine whether the best-fit expectation<br />
function fits the binned data in Figure 6.6 adequately. The results are shown in<br />
Figures 6.8 and 6.9.<br />
6.4.2 Effect <strong>of</strong> GC Mass and Color<br />
We first established a baseline assuming that the expected number <strong>of</strong> LMXBs per<br />
GC has no dependence on the GC properties (Table 6.4, row 1); our binned χ 2 was<br />
402.4 for 29 d<strong>of</strong>. We next individually varied the mass and color indices (Table 6.4,<br />
rows 2 and 3); mass clearly had the largest effect (−2∆ψ = 290.2); however, its<br />
binned χ 2 was still as large as 158.6 for 28 d<strong>of</strong>. If we included the effects <strong>of</strong> mass<br />
and color simultaneously (Table 6.4, row 4), we had a much improved fit from the<br />
mass-only fit (−2∆ψ = 37.6). We display this fit in Figure 6.8, which has a binned<br />
χ 2 <strong>of</strong> 106.4 for 27 d<strong>of</strong>. Although the effect <strong>of</strong> color on λt was included in this fit,<br />
the resulting expression does not provide a very good fit to the dependence <strong>of</strong> the<br />
fraction on color alone (Figure 6.8, upper right panel). The χ 2 is 26.5 for 10 bins in<br />
this figure. In general, the dependence <strong>of</strong> λt on mass and color does not adequately<br />
describe the observed number <strong>of</strong> LMXBs per GC as a function <strong>of</strong> the observed GC<br />
properties. Some variation with another property is required.<br />
261
Fig. 6.8.— Identical to Figure 6.6, except with the results <strong>of</strong> fitting the dependence<br />
<strong>of</strong> the expected number <strong>of</strong> LMXBs on GC mass and color (Table 6.4, row 4) overlaid.<br />
Note that fitting the effects <strong>of</strong> mass and color alone does not reproduce the observed<br />
dependence <strong>of</strong> the probability on radius or color very well.<br />
6.4.3 Effect <strong>of</strong> GC Size<br />
There are two GC sizes we considered in our fits: the half-light radius (r = rh),<br />
and the half-mass radius (r = rh,cor). Fitting half-light radius alone (Table 6.4, row<br />
5) leads to a better fit than fitting color alone; however, given the correlation between<br />
color and half-light radius, it is not clear if this is due in part to the dependence on<br />
color or a real dependence on the cluster size. On the other hand, only fitting the<br />
half-mass radius (Table 6.4, row 7) is nearly equivalent to only fitting the color (row<br />
3). This is consistent with the picture developed from the Wilcoxon tests.<br />
262
Fig. 6.9.— Identical to Figure 6.6, except with the results <strong>of</strong> fitting the dependence <strong>of</strong><br />
the expected number <strong>of</strong> LMXBs on GC mass, color, and half-mass radius (Table 6.4,<br />
row 8) overlaid. Note that simultaneously fitting the effects <strong>of</strong> GC mass, color, and<br />
half-mass radius reproduces the observed dependence <strong>of</strong> the probability on all <strong>of</strong> the<br />
observed parameters reasonably well.<br />
6.4.4 Simultaneous Effect <strong>of</strong> GC Mass, Color, and Size<br />
The best fits come from simultaneously fitting the effects <strong>of</strong> mass, color, and radius<br />
(Table 6.4, rows 6 and 8). Compared to just fitting the effects <strong>of</strong> mass and color, the<br />
fits are greatly improved (−2∆ψ = 97.6), and the binned χ 2 values are reasonable<br />
(35.0 for half-light radius and 20.2 for half-mass radius, both with 26 d<strong>of</strong>). Regardless<br />
<strong>of</strong> which size is chosen, the mass and radius exponents are the same. The addition <strong>of</strong><br />
the radius actually increases the mass exponent beyond the fitting errors one derives<br />
if radius is ignored. The color index also differs when size is ignored. If the half-light<br />
radius is used, one finds a smaller index; however, we believe the correlation between<br />
263
half-light radius and color affects this fit, so that this does not give an accurate view<br />
<strong>of</strong> the dependence on the size <strong>of</strong> the cluster. When the half-mass radius is used, one<br />
finds a larger index; however, the increase is only significant at the ∼1σ level. The<br />
sizes <strong>of</strong> GCs play a critical role in not only affecting the number <strong>of</strong> LMXBs per GC,<br />
but also our interpretation <strong>of</strong> how strongly GC mass and color affect the number <strong>of</strong><br />
LMXBs per GC.<br />
We believe that the simultaneous fitting <strong>of</strong> GC masses, colors, and half-mass radii<br />
provide the most physically accurate fit <strong>of</strong> the LMXB-GC connection to date. For<br />
this fit (Figure 6.9), we derive β = 1.237 +0.076<br />
−0.075, δ = 0.90 +0.15<br />
−0.14, and ɛ = −2.20 +0.31<br />
−0.36. We<br />
note that by including the effect <strong>of</strong> GCs falsely matched to LMXBs we increased the<br />
mass exponent by 13%, increased the color index by 16% and decreased the radius<br />
exponent by 16%.<br />
If we require that the expected number <strong>of</strong> LMXBs scales linearly with the mass<br />
(β ≡ 1), the negative log-likelihood function is increased by −2∆ψ = 10.7 for 1 more<br />
d<strong>of</strong>, and the binned χ 2 is 30.9 for 27 d<strong>of</strong>. Thus, we rule out a linear proportionality <strong>of</strong><br />
mass at the 99.89% confidence limit. We discuss the implications <strong>of</strong> this in the next<br />
subsection.<br />
From Figure 6.9, we see that the declining probability for a GC with G475 −Z850 ><br />
1.4 to contain an LMXB can be reproduced although we assume no break in the<br />
relation between color and λ. This suggests that the masses and half-mass radii <strong>of</strong><br />
GCs at these colors may be different than at bluer colors. One possible explanation<br />
is contamination by diffuse stellar clusters, which are redder, fainter cousins <strong>of</strong> GCs<br />
(e.g., Larsen & Brodie 2000; Peng et al. 2006b). Additionally, we note that the small<br />
variations <strong>of</strong> the probability with galactocentric distance are reproduced, even though<br />
the distance played no role in the fit.<br />
264
We used the indices from our best-fit to the Detected sample to determine the<br />
normalization for the Complete sample. Rescaling to the median GC color and radius,<br />
λt = 5.5 × 10 −10<br />
M<br />
M⊙<br />
1.237<br />
265<br />
−2.20 0.90 (G475−Z850−1.2) rh,cor<br />
10 . (6.10)<br />
2.6 pc<br />
Since our method predicts the expected number <strong>of</strong> LMXBs per GCs, we can deter-<br />
mine the likelihood that a GC would contain multiple LMXBs. Note that M15 in<br />
our Galaxy has two active LMXBs (White & Angelini 2001); however, the LMXBs<br />
in M15 have LX ∼ 10 36 erg s −1 and would not be detected at the distances <strong>of</strong> the<br />
galaxies in our sample. We calculate the number <strong>of</strong> GCs containing multiple LMXBs,<br />
<br />
[1−(1+λt)e−λt ] = 1.3. Normalizing this to the number <strong>of</strong> GCs with LMXBs in the<br />
X,nX<br />
Complete sample (61), we estimate that 2.2 +3.9<br />
−1.7% <strong>of</strong> GCs with LMXBs actually con-<br />
tain multiple LMXBs such that their combined luminosity is above 3.2 × 10 38 erg s −1 .<br />
This fraction should increase as the LMXB luminosity limit <strong>of</strong> the sample decreases.<br />
For example, the same calculation for our Detected sample with lower luminosity<br />
LMXBs gives an expected fraction <strong>of</strong> 8.2 +2.0<br />
−1.7% <strong>of</strong> GCs with multiple LMXBs.<br />
6.4.5 Implications <strong>of</strong> Simultaneous Fit<br />
For multivariate datasets, principal component analysis determines the set <strong>of</strong> or-<br />
thogonal eigenvectors, linear combinations <strong>of</strong> the original variables, that minimize the<br />
Euclidean distances to each eigenvector (Murtagh & Heck 1987). The normalized vari-<br />
ances <strong>of</strong> the data projected onto the eigenvectors, the eigenvalues, are used to order<br />
the eigenvectors. The eigenvectors with larger eigenvalues are the best-fit eigenvectors<br />
to the data. Often, only eigenvectors with eigenvalues greater than unity (i.e., those<br />
eigenvectors which are as good fits as the original variables) are retained. Principal<br />
component analysis among the masses, colors, and radii <strong>of</strong> GCs with LMXBs found
two eigenvectors whose eigenvalues were above unity. The first eigenvector has an<br />
eigenvalue <strong>of</strong> 1.22 and is dominated by an approximately equal combination <strong>of</strong> mass<br />
and half-mass radius, while the second eigenvector has an eigenvalue <strong>of</strong> 1.01 and is<br />
dominated by color. Therefore, we break our interpretation <strong>of</strong> the fits into two parts:<br />
an interpretation <strong>of</strong> the variation with color as a metallicity effect, and a discussion<br />
<strong>of</strong> the combined mass and half-mass radius variation as evidence for the dynamical<br />
formation <strong>of</strong> LMXBs in GCs.<br />
Metallicity Effect on the Formation <strong>of</strong> LMXBs<br />
We find a monotonic increase in the expected number <strong>of</strong> LMXBs with GC color<br />
<strong>of</strong> the form λt ∝ 10 0.90+0.15<br />
−0.14 (G475−Z850) . ACSVCS3 found that the probability a GC<br />
contains an LMXB (PX ∝ 10 0.87+0.22<br />
−0.22 (G475−Z850) ) using data from NGC 4486. For small<br />
values <strong>of</strong> the expected number (λt ≪ 1), these two quantities are identical (PX ≈ λt,<br />
eqn. [6.8]). Thus, our slightly different techniques are in good agreement with respect<br />
to the fit to color variation. In ACSVCS3, the color variation was directly converted<br />
into a metallicity variation applying the Bruzual & Charlot (2003) models, which<br />
gives (g475 − z850) ∼ (0.38 ± 0.05) log Z . In this chapter, we converted color to<br />
Z⊙<br />
metallicity following equation (2) <strong>of</strong> Peng et al. (2006a),<br />
log Z<br />
Z⊙<br />
⎧<br />
⎪⎨ −6.21 + (5.14 ± 0.67)(g475 − z850) for g475 − z850 ≤ 1.05 ;<br />
=<br />
⎪⎩ −2.75 + (1.83 ± 0.23)(g475 − z850) for g475 − z850 > 1.05 .<br />
266<br />
(6.11)<br />
We then replaced the 10 (G475−Z850) δ term from equation 6.6 with (Z/Z⊙) δ′ . We find<br />
δ ′ = 0.391 +0.070<br />
−0.067, with no change to the variation with mass or radius. Compared to<br />
fitting the effect <strong>of</strong> mass, radius, and color, the mass, radius, and metallicity fit is<br />
very slightly worst (−2∆ψ = 2.0); however, the binned χ 2 value is still reasonable
(20.3 for half-mass radius, both with 26 d<strong>of</strong>).<br />
There are several ideas that could explain the relation between metallicity and<br />
the likelihood a GC will contain an LMXB, most <strong>of</strong> which were well summarized in<br />
ACSVCS3. First, metal-rich stars may have larger radii and masses compared to<br />
metal-poor stars (Bellazzini et al. 1995), which would make it easier to form LMXBs.<br />
This would increase both the number <strong>of</strong> Roche-lobe overflow systems and the number<br />
<strong>of</strong> binary systems formed. Following Maccarone et al. (2004), we have estimated<br />
that the number <strong>of</strong> Roche-lobe overflow systems has a weak metallicity dependence,<br />
Z 0.11 . The number <strong>of</strong> NS binaries formed by tidal capture goes as Z 0.12 , but may<br />
have a lower exponent for exchange interactions. Thus, this model predicts a Z 0.2<br />
dependence and is inconsistent with our fit.<br />
Ivanova (2006) suggested that the link between metallicity and outer convective<br />
zones was responsible for the increased formation efficiency <strong>of</strong> LMXBs in metal-rich<br />
GC. In this model, metal-poor main-sequence stars lack an outer convective zone.<br />
This absence turns <strong>of</strong>f magnetic breaking. Since magnetic breaking leads to the<br />
strong orbital shrinkage that eventually leads to mass transfer as an LMXB, metal-<br />
poor stars fail to dynamically form many <strong>of</strong> the main-sequence/NS binaries that can<br />
appear as bright LMXBs. Although this model is intriguing, more work must be<br />
done to see if the removal <strong>of</strong> the outer convective zone would predict a power-law<br />
dependence <strong>of</strong> the expected number <strong>of</strong> LMXBs on the GC metallicity.<br />
If metal-rich GCs produce more NSs and BHs per unit mass, the larger number<br />
<strong>of</strong> NSs and BHs could increase the number <strong>of</strong> LMXBs that can form. For instance,<br />
the initial mass function (IMF) could vary with metallicity (Grindlay 1987). Follow-<br />
ing ACSVCS3, we assume a power-law IMF, with the number <strong>of</strong> stars with masses<br />
between m and m + dm varying as N(m) ∝ m −x dm. We also assume that the IMF<br />
267
slope depends on metallicity, dx/d[F e/H] ≡ A. The IMF metallicity dependence<br />
must be A = −0.32 +0.062<br />
−0.072 dex −1 to account for the metallicity dependence <strong>of</strong> the num-<br />
ber <strong>of</strong> LMXBs per GC. As in ACSVCS3, the IMF dependence is in rough agreement<br />
with the analysis <strong>of</strong> LMXBs in the Galactic and M31 GC systems, A ∼ −0.4 dex −1<br />
(Bellazzini et al. 1995), and IMF slope derived for Galactic GCs, A ≈ −0.5 dex −1<br />
(Djorgovski et al. 1993). A metallicity dependent IMF can explain the metallicity<br />
dependence <strong>of</strong> the number <strong>of</strong> LMXBs per GC. However, we caution that there is also<br />
evidence that massive star IMFs are metallicity independent (e.g., IMFs from OB<br />
associations; Massey et al. 1995).<br />
Irradiation-induced winds, which would be weaker in metal-rich stars due to more<br />
efficient metal line cooling, may affect the number <strong>of</strong> LMXBs observed in metal-richer<br />
systems. Maccarone et al. (2004) presents two basic models which consider the effect<br />
<strong>of</strong> these winds. In the first model, the wind is ejected at the escape velocity <strong>of</strong> the<br />
donor star. At the same accretion rate (i.e., X-ray luminosity), metal-richer stars<br />
will have lower mass-loss and longer lifetimes. Thus, the rough predicted metallicity<br />
dependence for the number <strong>of</strong> LMXBs per GC is approximately Z 0.35 . In the second<br />
model, a less dense, higher velocity wind is ejected. In this model, the mass-loss<br />
rates (i.e., lifetimes) <strong>of</strong> metal-poorer and metal-richer stars are about the same, but<br />
the accretion rates are not. Metal-richer stars are more luminous and the rough<br />
predicted metallicity dependence for the number <strong>of</strong> LMXBs per GC is Z ∼0.7(βlf−1) ,<br />
where βlf is the differential X-ray luminosity function slope. Typical values <strong>of</strong> βlf are<br />
1.8–2.2 (Kim & Fabbiano 2004) for a single power law; however, the X-ray luminosity<br />
function may be consistent with a broken power law. At the higher luminosities<br />
(LX > 5 × 10 38 erg s −1 ), βlf = 2.8 ± 0.6. At lower luminosities, where most LMXBs<br />
are βlf = 1.8 ± 0.2. Thus a wide range <strong>of</strong> metallicity exponents are possible, but<br />
268
most are steeper than Z ∼0.4 . Either <strong>of</strong> these models may be consistent with our fit;<br />
however, more detailed work developing irradiation-induced wind models is necessary<br />
to predict the metallicity dependence accurately.<br />
Finally, we note that many <strong>of</strong> the above models assume that the compact object<br />
in the LMXB binaries is a NS. However, our Complete sample contains GC-LMXBs<br />
above 3.2 × 10 38 erg s −1 . Such sources are above the Eddington limit for a hydrogen-<br />
accreting neutron star, and may be BH binaries. These models need to be developed<br />
to include the effects <strong>of</strong> such binary systems.<br />
Dynamical Formation <strong>of</strong> LMXBs in GCs<br />
Since the efficiency <strong>of</strong> the dynamical formation <strong>of</strong> LMXBs in GCs is likely to<br />
depend on a combination <strong>of</strong> the GC mass and size, we plot the two-dimensional<br />
confidence interval <strong>of</strong> the exponents for both properties in Figure 6.10. The effect<br />
<strong>of</strong> GC color was also included in these fits, but is not shown. On top <strong>of</strong> the figure,<br />
we have overlaid three lines: λt ∝ S θ (powers <strong>of</strong> the stellar crossing rate), λt ∝ Γ η<br />
h<br />
(powers <strong>of</strong> the binary encounter rate), and λt ∝ Γh,α = Γhρ α = M 3/2+α r −5/2−3α<br />
h,cor<br />
ACSVCS3 form <strong>of</strong> the binary encounter rate). The mass and radius exponents clearly<br />
indicate that powers <strong>of</strong> the stellar crossing rate do not fit the data.<br />
269<br />
(the<br />
The ACSVCS3 form <strong>of</strong> the binary encounter rate cannot be ruled out when con-<br />
sidering the 2-dimensional confidence interval. However, fitting<br />
<br />
M<br />
λt = A<br />
M⊙<br />
3/2+α −5/2−3α δ ′<br />
rh,cor<br />
Z<br />
1 pc<br />
Z⊙<br />
, (6.12)<br />
we find α = −0.200 +0.066<br />
−0.067 and δ = 0.389 +0.072<br />
−0.068 is a worst fit (−2∆ψ = −4.4) than<br />
fitting mass, radius, and metallicity. With only one more d<strong>of</strong>, this fit is ruled out at<br />
the 96.5% confidence limit. The slightly worst fit is also suggested by the binned χ 2
Fig. 6.10.— Two-dimensional confidence intervals (at 1σ, 90%, and 2σ) <strong>of</strong> the exponents<br />
<strong>of</strong> mass (β) and radius (ɛ) in the fit to the expected number <strong>of</strong> LMXBs per<br />
GC, λ ∝ M β 10δ (G475−Z850) ɛ rh,cor . The cross indicates the best-fit values β and ɛ. The<br />
overlaid lines indicate the dependences <strong>of</strong> three likely dynamical-formation properties<br />
that depend on mass and radius: λt ∝ Γ η<br />
h , λt ∝ Γh,α ≡ Γh ρα , and λt ∝ Sθ . The<br />
power-law dependence on Γh is the most consistent, and a power-law dependence on<br />
S can be ruled out.<br />
value <strong>of</strong> 33.56 for 27 d<strong>of</strong>. We do note that the value <strong>of</strong> α ∼ −0.2 is roughly consistent<br />
with analysis <strong>of</strong> pulsars (Johnston et al. 1992) and low-luminosity X-ray sources in<br />
Galactic GCs (Johnston & Verbunt 1996). We display the 2-dimensional confidence<br />
interval <strong>of</strong> α and δ ′ in Figure 6.11a.<br />
The best fit comes from powers <strong>of</strong> the binary encounter rate. When we fit<br />
λt = A Γ η<br />
δ ′<br />
Z<br />
h<br />
Z⊙<br />
270<br />
, (6.13)<br />
we find η = 0.818 +0.050<br />
−0.049 and δ = 0.389 +0.071<br />
−0.067 has only a slightly worst fit (−2∆ψ =
Fig. 6.11.— (Left:) Two-dimensional confidence intervals (at 1σ, 90%, and 2σ) <strong>of</strong> the<br />
exponents <strong>of</strong> density and metallicity in the fit to the expected number <strong>of</strong> LMXBs per<br />
GC, λ ∝ Γh (M/r3 h,cor )α (Z/Z⊙) δ′<br />
. The crosses indicate the best-fit values <strong>of</strong> α and δ ′ .<br />
(Right:) The confidence intervals for the exponents <strong>of</strong> the binary encounter rate and<br />
metallicity in the fit to the expected number <strong>of</strong> LMXBs per GC, λ ∝ Γ η<br />
δ′<br />
h (Z/Z⊙) .<br />
The crosses indicate the best-fit values <strong>of</strong> δ ′ and η.<br />
−0.6) than fitting mass, radius, and metallicity. Since it has one more d<strong>of</strong>, this is<br />
our preferred fit. Its binned χ 2 value was 22.2 for 27 d<strong>of</strong>. This dependence <strong>of</strong> λt on<br />
binary encounter rate matches the Galactic value found by Pooley et al. (2003) <strong>of</strong><br />
λ ∝ Γ 0.74±0.36 .<br />
The dependence <strong>of</strong> the expected number <strong>of</strong> LMXBs per GC on the encounter<br />
rate is shallower than a linear dependence on Γh. Furthermore, the dependence <strong>of</strong><br />
the expected number <strong>of</strong> Galactic low luminosity X-ray sources (Johnston & Verbunt<br />
1996; Pooley et al. 2003) and radio pulsars (Johnston et al. 1992) per GC on the<br />
encounter rate may also have a shallower than linear dependence on Γ. ACSVCS3<br />
suggested two mechanisms to account for this less than linear dependence on the<br />
encounter rate; it might result from the competing rate <strong>of</strong> destruction <strong>of</strong> binaries, or<br />
it might be due to hardening (shrinking) <strong>of</strong> binaries.<br />
271
If both the formation and destruction rates <strong>of</strong> the close binaries depend on the<br />
encounter rate parameter Γh, then in steady-state the encounter rate would cancel<br />
and the number <strong>of</strong> LMXBs per GC would just be proportional the number <strong>of</strong> stars,<br />
or λt ∝ M. This would be inconsistent with the dependencies <strong>of</strong> λt on mass, radius,<br />
and on Γh which we have found. However, if the destruction rate <strong>of</strong> binaries due<br />
to encounters is comparable to the rate <strong>of</strong> stellar evolution <strong>of</strong> the binaries, then an<br />
intermediate dependence on Γh (between linear and none) might result. Detailed<br />
simulations <strong>of</strong> binary formation, evolution, and destruction in GCs are needed to test<br />
this hypothesis.<br />
During exchange interactions, the orbits <strong>of</strong> wide binaries can be reduced, particu-<br />
larly in denser clusters. Following ACSVCS3, the binary encounter cross-section, C,<br />
can be written as a combination <strong>of</strong> the cross-section for tidal capture, σ2, and the<br />
cross section for binary exchange interactions, σ3 ζ(ρ), where ζ(ρ) encapsulates the<br />
effect <strong>of</strong> hardening as a function <strong>of</strong> density. If binary hardening is responsible for<br />
α = −0.2, then C = σ2 + ζ(ρ)σ3 ∝ ρ −0.2 . This would yield ζ(ρ) = (µ ρ −0.2 − σ2)/σ3,<br />
where µ is a consant, as a constraint on predictions for binary hardening.<br />
6.5 Conclusions<br />
We have compared the masses, colors, sizes, and galactocentric distances <strong>of</strong> 270<br />
GCs that contain LMXBs and 6488 GCs that do not contain LMXBs in a sample<br />
<strong>of</strong> eleven galaxies. There are clear differences between the masses, colors, and radii<br />
<strong>of</strong> GCs in these two samples, while the role <strong>of</strong> galactocentric distance has at most<br />
a weak effect. There is no significant difference between the masses, colors, or sizes<br />
<strong>of</strong> 61 GCs that contain LMXBs in the Complete sample and 209 GCs with fainter<br />
LMXBs; thus, there is no evidence that luminous and fainter LMXBs are affected<br />
272
differently by the properties <strong>of</strong> the GC they inhabit.<br />
We clearly show that GCs that are more massive and redder are more likely to<br />
contain LMXBs, confirming the findings <strong>of</strong> Kundu et al. (2003) and Sarazin et al.<br />
(2003). Although we find that red-GCs are 3.15±0.54 times as likely to have LMXBs<br />
as blue-GCs, we argue that the detailed dependence is due to its color, rather than<br />
the population to which it belongs. We believe this is the strongest evidence to date<br />
that GC metallicity affects LMXB formation and evolution.<br />
With the half-mass radius, we calculate the relaxation timescale. In contrast to<br />
Galactic GCs (BIS+2006), we find a large number <strong>of</strong> GCs that contain LMXBs have<br />
relaxation times > 2.5 Gyr. Based on the results from our sample, it does not appear<br />
necessary for GCs to survive for more than five relaxation timescales in order to<br />
produce LMXBs.<br />
Most notedly, we find that GCs that have smaller half-light radii or half-mass radii<br />
are more likely to contain LMXBs. This chapter presents the first clear indication<br />
that GC half-mass radius affects the likelihood a GC will contain an LMXB.<br />
Simultaneous fits <strong>of</strong> the dependence <strong>of</strong> the expected number <strong>of</strong> LMXBs per GC<br />
on the GC mass, color, and radius gave<br />
λt ∝ M 1.237+0.076<br />
−0.075 10 0.90+0.15<br />
−0.14 (G475−Z850) −2.20<br />
r +0.31<br />
−0.36<br />
273<br />
h,cor . (6.14)<br />
Including the radius is important because fitting mass and color alone does not provide<br />
an adequate fit to the expected number <strong>of</strong> LMXBs, and the form <strong>of</strong> the dependence<br />
on mass and color changes when the effects <strong>of</strong> the size are included. The simplest<br />
model for LMXBs, that the number <strong>of</strong> LMXBs per GC is linearly proportionality to<br />
GC mass, can be ruled out at the 99.89% confidence limit.
For our Complete sample, LX > 3.2 × 10 38 erg s −1 , we find<br />
λt = 5.5 × 10 −10<br />
M<br />
M⊙<br />
1.237<br />
274<br />
−2.20 0.90 (G475−Z850−1.2) rh,cor<br />
10 , (6.15)<br />
2.6 pc<br />
which predicts that 2.2 +3.9<br />
−1.7% <strong>of</strong> GCs with LMXBs actually contain multiple LMXBs<br />
such that their combined luminosity is above 3.2 × 10 38 erg s −1 . Thus, we predict that<br />
most GCs with high X-ray luminosities contain a single LMXB.<br />
Principle components analysis is used to show that the dependence <strong>of</strong> the expected<br />
number <strong>of</strong> LMXBs per GC on mass, color, and radius is mainly due to a dependence<br />
on a combination <strong>of</strong> mass and radius, and a dependence on color. We show that this<br />
result implies that the dependence on mass, color, and size is essentially equivalent<br />
to a dependence on the binary encounter rate Γh and the metallicity Z. The best-fit<br />
form is<br />
λt = A Γ 0.818+0.050<br />
−0.049<br />
h<br />
Z<br />
Z⊙<br />
0.389 +0.071<br />
−0.067<br />
. (6.16)<br />
We believe that this is the most direct evidence to date that dynamical formation<br />
plays a primary role in forming LMXBs in the dense stellar environs <strong>of</strong> GCs.<br />
The Γh exponent is consistent with that from low-luminosity X-ray sources in<br />
Galactic GCs (Pooley et al. 2003), but inconsistent with the simple theoretical pre-<br />
diction that the number <strong>of</strong> LMXBs per GC be linearly proportional to Γh. The hard-<br />
ening <strong>of</strong> binaries could explain the shallower dependence we observe. Alternatively,<br />
our use <strong>of</strong> Γh as a proxy for the encounter rate may affect the detailed dependence,<br />
particularly if core-collapsed extragalactic GCs preferentially contain LMXBs. On-<br />
going work with GCs and LMXBs in Centaurus A will test our use <strong>of</strong> Γh.<br />
The metallicity exponent is most consistent with either a metallicity dependent<br />
variation in the number <strong>of</strong> NSs/BHs per GC, such as one might find in a metallicity
dependent IMF (Grindlay 1987), or effects from an irradiation induced wind Mac-<br />
carone et al. (2004). The magnetic braking model <strong>of</strong> Ivanova (2006) may be consistent;<br />
however, this model needs to be developed over a wide range <strong>of</strong> metallicities.<br />
The combination <strong>of</strong> ongoing and upcoming deep CXO observations and wide-field<br />
HST-ACS observations <strong>of</strong> NGC 3379, 4278, 4365, 4697, and 5128 will be essential in<br />
extending our ability to test the LMXB-GC connection to lower X-ray luminosities<br />
across entire galaxies. The greater number <strong>of</strong> GC-LMXBs will more tightly constrain<br />
the GC-LMXB connection and the theoretical models to explain it. The spatial<br />
distribution <strong>of</strong> GC-LMXBs and field-LMXBs may determine the level at which GC-<br />
LMXBs that have since been removed from their GC birthplaces contribute to the<br />
field population <strong>of</strong> LMXBs. It would also be very useful to extend the studies <strong>of</strong><br />
LMXBs in early-type galaxies to include more lenticular galaxies. Our understanding<br />
<strong>of</strong> difference in the GC-LMXB connection between elliptical and lenticular galaxies<br />
is limited by the small number <strong>of</strong> lenticular galaxies observed with CXO. This limits<br />
our ability to use LMXBs to trace the star-formation history <strong>of</strong> galaxies.<br />
275
Chapter 7<br />
Summary and Future Directions<br />
7.1 Summary<br />
We have used the Chandra X-ray Observatory to resolve the X-ray content <strong>of</strong><br />
nearby early-type galaxies into low-mass X-ray binaries (LMXBs) and diffuse inter-<br />
stellar gas. In particular, we present detailed studies <strong>of</strong> the LMXBs and diffuse gas in<br />
four early-type galaxies and a study <strong>of</strong> the connection between LMXBs and globular<br />
clusters (GCs) in eleven early-type galaxies. We now summarize our results organized<br />
by scientific topic.<br />
7.1.1 Luminosity Functions <strong>of</strong> Low-Mass X-Ray Binaries<br />
Chandra allows us to measure the luminosity functions (LFs) <strong>of</strong> LMXBs in early-<br />
type galaxies for the first time. These complement the LFs derived for LMXBs in<br />
the Milky Way and Andromeda galaxy, local galaxies that are still undergoing star-<br />
formation. Among LFs fit to early-type galaxies, Sarazin et al. (2001) first presented<br />
a broken power-law fit with a break at 3 × 10 38 ergs s −1 , near the Eddington limit <strong>of</strong><br />
276
a 1.4M⊙ neutron star (NS). They suggested that such a break might be universal.<br />
In our detailed studies <strong>of</strong> NGC 4365, NGC 4382, and NGC 4697 we detect 99, 58,<br />
and 158 sources respectively. From our results it is clear that these early-type galaxies<br />
are fit by power law LFs with little contribution above ∼ 10 39 ergs s −1 . The broken<br />
power-law LF does not seem to be universal. In NGC 4365 and NGC 4382, the best-fit<br />
LF is a cut<strong>of</strong>f power law whose cut<strong>of</strong>f luminosity is ≈ 0.9−3.1×10 39 ergs s −1 . Although<br />
a cut<strong>of</strong>f power law whose cut<strong>of</strong>f luminosity is about half that <strong>of</strong> the above galaxies is<br />
an acceptable fit for LMXBs in NGC 4697, a broken power law at ∼ 10 38 ergs s −1 is<br />
a better fit. There are two implications if the non-universality <strong>of</strong> a broken power-law<br />
proves to be true. First, the break luminosity cannot be used to estimate distances<br />
as suggested in Sarazin et al. (2001). Second, some galaxy-wide property must affect<br />
the shape <strong>of</strong> the LF. For example, the star formation history might affect the number<br />
and types <strong>of</strong> LMXBs formed.<br />
In these galaxies, we did not find a significant number <strong>of</strong> Ultra-Luminous X-ray<br />
sources (ULXs) with LX > 2 × 10 39 ergs s −1 . The small numbers <strong>of</strong> such sources<br />
seen in these galaxies are consistent with background AGNs. This appears to be<br />
a characteristic <strong>of</strong> LMXBs in early-type galaxies (Irwin et al. 2003); however, our<br />
observation <strong>of</strong> NGC 1600 may prove to be an exception to this rule. Of the 71<br />
detected sources in this observation, 21 are ULX candidates. We expect that only<br />
11±2 are unrelated foreground/background sources. NGC 1600 may have the largest<br />
number <strong>of</strong> ULX candidates in an early-type galaxy to date; however, cosmic variance<br />
in the number <strong>of</strong> background AGN cannot be ruled out at this time. We also found<br />
evidence for a large number <strong>of</strong> lower luminosity LMXBs that we were unable to<br />
resolve, which may support there being a large number <strong>of</strong> ULXs.<br />
277
7.1.2 The Connection Between Globular Clusters and Low-<br />
Mass X-ray Binaries<br />
Low-mass X-ray binaries form efficiently in GCs. Our study <strong>of</strong> the connection<br />
between LMXBs and GCs in NGC 4697 was a trial study for our more developed sur-<br />
vey. By combining Chandra X-ray Observatory and Hubble Space Telescope-Advanced<br />
Camera for Surveys (HST-ACS) observations <strong>of</strong> early-type galaxies, the most accurate<br />
identification <strong>of</strong> LMXBs and GCs to date allows us to shed critical light on the GC-<br />
LMXB connection. We use a study <strong>of</strong> 270 GCs with LMXBs and 6,488 GCs without<br />
detectable X-ray emission from a sample <strong>of</strong> eleven massive early-type galaxies in the<br />
Virgo cluster. Globular clusters that are more massive, are redder, and have smaller<br />
radii are more likely to contain LMXBs. Unlike Galactic GCs, a large number <strong>of</strong> GCs<br />
with LMXBs have relaxation times > 2.5 Gyr; GCs do not need to survive for more<br />
than five relaxation timescales to produce LMXBs. The expected number <strong>of</strong> LMXBs<br />
per GC (λ) is found to vary with the GC mass, color, and half-mass radius as<br />
λ ∝ M 1.24±0.08 10 0.9+0.2<br />
−0.1 (G475−Z850) −2.2<br />
r +0.3<br />
−0.4<br />
278<br />
h,cor . (7.1)<br />
Earlier studies had suggested that the number <strong>of</strong> LMXBs per GC might just be<br />
linearly proportional to GC mass; we are able to rule out this simple dependence.<br />
Based on the expected number <strong>of</strong> LMXBs per GC, we predict that most GCs with<br />
high X-ray luminosities contain a single LMXB. The detailed dependence <strong>of</strong> λ on GC<br />
properties appears mainly due to a dependence on a combination <strong>of</strong> mass and radius,<br />
and a dependence on color. We show that these two dependencies are essentially
equivalent to a dependence on the binary encounter rate Γh and the metallicity Z:<br />
279<br />
λ ∝ Γ 0.82±0.05<br />
h Z 0.39±0.07 . (7.2)<br />
We believe our analysis is the most direct evidence to date that LMXBs are formed by<br />
dynamical processes in GCs. This is also the strongest evidence that metallicity plays<br />
an important role in the evolution <strong>of</strong> LMXBs in GCs. The encounter rate dependence<br />
is consistent with results for Galactic X-ray sources and radio pulsars in GCs. Binary<br />
hardening in GCs can explain this shallower than linear dependence for LMXBs, faint<br />
Galactic X-ray sources, and radio pulsars. However, we note that our use <strong>of</strong> the large-<br />
scale encounter rate parameter Γh may underestimate the encounter rate, particularly<br />
in core-collapsed GCs. The validity <strong>of</strong> Γh will be tested with ongoing observations <strong>of</strong><br />
the nearby Cen A galaxy. The metallicity dependence is most consistent with either<br />
a metallicity dependent variation in the number <strong>of</strong> neutron stars and black holes per<br />
GC or effects from irradiation induced winds.<br />
Since a large number <strong>of</strong> LMXBs are associated with GCs in early-type galaxies, the<br />
distribution <strong>of</strong> GCs will affect the observed distribution <strong>of</strong> LMXBs. For instance, GCs<br />
have a broader spatial distribution than the optical starlight in early-type galaxies.<br />
Thus, we could reproduce the broad spatial distribution <strong>of</strong> the LMXBs in NGC 4365<br />
and NGC 4382 if a large number <strong>of</strong> LMXBs are associated with GCs, particularly at<br />
larger galactocentric distances. Similarly, a large number <strong>of</strong> GCs in NGC 1600 could<br />
explain its large number <strong>of</strong> unresolved and resolved point sources.<br />
7.1.3 Spectra <strong>of</strong> Low-Mass X-Ray Binaries<br />
The spectra <strong>of</strong> LMXBs can be represented by either a bremsstrahlung model<br />
(NGC 4697: kT ∼ 9 keV) or power law model (NGC 1600, NGC 4365, and NGC 4382:
Γ ∼ 1.5–1.8). From our observations <strong>of</strong> NGC 4697, we find that GC-LMXBs are bet-<br />
ter fit with higher temperatures and greater absorbing columns compared to the<br />
field-LMXBs. Similarly, we find a difference between X-ray fainter and brighter<br />
LMXBs. The fainter LMXBs tend to have smaller absorbing columns, while the<br />
brighter LMXBs tend to have a small excess in absorption, which may be due to<br />
accreting material.<br />
7.1.4 Variability in Low-Mass X-Ray Binaries<br />
The study <strong>of</strong> variability plays a key role in understanding the behavior <strong>of</strong> Galactic<br />
LMXBs. Although we cannot study variability in the exquisite detail available for<br />
Milky Way LMXBs, we are beginning to probe variability <strong>of</strong> LMXBs in early-type<br />
galaxies (and other X-ray sources in the same FOV).<br />
Individual observations can reveal variability on timescales <strong>of</strong> minutes to hours.<br />
Although this has been traditionally probed with the Kolmogorov-Smirnov (KS) test,<br />
we have also developed a new method to detect flaring sources. This method has been<br />
applied to our observations <strong>of</strong> NGC 4697. Of the two most clearly flaring sources, one<br />
is a foreground star whose flare was also detected by the KS test. The other source<br />
is more interesting. Its flares, which were missed by the KS test, last for ∼ 70 s and<br />
are very super-Eddington for an NS (∼ 6 × 10 39 erg s −1 ). Although this source has<br />
no clear Galactic analog, we suggest it may be a microblazar, a microquasar observed<br />
along the jet axis.<br />
Our multi-epoch observations <strong>of</strong> NGC 4697 were planned to shed light on LMXB<br />
variability in elliptical galaxies over timescales <strong>of</strong> (11) days to (4.6) years. We deter-<br />
mine that 6.7 ± 1.0% <strong>of</strong> the Analysis Sample sources are variable between any two<br />
observations. There is a slight increase in the fraction <strong>of</strong> variable sources with the<br />
280
variability timescale, but it is not found to be statistically significant. The fraction <strong>of</strong><br />
variable sources is roughly consistent with those found in Centaurus A for a 0.5 year<br />
timescale (Kraft et al. 2001) and in NGC 4636 for a day timescale, but is lower than<br />
that found for a 3 year timescale in NGC 4636 (Posson-Brown et al. 2006). When<br />
we consider all five observations simultaneously, we find that ≈ 16 ± 4% <strong>of</strong> sources<br />
exhibit luminosity variability. Among these variable sources, we identify eleven tran-<br />
sient candidates. If all LMXBs in NGC 4697 are long-term transients, they are on<br />
for ∼ 100 yr and have a duty cycle (∼ 7%) comparable to that derived from Galactic<br />
GCs (Heinke et al. 2003). We clearly identify a supers<strong>of</strong>t transient source with no<br />
optical counterpart. Our analysis indicates this source could be consistent with an<br />
accreting BH with a mass in the range <strong>of</strong> ∼(7 × 10 3 –10 6 ) M⊙; however, the origin <strong>of</strong><br />
such a large BH outside <strong>of</strong> the center <strong>of</strong> a galaxy or <strong>of</strong> a GC is a formidable challenge<br />
to our current theories <strong>of</strong> BH formation.<br />
7.1.5 Spectra <strong>of</strong> Diffuse Gas<br />
In NGC 4365 and NGC 4382, two X-ray faint, early-type Virgo Cluster galaxies,<br />
the diffuse gas produces less emission than the LMXBs. The gas from both galaxies<br />
were fit by relatively s<strong>of</strong>t temperatures (kT ∼ 0.6 keV for NGC 4365 and kT ∼ 0.3 keV<br />
for NGC 4382) with subsolar heavy metal abundances. We note that the abundances<br />
were <strong>of</strong>ten poorly constrained due to the limited number <strong>of</strong> counts from the gas. In<br />
NGC 4365, there is some evidence that the temperature <strong>of</strong> the diffuse gas increases<br />
with increasing radius to kT ∼ 0.8 keV.<br />
On the other hand, NGC 1600 is an X-ray bright elliptical at the center <strong>of</strong> a group<br />
<strong>of</strong> galaxies. Although we expect the diffuse gas to dominate the X-ray emission,<br />
the LMXBs may account for ∼ 25–50% <strong>of</strong> the X-ray emission. Despite its greater<br />
281
distance compared to NGC 4365 and NGC 4382, there were enough counts to fit<br />
spectra in eight spatial bins. Rather than finding a temperature gradient, we find<br />
two phases <strong>of</strong> gas. We interpret the s<strong>of</strong>t inner component (a 25 ′′ , kT ∼ 0.85 keV)<br />
as the interstellar medium <strong>of</strong> NGC 1600 and the hotter outer component (a 25 ′′ ,<br />
kT ∼ 1.5 keV) as the intragroup medium <strong>of</strong> the NGC 1600 group.<br />
7.1.6 Gas Pr<strong>of</strong>iles <strong>of</strong> Diffuse Gas<br />
The gas pr<strong>of</strong>iles <strong>of</strong> both NGC 4365 and NGC 4382 are well fit by the standard<br />
beta model pr<strong>of</strong>iles. The pr<strong>of</strong>ile <strong>of</strong> NGC 4382 had a large core radius. We suggest<br />
that the gas in NGC 4382 may be partially supported by rotation.<br />
In the brighter galaxy NGC 1600, the gas pr<strong>of</strong>ile is best fitted by a double beta<br />
model. This surface brightness pr<strong>of</strong>ile is consistent with the inner component being<br />
due to interstellar medium in the galaxy, and the outer component being intragroup<br />
gas. The X-ray image <strong>of</strong> NGC 1600 also showed several interesting structures. Excess<br />
emission to the northeast <strong>of</strong> NGC 1600 is probably associated with the center <strong>of</strong> the<br />
NGC 1600 group. On smaller scales, we find a central region <strong>of</strong> excess emission<br />
which is roughly cospatial with Hα and dust filaments immediately west <strong>of</strong> the center<br />
<strong>of</strong> NGC 1600. This correlation <strong>of</strong> hot and cool gas could be explained by thermal<br />
conduction, radiative cooling, or mixing <strong>of</strong> the hot and cool gas components. Finally,<br />
we find holes roughly coincident with the lobes <strong>of</strong> the NGC 1600 radio source. This<br />
source may be blowing bubbles in the hot gas.<br />
7.2 Future Directions<br />
There are a large number <strong>of</strong> projects, ongoing and planned, that have resulted<br />
from the studies in this dissertation.<br />
282
7.2.1 X-ray Properties <strong>of</strong> the GC-LMXB connection<br />
The most immediate project involves examining the Virgo cluster early-type<br />
galaxy sample <strong>of</strong> LMXBs from Chapter 6 in more detail. Our study <strong>of</strong> NGC 4697<br />
raised some interesting questions. We will compare the X-ray luminosities <strong>of</strong> GC-<br />
LMXBs and field-LMXBs to test if GC-LMXBs tend to be brighter. Additionally,<br />
we will test whether the X-ray spectra <strong>of</strong> field-LMXBs, blue-GC-LMXBS, and red-<br />
GC-LMXBs are different. Finally, we will look for other difference between these<br />
populations that were not apparent in our analysis <strong>of</strong> NGC 4697.<br />
7.2.2 X-ray Observations <strong>of</strong> Early-type Galaxies<br />
We also intend to use our very deep data set on NGC 4697 to study the diffuse<br />
gas emission in this X-ray-faint elliptical. The increased sensitivity from multiple<br />
epochs does not apply only to the detection <strong>of</strong> LMXBs. Our deeper sensitivity limits<br />
to LMXBs will better isolate the diffuse gas for spectral fitting. We should be able<br />
to better constrain temperatures and abundances.<br />
It is important that single-epoch observations <strong>of</strong> new early-type galaxies contin-<br />
ues. In particular, we have probed early-type galaxies in the Virgo Cluster much<br />
better than we have in the Fornax Cluster. Although further than the Virgo Cluster,<br />
the Fornax Cluster is still near enough that reasonable X-ray detection limits can be<br />
achieved with Chandra. Fornax is a more compact, more regular, and denser cluster<br />
than Virgo. These differences should affect the histories <strong>of</strong> galaxy and star forma-<br />
tion. A comparison <strong>of</strong> galaxy samples from these two clusters will test whether these<br />
differences can be observed in the populations <strong>of</strong> LMXBs.<br />
Although our upcoming XMM X-ray observation <strong>of</strong> NGC 1600 will not have the<br />
spatial resolution <strong>of</strong> our Chandra observations, it will have an increased sensitivity.<br />
283
This will allow us to better probe the diffuse gas now that we know where the bright<br />
sources are. Additionally, the optical monitor on XMM will be useful in testing<br />
whether the candidate ULXs are in fact AGNs.<br />
We believe that one <strong>of</strong> the crucial lessons from our work is the value <strong>of</strong> multi-<br />
epoch strategies for X-ray observations <strong>of</strong> early-type galaxies. Such studies combine<br />
increased sensitivity and the ability to examine variability. To that end, we have<br />
undertaken a multi-epoch study <strong>of</strong> NGC 4365, similar in design to that <strong>of</strong> NGC 4697.<br />
Although NGC 4365 is farther away than NGC 4697, it has a much larger number <strong>of</strong><br />
sources. Preliminary analysis <strong>of</strong> four out <strong>of</strong> five observation has already detected 284<br />
sources. Other groups have also adopted similar observing strategies. Observations<br />
(<strong>of</strong> about twice the total exposure <strong>of</strong> NGC 4365 and NGC 4697) <strong>of</strong> two other early-<br />
type galaxies, NGC 3379 and NGC 4278, are being made publicly available as the<br />
observations occur.<br />
We are also involved in Chandra proposals for multi-epoch observations <strong>of</strong> addi-<br />
tional galaxies. Deep (∼ 1 Ms) observations <strong>of</strong> Cen A will extend the study <strong>of</strong> LMXBs<br />
down to ∼ 10 36 ergs s −1 and better sample variability timescales. Multiple, deep ob-<br />
servations (e.g., 2 × 100 ks) <strong>of</strong> NGC 4697 would give us the opportunity to better<br />
probe its intriguing sources, and provide the strongest variability timescale coverage.<br />
It is important that we continue to observe the same galaxy over multiple years to<br />
understand the long-term variability <strong>of</strong> sources.<br />
7.2.3 Optical Observation <strong>of</strong> Early-type Galaxies<br />
The combination <strong>of</strong> optical observations <strong>of</strong> GCs and X-ray observations <strong>of</strong> LMXBs<br />
were indispensable in probing the GC-LMXB connection. Extending these studies to<br />
more systems will better constrain our understanding, and, perhaps, resolve the cause<br />
284
<strong>of</strong> the metallicity dependence. As in the Virgo Cluster Survey (VCS), a large number<br />
<strong>of</strong> galaxies in the Fornax cluster have been observed by HST-ACS as part <strong>of</strong> the<br />
Fornax Cluster Survey (FCS). We are continuing our collaboration with members <strong>of</strong><br />
the VCS and FCS teams to extend our study <strong>of</strong> the GC-LMXB connection to more<br />
galaxies.<br />
There is a second approach that we have undertaken to extend our knowledge<br />
<strong>of</strong> the GC-LMXB connection. We have obtained HST-ACS observations <strong>of</strong> fields<br />
in NGC 4365 and NGC 4697 that flank the central fields used in Chapter 6. This<br />
will give us nearly complete coverage <strong>of</strong> the GC-LMXBs in these galaxies. Also, we<br />
have been approved for similar multiple-field HST-ACS observations <strong>of</strong> NGC 3379<br />
and NGC 4278. In addition to probing the optical properties <strong>of</strong> the GCs, we will<br />
compare the spatial distributions <strong>of</strong> GCs, and LMXBs in an attempt to understand<br />
the origin <strong>of</strong> field-LMXBs. The history <strong>of</strong> field-LMXBs should be encoded in their<br />
spatial distribution. Some are likely to be primordial binaries; they will follow the<br />
optical light <strong>of</strong> the galaxy. Some LMXBs that formed dynamically in GCs may have<br />
escaped from the GCs they were formed in or had their host GC destroyed after the<br />
LMXB formed; they will have different spatial distributions from the optical light <strong>of</strong><br />
the galaxy.<br />
With our collaborators, we will be examining the GCs and LMXBs in Cen A. This<br />
galaxy is close enough that we should be able to better measure concentrations and<br />
sizes <strong>of</strong> GCs. This will impact our understanding <strong>of</strong> the stellar encounter rate.<br />
Finally, it is critical that multi-epoch X-ray observation <strong>of</strong> a lenticular galaxy<br />
are undertaken with HST-ACS observations. Irwin (2005) has argued that approx-<br />
imately half <strong>of</strong> field-LMXBs in lenticular galaxies may have been formed in GCs.<br />
Comparisons <strong>of</strong> the spatial distribution <strong>of</strong> field-LMXBs and GCs can test this hy-<br />
285
pothesis; however, one must first identify a large number <strong>of</strong> LMXBs and GCs. We<br />
were recently approved for the first Chandra deep observations <strong>of</strong> a lenticular galaxy.<br />
Our multi-epoch observations <strong>of</strong> NGC 1023 should detect large number <strong>of</strong> LMXBs<br />
and explore the variability regime <strong>of</strong> LMXBs in a lenticular galaxy. With HST-ACS<br />
observations, large numbers <strong>of</strong> GCs will also be identified.<br />
7.2.4 Closing Remarks<br />
The study <strong>of</strong> LMXBs and GCs in early-type galaxies requires high spatial reso-<br />
lution in both X-ray and optical wavelengths. It is therefore important that these<br />
studies are undertaken while the facilities to do so (Chandra and Hubble) are still<br />
available. Although (currently planned) future X-ray observatories will have im-<br />
proved sensitivity and energy resolution, there are no planned facilities likely to come<br />
on line within the next two decades that will have spatial resolution comparable or<br />
better than Chandra.<br />
286
Appendix A<br />
Encounter Rate Parameter Γ h<br />
From Hut & Verbunt (1983), the total encounter rate Γ in a GC is related to the<br />
number densities <strong>of</strong> the two interacting populations n1 and n2, the interaction cross<br />
section A, and the GC dispersion velocity v as<br />
<br />
Γ ∝<br />
287<br />
n1 n2 A v dV . (A.1)<br />
Gravitational focusing implies that the interaction cross section for both tidal capture<br />
and binary exchange are proportional to the inverse square <strong>of</strong> the relative velocity,<br />
which will be proportional to the velocity dispersion in a cluster. Thus,<br />
Γ ∝<br />
n1 n2<br />
v<br />
dV ∝ ρ2 0 r 3 c<br />
v<br />
, (A.2)<br />
where the volume integral is approximated by the product <strong>of</strong> the central encounter<br />
rate per unit volume and the core volume <strong>of</strong> the GC. Here, ρ0 is the central mass<br />
density, and rc is the core radius. This assumption relies on the rapid drop <strong>of</strong> stellar<br />
number density with distance from the cluster center. The virial theorem implies
that v ∝ (Mc/rc) 1/2 ∝ rc ρ 1/2<br />
0 , where Mc is the core mass <strong>of</strong> the GC. This is a valid<br />
assumption as the empirically defined fundamental plane <strong>of</strong> GCs appears to reproduce<br />
this relation (McLaughlin 2000). Then, the encounter rate is typically written as<br />
288<br />
Γ ∝ ρ 3/2<br />
0 r 2 c. (A.3)<br />
Since the central densities and core radii <strong>of</strong> extragalactic GCs are difficult to<br />
accurately measure, particularly for those at distances beyond 10 Mpc, it is desirable<br />
to recast the encounter rate in terms <strong>of</strong> the larger scale properties <strong>of</strong> the cluster. A<br />
more easily determined radius is the half-mass radius r ′ h . If r′ h and the total luminosity<br />
can be measured, then is is straightforward to determine the average surface mass<br />
density within r ′ h , which is σh ≡ (1/2)M/[π(r ′ h )2 ]. Using the dimensionless quantities<br />
L = M/ρ0r 3 c and R = r ′ h /rc, we find<br />
Γ ∝ R5/2<br />
L 3/2<br />
M 3/2<br />
(r ′ , (A.4)<br />
h<br />
)5/2<br />
where both L and R depend on the concentration, c = log(rt/rc). If two samples<br />
<strong>of</strong> extragalactic GCs have the same distributions <strong>of</strong> concentrations, one can compare<br />
more easily the following encounter rate parameter,<br />
Γh ≡ σ 3/2<br />
h (r ′ h) 1/2 ∝ M 3/2 (r ′ h) −5/2 . (A.5)<br />
The GC concentration affects the accuracy <strong>of</strong> Γh as a proxy for the encounter<br />
rate through the quantity R 5/2 L −3/2 . This quantity can be calculated given the<br />
polynomial relationships in Appendix B <strong>of</strong> McLaughlin (2000) that apply over the<br />
range 0.5 c 3.6 (Figure A.1). Since R 5/2 L −3/2 varies only between 0.07 and 0.14
Fig. A.1.— Dimensionless quantity R 5/2 L −3/2 as a function <strong>of</strong> concentration, c, for<br />
GCs using the expressions in McLaughlin (2000). This quantity connects estimates<br />
<strong>of</strong> the encounter rate based on core and half-mass radius values, Γ ∝ R 5/2 L −3/2 Γh.<br />
The diamonds (non-core-collapse Galactic GCs) and asterisks (core-collapse Galactic<br />
GCs) indicate comparisons <strong>of</strong> Γ and Γh from the February 2003 revision <strong>of</strong> Harris<br />
(1996). The catalog Harris (1996) is based on arbitrarily adopted c = 2.5 for corecollapse<br />
Galactic GCs. The use <strong>of</strong> the large scale encounter rate parameter Γh will<br />
underestimate the encounter rate for globular clusters with high concentrations (c <br />
1.6).<br />
for 0.5 c 1.6, Γh is a relatively good proxy for the encounter rate Γ over that<br />
concentration range. The use <strong>of</strong> Γh will underestimate the encounter rate in GCs<br />
with higher concentrations (c 1.6).<br />
289
Appendix B<br />
Optical Properties <strong>of</strong> Globular<br />
Clusters<br />
Hubble Space Telescope Advanced Camera for Surveys observations <strong>of</strong> early-type<br />
galaxies can be used to identify globular clusters (GCs) and measure their properties.<br />
This appendix lists the optical properties <strong>of</strong> GCs from the galaxy sample we discuss<br />
in Chapter 6. In Table B.1, we list the 270 GCs that have X-ray emission associated<br />
with a point source within 1 ′′ <strong>of</strong> a GC (i.e., those GCs that contain low-mass X-<br />
ray binaries, LMXBs). Occaisonally two optical sources may be associated with a<br />
single X-ray source. Since we are unable to identify which optical source actually<br />
contains the X-ray source, we do not list the properties <strong>of</strong> GCs in Table B.1 that fall<br />
in this category. For this table, we separately list the GCs associated with LMXBs<br />
in the Complete Sample (LX ≥ 3.2 × 10 38 erg s −1 ) and GCs associated with fainter<br />
LMXBs. We list 6,488 Globular clusters without LMXBs (i.e., no X-ray point source<br />
emission within 1 ′′ ) in Table B.2. For both tables, we list the galaxy and ACS<br />
identification number (ID) in columns one and two. The RA and Dec. as derived<br />
by KINGPHOT (Jordán et al. 2005), are listed in decimal degrees in columns three<br />
290
and four; these positions do not include the astrometric corrections used to match<br />
with the Chandra detected point sources. From these positions, we calculate the<br />
galactocentric distances DGC <strong>of</strong> the GCs (column four). We display the KINGPHOT<br />
derived absolute magnitudes and half-light sizes <strong>of</strong> the GCs in columns six through<br />
eight. The GC properties are used to calculate the probability a source is a GC (Peng<br />
et al. 2006a), which we designate as the GC Class; we only include GCs with a Class<br />
> 0.5.<br />
291
Table B.1. Optical Properties <strong>of</strong> Globular Clusters (With LMXBs)<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
GCs with LMXBs in Complete Sample<br />
NGC 4365 541 186.11881 7.31837 0.09 −7.742 ± 0.407 −8.676 ± 0.085 8.44 ± 4.39 0.73<br />
NGC 4365 741 186.11396 7.32383 0.52 −10.115 ± 0.021 −11.439 ± 0.013 2.78 ± 0.22 1.00<br />
NGC 4365 470 186.12461 7.32130 0.55 −8.307 ± 0.057 −9.524 ± 0.457 2.34 ± 0.38 1.00<br />
NGC 4365 251 186.11883 7.30382 1.01 −7.884 ± 0.041 −9.340 ± 0.022 1.68 ± 0.19 0.97<br />
NGC 4365 836 186.12274 7.34087 1.71 −8.626 ± 0.027 −9.817 ± 0.020 2.48 ± 0.26 1.00<br />
NGC 4365 362 186.10498 7.29307 2.01 −6.061 ± 0.403 −7.573 ± 0.054 1.76 ± 0.52 0.94<br />
NGC 4365 1173 186.08658 7.32721 2.34 −8.576 ± 0.027 −9.889 ± 0.018 1.79 ± 0.14 0.98<br />
NGC 4374 164 186.25522 12.88736 0.72 −9.237 ± 0.022 −10.749 ± 0.014 2.44 ± 0.19 1.00<br />
NGC 4374 377 186.27228 12.89583 0.77 −9.891 ± 0.013 −11.246 ± 0.012 2.69 ± 0.09 1.00<br />
NGC 4374 439 186.27606 12.89223 0.81 −8.601 ± 0.015 −9.485 ± 0.020 2.94 ± 0.10 1.00<br />
NGC 4374 418 186.26621 12.86172 1.79 −7.834 ± 0.034 −8.765 ± 0.037 3.27 ± 0.22 1.00<br />
NGC 4382 531 186.35385 18.20167 0.73 −9.414 ± 0.020 −10.407 ± 0.016 3.02 ± 0.13 1.00<br />
NGC 4406 213 186.55507 12.94780 0.21 −7.765 ± 0.029 −8.659 ± 0.038 2.20 ± 0.19 1.00<br />
NGC 4406 226 186.55645 12.94974 0.28 −7.925 ± 0.028 −9.320 ± 0.029 1.71 ± 0.15 1.00<br />
NGC 4406 227 186.55868 12.95173 0.38 −10.218 ± 0.023 −11.614 ± 0.017 1.56 ± 0.16 0.64<br />
NGC 4406 376 186.53952 12.95120 0.36 −7.418 ± 0.042 −8.460 ± 0.287 2.98 ± 0.33 1.00<br />
NGC 4406 525 186.51509 12.94937 1.15 −7.280 ± 0.026 −8.450 ± 0.026 1.98 ± 0.22 1.00<br />
NGC 4472 509 187.43756 7.99727 0.27 −8.759 ± 0.023 −10.307 ± 0.017 2.02 ± 0.16 1.00<br />
NGC 4472 259 187.44886 7.99043 0.37 −7.903 ± 0.029 −9.392 ± 0.024 2.09 ± 0.18 1.00<br />
NGC 4472 169 187.45994 8.00374 0.53 −9.423 ± 0.027 −10.973 ± 0.023 2.38 ± 0.14 1.00<br />
NGC 4472 120 187.46190 8.00269 0.59 −7.008 ± 0.034 −8.432 ± 0.018 2.40 ± 0.25 1.00<br />
NGC 4472 737 187.42631 8.00214 0.64 −10.134 ± 0.014 −11.563 ± 0.011 2.62 ± 0.09 1.00<br />
NGC 4472 797 187.42325 8.00392 0.75 −7.754 ± 0.022 −9.288 ± 0.028 1.96 ± 0.25 1.00<br />
NGC 4472 665 187.44120 8.02413 0.83 −6.036 ± 0.076 −7.402 ± 0.340 1.82 ± 0.45 0.98<br />
NGC 4472 421 187.43367 7.97794 0.87 −6.676 ± 0.041 −8.295 ± 0.058 2.56 ± 0.27 1.00<br />
NGC 4486 815 187.70518 12.39300 0.08 −8.365 ± 0.018 −9.443 ± 0.031 2.25 ± 0.16 1.00<br />
NGC 4486 731 187.70340 12.39656 0.23 −8.684 ± 0.024 −10.048 ± 0.012 2.04 ± 0.16 1.00<br />
NGC 4486 540 187.69878 12.39311 0.28 −8.553 ± 0.033 −9.995 ± 0.017 1.07 ± 0.16 0.90<br />
NGC 4486 992 187.70885 12.38372 0.30 −9.236 ± 0.018 −10.764 ± 0.017 1.86 ± 0.12 1.00<br />
NGC 4486 960 187.70824 12.40019 0.35 −8.800 ± 0.030 −10.391 ± 0.019 2.59 ± 0.13 1.00<br />
NGC 4486 936 187.70755 12.40068 0.37 −6.569 ± 0.085 −8.010 ± 0.049 2.45 ± 0.34 1.00<br />
NGC 4486 464 187.69707 12.38603 0.38 −9.135 ± 0.022 −10.713 ± 0.011 2.39 ± 0.10 1.00<br />
NGC 4486 983 187.70862 12.38103 0.40 −9.035 ± 0.025 −10.573 ± 0.019 1.73 ± 0.16 1.00<br />
NGC 4486 289 187.69300 12.38986 0.48 −9.744 ± 0.015 −11.042 ± 0.008 2.14 ± 0.11 1.00<br />
NGC 4486 265 187.69246 12.39137 0.50 −9.906 ± 0.025 −10.899 ± 0.017 2.86 ± 0.13 1.00<br />
NGC 4486 1480 187.72188 12.39919 0.67 −7.127 ± 0.030 −8.538 ± 0.023 1.84 ± 0.24 1.00<br />
NGC 4526 95 188.52641 7.69240 1.26 −9.660 ± 0.014 −10.622 ± 0.015 2.41 ± 0.11 1.00<br />
NGC 4552 337 188.91653 12.55421 0.27 −9.692 ± 0.019 −10.682 ± 0.020 2.97 ± 0.10 1.00<br />
NGC 4552 439 188.91412 12.56115 0.63 −9.048 ± 0.127 −10.468 ± 0.387 1.23 ± 0.23 0.85<br />
NGC 4552 322 188.91545 12.54962 0.83 −8.513 ± 0.021 −9.858 ± 0.020 2.26 ± 0.18 1.00<br />
NGC 4552 490 188.90871 12.55732 0.87 −7.426 ± 0.128 −8.869 ± 0.034 2.25 ± 0.28 1.00<br />
NGC 4552 250 188.91879 12.54686 1.22 −7.867 ± 0.028 −9.313 ± 0.029 2.72 ± 0.20 1.00<br />
NGC 4552 141 188.92666 12.54786 1.66 −5.825 ± 0.105 −7.113 ± 0.063 1.70 ± 0.44 0.96<br />
NGC 4552 591 188.90019 12.55883 1.90 −9.404 ± 0.018 −10.534 ± 0.020 2.25 ± 0.11 1.00<br />
NGC 4552 68 188.93683 12.56090 2.57 −8.911 ± 0.031 −9.866 ± 0.014 2.18 ± 0.17 1.00<br />
NGC 4552 431 188.92186 12.58049 3.05 −10.747 ± 0.029 −11.953 ± 0.014 3.33 ± 0.11 1.00<br />
NGC 4621 216 190.51257 11.63987 0.69 −11.485 ± 0.020 −12.884 ± 0.028 3.56 ± 0.10 1.00<br />
NGC 4621 659 190.47670 11.64412 2.86 −6.855 ± 0.052 −8.357 ± 0.062 2.46 ± 0.30 1.00<br />
NGC 4649 420 190.91565 11.54659 0.33 −7.163 ± 0.033 −8.538 ± 0.386 1.38 ± 0.23 0.98<br />
NGC 4649 311 190.91934 11.54508 0.43 −6.480 ± 0.093 −8.049 ± 0.058 2.46 ± 0.40 1.00<br />
NGC 4649 667 190.90820 11.55774 0.51 −9.484 ± 0.030 −10.745 ± 0.016 2.38 ± 0.17 1.00<br />
Continued on Next Page. . .<br />
292
Table B.1—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4649 677 190.90998 11.56201 0.59 −8.521 ± 0.030 −9.976 ± 0.018 1.96 ± 0.12 1.00<br />
NGC 4649 438 190.92410 11.56417 0.71 −8.752 ± 0.019 −10.260 ± 0.020 2.02 ± 0.11 1.00<br />
NGC 4649 727 190.89541 11.54102 1.25 −6.502 ± 0.044 −7.937 ± 0.041 2.10 ± 0.26 1.00<br />
NGC 4649 416 190.90584 11.52870 1.38 −9.598 ± 1.480 −10.143 ± 0.047 1.99 ± 0.31 1.00<br />
NGC 4649 987 190.89194 11.56685 1.47 −8.214 ± 0.020 −9.655 ± 0.018 1.67 ± 0.15 1.00<br />
NGC 4649 856 190.88931 11.54429 1.47 −9.258 ± 0.023 −10.533 ± 0.016 1.77 ± 0.20 1.00<br />
NGC 4649 999 190.88117 11.55065 1.83 −8.961 ± 0.016 −10.162 ± 0.022 2.77 ± 0.14 1.00<br />
NGC 4697 106 192.13838 -5.79490 0.63 −5.018 ± 0.097 −6.496 ± 0.108 1.05 ± 0.22 0.72<br />
NGC 4697 487 192.16386 -5.80192 0.71 −8.194 ± 0.027 −9.488 ± 0.020 1.16 ± 0.06 1.00<br />
NGC 4697 74 192.12846 -5.81019 1.15 −6.832 ± 0.032 −8.106 ± 0.410 0.81 ± 0.10 0.68<br />
GCs with LMXBs not in Complete Sample<br />
NGC 4365 18 186.13289 7.30267 1.54 −9.265 ± 0.016 −10.417 ± 0.011 2.22 ± 0.13 1.00<br />
NGC 4365 50 186.12117 7.29167 1.90 −9.120 ± 0.011 −10.546 ± 0.014 2.16 ± 0.08 0.99<br />
NGC 4365 103 186.13127 7.30771 1.21 −9.865 ± 0.025 −11.203 ± 0.012 2.40 ± 0.18 1.00<br />
NGC 4365 213 186.12503 7.30906 0.82 −9.345 ± 0.025 −10.899 ± 0.016 2.28 ± 0.23 1.00<br />
NGC 4365 218 186.11174 7.29357 1.80 −9.943 ± 0.022 −11.243 ± 0.014 2.48 ± 0.21 1.00<br />
NGC 4365 271 186.13701 7.32649 1.52 −9.315 ± 0.019 −10.672 ± 0.017 2.41 ± 0.27 1.00<br />
NGC 4365 279 186.10784 7.29249 1.96 −9.542 ± 0.021 −10.904 ± 0.020 3.17 ± 0.12 1.00<br />
NGC 4365 290 186.13315 7.32316 1.17 −9.564 ± 0.616 −10.751 ± 0.034 2.18 ± 0.43 0.99<br />
NGC 4365 300 186.12236 7.31085 0.60 −9.270 ± 0.016 −10.536 ± 0.014 1.95 ± 0.15 0.98<br />
NGC 4365 358 186.12948 7.32192 0.89 −9.769 ± 0.030 −10.937 ± 0.020 2.70 ± 0.29 1.00<br />
NGC 4365 369 186.12251 7.31423 0.43 −9.284 ± 0.020 −10.194 ± 0.024 4.60 ± 0.17 1.00<br />
NGC 4365 374 186.12074 7.31231 0.45 −9.728 ± 0.029 −11.041 ± 0.021 2.77 ± 0.19 1.00<br />
NGC 4365 405 186.11754 7.30997 0.56 −9.652 ± 0.016 −10.669 ± 0.014 3.51 ± 0.16 1.00<br />
NGC 4365 421 186.13559 7.33204 1.64 −7.198 ± 0.040 −8.136 ± 0.041 3.79 ± 0.41 0.98<br />
NGC 4365 422 186.11827 7.31153 0.45 −7.193 ± 0.046 −8.549 ± 0.071 3.28 ± 0.50 1.00<br />
NGC 4365 439 186.12166 7.31633 0.30 −7.665 ± 0.037 −8.864 ± 0.037 2.89 ± 0.37 1.00<br />
NGC 4365 451 186.11981 7.31493 0.25 −10.175 ± 0.015 −11.315 ± 0.016 2.42 ± 0.14 1.00<br />
NGC 4365 520 186.13464 7.33626 1.80 −6.383 ± 0.098 −7.849 ± 0.045 3.17 ± 0.59 0.99<br />
NGC 4365 521 186.10046 7.29590 2.01 −9.057 ± 0.035 −9.983 ± 0.044 5.83 ± 0.39 1.00<br />
NGC 4365 534 186.11395 7.31230 0.48 −8.058 ± 0.032 −9.386 ± 0.103 3.01 ± 0.40 1.00<br />
NGC 4365 601 186.11644 7.31865 0.11 −8.066 ± 0.704 −9.494 ± 0.155 1.38 ± 0.87 0.95<br />
NGC 4365 636 186.10550 7.30736 1.16 −10.223 ± 0.015 −11.477 ± 0.015 4.28 ± 0.13 1.00<br />
NGC 4365 652 186.12851 7.33534 1.49 −8.302 ± 0.455 −8.819 ± 1.326 1.23 ± 0.39 0.93<br />
NGC 4365 673 186.11115 7.31558 0.50 −9.467 ± 0.019 −10.758 ± 0.017 2.73 ± 0.25 1.00<br />
NGC 4365 701 186.12644 7.33480 1.38 −9.942 ± 0.017 −11.086 ± 0.018 2.84 ± 0.24 1.00<br />
NGC 4365 826 186.11921 7.33594 1.32 −9.862 ± 0.017 −11.253 ± 0.019 3.01 ± 0.16 1.00<br />
NGC 4365 840 186.09668 7.31023 1.61 −8.667 ± 0.030 −9.819 ± 0.018 1.97 ± 0.25 0.98<br />
NGC 4365 880 186.11750 7.33849 1.50 −8.814 ± 0.018 −9.808 ± 0.017 2.74 ± 0.27 1.00<br />
NGC 4365 928 186.09362 7.31429 1.75 −9.170 ± 0.017 −10.353 ± 0.023 2.64 ± 0.28 1.00<br />
NGC 4365 1144 186.10417 7.34625 2.28 −8.986 ± 0.028 −10.285 ± 0.021 1.92 ± 0.21 0.98<br />
NGC 4365 1237 186.07390 7.31952 3.15 −8.871 ± 0.026 −10.155 ± 0.025 3.65 ± 0.23 1.00<br />
NGC 4374 25 186.24602 12.89199 1.39 −7.299 ± 0.023 −8.200 ± 0.057 2.69 ± 0.23 1.00<br />
NGC 4374 56 186.24913 12.89318 1.22 −7.751 ± 0.015 −8.708 ± 0.028 2.21 ± 0.15 1.00<br />
NGC 4374 70 186.24800 12.88488 1.22 −7.137 ± 0.035 −8.042 ± 0.074 3.19 ± 0.36 0.99<br />
NGC 4374 85 186.24414 12.86760 2.02 −8.111 ± 0.020 −8.934 ± 0.033 3.67 ± 0.18 1.00<br />
NGC 4374 152 186.25767 12.89804 0.95 −6.865 ± 0.069 −7.707 ± 0.104 4.60 ± 0.50 0.89<br />
NGC 4374 251 186.25864 12.87929 0.73 −7.855 ± 0.039 −9.228 ± 0.025 1.39 ± 0.20 0.94<br />
NGC 4374 274 186.26643 12.90168 1.04 −9.160 ± 0.017 −10.227 ± 0.017 2.53 ± 0.13 1.00<br />
NGC 4374 290 186.26546 12.89404 0.50 −7.813 ± 0.042 −9.045 ± 0.034 1.92 ± 0.22 1.00<br />
NGC 4374 310 186.26343 12.88171 0.40 −6.896 ± 0.068 −8.363 ± 0.194 2.29 ± 2.23 1.00<br />
NGC 4374 324 186.26491 12.88266 0.31 −8.268 ± 0.031 −9.643 ± 0.026 2.18 ± 0.20 1.00<br />
NGC 4374 540 186.28184 12.88511 1.13 −6.590 ± 0.062 −7.709 ± 0.143 3.89 ± 0.77 0.94<br />
NGC 4374 607 186.28622 12.88157 1.47 −7.399 ± 0.029 −8.826 ± 0.032 2.32 ± 0.29 1.00<br />
NGC 4374 658 186.29011 12.87594 1.86 −9.064 ± 0.012 −10.282 ± 0.012 2.21 ± 0.08 1.00<br />
NGC 4374 725 186.29523 12.87169 2.31 −6.893 ± 0.046 −8.125 ± 0.029 1.79 ± 0.30 0.98<br />
NGC 4382 164 186.33553 18.18961 0.93 −8.893 ± 0.020 −9.780 ± 0.023 3.04 ± 0.14 1.00<br />
NGC 4382 320 186.34054 18.17425 1.27 −8.821 ± 0.040 −9.974 ± 0.022 2.11 ± 0.19 1.00<br />
Continued on Next Page. . .<br />
293
Table B.1—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4382 397 186.34518 18.18186 0.69 −12.091 ± 0.028 −13.264 ± 0.593 1.88 ± 0.19 1.00<br />
NGC 4382 439 186.34838 18.19389 0.22 −6.898 ± 0.079 −8.160 ± 0.061 2.85 ± 0.41 0.97<br />
NGC 4382 450 186.34871 18.19427 0.23 −8.554 ± 0.031 −9.602 ± 0.022 1.50 ± 0.18 0.56<br />
NGC 4382 589 186.35414 18.18271 0.60 −9.646 ± 0.023 −10.877 ± 0.017 2.28 ± 0.17 1.00<br />
NGC 4382 600 186.35521 18.18737 0.40 −8.256 ± 0.032 −9.165 ± 0.036 2.38 ± 0.20 1.00<br />
NGC 4382 924 186.37294 18.19816 1.50 −7.894 ± 0.026 −9.188 ± 0.020 1.93 ± 0.20 1.00<br />
NGC 4382 1015 186.38045 18.20621 2.14 −8.957 ± 0.027 −10.268 ± 0.017 2.39 ± 0.20 1.00<br />
NGC 4406 302 186.52546 12.93174 0.94 −9.356 ± 0.030 −10.472 ± 0.017 2.56 ± 0.19 1.00<br />
NGC 4472 8 187.47224 8.00720 0.97 −10.586 ± 0.021 −12.055 ± 0.017 3.33 ± 0.13 1.00<br />
NGC 4472 16 187.46873 8.00045 0.82 −6.932 ± 0.034 −8.499 ± 0.050 2.25 ± 0.42 1.00<br />
NGC 4472 41 187.46901 8.00449 0.84 −9.012 ± 0.013 −10.465 ± 0.013 2.01 ± 0.08 1.00<br />
NGC 4472 54 187.46546 7.99993 0.71 −10.327 ± 0.009 −11.766 ± 0.010 3.15 ± 0.06 1.00<br />
NGC 4472 64 187.46286 7.99632 0.63 −9.849 ± 0.031 −11.325 ± 0.012 2.00 ± 0.20 1.00<br />
NGC 4472 118 187.45878 7.99539 0.51 −9.381 ± 0.017 −10.528 ± 0.013 2.78 ± 0.09 1.00<br />
NGC 4472 130 187.46911 8.01926 1.06 −6.811 ± 0.046 −8.277 ± 0.030 2.95 ± 0.24 1.00<br />
NGC 4472 147 187.45606 7.99289 0.47 −8.825 ± 0.015 −10.248 ± 0.017 2.56 ± 0.11 1.00<br />
NGC 4472 186 187.45633 7.99025 0.53 −9.076 ± 0.029 −10.577 ± 0.011 1.87 ± 0.12 1.00<br />
NGC 4472 223 187.44588 7.97961 0.72 −8.859 ± 0.025 −10.285 ± 0.018 2.16 ± 0.12 1.00<br />
NGC 4472 232 187.44940 7.98857 0.44 −9.279 ± 0.032 −10.629 ± 0.027 2.60 ± 0.23 1.00<br />
NGC 4472 301 187.45449 8.00753 0.41 −7.709 ± 0.035 −9.048 ± 0.025 2.13 ± 0.23 1.00<br />
NGC 4472 411 187.44284 7.99683 0.14 −9.466 ± 0.015 −10.749 ± 0.020 2.48 ± 0.10 1.00<br />
NGC 4472 465 187.43886 7.99442 0.29 −7.534 ± 0.030 −9.179 ± 0.022 2.31 ± 0.16 1.00<br />
NGC 4472 510 187.42901 7.97948 0.91 −9.409 ± 0.024 −10.769 ± 0.016 2.78 ± 0.13 1.00<br />
NGC 4472 525 187.43899 8.00432 0.24 −7.083 ± 0.110 −8.119 ± 0.111 3.61 ± 0.62 0.99<br />
NGC 4472 578 187.43324 7.99757 0.41 −7.519 ± 0.041 −8.873 ± 0.022 2.33 ± 0.29 1.00<br />
NGC 4472 607 187.43251 7.99904 0.43 −9.516 ± 0.016 −10.713 ± 0.007 2.37 ± 0.14 1.00<br />
NGC 4472 632 187.44308 8.02404 0.82 −6.452 ± 0.030 −7.650 ± 0.048 2.39 ± 0.30 0.99<br />
NGC 4472 678 187.43761 8.01845 0.67 −11.177 ± 0.021 −12.213 ± 0.039 7.15 ± 0.21 1.00<br />
NGC 4472 688 187.43405 8.01159 0.53 −9.748 ± 0.023 −11.179 ± 0.011 1.68 ± 0.08 1.00<br />
NGC 4472 712 187.43236 8.01132 0.57 −9.382 ± 0.027 −10.977 ± 0.017 2.71 ± 0.16 1.00<br />
NGC 4472 753 187.42931 8.01097 0.64 −9.634 ± 0.017 −10.682 ± 0.013 2.59 ± 0.10 1.00<br />
NGC 4472 814 187.42084 8.00083 0.82 −8.838 ± 0.024 −10.233 ± 0.020 2.30 ± 0.13 1.00<br />
NGC 4472 835 187.41742 7.99564 0.95 −9.901 ± 0.013 −11.207 ± 0.011 3.42 ± 0.09 1.00<br />
NGC 4472 849 187.41309 7.98874 1.16 −9.845 ± 0.022 −11.225 ± 0.014 2.41 ± 0.12 1.00<br />
NGC 4472 857 187.42335 8.01232 0.84 −9.079 ± 0.023 −10.515 ± 0.019 2.75 ± 0.14 1.00<br />
NGC 4472 881 187.41307 7.99470 1.11 −8.084 ± 0.019 −9.519 ± 0.023 1.98 ± 0.15 1.00<br />
NGC 4472 896 187.41033 7.99147 1.22 −8.302 ± 0.023 −9.738 ± 0.029 1.92 ± 0.12 1.00<br />
NGC 4472 991 187.40924 8.00342 1.22 −8.508 ± 0.020 −9.906 ± 0.022 2.19 ± 0.11 1.00<br />
NGC 4486 63 187.68576 12.41425 1.15 −9.512 ± 0.020 −10.479 ± 0.019 3.39 ± 0.11 1.00<br />
NGC 4486 112 187.68616 12.39135 0.73 −9.521 ± 0.012 −11.036 ± 0.013 2.57 ± 0.08 1.00<br />
NGC 4486 143 187.68850 12.40719 0.89 −10.048 ± 0.010 −11.090 ± 0.016 2.46 ± 0.12 1.00<br />
NGC 4486 222 187.69074 12.40282 0.72 −8.380 ± 0.024 −9.918 ± 0.016 1.85 ± 0.10 1.00<br />
NGC 4486 338 187.69384 12.41396 0.98 −6.333 ± 0.073 −7.798 ± 0.049 1.62 ± 0.29 0.99<br />
NGC 4486 339 187.69391 12.38526 0.50 −8.669 ± 0.018 −9.508 ± 0.023 2.92 ± 0.11 1.00<br />
NGC 4486 361 187.69434 12.37331 0.80 −8.266 ± 0.022 −9.591 ± 0.033 1.85 ± 0.19 1.00<br />
NGC 4486 373 187.69467 12.40082 0.56 −7.716 ± 0.029 −9.207 ± 0.036 2.49 ± 0.19 1.00<br />
NGC 4486 375 187.69475 12.41476 0.99 −7.865 ± 0.055 −9.382 ± 0.021 2.74 ± 0.25 1.00<br />
NGC 4486 378 187.69490 12.36394 1.11 −8.521 ± 0.027 −10.115 ± 0.015 2.63 ± 0.18 1.00<br />
NGC 4486 383 187.69513 12.38483 0.47 −6.570 ± 0.483 −7.391 ± 0.083 2.60 ± 0.35 0.99<br />
NGC 4486 399 187.69554 12.39024 0.39 −9.482 ± 0.017 −10.651 ± 0.013 3.05 ± 0.10 1.00<br />
NGC 4486 502 187.69771 12.39590 0.35 −6.869 ± 0.082 −7.531 ± 0.076 3.11 ± 0.45 0.99<br />
NGC 4486 513 187.69807 12.40650 0.65 −9.127 ± 0.021 −10.482 ± 0.012 2.18 ± 0.14 1.00<br />
NGC 4486 537 187.69867 12.37253 0.75 −8.589 ± 0.018 −10.053 ± 0.013 1.71 ± 0.16 1.00<br />
NGC 4486 564 187.69936 12.40130 0.46 −9.026 ± 0.017 −10.205 ± 0.017 2.81 ± 0.11 1.00<br />
NGC 4486 640 187.70134 12.41557 0.94 −8.740 ± 0.031 −9.803 ± 0.018 2.56 ± 0.13 1.00<br />
NGC 4486 722 187.70321 12.40414 0.50 −9.105 ± 0.022 −10.150 ± 0.015 2.68 ± 0.15 1.00<br />
NGC 4486 782 187.70451 12.40167 0.40 −8.745 ± 0.025 −10.131 ± 0.022 2.27 ± 0.22 1.00<br />
NGC 4486 888 187.70655 12.39889 0.30 −7.837 ± 0.028 −9.145 ± 0.023 2.31 ± 0.19 1.00<br />
NGC 4486 934 187.70755 12.37889 0.47 −8.494 ± 0.017 −9.773 ± 0.019 1.68 ± 0.11 1.00<br />
Continued on Next Page. . .<br />
294
Table B.1—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4486 941 187.70769 12.41000 0.72 −5.882 ± 0.115 −7.545 ± 0.148 3.48 ± 1.06 0.99<br />
NGC 4486 1052 187.70998 12.39244 0.16 −8.581 ± 0.032 −9.730 ± 0.031 2.18 ± 0.26 1.00<br />
NGC 4486 1065 187.71030 12.37026 0.81 −7.909 ± 0.029 −9.397 ± 0.023 1.28 ± 0.28 0.96<br />
NGC 4486 1411 187.71988 12.39362 0.53 −6.518 ± 0.062 −7.842 ± 0.040 2.39 ± 0.28 1.00<br />
NGC 4486 1566 187.72458 12.40854 0.96 −7.239 ± 0.047 −8.950 ± 0.026 2.54 ± 0.19 1.00<br />
NGC 4486 1631 187.72700 12.38415 0.82 −9.238 ± 0.018 −10.561 ± 0.013 1.86 ± 0.09 1.00<br />
NGC 4486 1662 187.72815 12.37290 1.08 −9.477 ± 0.015 −10.888 ± 0.018 1.91 ± 0.10 1.00<br />
NGC 4486 1691 187.72904 12.41075 1.14 −6.839 ± 0.027 −8.537 ± 0.034 1.92 ± 0.24 1.00<br />
NGC 4486 1753 187.73107 12.39535 0.95 −8.960 ± 1.026 −10.250 ± 0.440 2.10 ± 0.54 1.00<br />
NGC 4486 1853 187.73450 12.41320 1.35 −9.149 ± 0.024 −10.693 ± 0.014 2.65 ± 0.08 1.00<br />
NGC 4486 1944 187.73860 12.38479 1.23 −9.429 ± 0.016 −10.752 ± 0.014 2.63 ± 0.11 1.00<br />
NGC 4526 104 188.52655 7.69397 1.22 −8.692 ± 0.031 −10.154 ± 0.022 3.74 ± 0.16 1.00<br />
NGC 4526 108 188.51988 7.67559 2.02 −7.925 ± 0.024 −8.837 ± 0.023 2.51 ± 0.12 1.00<br />
NGC 4526 301 188.51391 7.69694 0.23 −8.243 ± 0.023 −9.427 ± 0.031 1.88 ± 0.21 1.00<br />
NGC 4526 472 188.50261 7.70052 0.80 −8.867 ± 0.018 −9.811 ± 0.016 2.74 ± 0.12 1.00<br />
NGC 4526 673 188.48879 7.70792 2.03 −7.843 ± 0.075 −9.036 ± 0.055 7.16 ± 0.62 0.73<br />
NGC 4526 793 188.47636 7.69941 2.90 −9.585 ± 0.016 −10.798 ± 0.022 3.35 ± 0.16 1.00<br />
NGC 4552 2 188.94820 12.57475 4.49 −7.104 ± 0.056 −8.619 ± 0.026 3.71 ± 0.23 1.00<br />
NGC 4552 161 188.92578 12.54962 1.45 −8.142 ± 0.022 −9.523 ± 0.027 1.71 ± 0.15 1.00<br />
NGC 4552 208 188.92082 12.54622 1.38 −10.732 ± 0.015 −12.119 ± 0.029 1.84 ± 0.13 1.00<br />
NGC 4552 264 188.91788 12.54654 1.23 −5.486 ± 0.556 −6.884 ± 0.123 1.63 ± 0.62 0.94<br />
NGC 4552 291 188.91803 12.55224 0.57 −8.973 ± 0.030 −10.053 ± 0.016 2.27 ± 0.15 1.00<br />
NGC 4552 296 188.91371 12.54172 1.81 −9.452 ± 0.023 −10.557 ± 0.013 2.37 ± 0.14 1.00<br />
NGC 4552 316 188.92216 12.56603 1.41 −9.231 ± 0.022 −10.266 ± 0.017 2.60 ± 0.11 1.00<br />
NGC 4552 323 188.90918 12.53376 2.89 −8.142 ± 0.039 −9.597 ± 0.017 2.71 ± 0.13 1.00<br />
NGC 4552 325 188.91894 12.55870 0.47 −7.718 ± 0.021 −8.955 ± 0.022 1.64 ± 0.17 1.00<br />
NGC 4552 393 188.91642 12.56283 0.80 −9.720 ± 0.017 −11.153 ± 0.017 2.42 ± 0.13 1.00<br />
NGC 4552 399 188.91739 12.56564 1.16 −8.344 ± 0.026 −9.783 ± 0.022 1.11 ± 0.16 0.83<br />
NGC 4552 445 188.90947 12.55025 1.07 −10.058 ± 0.019 −11.392 ± 0.018 2.74 ± 0.13 1.00<br />
NGC 4552 466 188.90974 12.55451 0.77 −8.494 ± 0.021 −9.666 ± 0.016 2.41 ± 0.11 1.00<br />
NGC 4552 494 188.91545 12.57538 2.34 −9.300 ± 0.030 −10.696 ± 0.018 2.12 ± 0.18 1.00<br />
NGC 4552 496 188.91077 12.56364 1.08 −7.853 ± 0.026 −9.204 ± 0.037 1.91 ± 0.17 1.00<br />
NGC 4552 502 188.91324 12.57055 1.77 −8.136 ± 0.078 −9.515 ± 0.249 1.27 ± 0.24 0.91<br />
NGC 4552 542 188.90199 12.55045 1.81 −6.325 ± 0.536 −7.717 ± 0.181 1.44 ± 0.33 0.96<br />
NGC 4552 599 188.89697 12.55158 2.34 −8.111 ± 0.023 −9.747 ± 0.022 2.45 ± 0.19 1.00<br />
NGC 4552 688 188.89044 12.55991 3.08 −8.262 ± 0.022 −9.746 ± 0.021 1.85 ± 0.13 1.00<br />
NGC 4552 703 188.89521 12.57714 3.56 −8.538 ± 0.023 −10.064 ± 0.025 2.07 ± 0.20 1.00<br />
NGC 4552 750 188.88924 12.57647 4.04 −10.492 ± 0.018 −11.481 ± 0.020 3.81 ± 0.13 1.00<br />
NGC 4621 66 190.52064 11.62755 1.99 −5.438 ± 0.471 −6.555 ± 0.327 1.60 ± 2.30 0.89<br />
NGC 4621 196 190.50918 11.62407 2.04 −10.607 ± 0.033 −12.134 ± 0.021 3.30 ± 0.14 1.00<br />
NGC 4621 208 190.52182 11.66749 2.12 −8.241 ± 0.023 −9.642 ± 0.020 2.91 ± 0.14 1.00<br />
NGC 4621 220 190.51068 11.63433 1.13 −9.800 ± 0.021 −11.128 ± 0.013 2.28 ± 0.08 1.00<br />
NGC 4621 224 190.51082 11.63569 1.01 −10.596 ± 0.032 −11.895 ± 0.013 3.02 ± 0.10 1.00<br />
NGC 4621 250 190.51168 11.64475 0.28 −8.787 ± 0.020 −10.136 ± 0.022 1.89 ± 0.15 1.00<br />
NGC 4621 263 190.51022 11.64381 0.29 −8.796 ± 0.024 −10.010 ± 0.015 1.79 ± 0.11 1.00<br />
NGC 4621 283 190.51211 11.65365 0.64 −7.870 ± 0.034 −9.320 ± 0.023 1.19 ± 0.16 0.83<br />
NGC 4621 343 190.51174 11.66496 1.61 −9.008 ± 0.025 −10.459 ± 0.031 3.20 ± 0.26 1.00<br />
NGC 4621 353 190.50952 11.65949 1.11 −7.492 ± 0.024 −8.435 ± 0.036 2.51 ± 0.20 1.00<br />
NGC 4621 536 190.49516 11.66519 2.04 −7.153 ± 0.031 −8.605 ± 0.023 1.82 ± 0.13 1.00<br />
NGC 4621 564 190.48627 11.64448 2.03 −9.404 ± 0.024 −10.621 ± 0.017 2.37 ± 0.11 1.00<br />
NGC 4621 653 190.48303 11.66362 2.73 −8.293 ± 0.021 −9.598 ± 0.017 2.09 ± 0.10 1.00<br />
NGC 4621 676 190.47070 11.62996 3.69 −11.399 ± 0.023 −12.724 ± 0.016 3.66 ± 0.14 1.00<br />
NGC 4649 16 190.93729 11.54831 1.08 −9.834 ± 0.018 −11.263 ± 0.023 3.31 ± 0.11 1.00<br />
NGC 4649 233 190.92067 11.54054 0.67 −8.503 ± 0.025 −10.007 ± 0.016 2.18 ± 0.19 1.00<br />
NGC 4649 257 190.93118 11.56135 0.87 −7.181 ± 0.049 −8.686 ± 0.041 2.28 ± 0.31 1.00<br />
NGC 4649 273 190.91728 11.53833 0.76 −8.590 ± 0.025 −10.073 ± 0.012 1.75 ± 0.12 1.00<br />
NGC 4649 334 190.92957 11.56547 0.94 −8.851 ± 0.011 −10.334 ± 0.014 2.51 ± 0.10 1.00<br />
NGC 4649 435 190.90793 11.53469 1.05 −8.133 ± 0.126 −9.570 ± 0.133 1.65 ± 0.36 1.00<br />
Continued on Next Page. . .<br />
295
Table B.1—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4649 448 190.91257 11.54461 0.48 −9.085 ± 0.014 −10.364 ± 0.012 2.27 ± 0.11 1.00<br />
NGC 4649 510 190.92826 11.57796 1.45 −7.314 ± 0.028 −8.711 ± 0.022 1.90 ± 0.20 1.00<br />
NGC 4649 638 190.90577 11.55101 0.57 −8.600 ± 0.025 −9.885 ± 0.026 2.72 ± 0.18 1.00<br />
NGC 4649 639 190.90646 11.55238 0.52 −9.614 ± 0.019 −11.025 ± 0.016 2.68 ± 0.14 1.00<br />
NGC 4649 646 190.91182 11.56170 0.53 −8.466 ± 0.033 −9.918 ± 0.016 2.06 ± 0.13 1.00<br />
NGC 4649 732 190.90457 11.55810 0.68 −6.544 ± 1.111 −8.264 ± 0.042 1.83 ± 0.34 1.00<br />
NGC 4649 740 190.90970 11.56799 0.87 −7.796 ± 1.174 −9.116 ± 0.020 1.67 ± 0.37 1.00<br />
NGC 4649 742 190.90138 11.55345 0.79 −8.428 ± 0.019 −9.825 ± 0.014 2.34 ± 0.15 1.00<br />
NGC 4649 778 190.88975 11.53667 1.62 −8.726 ± 0.026 −10.451 ± 0.015 2.69 ± 0.12 1.00<br />
NGC 4649 833 190.88918 11.54134 1.53 −7.580 ± 0.029 −9.024 ± 0.018 2.27 ± 0.17 1.00<br />
NGC 4649 860 190.89384 11.55274 1.17 −8.273 ± 0.020 −9.383 ± 0.019 2.10 ± 0.13 1.00<br />
NGC 4649 863 190.89983 11.56395 1.04 −8.342 ± 0.016 −9.925 ± 0.012 1.59 ± 0.09 1.00<br />
NGC 4649 888 190.88846 11.54614 1.49 −7.774 ± 0.019 −9.214 ± 0.030 1.82 ± 0.19 1.00<br />
NGC 4649 982 190.89079 11.56344 1.44 −8.332 ± 0.038 −9.680 ± 0.018 1.77 ± 0.22 1.00<br />
NGC 4649 1041 190.88369 11.56369 1.79 −8.297 ± 0.023 −9.917 ± 0.016 2.06 ± 0.17 1.00<br />
NGC 4649 1056 190.87966 11.56042 1.94 −8.674 ± 0.014 −10.199 ± 0.012 2.10 ± 0.08 1.00<br />
NGC 4697 75 192.12959 -5.80791 1.06 −9.882 ± 0.026 −11.282 ± 0.016 2.51 ± 0.07 1.00<br />
NGC 4697 123 192.13272 -5.81061 0.97 −8.514 ± 0.042 −9.464 ± 0.012 1.77 ± 0.06 1.00<br />
NGC 4697 128 192.13222 -5.81287 1.06 −6.367 ± 0.063 −7.756 ± 0.094 2.35 ± 0.42 1.00<br />
NGC 4697 150 192.14917 -5.77785 1.14 −9.587 ± 0.031 −10.940 ± 0.015 1.56 ± 0.05 1.00<br />
NGC 4697 158 192.14439 -5.79083 0.56 −7.288 ± 0.033 −8.767 ± 0.034 1.98 ± 0.10 1.00<br />
NGC 4697 184 192.13607 -5.81414 0.95 −8.644 ± 0.023 −9.632 ± 0.019 2.18 ± 0.06 1.00<br />
NGC 4697 229 192.14147 -5.80950 0.60 −8.658 ± 0.040 −10.022 ± 0.021 1.37 ± 0.11 1.00<br />
NGC 4697 233 192.14006 -5.81354 0.80 −7.468 ± 0.027 −8.615 ± 0.029 1.73 ± 0.08 1.00<br />
NGC 4697 241 192.14806 -5.79562 0.27 −5.694 ± 0.075 −7.095 ± 0.033 1.48 ± 0.14 0.95<br />
NGC 4697 242 192.14456 -5.80397 0.30 −7.378 ± 0.043 −8.706 ± 0.036 1.43 ± 0.16 1.00<br />
NGC 4697 248 192.14904 -5.79484 0.29 −9.320 ± 0.036 −10.588 ± 0.014 2.08 ± 0.08 1.00<br />
NGC 4697 249 192.13831 -5.82020 1.12 −8.722 ± 0.052 −10.021 ± 0.023 2.30 ± 0.12 1.00<br />
NGC 4697 284 192.14992 -5.79893 0.09 −8.781 ± 0.046 −9.845 ± 0.033 2.37 ± 0.13 1.00<br />
NGC 4697 286 192.15305 -5.79209 0.46 −7.803 ± 0.061 −9.185 ± 0.028 1.97 ± 0.13 1.00<br />
NGC 4697 288 192.15781 -5.78124 1.06 −8.559 ± 0.037 −9.524 ± 0.015 1.39 ± 0.08 1.00<br />
NGC 4697 339 192.15718 -5.79137 0.60 −9.729 ± 0.041 −10.993 ± 0.017 2.01 ± 0.08 1.00<br />
NGC 4697 352 192.15407 -5.80022 0.23 −10.972 ± 0.037 −12.325 ± 0.016 2.12 ± 0.08 1.00<br />
NGC 4697 354 192.15044 -5.80925 0.43 −9.331 ± 0.030 −10.701 ± 0.014 1.07 ± 0.07 1.00<br />
NGC 4697 355 192.15633 -5.79533 0.43 −7.951 ± 0.058 −9.278 ± 0.017 1.42 ± 0.11 1.00<br />
NGC 4697 359 192.15573 -5.79696 0.36 −7.054 ± 0.060 −8.348 ± 0.029 1.47 ± 0.14 1.00<br />
NGC 4697 370 192.15393 -5.80292 0.24 −7.168 ± 0.047 −8.635 ± 0.035 1.43 ± 0.10 1.00<br />
NGC 4697 410 192.15490 -5.80831 0.46 −7.489 ± 0.029 −8.934 ± 0.022 1.25 ± 0.06 1.00<br />
NGC 4697 426 192.16116 -5.79626 0.62 −7.737 ± 0.049 −8.950 ± 0.027 2.17 ± 0.10 1.00<br />
NGC 4697 474 192.16615 -5.79370 0.90 −8.758 ± 0.029 −9.777 ± 0.014 1.79 ± 0.05 1.00<br />
NGC 4697 518 192.16710 -5.80002 0.87 −9.557 ± 0.054 −10.961 ± 0.022 2.57 ± 0.15 1.00<br />
NGC 4697 519 192.17054 -5.79197 1.13 −10.081 ± 0.035 −11.428 ± 0.286 1.54 ± 0.17 1.00<br />
NGC 4697 550 192.17295 -5.79359 1.22 −7.732 ± 0.030 −9.044 ± 0.018 1.39 ± 0.08 1.00<br />
NGC 4697 578 192.17029 -5.80629 1.07 −9.404 ± 0.030 −10.393 ± 0.023 1.88 ± 0.13 1.00<br />
NGC 4697 637 192.17358 -5.81294 1.34 −8.132 ± 0.025 −9.315 ± 0.013 1.33 ± 0.05 1.00<br />
296
Table B.2. Optical Properties <strong>of</strong> Globular Clusters (Without LMXBs)<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4365 4 186.13743 7.30671 1.62 −8.476 ± 0.021 −9.319 ± 0.029 3.02 ± 0.20 1.00<br />
NGC 4365 5 186.13774 7.30709 1.63 −8.600 ± 0.025 −9.516 ± 0.024 2.84 ± 0.19 1.00<br />
NGC 4365 6 186.14687 7.31789 2.09 −7.891 ± 0.029 −8.806 ± 0.036 4.54 ± 0.24 0.98<br />
NGC 4365 9 186.14220 7.31259 1.79 −9.163 ± 0.018 −10.405 ± 0.020 3.47 ± 0.14 1.00<br />
NGC 4365 10 186.14163 7.31172 1.77 −7.600 ± 0.030 −8.569 ± 0.030 3.57 ± 0.23 0.99<br />
NGC 4365 11 186.13360 7.30270 1.57 −6.302 ± 1.061 −7.284 ± 0.105 1.34 ± 0.43 0.88<br />
NGC 4365 12 186.13897 7.30917 1.64 −8.392 ± 0.028 −9.847 ± 0.024 2.27 ± 0.22 1.00<br />
NGC 4365 13 186.13802 7.30821 1.61 −7.021 ± 1.384 −8.048 ± 0.030 1.83 ± 0.39 0.97<br />
NGC 4365 16 186.12729 7.29571 1.74 −7.626 ± 0.040 −8.514 ± 0.048 3.85 ± 0.35 0.99<br />
NGC 4365 17 186.13016 7.29932 1.60 −7.133 ± 0.047 −8.045 ± 0.059 3.95 ± 0.33 0.98<br />
NGC 4365 19 186.15138 7.32458 2.46 −6.706 ± 0.050 −7.870 ± 0.317 2.01 ± 0.37 0.97<br />
NGC 4365 21 186.12652 7.29526 1.74 −7.469 ± 0.032 −8.566 ± 0.032 2.83 ± 0.33 1.00<br />
NGC 4365 22 186.14807 7.32101 2.19 −7.297 ± 0.138 −8.206 ± 0.096 3.58 ± 0.61 0.99<br />
NGC 4365 24 186.14500 7.31771 1.95 −9.289 ± 0.014 −10.354 ± 0.018 2.67 ± 0.14 1.00<br />
NGC 4365 26 186.14457 7.31730 1.92 −6.279 ± 0.129 −7.924 ± 0.217 6.54 ± 3.26 0.70<br />
NGC 4365 27 186.14111 7.31327 1.70 −7.206 ± 0.039 −8.564 ± 0.045 3.94 ± 0.26 0.99<br />
NGC 4365 32 186.11842 7.28703 2.22 −7.757 ± 0.037 −8.530 ± 0.041 4.20 ± 0.32 0.99<br />
NGC 4365 36 186.12182 7.29118 1.94 −7.837 ± 0.029 −9.194 ± 0.028 2.41 ± 0.24 1.00<br />
NGC 4365 38 186.11810 7.28698 2.23 −7.446 ± 0.042 −8.496 ± 0.124 5.93 ± 0.74 0.93<br />
NGC 4365 39 186.13467 7.30671 1.45 −6.581 ± 0.071 −7.472 ± 0.070 2.93 ± 0.45 0.98<br />
NGC 4365 41 186.15072 7.32584 2.43 −6.429 ± 0.082 −7.331 ± 0.142 3.36 ± 0.73 0.96<br />
NGC 4365 42 186.14905 7.32403 2.29 −7.546 ± 0.033 −8.728 ± 0.034 3.18 ± 0.23 1.00<br />
NGC 4365 45 186.13832 7.31144 1.54 −7.403 ± 0.033 −8.865 ± 0.281 2.21 ± 0.30 1.00<br />
NGC 4365 46 186.12841 7.29989 1.50 −6.765 ± 0.064 −7.717 ± 0.104 5.58 ± 0.55 0.76<br />
NGC 4365 48 186.11684 7.28644 2.27 −6.981 ± 0.064 −7.860 ± 0.076 4.30 ± 0.41 0.94<br />
NGC 4365 51 186.14544 7.32037 1.99 −7.768 ± 0.024 −9.205 ± 0.026 3.83 ± 0.21 1.00<br />
NGC 4365 57 186.13486 7.30823 1.41 −5.672 ± 0.930 −7.173 ± 0.103 2.70 ± 0.74 0.96<br />
NGC 4365 60 186.12312 7.29460 1.72 −9.385 ± 0.015 −10.637 ± 0.008 2.59 ± 0.13 1.00<br />
NGC 4365 61 186.12123 7.29239 1.85 −6.725 ± 0.069 −7.883 ± 0.115 4.93 ± 0.75 0.88<br />
NGC 4365 62 186.14962 7.32601 2.36 −8.409 ± 2.009 −9.381 ± 0.793 1.14 ± 0.35 0.91<br />
NGC 4365 63 186.11991 7.29106 1.94 −9.318 ± 0.021 −10.434 ± 0.015 3.10 ± 0.20 1.00<br />
NGC 4365 65 186.13440 7.30860 1.36 −6.199 ± 0.287 −7.117 ± 0.214 4.54 ± 1.71 0.81<br />
NGC 4365 66 186.14804 7.32481 2.23 −6.876 ± 0.069 −8.031 ± 0.042 3.28 ± 0.48 0.99<br />
NGC 4365 67 186.13070 7.30429 1.35 −5.779 ± 0.482 −7.086 ± 0.161 3.43 ± 1.38 0.94<br />
NGC 4365 68 186.14252 7.31843 1.78 −7.206 ± 0.047 −8.650 ± 0.026 3.55 ± 0.25 1.00<br />
NGC 4365 69 186.14319 7.31941 1.83 −9.041 ± 0.027 −10.012 ± 0.021 3.92 ± 0.20 1.00<br />
NGC 4365 70 186.13481 7.30936 1.36 −6.610 ± 0.238 −7.705 ± 0.053 2.20 ± 0.49 0.97<br />
NGC 4365 71 186.12788 7.30144 1.39 −6.995 ± 0.032 −7.794 ± 1.934 3.35 ± 0.67 0.99<br />
NGC 4365 72 186.13214 7.30649 1.31 −6.137 ± 0.468 −7.228 ± 0.207 2.00 ± 0.70 0.95<br />
NGC 4365 73 186.13450 7.30929 1.35 −7.270 ± 0.563 −8.508 ± 0.581 1.53 ± 0.56 0.96<br />
NGC 4365 74 186.13325 7.30788 1.32 −7.385 ± 0.040 −8.750 ± 0.065 6.24 ± 0.35 0.95<br />
NGC 4365 76 186.13893 7.31478 1.53 −7.373 ± 0.307 −8.229 ± 0.039 2.36 ± 0.42 0.99<br />
NGC 4365 77 186.12442 7.29760 1.53 −6.612 ± 0.067 −7.950 ± 0.036 2.32 ± 0.44 0.98<br />
NGC 4365 78 186.13453 7.30960 1.34 −6.374 ± 0.073 −7.810 ± 0.363 2.72 ± 0.51 0.99<br />
NGC 4365 84 186.12972 7.30420 1.30 −5.942 ± 0.324 −7.237 ± 0.119 5.26 ± 1.77 0.68<br />
NGC 4365 85 186.13144 7.30634 1.28 −6.742 ± 0.046 −7.589 ± 0.903 2.59 ± 0.59 0.98<br />
NGC 4365 86 186.12895 7.30342 1.31 −6.449 ± 0.424 −7.717 ± 0.046 2.99 ± 0.62 0.99<br />
NGC 4365 89 186.14810 7.32679 2.27 −6.711 ± 0.139 −8.545 ± 0.171 7.53 ± 1.59 0.82<br />
NGC 4365 92 186.11371 7.28620 2.30 −8.248 ± 0.073 −9.557 ± 0.020 7.56 ± 0.59 0.94<br />
NGC 4365 93 186.14926 7.32831 2.38 −6.662 ± 0.059 −7.326 ± 0.599 2.79 ± 0.40 0.97<br />
NGC 4365 94 186.12660 7.30173 1.32 −8.046 ± 0.028 −9.154 ± 0.022 2.12 ± 0.19 0.99<br />
NGC 4365 95 186.13331 7.30973 1.26 −7.791 ± 0.745 −9.033 ± 0.021 2.40 ± 0.33 1.00<br />
NGC 4365 96 186.14125 7.31909 1.69 −6.855 ± 0.257 −8.105 ± 1.566 2.37 ± 0.48 0.99<br />
NGC 4365 97 186.14056 7.31834 1.63 −8.966 ± 0.019 −10.380 ± 0.012 2.30 ± 0.20 1.00<br />
NGC 4365 98 186.13190 7.30805 1.23 −6.801 ± 0.102 −7.498 ± 0.082 5.01 ± 0.64 0.79<br />
NGC 4365 99 186.14838 7.32802 2.32 −7.990 ± 0.037 −8.975 ± 0.024 2.92 ± 0.29 1.00<br />
NGC 4365 100 186.14111 7.31908 1.68 −9.098 ± 0.019 −10.526 ± 0.015 2.14 ± 0.14 0.99<br />
NGC 4365 101 186.12748 7.30313 1.27 −6.650 ± 0.053 −7.631 ± 0.110 3.28 ± 0.61 0.98<br />
NGC 4365 104 186.11514 7.28852 2.12 −8.267 ± 0.029 −9.661 ± 0.017 2.99 ± 0.14 1.00<br />
NGC 4365 107 186.13595 7.31379 1.34 −7.093 ± 0.356 −7.834 ± 0.364 2.79 ± 0.69 0.99<br />
NGC 4365 108 186.11667 7.29121 1.92 −7.526 ± 0.050 −8.246 ± 0.045 4.81 ± 0.30 0.95<br />
NGC 4365 109 186.14573 7.32562 2.08 −7.055 ± 0.054 −8.211 ± 0.021 3.50 ± 0.35 0.99<br />
Continued on Next Page. . .<br />
297
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4365 110 186.12552 7.30200 1.27 −7.722 ± 0.039 −8.650 ± 0.048 4.38 ± 0.43 0.98<br />
NGC 4365 111 186.14520 7.32538 2.04 −7.550 ± 0.023 −8.932 ± 0.024 2.60 ± 0.18 1.00<br />
NGC 4365 112 186.12125 7.29705 1.52 −5.886 ± 0.620 −7.270 ± 0.166 2.66 ± 0.59 0.97<br />
NGC 4365 113 186.14670 7.32693 2.18 −6.442 ± 0.073 −8.058 ± 0.069 2.90 ± 0.40 0.99<br />
NGC 4365 114 186.13315 7.31125 1.20 −5.898 ± 0.346 −7.408 ± 0.056 3.73 ± 0.76 0.94<br />
NGC 4365 115 186.12082 7.29670 1.54 −6.147 ± 0.093 −7.732 ± 0.048 5.51 ± 0.50 0.77<br />
NGC 4365 116 186.14296 7.32299 1.85 −8.703 ± 0.026 −9.958 ± 0.025 2.82 ± 0.18 1.00<br />
NGC 4365 117 186.12603 7.30296 1.22 −5.831 ± 0.841 −7.679 ± 0.084 2.76 ± 0.81 0.99<br />
NGC 4365 118 186.13546 7.31416 1.29 −7.692 ± 0.295 −9.219 ± 0.025 2.28 ± 0.32 1.00<br />
NGC 4365 119 186.11791 7.29340 1.76 −6.310 ± 0.103 −7.573 ± 0.106 2.63 ± 0.87 0.98<br />
NGC 4365 120 186.11531 7.29042 1.99 −8.359 ± 0.025 −9.116 ± 0.034 4.26 ± 0.32 1.00<br />
NGC 4365 121 186.11796 7.29367 1.74 −7.682 ± 0.051 −8.579 ± 0.108 5.95 ± 0.63 0.94<br />
NGC 4365 123 186.13012 7.30813 1.13 −7.680 ± 0.121 −9.008 ± 0.037 2.00 ± 0.33 0.99<br />
NGC 4365 126 186.11421 7.28962 2.05 −7.270 ± 0.110 −8.267 ± 0.149 7.92 ± 1.00 0.66<br />
NGC 4365 127 186.12756 7.30551 1.13 −7.044 ± 0.403 −8.383 ± 0.323 1.71 ± 0.51 0.97<br />
NGC 4365 129 186.14040 7.32078 1.64 −6.236 ± 0.844 −7.739 ± 0.530 2.43 ± 0.69 0.98<br />
NGC 4365 130 186.12396 7.30136 1.27 −8.486 ± 0.014 −9.368 ± 0.031 2.58 ± 0.19 1.00<br />
NGC 4365 131 186.13191 7.31091 1.13 −9.768 ± 0.016 −10.610 ± 0.013 3.78 ± 0.20 1.00<br />
NGC 4365 132 186.12492 7.30268 1.21 −7.487 ± 0.304 −8.767 ± 0.039 1.96 ± 0.41 0.99<br />
NGC 4365 133 186.12389 7.30148 1.26 −8.037 ± 0.028 −8.948 ± 0.028 3.24 ± 0.26 1.00<br />
NGC 4365 134 186.11917 7.29604 1.57 −9.244 ± 0.015 −10.128 ± 0.022 2.49 ± 0.19 1.00<br />
NGC 4365 135 186.12349 7.30125 1.26 −9.704 ± 0.013 −10.636 ± 0.020 5.75 ± 0.12 1.00<br />
NGC 4365 136 186.12070 7.29787 1.45 −8.192 ± 0.038 −9.348 ± 0.045 4.16 ± 0.34 1.00<br />
NGC 4365 137 186.13650 7.31664 1.35 −8.689 ± 0.013 −9.790 ± 0.027 2.20 ± 0.22 1.00<br />
NGC 4365 138 186.13684 7.31710 1.37 −6.187 ± 0.055 −7.525 ± 0.067 2.48 ± 0.41 0.98<br />
NGC 4365 140 186.14232 7.32369 1.81 −6.936 ± 1.494 −7.836 ± 0.817 1.51 ± 0.57 0.94<br />
NGC 4365 141 186.11412 7.29041 2.00 −8.677 ± 0.019 −10.304 ± 0.018 3.56 ± 0.22 1.00<br />
NGC 4365 142 186.12873 7.30769 1.07 −7.582 ± 0.025 −8.755 ± 0.059 3.36 ± 0.35 1.00<br />
NGC 4365 144 186.12912 7.30834 1.06 −6.297 ± 0.073 −7.352 ± 0.165 2.25 ± 0.51 0.96<br />
NGC 4365 145 186.13112 7.31074 1.08 −7.962 ± 0.030 −9.182 ± 0.024 2.63 ± 0.28 1.00<br />
NGC 4365 146 186.14004 7.32151 1.62 −6.761 ± 0.046 −8.166 ± 0.226 2.70 ± 0.46 0.99<br />
NGC 4365 147 186.13567 7.31624 1.29 −7.036 ± 0.503 −8.579 ± 0.459 2.23 ± 0.50 0.99<br />
NGC 4365 149 186.13802 7.31920 1.46 −6.360 ± 0.118 −6.895 ± 0.553 2.83 ± 0.79 0.95<br />
NGC 4365 151 186.12308 7.30179 1.22 −6.987 ± 0.816 −8.720 ± 0.511 1.51 ± 0.43 0.96<br />
NGC 4365 152 186.11702 7.29470 1.67 −8.525 ± 0.028 −10.047 ± 0.261 2.95 ± 0.34 1.00<br />
NGC 4365 154 186.12810 7.30804 1.02 −7.377 ± 0.292 −8.714 ± 1.149 2.25 ± 0.51 0.99<br />
NGC 4365 155 186.13767 7.31941 1.43 −7.825 ± 0.039 −8.979 ± 0.041 3.11 ± 0.32 1.00<br />
NGC 4365 156 186.11316 7.29042 2.01 −7.014 ± 0.938 −8.500 ± 1.591 1.29 ± 0.39 0.94<br />
NGC 4365 157 186.11688 7.29492 1.65 −7.775 ± 0.040 −8.756 ± 0.049 2.53 ± 0.27 1.00<br />
NGC 4365 158 186.11336 7.29088 1.97 −8.666 ± 0.024 −9.523 ± 0.040 2.87 ± 0.25 1.00<br />
NGC 4365 159 186.12787 7.30824 1.00 −8.481 ± 0.036 −9.178 ± 0.118 2.24 ± 0.31 1.00<br />
NGC 4365 160 186.14212 7.32514 1.83 −5.761 ± 0.290 −7.432 ± 0.061 1.95 ± 0.55 0.95<br />
NGC 4365 161 186.12972 7.31072 1.00 −7.859 ± 0.033 −8.777 ± 0.042 5.04 ± 0.33 0.98<br />
NGC 4365 162 186.12062 7.30010 1.29 −10.298 ± 0.034 −11.179 ± 0.023 4.14 ± 0.25 1.00<br />
NGC 4365 163 186.13620 7.31843 1.32 −6.752 ± 0.048 −7.791 ± 0.058 2.18 ± 0.47 0.97<br />
NGC 4365 164 186.14662 7.33080 2.27 −6.153 ± 0.090 −7.495 ± 0.820 2.56 ± 0.65 0.98<br />
NGC 4365 166 186.11808 7.29711 1.49 −7.178 ± 0.394 −8.084 ± 0.050 2.91 ± 0.43 0.99<br />
NGC 4365 167 186.12567 7.30610 1.02 −8.447 ± 0.033 −9.634 ± 0.042 2.76 ± 0.34 1.00<br />
NGC 4365 168 186.13084 7.31230 1.02 −7.101 ± 0.036 −7.848 ± 0.561 2.11 ± 0.46 0.97<br />
NGC 4365 169 186.13414 7.31631 1.18 −7.387 ± 0.029 −8.256 ± 0.033 2.46 ± 0.25 0.99<br />
NGC 4365 170 186.13382 7.31598 1.16 −7.303 ± 0.030 −8.205 ± 0.236 2.04 ± 0.34 0.98<br />
NGC 4365 171 186.12766 7.30906 0.95 −6.859 ± 0.042 −8.384 ± 0.054 2.27 ± 0.35 0.99<br />
NGC 4365 172 186.11265 7.29138 1.94 −6.550 ± 0.234 −7.902 ± 0.071 2.43 ± 0.38 0.98<br />
NGC 4365 175 186.12273 7.30345 1.10 −6.919 ± 0.052 −7.769 ± 0.301 3.28 ± 0.54 0.99<br />
NGC 4365 176 186.13512 7.31837 1.24 −7.860 ± 0.045 −9.263 ± 0.030 2.72 ± 0.36 1.00<br />
NGC 4365 177 186.11078 7.28972 2.09 −7.844 ± 0.033 −9.256 ± 0.022 2.66 ± 0.18 1.00<br />
NGC 4365 178 186.12753 7.30967 0.91 −7.436 ± 0.036 −8.524 ± 0.066 3.01 ± 0.38 1.00<br />
NGC 4365 179 186.12334 7.30448 1.04 −7.689 ± 0.663 −8.525 ± 0.027 1.96 ± 0.48 0.98<br />
NGC 4365 180 186.13004 7.31271 0.95 −7.425 ± 0.040 −8.211 ± 0.037 2.77 ± 0.30 0.99<br />
NGC 4365 181 186.14491 7.33037 2.15 −8.409 ± 0.024 −9.766 ± 0.027 3.86 ± 0.20 1.00<br />
NGC 4365 182 186.12076 7.30177 1.18 −8.070 ± 0.039 −9.241 ± 0.277 1.88 ± 0.30 0.98<br />
NGC 4365 184 186.13046 7.31335 0.96 −7.777 ± 0.066 −9.141 ± 0.049 2.79 ± 0.50 1.00<br />
Continued on Next Page. . .<br />
298
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4365 186 186.12932 7.31206 0.93 −7.305 ± 0.348 −8.590 ± 0.042 2.02 ± 0.50 0.99<br />
NGC 4365 188 186.12975 7.31302 0.93 −9.494 ± 0.020 −10.570 ± 0.015 2.07 ± 0.14 0.99<br />
NGC 4365 189 186.13173 7.31536 1.02 −7.606 ± 0.514 −8.540 ± 0.050 3.35 ± 0.48 1.00<br />
NGC 4365 190 186.14383 7.32973 2.06 −8.426 ± 0.025 −9.556 ± 0.023 3.44 ± 0.22 1.00<br />
NGC 4365 191 186.12375 7.30605 0.95 −6.940 ± 0.131 −7.949 ± 0.053 3.44 ± 0.38 0.99<br />
NGC 4365 192 186.13576 7.32059 1.31 −8.595 ± 0.017 −9.539 ± 0.025 3.20 ± 0.18 1.00<br />
NGC 4365 196 186.12329 7.30613 0.93 −6.311 ± 0.348 −7.610 ± 0.108 2.79 ± 0.80 0.98<br />
NGC 4365 197 186.11581 7.29733 1.48 −6.754 ± 0.079 −8.125 ± 0.217 6.33 ± 1.75 0.81<br />
NGC 4365 198 186.13170 7.31615 1.01 −6.009 ± 0.106 −7.073 ± 0.077 2.01 ± 0.53 0.94<br />
NGC 4365 199 186.11743 7.29936 1.33 −7.767 ± 0.027 −9.023 ± 0.028 2.73 ± 0.25 1.00<br />
NGC 4365 200 186.13202 7.31657 1.03 −5.812 ± 0.087 −7.066 ± 0.768 2.29 ± 0.76 0.96<br />
NGC 4365 201 186.12326 7.30633 0.92 −8.246 ± 0.029 −9.402 ± 0.027 2.30 ± 0.19 1.00<br />
NGC 4365 203 186.11984 7.30249 1.12 −7.567 ± 0.624 −9.059 ± 0.020 1.78 ± 0.28 0.98<br />
NGC 4365 204 186.12181 7.30485 0.98 −7.440 ± 0.544 −8.265 ± 0.766 2.14 ± 0.66 0.99<br />
NGC 4365 205 186.11730 7.29960 1.31 −8.839 ± 0.021 −10.144 ± 0.118 2.43 ± 0.24 1.00<br />
NGC 4365 206 186.12120 7.30419 1.01 −6.800 ± 0.046 −8.116 ± 0.070 2.19 ± 0.39 0.98<br />
NGC 4365 208 186.11522 7.29719 1.50 −8.010 ± 0.030 −9.420 ± 0.022 2.35 ± 0.20 1.00<br />
NGC 4365 211 186.11403 7.29586 1.61 −7.854 ± 0.027 −8.981 ± 0.317 2.03 ± 0.25 0.99<br />
NGC 4365 215 186.11715 7.29971 1.31 −6.996 ± 0.037 −8.450 ± 0.037 2.27 ± 0.30 0.99<br />
NGC 4365 216 186.12635 7.31074 0.80 −9.203 ± 0.021 −10.464 ± 0.013 2.29 ± 0.15 1.00<br />
NGC 4365 219 186.14172 7.32917 1.90 −6.667 ± 0.046 −8.181 ± 0.036 2.38 ± 0.36 0.99<br />
NGC 4365 220 186.11352 7.29582 1.62 −7.245 ± 0.041 −8.000 ± 0.098 2.54 ± 0.44 0.99<br />
NGC 4365 222 186.13762 7.32440 1.50 −8.205 ± 0.032 −9.738 ± 0.413 3.81 ± 0.49 1.00<br />
NGC 4365 223 186.13003 7.31548 0.89 −7.902 ± 0.022 −9.184 ± 0.014 2.02 ± 0.22 0.99<br />
NGC 4365 224 186.12446 7.30896 0.80 −8.364 ± 0.026 −9.294 ± 0.202 2.72 ± 0.36 1.00<br />
NGC 4365 225 186.13252 7.31843 1.06 −6.872 ± 0.056 −7.659 ± 1.154 1.95 ± 0.54 0.96<br />
NGC 4365 226 186.13438 7.32068 1.21 −6.815 ± 0.140 −8.341 ± 0.088 6.91 ± 0.92 0.81<br />
NGC 4365 227 186.12468 7.30929 0.79 −8.078 ± 0.029 −9.142 ± 0.033 1.72 ± 0.16 0.98<br />
NGC 4365 228 186.13805 7.32518 1.55 −7.522 ± 0.066 −8.489 ± 0.053 3.97 ± 0.47 0.99<br />
NGC 4365 229 186.12651 7.31154 0.77 −7.421 ± 0.074 −8.545 ± 0.038 1.97 ± 0.37 0.99<br />
NGC 4365 230 186.13207 7.31824 1.03 −7.134 ± 0.215 −8.592 ± 0.299 1.95 ± 0.38 0.98<br />
NGC 4365 231 186.12976 7.31553 0.87 −9.105 ± 0.018 −10.051 ± 0.023 3.16 ± 0.16 1.00<br />
NGC 4365 232 186.13962 7.32718 1.71 −7.669 ± 0.063 −8.488 ± 0.056 4.85 ± 0.42 0.97<br />
NGC 4365 234 186.13525 7.32205 1.29 −7.737 ± 0.600 −9.115 ± 0.431 2.13 ± 0.42 0.99<br />
NGC 4365 238 186.12378 7.30877 0.78 −9.857 ± 0.022 −11.116 ± 0.012 3.11 ± 0.21 1.00<br />
NGC 4365 239 186.11394 7.29731 1.50 −9.558 ± 0.016 −10.474 ± 0.019 3.79 ± 0.19 1.00<br />
NGC 4365 242 186.12107 7.30574 0.90 −6.468 ± 0.055 −7.650 ± 0.066 2.25 ± 0.40 0.97<br />
NGC 4365 246 186.11028 7.29321 1.86 −7.164 ± 0.057 −7.866 ± 0.068 4.09 ± 0.42 0.96<br />
NGC 4365 247 186.14238 7.33141 2.02 −9.829 ± 0.041 −10.812 ± 0.033 4.91 ± 0.33 1.00<br />
NGC 4365 248 186.11361 7.29734 1.51 −7.742 ± 0.027 −8.468 ± 0.030 2.99 ± 0.31 1.00<br />
NGC 4365 249 186.12822 7.31463 0.78 −7.880 ± 0.038 −9.273 ± 0.030 2.62 ± 0.29 1.00<br />
NGC 4365 252 186.12115 7.30657 0.85 −7.564 ± 0.030 −9.131 ± 0.027 2.54 ± 0.26 1.00<br />
NGC 4365 253 186.14023 7.32928 1.81 −9.147 ± 0.023 −10.208 ± 0.017 2.58 ± 0.19 1.00<br />
NGC 4365 254 186.12833 7.31519 0.78 −7.779 ± 0.031 −9.293 ± 0.026 2.32 ± 0.30 1.00<br />
NGC 4365 255 186.12720 7.31397 0.73 −10.717 ± 0.010 −11.910 ± 0.009 3.67 ± 0.12 1.00<br />
NGC 4365 257 186.13637 7.32474 1.43 −6.537 ± 0.082 −7.537 ± 0.075 4.52 ± 0.43 0.87<br />
NGC 4365 258 186.12578 7.31238 0.69 −9.137 ± 0.022 −10.234 ± 0.023 2.62 ± 0.22 1.00<br />
NGC 4365 259 186.11471 7.29934 1.35 −7.112 ± 0.048 −8.259 ± 0.044 2.46 ± 0.35 0.99<br />
NGC 4365 260 186.12305 7.30896 0.74 −7.700 ± 0.029 −8.894 ± 0.039 3.10 ± 0.41 1.00<br />
NGC 4365 261 186.14214 7.33197 2.03 −8.108 ± 0.022 −9.104 ± 0.027 2.72 ± 0.28 1.00<br />
NGC 4365 262 186.13915 7.32840 1.71 −7.038 ± 0.072 −7.802 ± 0.074 4.62 ± 0.48 0.90<br />
NGC 4365 263 186.11472 7.29959 1.33 −7.392 ± 0.059 −8.136 ± 0.119 5.80 ± 0.78 0.87<br />
NGC 4365 265 186.12833 7.31584 0.77 −8.210 ± 0.051 −9.421 ± 0.027 1.55 ± 0.31 0.96<br />
NGC 4365 266 186.11614 7.30144 1.19 −7.888 ± 0.047 −8.703 ± 0.036 1.93 ± 0.29 0.98<br />
NGC 4365 267 186.11215 7.29674 1.57 −7.443 ± 0.656 −8.698 ± 0.453 2.42 ± 0.53 0.99<br />
NGC 4365 269 186.13968 7.32936 1.78 −7.369 ± 0.056 −8.283 ± 0.042 3.35 ± 0.36 0.99<br />
NGC 4365 272 186.13783 7.32755 1.60 −8.438 ± 0.036 −9.884 ± 0.037 3.99 ± 0.42 1.00<br />
NGC 4365 273 186.14142 7.33174 1.97 −6.091 ± 0.118 −7.335 ± 0.491 4.12 ± 0.95 0.90<br />
NGC 4365 274 186.11940 7.30577 0.88 −7.734 ± 0.046 −8.802 ± 0.034 2.00 ± 0.39 0.99<br />
NGC 4365 275 186.11099 7.29597 1.65 −9.459 ± 0.033 −10.344 ± 0.018 2.97 ± 0.23 1.00<br />
NGC 4365 276 186.14295 7.33375 2.14 −7.567 ± 0.042 −8.477 ± 0.039 4.01 ± 0.43 0.99<br />
NGC 4365 277 186.11232 7.29751 1.52 −6.735 ± 0.526 −7.742 ± 0.315 1.55 ± 0.51 0.94<br />
Continued on Next Page. . .<br />
299
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4365 278 186.12978 7.31826 0.86 −7.916 ± 0.030 −9.219 ± 0.032 1.43 ± 0.31 0.95<br />
NGC 4365 280 186.11728 7.30389 1.00 −6.376 ± 0.093 −7.465 ± 0.346 3.00 ± 0.82 0.98<br />
NGC 4365 281 186.13192 7.32097 1.04 −9.423 ± 0.012 −10.418 ± 0.016 2.50 ± 0.12 1.00<br />
NGC 4365 282 186.13659 7.32680 1.50 −8.702 ± 0.033 −9.694 ± 0.025 3.05 ± 0.27 1.00<br />
NGC 4365 283 186.13242 7.32179 1.09 −5.612 ± 0.227 −6.900 ± 0.551 3.86 ± 1.54 0.88<br />
NGC 4365 284 186.13547 7.32549 1.39 −7.084 ± 0.102 −7.730 ± 0.078 5.63 ± 0.68 0.75<br />
NGC 4365 285 186.13402 7.32387 1.25 −8.560 ± 0.041 −9.560 ± 0.031 4.57 ± 0.28 1.00<br />
NGC 4365 286 186.11267 7.29865 1.43 −6.763 ± 0.129 −7.748 ± 0.092 2.83 ± 0.57 0.99<br />
NGC 4365 287 186.13350 7.32334 1.20 −6.901 ± 0.054 −7.879 ± 0.619 2.83 ± 0.60 0.99<br />
NGC 4365 288 186.12794 7.31685 0.73 −8.542 ± 0.023 −9.436 ± 0.028 2.47 ± 0.21 1.00<br />
NGC 4365 289 186.11868 7.30593 0.86 −8.738 ± 0.031 −9.872 ± 0.019 2.59 ± 0.25 1.00<br />
NGC 4365 291 186.11368 7.30014 1.31 −8.292 ± 0.015 −9.655 ± 0.190 2.67 ± 0.34 1.00<br />
NGC 4365 292 186.11287 7.29926 1.38 −9.543 ± 0.016 −10.569 ± 0.017 3.06 ± 0.14 1.00<br />
NGC 4365 294 186.11680 7.30393 1.00 −8.701 ± 0.025 −9.613 ± 0.238 3.14 ± 0.33 1.00<br />
NGC 4365 295 186.11696 7.30416 0.99 −8.325 ± 0.025 −9.653 ± 0.036 4.50 ± 0.31 1.00<br />
NGC 4365 296 186.12371 7.31207 0.59 −6.457 ± 0.100 −7.206 ± 0.217 3.77 ± 1.74 0.92<br />
NGC 4365 299 186.13185 7.32196 1.05 −10.013 ± 0.018 −11.351 ± 0.014 2.16 ± 0.15 0.99<br />
NGC 4365 302 186.13664 7.32788 1.54 −9.686 ± 0.017 −11.070 ± 0.017 2.74 ± 0.15 1.00<br />
NGC 4365 305 186.11615 7.30365 1.03 −7.412 ± 0.034 −8.288 ± 0.038 2.82 ± 0.23 1.00<br />
NGC 4365 306 186.12920 7.31913 0.83 −6.512 ± 0.188 −7.668 ± 0.097 2.49 ± 0.57 0.98<br />
NGC 4365 307 186.13377 7.32456 1.25 −5.924 ± 1.959 −7.319 ± 0.314 2.87 ± 0.82 0.97<br />
NGC 4365 308 186.10963 7.29608 1.67 −7.409 ± 0.420 −8.815 ± 0.023 2.38 ± 0.44 0.99<br />
NGC 4365 309 186.12774 7.31752 0.72 −7.489 ± 0.131 −8.726 ± 0.038 2.54 ± 0.32 1.00<br />
NGC 4365 310 186.10777 7.29393 1.87 −6.492 ± 0.082 −7.435 ± 0.270 3.53 ± 0.63 0.96<br />
NGC 4365 311 186.13797 7.32973 1.69 −7.148 ± 0.033 −8.485 ± 0.477 2.22 ± 0.49 0.99<br />
NGC 4365 312 186.14021 7.33236 1.92 −7.038 ± 0.092 −8.386 ± 0.045 2.73 ± 0.43 1.00<br />
NGC 4365 313 186.12248 7.31148 0.57 −7.105 ± 0.032 −8.264 ± 0.062 3.56 ± 0.45 0.99<br />
NGC 4365 314 186.14153 7.33407 2.07 −8.788 ± 0.024 −9.825 ± 0.020 3.09 ± 0.20 1.00<br />
NGC 4365 315 186.12657 7.31635 0.64 −8.642 ± 0.023 −9.592 ± 0.025 3.06 ± 0.25 1.00<br />
NGC 4365 316 186.11436 7.30193 1.17 −6.779 ± 0.079 −7.785 ± 0.138 4.76 ± 0.81 0.88<br />
NGC 4365 317 186.13121 7.32190 1.01 −6.065 ± 0.715 −7.038 ± 1.170 2.35 ± 0.72 0.96<br />
NGC 4365 318 186.12580 7.31557 0.60 −7.132 ± 0.074 −8.454 ± 0.232 2.25 ± 0.55 0.99<br />
NGC 4365 320 186.11848 7.30697 0.78 −6.882 ± 0.063 −8.043 ± 0.072 3.12 ± 0.53 0.99<br />
NGC 4365 321 186.12327 7.31266 0.54 −6.470 ± 0.063 −7.659 ± 0.286 2.99 ± 4.52 0.99<br />
NGC 4365 322 186.11395 7.30163 1.20 −6.553 ± 0.816 −7.904 ± 0.056 2.02 ± 0.52 0.97<br />
NGC 4365 323 186.13690 7.32880 1.59 −5.752 ± 0.232 −6.820 ± 0.219 3.53 ± 1.75 0.91<br />
NGC 4365 325 186.12770 7.31819 0.71 −6.761 ± 1.152 −8.104 ± 0.694 1.55 ± 0.50 0.96<br />
NGC 4365 326 186.12964 7.32055 0.87 −7.058 ± 0.047 −8.866 ± 0.109 6.00 ± 0.71 0.97<br />
NGC 4365 327 186.12137 7.31080 0.57 −7.335 ± 0.062 −8.539 ± 0.061 4.39 ± 0.41 0.98<br />
NGC 4365 328 186.12644 7.31680 0.63 −6.389 ± 0.148 −7.889 ± 0.283 7.16 ± 2.18 0.55<br />
NGC 4365 329 186.11785 7.30665 0.80 −7.990 ± 0.025 −8.767 ± 0.045 3.58 ± 0.29 1.00<br />
NGC 4365 330 186.10672 7.29361 1.92 −7.270 ± 0.056 −8.597 ± 0.041 3.23 ± 0.31 1.00<br />
NGC 4365 332 186.14019 7.33338 1.96 −9.504 ± 0.022 −10.660 ± 0.019 3.45 ± 0.18 1.00<br />
NGC 4365 333 186.11508 7.30365 1.04 −7.139 ± 0.130 −8.648 ± 0.041 2.56 ± 0.32 1.00<br />
NGC 4365 334 186.12715 7.31799 0.67 −7.224 ± 0.028 −8.189 ± 0.056 2.14 ± 0.42 0.98<br />
NGC 4365 335 186.12233 7.31237 0.51 −8.220 ± 0.026 −9.474 ± 0.020 1.82 ± 0.20 0.98<br />
NGC 4365 336 186.13350 7.32561 1.26 −7.069 ± 0.039 −8.363 ± 0.052 2.32 ± 0.42 0.99<br />
NGC 4365 337 186.11928 7.30886 0.65 −8.330 ± 0.026 −9.697 ± 0.423 1.85 ± 0.35 0.98<br />
NGC 4365 338 186.13404 7.32643 1.32 −7.362 ± 0.043 −8.465 ± 0.042 3.83 ± 0.34 0.99<br />
NGC 4365 339 186.12681 7.31788 0.65 −8.631 ± 0.029 −9.873 ± 0.022 1.72 ± 0.27 0.97<br />
NGC 4365 340 186.11094 7.29929 1.42 −9.115 ± 0.045 −10.102 ± 0.019 2.75 ± 0.32 1.00<br />
NGC 4365 341 186.11949 7.30937 0.62 −7.397 ± 0.056 −8.607 ± 0.044 2.37 ± 0.32 0.99<br />
NGC 4365 342 186.12337 7.31406 0.48 −8.034 ± 0.352 −9.254 ± 0.455 2.26 ± 0.48 1.00<br />
NGC 4365 343 186.12311 7.31388 0.48 −7.148 ± 0.067 −8.671 ± 0.314 3.50 ± 0.73 1.00<br />
NGC 4365 344 186.12276 7.31357 0.47 −9.675 ± 0.014 −10.531 ± 0.017 4.30 ± 0.14 1.00<br />
NGC 4365 345 186.11538 7.30476 0.96 −7.711 ± 0.052 −9.147 ± 0.027 1.47 ± 0.26 0.95<br />
NGC 4365 346 186.13588 7.32868 1.52 −7.712 ± 0.033 −8.587 ± 0.034 3.35 ± 0.28 1.00<br />
NGC 4365 347 186.13448 7.32752 1.39 −9.706 ± 0.013 −11.047 ± 0.029 4.05 ± 0.16 1.00<br />
NGC 4365 348 186.13575 7.32901 1.52 −7.412 ± 0.022 −8.338 ± 0.266 2.79 ± 0.39 1.00<br />
NGC 4365 349 186.12451 7.31567 0.51 −6.056 ± 0.941 −7.532 ± 0.217 3.03 ± 0.85 0.98<br />
NGC 4365 351 186.13532 7.32872 1.49 −9.100 ± 0.026 −10.368 ± 0.022 3.34 ± 0.26 1.00<br />
NGC 4365 352 186.13303 7.32595 1.24 −7.045 ± 0.052 −8.043 ± 0.063 3.26 ± 0.40 0.99<br />
Continued on Next Page. . .<br />
300
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4365 353 186.11978 7.30969 0.60 −9.717 ± 0.018 −10.989 ± 0.015 3.05 ± 0.31 1.00<br />
NGC 4365 355 186.11992 7.31051 0.55 −9.287 ± 0.025 −10.259 ± 0.022 3.03 ± 0.31 1.00<br />
NGC 4365 356 186.12436 7.31577 0.49 −8.180 ± 0.026 −9.702 ± 0.024 3.68 ± 0.21 1.00<br />
NGC 4365 357 186.14015 7.33450 2.01 −8.919 ± 0.035 −9.828 ± 0.020 3.04 ± 0.26 1.00<br />
NGC 4365 359 186.12139 7.31234 0.47 −7.638 ± 0.054 −8.417 ± 0.059 1.90 ± 0.38 0.98<br />
NGC 4365 361 186.13879 7.33294 1.86 −7.128 ± 0.056 −8.297 ± 1.315 2.34 ± 0.53 0.99<br />
NGC 4365 363 186.14047 7.33500 2.05 −7.512 ± 0.048 −8.588 ± 0.040 3.88 ± 0.39 0.99<br />
NGC 4365 365 186.13434 7.32800 1.40 −7.207 ± 0.049 −8.064 ± 0.057 2.36 ± 0.45 0.99<br />
NGC 4365 366 186.13153 7.32468 1.11 −6.104 ± 0.189 −7.835 ± 0.226 7.00 ± 2.94 0.55<br />
NGC 4365 367 186.12424 7.31607 0.48 −6.816 ± 0.061 −8.311 ± 0.136 4.30 ± 0.85 0.98<br />
NGC 4365 368 186.12697 7.31887 0.66 −6.573 ± 0.093 −7.234 ± 0.584 1.70 ± 0.86 0.92<br />
NGC 4365 370 186.13336 7.32707 1.30 −7.645 ± 0.025 −8.714 ± 0.028 2.26 ± 0.31 0.99<br />
NGC 4365 371 186.11915 7.31032 0.55 −7.055 ± 0.039 −8.112 ± 0.099 3.94 ± 0.60 0.98<br />
NGC 4365 372 186.11255 7.30253 1.16 −6.005 ± 0.546 −7.501 ± 0.048 3.03 ± 0.66 0.98<br />
NGC 4365 375 186.13989 7.33504 2.02 −8.590 ± 0.030 −9.477 ± 0.020 2.94 ± 0.26 1.00<br />
NGC 4365 378 186.12854 7.32173 0.82 −6.324 ± 1.001 −8.003 ± 0.120 2.75 ± 0.76 0.99<br />
NGC 4365 380 186.11694 7.30807 0.70 −7.910 ± 0.029 −9.525 ± 0.026 3.97 ± 0.21 1.00<br />
NGC 4365 381 186.12428 7.31686 0.47 −6.906 ± 0.173 −8.534 ± 0.252 1.85 ± 0.67 0.98<br />
NGC 4365 382 186.11991 7.31179 0.46 −9.135 ± 0.025 −10.073 ± 0.021 2.79 ± 0.21 1.00<br />
NGC 4365 383 186.12030 7.31224 0.44 −7.443 ± 0.044 −9.060 ± 0.034 2.84 ± 0.38 1.00<br />
NGC 4365 384 186.10852 7.29835 1.55 −8.681 ± 0.044 −9.526 ± 0.031 3.43 ± 0.41 1.00<br />
NGC 4365 386 186.12751 7.32079 0.73 −6.993 ± 0.051 −8.133 ± 0.409 2.11 ± 0.52 0.98<br />
NGC 4365 387 186.11945 7.31126 0.49 −7.625 ± 0.023 −8.811 ± 0.038 3.08 ± 0.27 1.00<br />
NGC 4365 388 186.11655 7.30785 0.72 −7.298 ± 0.047 −8.196 ± 0.328 3.48 ± 0.64 0.99<br />
NGC 4365 389 186.13808 7.33332 1.84 −6.899 ± 0.049 −8.281 ± 0.439 3.09 ± 0.51 1.00<br />
NGC 4365 392 186.13530 7.33023 1.55 −6.968 ± 0.045 −7.918 ± 0.059 2.80 ± 0.48 0.99<br />
NGC 4365 393 186.11382 7.30488 0.97 −7.434 ± 0.025 −8.695 ± 0.041 2.76 ± 0.39 1.00<br />
NGC 4365 394 186.11217 7.30295 1.14 −6.573 ± 0.056 −7.794 ± 0.051 3.37 ± 0.48 0.98<br />
NGC 4365 395 186.12128 7.31392 0.38 −9.657 ± 0.025 −10.706 ± 0.016 2.79 ± 0.23 1.00<br />
NGC 4365 396 186.11170 7.30263 1.18 −7.185 ± 0.029 −8.198 ± 0.057 2.83 ± 0.35 0.99<br />
NGC 4365 397 186.12523 7.31865 0.54 −6.961 ± 0.068 −8.245 ± 0.594 2.70 ± 0.57 0.99<br />
NGC 4365 398 186.10844 7.29890 1.52 −6.596 ± 0.058 −7.769 ± 1.861 2.33 ± 0.61 0.98<br />
NGC 4365 401 186.12836 7.32252 0.83 −7.868 ± 0.028 −8.706 ± 0.032 2.47 ± 0.40 1.00<br />
NGC 4365 402 186.11030 7.30118 1.31 −7.771 ± 0.027 −8.596 ± 0.034 2.70 ± 0.34 1.00<br />
NGC 4365 403 186.12119 7.31410 0.36 −7.535 ± 0.058 −8.911 ± 0.170 2.34 ± 0.41 1.00<br />
NGC 4365 406 186.11333 7.30496 0.98 −8.478 ± 0.027 −9.611 ± 0.019 2.60 ± 0.21 1.00<br />
NGC 4365 407 186.10933 7.30031 1.40 −8.538 ± 0.038 −10.023 ± 0.026 3.85 ± 0.35 1.00<br />
NGC 4365 408 186.13884 7.33519 1.97 −7.094 ± 0.056 −7.942 ± 0.055 2.96 ± 0.44 0.99<br />
NGC 4365 409 186.11590 7.30808 0.71 −7.221 ± 0.051 −8.578 ± 0.106 4.65 ± 0.87 0.98<br />
NGC 4365 410 186.12955 7.32438 0.97 −10.006 ± 0.019 −11.247 ± 0.013 3.18 ± 0.17 1.00<br />
NGC 4365 412 186.11952 7.31246 0.40 −7.964 ± 0.032 −8.880 ± 0.037 2.64 ± 0.26 1.00<br />
NGC 4365 414 186.11512 7.30738 0.77 −7.443 ± 0.040 −8.372 ± 0.063 3.32 ± 0.45 1.00<br />
NGC 4365 415 186.12360 7.31745 0.42 −7.869 ± 0.032 −8.628 ± 0.430 2.01 ± 0.35 0.99<br />
NGC 4365 416 186.11804 7.31091 0.50 −7.284 ± 0.053 −8.145 ± 0.303 3.39 ± 0.63 0.99<br />
NGC 4365 417 186.11051 7.30202 1.25 −7.633 ± 0.270 −8.896 ± 0.033 1.93 ± 0.35 0.98<br />
NGC 4365 418 186.11356 7.30589 0.91 −10.346 ± 0.024 −11.567 ± 0.016 3.33 ± 0.21 1.00<br />
NGC 4365 420 186.12956 7.32482 0.99 −6.773 ± 1.152 −7.573 ± 0.051 1.57 ± 0.44 0.93<br />
NGC 4365 423 186.12312 7.31732 0.38 −6.692 ± 1.081 −8.183 ± 0.141 2.73 ± 1.02 0.99<br />
NGC 4365 425 186.10600 7.29688 1.73 −8.022 ± 0.030 −8.845 ± 0.763 1.66 ± 0.34 0.97<br />
NGC 4365 426 186.12234 7.31652 0.34 −8.066 ± 0.048 −8.968 ± 0.360 2.59 ± 0.68 1.00<br />
NGC 4365 427 186.11058 7.30258 1.21 −6.099 ± 0.066 −7.544 ± 0.249 2.99 ± 1.31 0.98<br />
NGC 4365 428 186.12447 7.31917 0.49 −8.354 ± 0.028 −9.487 ± 0.029 1.73 ± 0.27 0.98<br />
NGC 4365 429 186.12162 7.31580 0.31 −7.902 ± 0.039 −9.393 ± 0.040 2.20 ± 0.33 1.00<br />
NGC 4365 430 186.13309 7.32940 1.38 −7.452 ± 0.046 −8.386 ± 0.046 3.65 ± 0.33 0.99<br />
NGC 4365 431 186.13002 7.32593 1.06 −9.452 ± 0.019 −10.711 ± 0.022 3.79 ± 0.13 1.00<br />
NGC 4365 432 186.11322 7.30600 0.91 −6.487 ± 0.312 −7.628 ± 0.359 2.27 ± 0.70 0.97<br />
NGC 4365 433 186.12900 7.32470 0.95 −7.630 ± 0.032 −8.888 ± 0.044 1.64 ± 0.31 0.97<br />
NGC 4365 434 186.12276 7.31733 0.36 −8.141 ± 0.046 −9.343 ± 0.069 4.35 ± 0.38 1.00<br />
NGC 4365 435 186.11560 7.30903 0.65 −8.412 ± 0.025 −9.582 ± 0.020 2.05 ± 0.19 0.99<br />
NGC 4365 437 186.12611 7.32150 0.66 −6.701 ± 0.228 −8.230 ± 0.059 1.89 ± 0.74 0.98<br />
NGC 4365 438 186.11574 7.30927 0.63 −6.461 ± 0.199 −7.557 ± 0.118 3.12 ± 0.65 0.98<br />
NGC 4365 441 186.10363 7.29502 1.93 −5.625 ± 0.282 −6.895 ± 0.110 3.68 ± 0.75 0.90<br />
Continued on Next Page. . .<br />
301
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4365 443 186.12866 7.32468 0.93 −7.143 ± 0.141 −8.420 ± 0.050 2.45 ± 0.41 0.99<br />
NGC 4365 444 186.11702 7.31094 0.50 −7.746 ± 0.052 −9.209 ± 0.787 1.47 ± 0.41 0.95<br />
NGC 4365 445 186.12285 7.31790 0.36 −9.121 ± 0.038 −9.904 ± 0.019 3.04 ± 0.20 1.00<br />
NGC 4365 448 186.11712 7.31116 0.48 −7.211 ± 0.073 −8.521 ± 0.069 4.09 ± 0.37 0.99<br />
NGC 4365 449 186.11970 7.31438 0.28 −8.750 ± 0.033 −9.886 ± 0.041 2.89 ± 0.33 1.00<br />
NGC 4365 450 186.12605 7.32215 0.67 −7.789 ± 0.028 −8.884 ± 0.052 2.69 ± 0.32 1.00<br />
NGC 4365 452 186.12239 7.31796 0.33 −8.651 ± 0.024 −9.998 ± 0.025 2.93 ± 0.30 1.00<br />
NGC 4365 453 186.12461 7.32069 0.53 −8.779 ± 0.018 −9.625 ± 0.023 2.41 ± 0.22 1.00<br />
NGC 4365 454 186.13395 7.33171 1.54 −7.003 ± 0.045 −7.845 ± 0.053 3.34 ± 0.57 0.99<br />
NGC 4365 455 186.13252 7.33009 1.38 −7.570 ± 0.028 −8.720 ± 0.847 2.18 ± 0.53 0.99<br />
NGC 4365 456 186.12230 7.31802 0.32 −7.599 ± 0.606 −8.886 ± 0.058 2.21 ± 0.46 1.00<br />
NGC 4365 459 186.11945 7.31476 0.25 −6.984 ± 0.392 −8.416 ± 0.401 2.81 ± 0.96 1.00<br />
NGC 4365 460 186.13446 7.33252 1.60 −6.140 ± 0.411 −7.411 ± 0.066 3.41 ± 0.76 0.96<br />
NGC 4365 462 186.11890 7.31418 0.27 −9.162 ± 0.018 −10.069 ± 0.030 2.58 ± 0.27 1.00<br />
NGC 4365 464 186.11876 7.31435 0.26 −7.942 ± 0.041 −9.396 ± 0.049 2.90 ± 0.37 1.00<br />
NGC 4365 465 186.11022 7.30428 1.12 −8.087 ± 0.038 −9.104 ± 0.030 3.19 ± 0.28 1.00<br />
NGC 4365 466 186.10707 7.30059 1.46 −9.434 ± 0.017 −10.402 ± 0.031 3.46 ± 0.27 1.00<br />
NGC 4365 467 186.12178 7.31798 0.29 −6.956 ± 0.096 −8.418 ± 0.348 3.95 ± 0.76 0.99<br />
NGC 4365 468 186.12248 7.31885 0.35 −8.261 ± 0.037 −9.258 ± 0.029 2.47 ± 0.24 1.00<br />
NGC 4365 469 186.11606 7.31134 0.48 −8.546 ± 0.029 −9.857 ± 0.326 1.92 ± 0.28 0.98<br />
NGC 4365 471 186.12179 7.31830 0.29 −6.982 ± 0.089 −8.575 ± 0.098 2.43 ± 0.47 0.99<br />
NGC 4365 472 186.10622 7.29871 1.61 −9.102 ± 0.026 −10.104 ± 0.017 3.20 ± 0.28 1.00<br />
NGC 4365 473 186.11397 7.30960 0.65 −9.484 ± 0.019 −10.568 ± 0.034 3.79 ± 0.28 1.00<br />
NGC 4365 475 186.12123 7.31781 0.25 −9.126 ± 0.028 −10.203 ± 0.028 3.02 ± 0.26 1.00<br />
NGC 4365 477 186.13262 7.33131 1.45 −6.338 ± 0.186 −7.920 ± 0.085 2.66 ± 0.65 0.99<br />
NGC 4365 478 186.11002 7.30465 1.10 −8.219 ± 0.028 −9.566 ± 0.018 3.04 ± 0.28 1.00<br />
NGC 4365 479 186.12463 7.32197 0.58 −8.081 ± 0.049 −9.381 ± 0.028 2.16 ± 0.34 0.99<br />
NGC 4365 480 186.13330 7.33224 1.53 −6.393 ± 0.060 −7.912 ± 0.044 2.65 ± 0.45 0.99<br />
NGC 4365 481 186.10641 7.30052 1.49 −7.970 ± 0.033 −9.231 ± 0.057 3.17 ± 0.36 1.00<br />
NGC 4365 483 186.11185 7.30711 0.88 −7.863 ± 0.026 −8.816 ± 0.036 2.46 ± 0.28 1.00<br />
NGC 4365 484 186.10527 7.29945 1.60 −7.715 ± 0.029 −8.746 ± 0.027 3.71 ± 0.37 0.99<br />
NGC 4365 485 186.11417 7.30999 0.62 −6.542 ± 0.135 −7.848 ± 0.095 4.30 ± 1.00 0.94<br />
NGC 4365 486 186.13313 7.33248 1.53 −6.235 ± 0.170 −7.233 ± 0.136 5.56 ± 1.11 0.61<br />
NGC 4365 487 186.10635 7.30085 1.47 −7.133 ± 0.046 −7.871 ± 0.287 3.13 ± 0.45 0.99<br />
NGC 4365 488 186.12813 7.32668 0.98 −7.646 ± 0.399 −8.997 ± 0.043 2.55 ± 0.49 1.00<br />
NGC 4365 489 186.12491 7.32290 0.63 −7.270 ± 0.203 −8.216 ± 0.881 1.50 ± 0.43 0.96<br />
NGC 4365 490 186.11121 7.30676 0.92 −8.013 ± 0.033 −9.060 ± 0.035 3.53 ± 0.29 1.00<br />
NGC 4365 492 186.13684 7.33717 1.96 −7.673 ± 0.027 −8.960 ± 0.031 2.24 ± 0.27 1.00<br />
NGC 4365 493 186.11049 7.30603 1.00 −5.973 ± 0.310 −7.246 ± 0.086 3.24 ± 0.65 0.96<br />
NGC 4365 495 186.12896 7.32789 1.09 −6.293 ± 0.513 −7.412 ± 0.082 4.09 ± 0.97 0.91<br />
NGC 4365 496 186.12344 7.32149 0.49 −8.837 ± 0.034 −9.762 ± 0.034 3.41 ± 0.29 1.00<br />
NGC 4365 498 186.13202 7.33176 1.44 −6.118 ± 0.184 −7.409 ± 0.071 3.41 ± 0.54 0.96<br />
NGC 4365 499 186.12276 7.32082 0.42 −7.314 ± 0.052 −8.713 ± 0.078 1.96 ± 0.49 0.99<br />
NGC 4365 500 186.13350 7.33356 1.60 −7.385 ± 0.046 −8.858 ± 0.028 2.31 ± 0.36 1.00<br />
NGC 4365 501 186.11462 7.31130 0.52 −9.904 ± 0.010 −10.960 ± 0.015 4.87 ± 0.12 1.00<br />
NGC 4365 502 186.11673 7.31375 0.30 −8.221 ± 0.161 −9.684 ± 0.449 2.36 ± 0.47 1.00<br />
NGC 4365 503 186.13697 7.33811 2.01 −6.272 ± 0.077 −7.488 ± 0.056 3.99 ± 0.58 0.93<br />
NGC 4365 504 186.13585 7.33681 1.89 −6.941 ± 0.049 −8.254 ± 0.026 2.23 ± 0.35 0.99<br />
NGC 4365 505 186.11050 7.30691 0.94 −8.144 ± 0.036 −9.104 ± 0.026 2.76 ± 0.19 1.00<br />
NGC 4365 509 186.13165 7.33212 1.44 −7.717 ± 0.027 −8.939 ± 0.028 1.76 ± 0.20 0.98<br />
NGC 4365 510 186.12181 7.32050 0.35 −7.749 ± 0.040 −8.860 ± 0.079 2.53 ± 0.58 1.00<br />
NGC 4365 511 186.10631 7.30221 1.39 −9.022 ± 0.049 −10.238 ± 0.024 2.02 ± 0.33 0.98<br />
NGC 4365 512 186.12619 7.32574 0.83 −7.718 ± 1.306 −9.129 ± 0.926 2.69 ± 0.69 1.00<br />
NGC 4365 513 186.10954 7.30625 1.02 −8.561 ± 0.024 −9.374 ± 0.028 3.05 ± 0.25 1.00<br />
NGC 4365 515 186.11357 7.31107 0.57 −7.482 ± 0.068 −8.884 ± 0.030 2.77 ± 0.42 1.00<br />
NGC 4365 516 186.12769 7.32783 1.02 −8.214 ± 0.265 −9.317 ± 0.027 1.60 ± 0.34 0.97<br />
NGC 4365 517 186.11926 7.31783 0.11 −7.754 ± 0.287 −9.313 ± 0.111 2.55 ± 1.14 1.00<br />
NGC 4365 518 186.12458 7.32426 0.68 −7.033 ± 0.627 −8.108 ± 0.621 3.13 ± 0.81 0.99<br />
NGC 4365 522 186.13428 7.33592 1.77 −6.785 ± 0.097 −7.665 ± 0.091 6.78 ± 0.73 0.51<br />
NGC 4365 523 186.11963 7.31861 0.15 −7.173 ± 0.144 −8.821 ± 0.391 3.54 ± 0.87 1.00<br />
NGC 4365 524 186.10390 7.30012 1.62 −7.698 ± 0.032 −8.530 ± 0.043 2.44 ± 0.34 0.99<br />
NGC 4365 526 186.11789 7.31673 0.08 −7.663 ± 0.104 −9.138 ± 0.407 1.95 ± 0.47 0.99<br />
Continued on Next Page. . .<br />
302
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4365 529 186.11621 7.31482 0.24 −7.317 ± 0.075 −8.756 ± 0.042 2.07 ± 0.47 0.99<br />
NGC 4365 530 186.10896 7.30630 1.04 −7.522 ± 0.053 −9.047 ± 0.028 3.63 ± 0.31 1.00<br />
NGC 4365 531 186.12215 7.32189 0.43 −7.092 ± 0.440 −8.073 ± 0.760 1.79 ± 0.42 0.97<br />
NGC 4365 532 186.12003 7.31942 0.20 −7.224 ± 0.301 −8.530 ± 0.068 2.34 ± 0.70 0.99<br />
NGC 4365 533 186.13033 7.33165 1.35 −6.892 ± 0.061 −8.100 ± 0.030 2.74 ± 0.36 0.99<br />
NGC 4365 536 186.11725 7.31625 0.12 −8.429 ± 0.030 −9.825 ± 0.154 2.99 ± 0.34 1.00<br />
NGC 4365 537 186.11237 7.31060 0.65 −7.719 ± 0.047 −8.769 ± 0.058 2.65 ± 0.37 1.00<br />
NGC 4365 539 186.12390 7.32434 0.65 −8.483 ± 0.027 −9.714 ± 0.030 2.28 ± 0.24 1.00<br />
NGC 4365 540 186.11271 7.31110 0.60 −7.934 ± 0.345 −8.932 ± 0.077 3.06 ± 0.48 1.00<br />
NGC 4365 542 186.12961 7.33154 1.31 −9.701 ± 0.018 −11.028 ± 0.018 2.44 ± 0.14 1.00<br />
NGC 4365 543 186.13587 7.33872 1.99 −5.763 ± 0.193 −7.126 ± 0.217 5.41 ± 1.65 0.61<br />
NGC 4365 544 186.11389 7.31302 0.44 −9.213 ± 0.028 −10.282 ± 0.021 2.14 ± 0.29 0.99<br />
NGC 4365 545 186.12712 7.32870 1.04 −8.795 ± 0.023 −9.645 ± 0.021 3.01 ± 0.21 1.00<br />
NGC 4365 546 186.10864 7.30679 1.03 −6.749 ± 0.096 −7.801 ± 0.523 1.83 ± 0.52 0.96<br />
NGC 4365 547 186.12230 7.32301 0.50 −6.649 ± 0.374 −8.060 ± 0.112 3.18 ± 0.77 0.99<br />
NGC 4365 548 186.11278 7.31182 0.56 −7.339 ± 0.046 −8.596 ± 0.041 2.85 ± 0.36 1.00<br />
NGC 4365 549 186.12170 7.32239 0.44 −6.763 ± 0.544 −8.017 ± 0.494 1.62 ± 0.46 0.96<br />
NGC 4365 551 186.12153 7.32231 0.42 −7.113 ± 1.230 −8.222 ± 0.093 1.63 ± 0.71 0.97<br />
NGC 4365 552 186.11466 7.31421 0.34 −7.238 ± 0.297 −8.259 ± 0.169 2.42 ± 0.65 0.99<br />
NGC 4365 553 186.11574 7.31554 0.22 −9.395 ± 0.024 −10.789 ± 0.031 4.13 ± 0.26 1.00<br />
NGC 4365 554 186.11581 7.31580 0.20 −7.005 ± 0.099 −8.410 ± 0.838 2.78 ± 0.65 1.00<br />
NGC 4365 555 186.11624 7.31637 0.15 −6.523 ± 0.970 −8.367 ± 0.260 3.81 ± 2.16 0.99<br />
NGC 4365 556 186.10699 7.30553 1.18 −8.020 ± 0.030 −8.745 ± 0.030 3.64 ± 0.30 1.00<br />
NGC 4365 557 186.10930 7.30824 0.92 −8.323 ± 0.047 −9.336 ± 0.030 3.06 ± 0.33 1.00<br />
NGC 4365 560 186.12451 7.32636 0.79 −7.064 ± 0.086 −8.573 ± 0.030 3.10 ± 0.35 1.00<br />
NGC 4365 561 186.11749 7.31815 0.03 −8.438 ± 0.047 −9.520 ± 0.314 2.13 ± 0.37 0.99<br />
NGC 4365 562 186.13428 7.33805 1.88 −5.937 ± 0.082 −7.556 ± 0.064 3.27 ± 0.59 0.98<br />
NGC 4365 563 186.11671 7.31736 0.08 −9.068 ± 0.038 −10.628 ± 0.072 5.16 ± 0.44 1.00<br />
NGC 4365 564 186.11670 7.31749 0.08 −9.293 ± 0.025 −10.384 ± 0.029 1.73 ± 0.23 0.97<br />
NGC 4365 565 186.11209 7.31193 0.59 −7.600 ± 0.037 −8.566 ± 0.046 2.99 ± 0.42 1.00<br />
NGC 4365 566 186.10733 7.30626 1.12 −6.224 ± 0.120 −7.873 ± 0.051 6.06 ± 0.85 0.75<br />
NGC 4365 567 186.11732 7.31814 0.04 −9.438 ± 0.026 −10.647 ± 0.031 2.96 ± 0.34 1.00<br />
NGC 4365 569 186.10654 7.30558 1.19 −8.496 ± 0.020 −9.493 ± 0.020 3.30 ± 0.22 1.00<br />
NGC 4365 571 186.10870 7.30813 0.95 −7.057 ± 0.037 −7.797 ± 0.083 2.70 ± 0.37 0.99<br />
NGC 4365 572 186.10765 7.30698 1.07 −8.754 ± 0.023 −10.136 ± 0.028 4.91 ± 0.21 1.00<br />
NGC 4365 573 186.12084 7.32252 0.41 −7.227 ± 0.030 −8.457 ± 0.610 1.84 ± 0.55 0.98<br />
NGC 4365 575 186.13301 7.33700 1.77 −8.450 ± 0.037 −9.706 ± 0.023 4.02 ± 0.26 1.00<br />
NGC 4365 576 186.11963 7.32125 0.29 −6.678 ± 0.398 −8.306 ± 0.175 5.21 ± 1.33 0.94<br />
NGC 4365 578 186.12357 7.32591 0.72 −6.455 ± 1.211 −7.797 ± 0.365 1.62 ± 0.53 0.94<br />
NGC 4365 580 186.12420 7.32674 0.80 −6.928 ± 0.047 −7.684 ± 0.086 2.81 ± 0.47 0.99<br />
NGC 4365 581 186.12068 7.32271 0.41 −8.473 ± 0.028 −9.918 ± 0.020 2.38 ± 0.21 1.00<br />
NGC 4365 582 186.11304 7.31366 0.45 −9.231 ± 0.013 −10.297 ± 0.020 3.46 ± 0.17 1.00<br />
NGC 4365 583 186.12677 7.33000 1.09 −7.136 ± 0.287 −8.506 ± 0.346 2.31 ± 0.53 0.99<br />
NGC 4365 584 186.13078 7.33478 1.54 −6.494 ± 0.095 −7.494 ± 0.316 3.95 ± 1.13 0.94<br />
NGC 4365 585 186.11311 7.31392 0.44 −6.127 ± 0.775 −7.686 ± 0.119 3.06 ± 0.76 0.99<br />
NGC 4365 586 186.10598 7.30558 1.22 −6.002 ± 1.106 −7.814 ± 0.885 1.28 ± 0.55 0.90<br />
NGC 4365 587 186.12059 7.32291 0.42 −7.318 ± 0.065 −9.138 ± 0.922 1.15 ± 0.42 0.91<br />
NGC 4365 589 186.11777 7.31974 0.14 −9.477 ± 0.014 −10.505 ± 0.026 2.54 ± 0.19 1.00<br />
NGC 4365 590 186.11418 7.31548 0.31 −7.831 ± 0.034 −9.331 ± 0.350 3.53 ± 0.37 1.00<br />
NGC 4365 592 186.11434 7.31577 0.29 −8.435 ± 0.035 −9.809 ± 0.029 2.56 ± 0.36 1.00<br />
NGC 4365 593 186.10245 7.30172 1.60 −6.527 ± 0.089 −7.201 ± 0.605 1.96 ± 0.59 0.94<br />
NGC 4365 594 186.12184 7.32476 0.58 −7.921 ± 0.047 −9.175 ± 0.044 1.39 ± 0.36 0.95<br />
NGC 4365 595 186.11438 7.31588 0.28 −6.898 ± 0.939 −8.451 ± 0.474 2.46 ± 0.61 0.99<br />
NGC 4365 596 186.13109 7.33586 1.62 −10.212 ± 0.019 −11.498 ± 0.014 2.78 ± 0.11 1.00<br />
NGC 4365 597 186.12282 7.32597 0.69 −7.714 ± 0.033 −9.112 ± 0.029 1.91 ± 0.28 0.98<br />
NGC 4365 598 186.11778 7.32001 0.16 −8.712 ± 0.033 −9.923 ± 0.025 3.30 ± 0.27 1.00<br />
NGC 4365 599 186.10042 7.29949 1.82 −8.820 ± 0.030 −10.141 ± 0.024 2.23 ± 0.28 1.00<br />
NGC 4365 600 186.12767 7.33181 1.24 −6.557 ± 0.597 −7.171 ± 0.603 2.03 ± 0.67 0.95<br />
NGC 4365 602 186.11580 7.31793 0.14 −8.034 ± 0.089 −9.235 ± 0.035 2.26 ± 0.37 1.00<br />
NGC 4365 603 186.11978 7.32265 0.38 −6.417 ± 0.436 −7.979 ± 0.111 3.79 ± 0.60 0.98<br />
NGC 4365 606 186.11334 7.31507 0.37 −6.994 ± 0.089 −8.404 ± 0.079 2.30 ± 0.56 0.99<br />
NGC 4365 607 186.12166 7.32511 0.60 −10.318 ± 0.020 −11.553 ± 0.020 4.23 ± 0.16 1.00<br />
Continued on Next Page. . .<br />
303
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4365 609 186.11197 7.31380 0.51 −8.161 ± 0.030 −9.395 ± 0.282 3.45 ± 0.40 1.00<br />
NGC 4365 610 186.11818 7.32113 0.24 −7.677 ± 0.060 −9.127 ± 0.075 2.18 ± 0.48 0.99<br />
NGC 4365 611 186.12564 7.33000 1.05 −6.915 ± 0.089 −7.688 ± 0.574 2.43 ± 0.52 0.98<br />
NGC 4365 612 186.11923 7.32246 0.35 −8.650 ± 0.045 −10.056 ± 0.025 2.90 ± 0.37 1.00<br />
NGC 4365 613 186.10134 7.30124 1.68 −7.168 ± 0.240 −8.590 ± 0.033 1.93 ± 0.36 0.98<br />
NGC 4365 614 186.11348 7.31564 0.34 −8.156 ± 0.348 −9.102 ± 0.487 2.02 ± 0.94 0.99<br />
NGC 4365 615 186.12831 7.33324 1.35 −8.156 ± 0.149 −9.571 ± 0.032 2.70 ± 0.45 1.00<br />
NGC 4365 616 186.11744 7.32035 0.19 −7.642 ± 0.468 −8.470 ± 0.097 3.35 ± 0.62 1.00<br />
NGC 4365 617 186.11908 7.32231 0.34 −6.856 ± 0.069 −7.966 ± 1.742 2.04 ± 0.60 0.98<br />
NGC 4365 618 186.13362 7.33964 1.95 −5.577 ± 0.429 −7.187 ± 0.287 4.33 ± 1.85 0.86<br />
NGC 4365 619 186.11566 7.31851 0.16 −9.427 ± 0.025 −10.398 ± 0.024 2.83 ± 0.26 1.00<br />
NGC 4365 620 186.10335 7.30397 1.44 −8.439 ± 0.029 −9.656 ± 0.017 2.05 ± 0.26 0.99<br />
NGC 4365 621 186.12256 7.32674 0.73 −9.105 ± 0.028 −10.332 ± 0.015 1.92 ± 0.19 0.98<br />
NGC 4365 622 186.12375 7.32816 0.86 −8.394 ± 0.119 −9.858 ± 0.024 1.73 ± 0.31 0.97<br />
NGC 4365 623 186.11435 7.31707 0.25 −7.004 ± 1.358 −8.293 ± 0.585 1.53 ± 0.59 0.96<br />
NGC 4365 624 186.10943 7.31127 0.76 −6.506 ± 0.127 −7.895 ± 0.617 1.87 ± 0.75 0.96<br />
NGC 4365 625 186.09962 7.29968 1.85 −6.109 ± 0.218 −7.101 ± 0.313 4.01 ± 1.68 0.89<br />
NGC 4365 626 186.12168 7.32591 0.65 −7.187 ± 0.050 −8.370 ± 0.047 2.60 ± 0.41 0.99<br />
NGC 4365 627 186.11237 7.31485 0.44 −6.787 ± 0.079 −7.693 ± 0.074 3.17 ± 0.60 0.99<br />
NGC 4365 628 186.10768 7.30946 0.94 −8.068 ± 0.031 −9.417 ± 0.018 2.52 ± 0.17 1.00<br />
NGC 4365 629 186.10849 7.31050 0.85 −8.822 ± 0.020 −10.042 ± 0.015 2.41 ± 0.09 1.00<br />
NGC 4365 630 186.11568 7.31898 0.17 −6.545 ± 0.164 −8.029 ± 1.078 1.70 ± 0.44 0.96<br />
NGC 4365 631 186.12501 7.33006 1.03 −6.595 ± 0.133 −7.764 ± 0.052 2.65 ± 0.93 0.99<br />
NGC 4365 632 186.11745 7.32123 0.25 −8.397 ± 0.215 −9.861 ± 0.024 1.96 ± 0.34 0.98<br />
NGC 4365 633 186.12502 7.33017 1.04 −7.422 ± 0.043 −8.233 ± 0.054 3.71 ± 0.42 0.99<br />
NGC 4365 634 186.10988 7.31231 0.69 −6.612 ± 0.186 −7.369 ± 0.626 1.50 ± 0.99 0.91<br />
NGC 4365 635 186.10596 7.30781 1.11 −8.664 ± 0.019 −10.235 ± 0.021 3.83 ± 0.16 1.00<br />
NGC 4365 637 186.10457 7.30622 1.26 −9.043 ± 0.023 −10.330 ± 0.018 3.21 ± 0.16 1.00<br />
NGC 4365 638 186.12834 7.33437 1.42 −8.974 ± 0.026 −10.244 ± 0.020 4.07 ± 0.14 1.00<br />
NGC 4365 639 186.11423 7.31768 0.25 −8.847 ± 0.032 −9.865 ± 0.029 2.26 ± 0.30 1.00<br />
NGC 4365 640 186.11177 7.31473 0.48 −7.038 ± 0.437 −8.149 ± 0.182 4.16 ± 1.18 0.97<br />
NGC 4365 641 186.09900 7.29971 1.88 −6.120 ± 0.168 −6.759 ± 0.900 2.27 ± 0.74 0.95<br />
NGC 4365 642 186.11030 7.31323 0.63 −7.999 ± 0.116 −8.652 ± 0.106 5.75 ± 1.22 0.96<br />
NGC 4365 644 186.10259 7.30409 1.47 −7.851 ± 0.039 −8.849 ± 0.023 2.16 ± 0.28 0.99<br />
NGC 4365 645 186.11107 7.31419 0.55 −8.197 ± 0.022 −9.305 ± 0.016 3.08 ± 0.31 1.00<br />
NGC 4365 646 186.10301 7.30484 1.41 −7.787 ± 0.033 −8.918 ± 0.045 3.52 ± 0.36 1.00<br />
NGC 4365 647 186.11325 7.31701 0.33 −8.961 ± 0.018 −10.457 ± 0.016 3.05 ± 0.18 1.00<br />
NGC 4365 648 186.10765 7.31043 0.90 −6.937 ± 0.115 −7.725 ± 0.149 6.77 ± 1.08 0.55<br />
NGC 4365 649 186.10593 7.30840 1.09 −7.429 ± 0.041 −8.845 ± 0.056 3.95 ± 0.35 1.00<br />
NGC 4365 650 186.11563 7.31987 0.22 −6.622 ± 0.097 −7.868 ± 0.237 3.13 ± 0.71 0.99<br />
NGC 4365 651 186.09807 7.29919 1.95 −8.022 ± 0.031 −9.350 ± 0.049 1.81 ± 0.44 0.98<br />
NGC 4365 653 186.10854 7.31168 0.80 −7.110 ± 0.051 −8.272 ± 0.090 6.35 ± 0.47 0.85<br />
NGC 4365 654 186.11625 7.32088 0.25 −9.000 ± 0.169 −10.126 ± 0.019 2.67 ± 0.34 1.00<br />
NGC 4365 655 186.11333 7.31746 0.32 −8.489 ± 0.023 −9.527 ± 0.035 2.60 ± 0.25 1.00<br />
NGC 4365 656 186.10513 7.30774 1.16 −6.960 ± 0.482 −7.706 ± 0.418 2.53 ± 0.65 0.98<br />
NGC 4365 657 186.10956 7.31303 0.68 −6.863 ± 0.100 −7.751 ± 0.352 2.79 ± 0.82 0.99<br />
NGC 4365 663 186.10338 7.30579 1.35 −7.628 ± 0.032 −8.787 ± 0.027 3.97 ± 0.44 0.99<br />
NGC 4365 665 186.11007 7.31374 0.62 −8.819 ± 0.022 −10.035 ± 0.030 2.88 ± 0.35 1.00<br />
NGC 4365 666 186.10758 7.31081 0.89 −6.912 ± 0.065 −8.259 ± 0.254 2.42 ± 0.61 0.99<br />
NGC 4365 668 186.12343 7.32966 0.95 −7.810 ± 0.090 −8.961 ± 0.034 2.52 ± 0.37 1.00<br />
NGC 4365 670 186.12649 7.33355 1.30 −6.694 ± 0.076 −8.148 ± 0.081 3.20 ± 0.68 0.99<br />
NGC 4365 671 186.11084 7.31507 0.53 −6.876 ± 0.107 −7.712 ± 0.069 4.11 ± 0.65 0.94<br />
NGC 4365 672 186.13063 7.33853 1.76 −7.011 ± 1.163 −8.449 ± 0.504 2.25 ± 0.50 0.99<br />
NGC 4365 674 186.12536 7.33236 1.19 −7.044 ± 0.322 −8.304 ± 0.053 1.44 ± 0.43 0.95<br />
NGC 4365 675 186.12376 7.33051 1.02 −7.170 ± 0.476 −8.474 ± 0.284 2.32 ± 0.49 0.99<br />
NGC 4365 676 186.09759 7.29957 1.96 −6.654 ± 0.040 −7.969 ± 0.076 3.62 ± 0.46 0.98<br />
NGC 4365 677 186.12982 7.33774 1.68 −6.593 ± 0.170 −8.186 ± 0.051 2.43 ± 0.40 0.99<br />
NGC 4365 679 186.10054 7.30313 1.63 −7.465 ± 0.037 −8.857 ± 0.035 2.30 ± 0.36 1.00<br />
NGC 4365 680 186.12772 7.33529 1.45 −6.202 ± 0.156 −7.551 ± 0.096 4.49 ± 1.03 0.88<br />
NGC 4365 682 186.12262 7.32943 0.91 −9.841 ± 0.023 −10.800 ± 0.028 2.21 ± 0.16 1.00<br />
NGC 4365 683 186.10532 7.30892 1.10 −7.105 ± 0.228 −8.887 ± 1.446 1.44 ± 0.42 0.95<br />
NGC 4365 685 186.12242 7.32927 0.90 −8.746 ± 1.439 −9.976 ± 0.019 1.86 ± 0.34 0.98<br />
Continued on Next Page. . .<br />
304
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4365 686 186.11203 7.31699 0.42 −6.085 ± 0.419 −7.640 ± 0.381 2.58 ± 0.92 0.98<br />
NGC 4365 687 186.11600 7.32172 0.31 −8.280 ± 0.023 −9.161 ± 0.036 3.01 ± 0.26 1.00<br />
NGC 4365 688 186.10578 7.30974 1.04 −9.079 ± 0.023 −10.569 ± 0.027 2.70 ± 0.26 1.00<br />
NGC 4365 690 186.11795 7.32416 0.46 −7.960 ± 0.074 −9.248 ± 0.315 2.56 ± 0.39 1.00<br />
NGC 4365 692 186.10733 7.31162 0.87 −7.259 ± 0.070 −8.283 ± 0.082 4.14 ± 0.54 0.98<br />
NGC 4365 693 186.10047 7.30360 1.61 −6.863 ± 0.054 −7.958 ± 0.054 2.89 ± 0.37 0.99<br />
NGC 4365 694 186.11212 7.31739 0.41 −6.845 ± 0.122 −8.044 ± 0.368 2.35 ± 0.71 0.99<br />
NGC 4365 695 186.11961 7.32637 0.64 −6.980 ± 1.256 −8.298 ± 0.337 1.92 ± 0.53 0.98<br />
NGC 4365 696 186.12287 7.33030 0.98 −6.937 ± 0.064 −8.320 ± 0.097 3.38 ± 0.64 0.99<br />
NGC 4365 697 186.12116 7.32830 0.80 −6.813 ± 0.587 −7.927 ± 0.638 1.89 ± 0.65 0.97<br />
NGC 4365 699 186.11194 7.31758 0.42 −7.743 ± 0.054 −8.945 ± 0.039 2.62 ± 0.46 1.00<br />
NGC 4365 700 186.10349 7.30755 1.26 −6.090 ± 0.140 −6.708 ± 0.783 3.08 ± 1.28 0.94<br />
NGC 4365 702 186.09928 7.30265 1.72 −7.455 ± 0.940 −8.827 ± 0.040 3.51 ± 0.40 1.00<br />
NGC 4365 704 186.11560 7.32207 0.35 −7.225 ± 0.100 −8.874 ± 0.091 2.80 ± 0.59 1.00<br />
NGC 4365 705 186.11856 7.32557 0.57 −7.782 ± 0.030 −8.778 ± 0.106 2.72 ± 0.39 1.00<br />
NGC 4365 706 186.12847 7.33745 1.62 −7.801 ± 0.031 −8.717 ± 0.024 2.78 ± 0.32 1.00<br />
NGC 4365 708 186.12195 7.32999 0.93 −7.390 ± 0.031 −8.538 ± 0.033 2.74 ± 0.33 1.00<br />
NGC 4365 709 186.10557 7.31061 1.02 −6.822 ± 0.392 −8.376 ± 0.035 2.05 ± 0.41 0.99<br />
NGC 4365 710 186.12261 7.33085 1.01 −9.968 ± 0.025 −11.147 ± 0.017 2.34 ± 0.23 1.00<br />
NGC 4365 712 186.10968 7.31565 0.60 −6.301 ± 0.098 −7.653 ± 0.131 5.29 ± 0.63 0.79<br />
NGC 4365 713 186.12454 7.33331 1.22 −8.104 ± 0.029 −9.642 ± 0.019 2.05 ± 0.25 0.99<br />
NGC 4365 714 186.10165 7.30627 1.42 −8.022 ± 0.029 −9.403 ± 0.020 1.94 ± 0.23 0.99<br />
NGC 4365 715 186.11820 7.32596 0.59 −7.511 ± 0.044 −8.347 ± 0.085 3.25 ± 0.59 1.00<br />
NGC 4365 716 186.11679 7.32433 0.48 −7.453 ± 0.026 −8.575 ± 0.051 4.09 ± 0.38 0.99<br />
NGC 4365 718 186.10436 7.30980 1.12 −6.714 ± 0.264 −8.045 ± 0.042 1.75 ± 0.52 0.97<br />
NGC 4365 719 186.11740 7.32536 0.55 −8.329 ± 0.027 −9.816 ± 0.026 2.54 ± 0.21 1.00<br />
NGC 4365 720 186.09932 7.30368 1.67 −8.458 ± 0.162 −9.332 ± 0.390 3.38 ± 0.59 1.00<br />
NGC 4365 721 186.10496 7.31071 1.05 −8.235 ± 0.027 −9.100 ± 0.028 3.14 ± 0.28 1.00<br />
NGC 4365 722 186.11264 7.31980 0.40 −7.359 ± 0.041 −8.564 ± 0.054 3.16 ± 0.33 1.00<br />
NGC 4365 723 186.11606 7.32408 0.47 −7.353 ± 0.324 −8.336 ± 0.073 3.96 ± 0.74 0.99<br />
NGC 4365 725 186.11385 7.32159 0.39 −8.887 ± 0.041 −9.862 ± 0.767 2.21 ± 0.50 1.00<br />
NGC 4365 727 186.10139 7.30732 1.40 −9.610 ± 0.025 −10.670 ± 0.019 2.03 ± 0.28 0.99<br />
NGC 4365 730 186.12404 7.33434 1.28 −7.458 ± 0.111 −8.440 ± 0.040 2.19 ± 0.32 0.99<br />
NGC 4365 732 186.12130 7.33123 1.01 −6.397 ± 0.110 −7.686 ± 0.054 3.16 ± 0.64 0.99<br />
NGC 4365 733 186.12689 7.33787 1.59 −6.490 ± 0.041 −7.463 ± 0.057 2.89 ± 0.44 0.98<br />
NGC 4365 734 186.11872 7.32829 0.76 −6.820 ± 0.142 −8.284 ± 0.123 6.41 ± 1.09 0.85<br />
NGC 4365 735 186.12561 7.33677 1.48 −10.398 ± 0.043 −11.755 ± 0.017 4.11 ± 0.23 1.00<br />
NGC 4365 736 186.12076 7.33107 0.98 −5.787 ± 0.400 −7.142 ± 0.660 2.41 ± 1.23 0.96<br />
NGC 4365 737 186.11611 7.32572 0.59 −8.394 ± 0.021 −9.900 ± 0.022 2.56 ± 0.20 1.00<br />
NGC 4365 738 186.12935 7.34143 1.90 −7.554 ± 0.028 −8.469 ± 0.037 3.33 ± 0.30 1.00<br />
NGC 4365 739 186.09642 7.30241 1.89 −7.402 ± 0.048 −8.557 ± 0.022 2.28 ± 0.43 0.99<br />
NGC 4365 740 186.12833 7.34033 1.80 −8.574 ± 0.025 −9.927 ± 0.022 3.13 ± 0.18 1.00<br />
NGC 4365 742 186.10472 7.31304 1.00 −8.319 ± 0.183 −9.694 ± 0.029 2.37 ± 0.40 1.00<br />
NGC 4365 743 186.11070 7.32017 0.54 −6.722 ± 0.105 −8.043 ± 0.099 3.52 ± 0.72 0.99<br />
NGC 4365 745 186.10922 7.31847 0.62 −6.336 ± 0.090 −7.875 ± 0.153 5.55 ± 1.02 0.81<br />
NGC 4365 747 186.10608 7.31509 0.86 −6.589 ± 0.061 −7.864 ± 0.123 4.55 ± 0.86 0.92<br />
NGC 4365 748 186.12665 7.33955 1.70 −9.979 ± 0.023 −11.100 ± 0.015 2.07 ± 0.20 0.99<br />
NGC 4365 749 186.11737 7.32849 0.78 −8.087 ± 0.045 −9.220 ± 0.030 2.45 ± 0.38 1.00<br />
NGC 4365 750 186.12291 7.33508 1.30 −8.574 ± 0.023 −9.970 ± 0.027 2.24 ± 0.27 1.00<br />
NGC 4365 751 186.12113 7.33312 1.14 −7.919 ± 0.044 −9.331 ± 0.022 2.18 ± 0.32 0.99<br />
NGC 4365 752 186.12425 7.33690 1.46 −8.866 ± 0.024 −9.782 ± 0.022 3.48 ± 0.22 1.00<br />
NGC 4365 753 186.12337 7.33588 1.37 −7.971 ± 0.035 −8.938 ± 0.045 3.59 ± 0.34 1.00<br />
NGC 4365 755 186.09944 7.30777 1.50 −8.469 ± 0.026 −9.735 ± 0.022 2.97 ± 0.17 1.00<br />
NGC 4365 756 186.10091 7.30949 1.35 −7.730 ± 0.025 −8.532 ± 0.035 2.06 ± 0.21 0.99<br />
NGC 4365 757 186.09618 7.30397 1.84 −6.543 ± 0.676 −7.972 ± 0.036 1.78 ± 0.55 0.96<br />
NGC 4365 758 186.11551 7.32689 0.68 −7.013 ± 0.053 −8.480 ± 0.029 2.38 ± 0.35 0.99<br />
NGC 4365 760 186.11941 7.33165 1.01 −6.596 ± 1.560 −8.150 ± 1.124 2.16 ± 0.55 0.98<br />
NGC 4365 761 186.10426 7.31380 1.01 −6.846 ± 0.055 −8.326 ± 0.096 3.69 ± 0.70 0.99<br />
NGC 4365 762 186.11003 7.32071 0.59 −6.838 ± 0.044 −8.269 ± 0.409 3.11 ± 0.64 1.00<br />
NGC 4365 764 186.11732 7.32950 0.85 −8.444 ± 0.023 −10.022 ± 0.016 2.24 ± 0.14 1.00<br />
NGC 4365 767 186.11688 7.32915 0.83 −7.816 ± 0.037 −9.071 ± 0.030 2.75 ± 0.41 1.00<br />
NGC 4365 769 186.10274 7.31252 1.14 −6.926 ± 0.055 −7.793 ± 0.281 2.38 ± 2.80 0.98<br />
Continued on Next Page. . .<br />
305
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4365 770 186.11743 7.33002 0.89 −8.053 ± 0.375 −9.088 ± 0.203 3.26 ± 0.67 1.00<br />
NGC 4365 771 186.10921 7.32038 0.64 −8.076 ± 0.042 −9.381 ± 0.347 1.93 ± 0.30 0.98<br />
NGC 4365 772 186.10370 7.31390 1.05 −8.246 ± 0.027 −9.160 ± 0.031 3.25 ± 0.31 1.00<br />
NGC 4365 773 186.10675 7.31755 0.79 −7.797 ± 0.042 −9.225 ± 0.018 3.52 ± 0.25 1.00<br />
NGC 4365 774 186.11505 7.32748 0.73 −7.294 ± 0.053 −8.472 ± 0.041 3.34 ± 0.39 1.00<br />
NGC 4365 775 186.10402 7.31463 1.01 −7.158 ± 0.037 −8.582 ± 0.051 3.37 ± 0.28 1.00<br />
NGC 4365 776 186.11377 7.32626 0.68 −7.226 ± 0.039 −8.219 ± 0.106 3.90 ± 0.53 0.98<br />
NGC 4365 777 186.12296 7.33717 1.45 −6.937 ± 0.056 −7.650 ± 0.684 2.56 ± 1.09 0.98<br />
NGC 4365 778 186.12798 7.34318 1.98 −9.103 ± 0.030 −10.465 ± 0.015 2.07 ± 0.24 0.99<br />
NGC 4365 779 186.09404 7.30307 2.01 −8.156 ± 0.037 −9.263 ± 0.026 1.65 ± 0.21 0.97<br />
NGC 4365 780 186.11339 7.32597 0.67 −9.460 ± 0.016 −10.622 ± 0.403 2.78 ± 0.37 1.00<br />
NGC 4365 781 186.09493 7.30434 1.90 −7.941 ± 0.026 −8.740 ± 0.028 2.22 ± 0.21 0.99<br />
NGC 4365 782 186.09796 7.30805 1.59 −7.886 ± 0.022 −8.934 ± 0.039 4.27 ± 0.25 1.00<br />
NGC 4365 783 186.09268 7.30180 2.14 −7.020 ± 0.050 −7.872 ± 0.392 3.77 ± 0.54 0.97<br />
NGC 4365 784 186.10774 7.31965 0.73 −6.887 ± 0.066 −7.823 ± 0.116 2.65 ± 0.46 0.99<br />
NGC 4365 785 186.09662 7.30650 1.72 −6.836 ± 0.065 −8.053 ± 0.073 4.57 ± 0.48 0.94<br />
NGC 4365 787 186.12465 7.33974 1.66 −8.658 ± 0.018 −9.457 ± 0.019 2.35 ± 0.22 1.00<br />
NGC 4365 788 186.12749 7.34307 1.96 −5.803 ± 0.390 −7.235 ± 0.644 1.32 ± 0.79 0.87<br />
NGC 4365 789 186.09357 7.30306 2.04 −7.914 ± 0.031 −9.399 ± 0.014 2.61 ± 0.25 1.00<br />
NGC 4365 792 186.10089 7.31220 1.28 −9.793 ± 0.033 −10.934 ± 0.022 3.95 ± 0.20 1.00<br />
NGC 4365 794 186.11600 7.32996 0.89 −6.711 ± 0.679 −7.503 ± 0.250 1.75 ± 0.50 0.94<br />
NGC 4365 795 186.10372 7.31583 1.02 −7.987 ± 0.040 −9.056 ± 0.031 2.99 ± 0.36 1.00<br />
NGC 4365 796 186.09659 7.30753 1.69 −6.882 ± 0.042 −8.002 ± 0.108 3.12 ± 0.97 0.99<br />
NGC 4365 797 186.11434 7.32866 0.82 −9.361 ± 0.022 −10.675 ± 0.016 2.67 ± 0.16 1.00<br />
NGC 4365 798 186.10364 7.31637 1.02 −8.613 ± 0.019 −9.743 ± 0.015 2.82 ± 0.17 1.00<br />
NGC 4365 799 186.12485 7.34149 1.79 −8.651 ± 0.108 −9.813 ± 0.181 11.32 ± 2.09 0.84<br />
NGC 4365 800 186.11157 7.32581 0.73 −7.745 ± 0.023 −9.200 ± 0.030 2.16 ± 0.24 0.99<br />
NGC 4365 801 186.10073 7.31303 1.27 −8.828 ± 0.021 −9.739 ± 0.025 3.42 ± 0.26 1.00<br />
NGC 4365 802 186.11121 7.32547 0.73 −9.650 ± 0.022 −11.062 ± 0.013 3.12 ± 0.21 1.00<br />
NGC 4365 803 186.10261 7.31534 1.10 −7.367 ± 0.046 −9.028 ± 0.051 4.00 ± 0.48 1.00<br />
NGC 4365 804 186.12271 7.33912 1.58 −7.370 ± 0.967 −8.616 ± 0.520 2.20 ± 0.67 0.99<br />
NGC 4365 805 186.12619 7.34328 1.94 −6.687 ± 0.087 −7.472 ± 0.085 4.64 ± 0.69 0.84<br />
NGC 4365 806 186.10223 7.31504 1.13 −8.751 ± 0.016 −9.948 ± 0.020 2.46 ± 0.20 1.00<br />
NGC 4365 807 186.11494 7.33017 0.92 −6.907 ± 0.118 −8.435 ± 0.060 1.88 ± 0.43 0.98<br />
NGC 4365 808 186.11312 7.32805 0.81 −5.935 ± 0.131 −7.425 ± 0.070 4.55 ± 0.64 0.85<br />
NGC 4365 809 186.10162 7.31459 1.18 −7.439 ± 0.051 −8.247 ± 0.045 1.59 ± 0.34 0.96<br />
NGC 4365 810 186.10118 7.31406 1.22 −8.218 ± 0.024 −9.317 ± 0.271 1.83 ± 0.26 0.98<br />
NGC 4365 811 186.09923 7.31174 1.40 −7.032 ± 0.051 −8.285 ± 0.272 2.10 ± 0.37 0.99<br />
NGC 4365 813 186.10929 7.32370 0.74 −7.068 ± 0.358 −8.369 ± 0.280 2.71 ± 0.56 1.00<br />
NGC 4365 814 186.09532 7.30724 1.78 −8.253 ± 0.020 −9.164 ± 0.027 3.37 ± 0.24 1.00<br />
NGC 4365 816 186.10181 7.31509 1.16 −7.145 ± 0.047 −8.529 ± 0.046 3.78 ± 0.34 0.99<br />
NGC 4365 817 186.10628 7.32041 0.85 −7.032 ± 0.144 −8.551 ± 0.085 3.14 ± 0.73 1.00<br />
NGC 4365 819 186.11768 7.33391 1.17 −7.377 ± 1.280 −8.756 ± 0.038 2.28 ± 0.50 0.99<br />
NGC 4365 820 186.10414 7.31793 0.98 −6.700 ± 0.077 −8.337 ± 0.056 3.02 ± 0.47 1.00<br />
NGC 4365 821 186.09978 7.31275 1.34 −6.534 ± 0.045 −7.725 ± 0.223 1.98 ± 0.45 0.96<br />
NGC 4365 822 186.10756 7.32198 0.79 −5.724 ± 0.170 −7.061 ± 0.060 3.42 ± 0.78 0.93<br />
NGC 4365 823 186.10670 7.32100 0.83 −8.170 ± 0.024 −9.338 ± 0.019 2.39 ± 0.20 1.00<br />
NGC 4365 824 186.11999 7.33674 1.38 −8.943 ± 0.019 −10.047 ± 0.016 2.97 ± 0.17 1.00<br />
NGC 4365 825 186.10659 7.32094 0.83 −6.754 ± 0.064 −8.298 ± 0.101 2.96 ± 1.05 1.00<br />
NGC 4365 827 186.11769 7.33411 1.18 −7.918 ± 0.026 −9.032 ± 0.046 3.27 ± 0.29 1.00<br />
NGC 4365 828 186.09639 7.30891 1.66 −6.991 ± 0.035 −8.112 ± 0.058 3.05 ± 0.45 0.99<br />
NGC 4365 829 186.09154 7.30320 2.16 −6.311 ± 0.651 −7.208 ± 0.207 2.18 ± 0.62 0.96<br />
NGC 4365 830 186.10603 7.32042 0.86 −8.384 ± 0.028 −9.637 ± 0.017 1.97 ± 0.20 0.98<br />
NGC 4365 831 186.10433 7.31848 0.97 −8.182 ± 0.030 −9.158 ± 0.029 3.62 ± 0.28 1.00<br />
NGC 4365 832 186.11458 7.33069 0.96 −7.140 ± 0.051 −8.212 ± 0.062 3.60 ± 0.39 0.99<br />
NGC 4365 834 186.10205 7.31598 1.13 −6.442 ± 0.149 −7.817 ± 0.173 4.50 ± 2.59 0.92<br />
NGC 4365 835 186.10423 7.31864 0.97 −6.292 ± 0.448 −7.354 ± 0.105 2.59 ± 0.68 0.97<br />
NGC 4365 837 186.10605 7.32125 0.88 −10.287 ± 0.013 −11.479 ± 0.014 3.36 ± 0.12 1.00<br />
NGC 4365 838 186.10016 7.31425 1.29 −8.782 ± 0.021 −10.061 ± 0.015 2.85 ± 0.14 1.00<br />
NGC 4365 839 186.12505 7.34366 1.94 −6.644 ± 0.188 −7.868 ± 0.048 2.22 ± 0.47 0.98<br />
NGC 4365 842 186.11542 7.33244 1.07 −7.344 ± 0.035 −8.634 ± 0.043 2.84 ± 0.33 1.00<br />
NGC 4365 843 186.11515 7.33211 1.05 −6.286 ± 0.518 −7.595 ± 0.073 1.70 ± 0.68 0.94<br />
Continued on Next Page. . .<br />
306
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4365 844 186.09201 7.30477 2.07 −7.573 ± 0.048 −8.454 ± 0.036 2.64 ± 0.33 1.00<br />
NGC 4365 845 186.10866 7.32464 0.82 −9.697 ± 0.015 −10.654 ± 0.028 3.27 ± 0.28 1.00<br />
NGC 4365 847 186.11708 7.33474 1.23 −7.631 ± 0.077 −8.956 ± 0.037 2.71 ± 0.44 1.00<br />
NGC 4365 848 186.10954 7.32586 0.83 −7.441 ± 0.040 −8.671 ± 0.235 2.04 ± 0.26 0.99<br />
NGC 4365 849 186.10806 7.32417 0.84 −9.160 ± 0.029 −10.527 ± 0.019 2.26 ± 0.21 1.00<br />
NGC 4365 850 186.11941 7.33760 1.44 −9.414 ± 0.024 −10.326 ± 0.020 2.60 ± 0.26 1.00<br />
NGC 4365 851 186.10359 7.31899 1.02 −6.753 ± 0.058 −7.680 ± 0.066 4.33 ± 0.39 0.92<br />
NGC 4365 852 186.11237 7.32950 0.93 −7.321 ± 0.150 −8.508 ± 0.049 2.84 ± 0.47 1.00<br />
NGC 4365 853 186.09920 7.31396 1.36 −7.981 ± 0.031 −8.795 ± 0.038 2.97 ± 0.32 1.00<br />
NGC 4365 854 186.09656 7.31088 1.60 −6.715 ± 0.052 −7.663 ± 0.077 1.64 ± 0.46 0.94<br />
NGC 4365 855 186.10556 7.32158 0.92 −7.779 ± 0.123 −9.190 ± 0.078 2.57 ± 0.53 1.00<br />
NGC 4365 856 186.10688 7.32324 0.88 −8.527 ± 0.021 −9.552 ± 0.030 3.88 ± 0.23 1.00<br />
NGC 4365 857 186.12313 7.34246 1.83 −5.754 ± 0.373 −6.774 ± 0.105 3.02 ± 0.86 0.94<br />
NGC 4365 858 186.09990 7.31509 1.30 −7.352 ± 0.031 −8.517 ± 0.063 3.22 ± 0.40 1.00<br />
NGC 4365 859 186.10214 7.31772 1.12 −6.779 ± 0.075 −8.127 ± 0.053 2.28 ± 0.63 0.99<br />
NGC 4365 860 186.10618 7.32256 0.90 −7.365 ± 0.080 −8.721 ± 0.033 2.80 ± 0.35 1.00<br />
NGC 4365 861 186.10132 7.31697 1.18 −8.701 ± 0.031 −9.743 ± 0.016 2.08 ± 0.29 0.99<br />
NGC 4365 862 186.11592 7.33452 1.22 −6.664 ± 0.091 −8.117 ± 0.067 2.60 ± 0.54 0.99<br />
NGC 4365 863 186.11229 7.33029 0.99 −8.324 ± 0.021 −9.132 ± 0.029 2.54 ± 0.30 1.00<br />
NGC 4365 864 186.11697 7.33582 1.31 −6.763 ± 0.044 −8.265 ± 0.848 2.20 ± 0.45 0.99<br />
NGC 4365 865 186.10994 7.32766 0.91 −7.131 ± 0.048 −8.086 ± 0.055 4.01 ± 0.34 0.98<br />
NGC 4365 866 186.11609 7.33521 1.27 −7.779 ± 0.021 −9.118 ± 0.026 2.72 ± 0.28 1.00<br />
NGC 4365 867 186.10790 7.32555 0.90 −9.699 ± 0.018 −10.640 ± 0.020 3.95 ± 0.21 1.00<br />
NGC 4365 868 186.11679 7.33615 1.33 −6.847 ± 0.045 −7.952 ± 0.092 5.37 ± 0.49 0.86<br />
NGC 4365 869 186.10834 7.32620 0.91 −6.042 ± 0.126 −7.602 ± 0.821 2.24 ± 0.48 0.97<br />
NGC 4365 871 186.11279 7.33203 1.09 −10.461 ± 0.014 −11.906 ± 0.014 3.15 ± 0.12 1.00<br />
NGC 4365 872 186.10806 7.32654 0.94 −10.038 ± 0.020 −11.243 ± 0.011 3.12 ± 0.24 1.00<br />
NGC 4365 874 186.11336 7.33312 1.15 −7.552 ± 0.033 −9.122 ± 0.025 3.65 ± 0.38 1.00<br />
NGC 4365 876 186.09298 7.30903 1.89 −7.074 ± 0.031 −7.917 ± 0.044 3.04 ± 0.36 0.99<br />
NGC 4365 877 186.10309 7.32118 1.08 −7.216 ± 0.030 −8.779 ± 0.052 2.97 ± 0.55 1.00<br />
NGC 4365 878 186.10162 7.31942 1.16 −6.570 ± 0.129 −7.893 ± 0.085 6.52 ± 0.67 0.69<br />
NGC 4365 883 186.11047 7.33031 1.05 −8.887 ± 0.021 −10.046 ± 0.023 2.21 ± 0.27 1.00<br />
NGC 4365 884 186.09499 7.31199 1.69 −6.501 ± 0.713 −8.092 ± 0.045 2.20 ± 0.47 0.98<br />
NGC 4365 885 186.10734 7.32671 0.99 −6.005 ± 0.107 −6.957 ± 0.076 4.06 ± 0.70 0.87<br />
NGC 4365 886 186.11437 7.33507 1.27 −5.675 ± 0.329 −7.241 ± 0.174 3.69 ± 1.71 0.93<br />
NGC 4365 887 186.11032 7.33065 1.07 −6.483 ± 0.204 −7.793 ± 0.089 2.20 ± 0.52 0.98<br />
NGC 4365 888 186.11828 7.34015 1.62 −8.596 ± 0.026 −9.985 ± 0.017 2.93 ± 0.26 1.00<br />
NGC 4365 889 186.11044 7.33098 1.09 −7.437 ± 0.040 −8.157 ± 0.064 3.31 ± 0.49 0.99<br />
NGC 4365 890 186.09873 7.31720 1.37 −8.141 ± 0.035 −9.557 ± 0.018 2.57 ± 0.15 1.00<br />
NGC 4365 891 186.11180 7.33269 1.16 −5.874 ± 0.408 −6.874 ± 0.798 1.71 ± 1.60 0.91<br />
NGC 4365 892 186.09990 7.31871 1.28 −6.909 ± 0.049 −8.157 ± 0.043 3.28 ± 0.37 0.99<br />
NGC 4365 894 186.11066 7.33158 1.12 −7.445 ± 0.038 −8.554 ± 0.038 2.28 ± 0.38 0.99<br />
NGC 4365 896 186.09358 7.31146 1.79 −7.725 ± 0.031 −8.762 ± 0.038 4.32 ± 0.21 0.99<br />
NGC 4365 898 186.09215 7.30991 1.92 −8.644 ± 0.022 −9.684 ± 0.023 3.43 ± 0.26 1.00<br />
NGC 4365 899 186.10083 7.32032 1.23 −8.532 ± 0.027 −10.029 ± 0.022 2.51 ± 0.20 1.00<br />
NGC 4365 900 186.11755 7.34005 1.61 −6.806 ± 0.061 −8.034 ± 0.209 7.83 ± 2.08 0.53<br />
NGC 4365 903 186.09650 7.31541 1.54 −7.011 ± 0.618 −8.457 ± 0.037 3.45 ± 0.47 0.99<br />
NGC 4365 904 186.12282 7.34670 2.12 −5.988 ± 0.785 −7.554 ± 0.101 2.44 ± 1.83 0.98<br />
NGC 4365 907 186.10046 7.32104 1.26 −9.614 ± 0.017 −11.074 ± 0.009 3.85 ± 0.13 1.00<br />
NGC 4365 908 186.11395 7.33703 1.42 −7.877 ± 0.033 −9.184 ± 0.022 2.79 ± 0.29 1.00<br />
NGC 4365 910 186.10124 7.32209 1.23 −8.366 ± 0.034 −9.723 ± 0.025 1.92 ± 0.21 0.98<br />
NGC 4365 911 186.11053 7.33338 1.24 −7.050 ± 0.061 −8.204 ± 0.124 1.38 ± 0.31 0.94<br />
NGC 4365 912 186.10234 7.32370 1.19 −6.776 ± 0.902 −7.744 ± 0.039 1.76 ± 0.64 0.95<br />
NGC 4365 913 186.10994 7.33275 1.22 −6.182 ± 0.131 −7.703 ± 0.092 6.66 ± 0.91 0.56<br />
NGC 4365 915 186.10852 7.33115 1.17 −7.103 ± 0.048 −8.379 ± 0.042 2.61 ± 0.40 0.99<br />
NGC 4365 917 186.09131 7.31083 1.96 −8.117 ± 0.332 −9.311 ± 0.027 2.62 ± 0.44 1.00<br />
NGC 4365 918 186.12089 7.34583 2.04 −5.866 ± 0.205 −7.222 ± 0.302 3.45 ± 1.50 0.94<br />
NGC 4365 919 186.09457 7.31472 1.68 −6.588 ± 0.187 −7.509 ± 0.107 3.35 ± 0.87 0.97<br />
NGC 4365 921 186.11908 7.34390 1.89 −8.153 ± 0.260 −9.068 ± 0.202 2.87 ± 0.68 1.00<br />
NGC 4365 922 186.11674 7.34109 1.69 −5.659 ± 0.215 −6.914 ± 0.073 3.23 ± 0.70 0.94<br />
NGC 4365 923 186.09635 7.31732 1.54 −10.934 ± 0.016 −12.059 ± 0.021 4.05 ± 0.13 1.00<br />
NGC 4365 924 186.09682 7.31777 1.50 −6.202 ± 0.102 −7.468 ± 0.057 2.36 ± 0.52 0.97<br />
Continued on Next Page. . .<br />
307
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4365 925 186.09160 7.31165 1.93 −6.412 ± 0.070 −7.721 ± 0.056 3.00 ± 0.43 0.99<br />
NGC 4365 926 186.11153 7.33534 1.35 −7.560 ± 0.039 −8.764 ± 0.034 1.97 ± 0.36 0.99<br />
NGC 4365 927 186.08979 7.30966 2.09 −7.922 ± 0.029 −8.896 ± 0.021 2.86 ± 0.30 1.00<br />
NGC 4365 929 186.10603 7.32898 1.17 −6.889 ± 0.042 −7.948 ± 0.055 2.83 ± 0.45 0.99<br />
NGC 4365 930 186.11026 7.33411 1.30 −8.217 ± 0.026 −9.567 ± 0.026 2.08 ± 0.22 0.99<br />
NGC 4365 932 186.12085 7.34667 2.10 −6.857 ± 0.040 −7.960 ± 0.138 7.55 ± 0.93 0.52<br />
NGC 4365 933 186.11676 7.34191 1.75 −6.429 ± 0.075 −7.910 ± 0.074 4.46 ± 0.68 0.93<br />
NGC 4365 934 186.10248 7.32514 1.22 −6.468 ± 0.096 −7.842 ± 0.060 2.71 ± 0.51 0.99<br />
NGC 4365 935 186.11263 7.33734 1.46 −7.597 ± 0.457 −8.672 ± 0.029 2.13 ± 0.46 0.99<br />
NGC 4365 936 186.11885 7.34464 1.94 −7.304 ± 0.044 −8.212 ± 0.028 2.85 ± 0.27 0.99<br />
NGC 4365 937 186.10096 7.32354 1.28 −7.957 ± 0.026 −9.309 ± 0.024 2.62 ± 0.38 1.00<br />
NGC 4365 938 186.09906 7.32136 1.37 −7.403 ± 1.370 −8.247 ± 1.633 1.69 ± 0.53 0.97<br />
NGC 4365 940 186.10703 7.33094 1.22 −6.507 ± 0.178 −8.168 ± 0.122 6.76 ± 1.29 0.77<br />
NGC 4365 941 186.09092 7.31201 1.97 −6.490 ± 0.118 −7.930 ± 0.091 2.87 ± 1.06 0.99<br />
NGC 4365 942 186.11397 7.33928 1.58 −7.254 ± 0.039 −8.399 ± 0.042 2.29 ± 0.31 0.99<br />
NGC 4365 943 186.12155 7.34845 2.23 −8.098 ± 0.043 −9.027 ± 0.027 3.04 ± 0.37 1.00<br />
NGC 4365 944 186.11300 7.33841 1.53 −8.804 ± 0.019 −10.055 ± 0.034 2.82 ± 0.38 1.00<br />
NGC 4365 945 186.12084 7.34767 2.17 −7.461 ± 0.041 −8.505 ± 0.036 3.52 ± 0.35 0.99<br />
NGC 4365 947 186.10126 7.32447 1.28 −6.483 ± 0.050 −7.657 ± 0.230 3.75 ± 0.40 0.96<br />
NGC 4365 948 186.11333 7.33877 1.55 −6.786 ± 0.046 −7.918 ± 1.236 1.79 ± 0.38 0.96<br />
NGC 4365 949 186.09471 7.31681 1.66 −6.764 ± 0.045 −7.891 ± 0.067 2.83 ± 0.43 0.99<br />
NGC 4365 950 186.12113 7.34806 2.20 −6.824 ± 0.044 −8.130 ± 0.033 2.55 ± 0.38 0.99<br />
NGC 4365 951 186.09167 7.31350 1.90 −7.156 ± 0.045 −8.327 ± 0.074 4.11 ± 0.93 0.98<br />
NGC 4365 957 186.10439 7.32883 1.25 −7.872 ± 0.045 −9.052 ± 0.032 2.67 ± 0.28 1.00<br />
NGC 4365 960 186.10384 7.32840 1.26 −7.108 ± 0.074 −8.184 ± 0.052 4.99 ± 0.56 0.93<br />
NGC 4365 963 186.10142 7.32595 1.31 −9.018 ± 0.030 −10.149 ± 0.016 2.55 ± 0.22 1.00<br />
NGC 4365 964 186.09496 7.31826 1.64 −6.839 ± 0.041 −8.197 ± 0.511 2.56 ± 0.45 0.99<br />
NGC 4365 965 186.11900 7.34697 2.11 −6.543 ± 0.119 −7.153 ± 0.216 3.58 ± 0.85 0.93<br />
NGC 4365 966 186.08867 7.31113 2.14 −5.539 ± 0.576 −6.984 ± 0.084 1.47 ± 0.65 0.88<br />
NGC 4365 967 186.11442 7.34189 1.76 −7.459 ± 0.048 −8.706 ± 0.274 2.86 ± 0.45 1.00<br />
NGC 4365 968 186.09371 7.31750 1.73 −7.036 ± 0.297 −8.175 ± 0.296 2.18 ± 0.64 0.99<br />
NGC 4365 969 186.08565 7.30803 2.41 −8.011 ± 0.032 −8.944 ± 0.043 3.72 ± 0.27 1.00<br />
NGC 4365 973 186.09409 7.31833 1.70 −8.988 ± 0.012 −10.356 ± 0.016 3.17 ± 0.12 1.00<br />
NGC 4365 979 186.11792 7.34673 2.09 −6.950 ± 0.056 −8.045 ± 0.049 2.44 ± 0.46 0.99<br />
NGC 4365 981 186.10070 7.32664 1.38 −10.290 ± 0.016 −11.369 ± 0.009 3.49 ± 0.17 1.00<br />
NGC 4365 983 186.08480 7.30798 2.47 −8.512 ± 0.024 −9.344 ± 0.162 2.37 ± 0.35 1.00<br />
NGC 4365 988 186.10246 7.32913 1.37 −7.253 ± 0.032 −8.433 ± 0.033 3.04 ± 0.35 1.00<br />
NGC 4365 989 186.08956 7.31383 2.04 −6.715 ± 0.134 −8.042 ± 0.072 4.25 ± 0.60 0.96<br />
NGC 4365 990 186.11118 7.33949 1.64 −5.992 ± 0.469 −7.504 ± 0.185 4.85 ± 1.21 0.82<br />
NGC 4365 991 186.09120 7.31589 1.91 −6.206 ± 1.168 −7.233 ± 0.501 1.35 ± 0.68 0.88<br />
NGC 4365 994 186.08896 7.31347 2.09 −9.114 ± 0.033 −10.041 ± 0.030 2.63 ± 0.29 1.00<br />
NGC 4365 995 186.11110 7.33977 1.66 −7.887 ± 0.031 −8.791 ± 0.029 2.40 ± 0.28 0.99<br />
NGC 4365 996 186.09341 7.31888 1.75 −7.934 ± 0.676 −8.966 ± 0.034 2.89 ± 0.41 1.00<br />
NGC 4365 997 186.11532 7.34479 1.96 −7.385 ± 0.060 −8.460 ± 0.656 3.22 ± 0.68 1.00<br />
NGC 4365 998 186.10526 7.33296 1.42 −6.009 ± 1.286 −7.650 ± 0.036 2.16 ± 0.45 0.97<br />
NGC 4365 999 186.08693 7.31160 2.26 −11.420 ± 0.026 −12.661 ± 0.017 6.29 ± 0.19 0.94<br />
NGC 4365 1002 186.11753 7.34798 2.18 −7.882 ± 0.064 −8.698 ± 0.045 7.08 ± 0.42 0.89<br />
NGC 4365 1005 186.09398 7.32032 1.72 −8.818 ± 0.024 −10.281 ± 0.039 1.38 ± 0.23 0.93<br />
NGC 4365 1006 186.08823 7.31346 2.14 −7.871 ± 0.181 −9.142 ± 0.486 2.63 ± 0.51 1.00<br />
NGC 4365 1008 186.11760 7.34833 2.21 −7.268 ± 0.066 −8.504 ± 0.040 3.02 ± 0.41 1.00<br />
NGC 4365 1009 186.09467 7.32131 1.68 −6.661 ± 0.142 −7.529 ± 0.131 5.49 ± 1.29 0.71<br />
NGC 4365 1010 186.08592 7.31109 2.33 −6.856 ± 0.074 −7.577 ± 0.340 3.28 ± 0.55 0.98<br />
NGC 4365 1012 186.08678 7.31228 2.26 −6.748 ± 0.063 −8.252 ± 0.052 4.20 ± 0.50 0.98<br />
NGC 4365 1013 186.10519 7.33413 1.49 −6.428 ± 0.074 −8.187 ± 0.045 4.96 ± 0.38 0.93<br />
NGC 4365 1015 186.09244 7.31946 1.82 −7.948 ± 0.028 −9.095 ± 0.027 2.34 ± 0.18 1.00<br />
NGC 4365 1016 186.10469 7.33403 1.50 −6.648 ± 0.052 −7.452 ± 0.412 1.70 ± 0.45 0.93<br />
NGC 4365 1017 186.09784 7.32602 1.55 −7.915 ± 0.027 −8.790 ± 0.043 3.68 ± 0.24 1.00<br />
NGC 4365 1018 186.10173 7.33071 1.48 −6.604 ± 0.164 −7.546 ± 0.628 2.41 ± 0.62 0.98<br />
NGC 4365 1019 186.08795 7.31448 2.15 −7.552 ± 0.219 −8.527 ± 0.043 2.59 ± 0.32 1.00<br />
NGC 4365 1020 186.11246 7.34350 1.90 −7.597 ± 1.366 −8.886 ± 0.023 2.54 ± 0.56 1.00<br />
NGC 4365 1021 186.10651 7.33660 1.58 −8.723 ± 0.028 −9.979 ± 0.017 3.68 ± 0.24 1.00<br />
NGC 4365 1022 186.10129 7.33054 1.50 −7.434 ± 0.050 −8.526 ± 0.042 3.12 ± 0.43 1.00<br />
Continued on Next Page. . .<br />
308
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4365 1024 186.10947 7.34025 1.73 −8.836 ± 0.022 −9.818 ± 0.033 2.61 ± 0.36 1.00<br />
NGC 4365 1026 186.10850 7.33910 1.68 −7.237 ± 0.040 −8.655 ± 0.044 4.04 ± 0.42 0.99<br />
NGC 4365 1028 186.11081 7.34225 1.84 −7.262 ± 0.282 −8.108 ± 0.046 2.24 ± 0.39 0.99<br />
NGC 4365 1029 186.08334 7.30983 2.54 −7.418 ± 0.155 −8.760 ± 0.154 9.41 ± 1.98 0.55<br />
NGC 4365 1031 186.10472 7.33511 1.56 −7.155 ± 0.034 −8.122 ± 0.051 2.85 ± 0.32 0.99<br />
NGC 4365 1033 186.08953 7.31733 2.03 −6.280 ± 0.534 −6.885 ± 0.581 1.75 ± 1.10 0.91<br />
NGC 4365 1034 186.08368 7.31050 2.50 −7.466 ± 0.034 −8.362 ± 0.043 3.42 ± 0.35 0.99<br />
NGC 4365 1035 186.08354 7.31036 2.51 −6.855 ± 0.107 −7.930 ± 0.051 5.86 ± 0.57 0.80<br />
NGC 4365 1036 186.09151 7.31986 1.89 −6.864 ± 0.032 −8.236 ± 0.661 2.04 ± 0.42 0.98<br />
NGC 4365 1038 186.10760 7.33920 1.71 −7.318 ± 0.095 −8.231 ± 0.024 2.71 ± 0.34 0.99<br />
NGC 4365 1040 186.09145 7.32042 1.90 −9.665 ± 0.020 −10.566 ± 0.018 3.54 ± 0.15 1.00<br />
NGC 4365 1045 186.10370 7.33516 1.61 −7.375 ± 0.174 −8.608 ± 0.053 3.41 ± 0.67 1.00<br />
NGC 4365 1046 186.10543 7.33724 1.66 −7.441 ± 0.071 −8.305 ± 0.325 3.60 ± 0.65 0.99<br />
NGC 4365 1050 186.09533 7.32545 1.70 −6.256 ± 0.129 −7.092 ± 0.053 1.80 ± 0.43 0.93<br />
NGC 4365 1051 186.08200 7.30978 2.63 −7.800 ± 0.096 −8.932 ± 0.266 9.41 ± 3.54 0.63<br />
NGC 4365 1053 186.11783 7.35235 2.50 −9.263 ± 0.022 −10.362 ± 0.021 1.71 ± 0.16 0.97<br />
NGC 4365 1056 186.08846 7.31767 2.10 −7.105 ± 0.464 −8.184 ± 0.042 1.72 ± 0.44 0.97<br />
NGC 4365 1057 186.09715 7.32813 1.66 −7.017 ± 0.045 −8.042 ± 0.101 4.96 ± 0.66 0.91<br />
NGC 4365 1058 186.10928 7.34253 1.89 −6.348 ± 0.060 −8.092 ± 0.100 4.30 ± 0.69 0.96<br />
NGC 4365 1060 186.08422 7.31303 2.43 −7.630 ± 0.050 −8.526 ± 0.039 2.80 ± 0.32 1.00<br />
NGC 4365 1061 186.09635 7.32745 1.69 −6.066 ± 0.109 −7.044 ± 0.495 2.38 ± 0.99 0.96<br />
NGC 4365 1062 186.08571 7.31522 2.31 −7.977 ± 0.050 −9.274 ± 0.027 1.86 ± 0.29 0.98<br />
NGC 4365 1063 186.10554 7.33873 1.75 −5.660 ± 0.113 −7.207 ± 0.221 5.27 ± 1.52 0.67<br />
NGC 4365 1065 186.11196 7.34656 2.12 −6.835 ± 0.052 −7.840 ± 0.060 2.76 ± 0.48 0.99<br />
NGC 4365 1067 186.11006 7.34436 2.00 −6.088 ± 0.117 −7.740 ± 0.102 4.78 ± 0.76 0.87<br />
NGC 4365 1071 186.11391 7.34934 2.30 −6.184 ± 0.550 −7.480 ± 0.049 1.57 ± 0.54 0.92<br />
NGC 4365 1074 186.08605 7.31673 2.28 −9.022 ± 0.024 −10.638 ± 0.025 4.21 ± 0.21 1.00<br />
NGC 4365 1075 186.10250 7.33627 1.73 −8.298 ± 0.036 −9.502 ± 0.027 2.58 ± 0.29 1.00<br />
NGC 4365 1076 186.11333 7.34921 2.30 −7.659 ± 0.024 −8.574 ± 0.040 3.32 ± 0.31 1.00<br />
NGC 4365 1077 186.11686 7.35351 2.58 −6.603 ± 0.072 −7.572 ± 0.059 4.33 ± 0.46 0.90<br />
NGC 4365 1078 186.09391 7.32635 1.82 −9.335 ± 0.012 −10.349 ± 0.025 2.74 ± 0.14 1.00<br />
NGC 4365 1079 186.11329 7.34978 2.34 −7.672 ± 0.034 −8.639 ± 0.044 3.01 ± 0.36 1.00<br />
NGC 4365 1083 186.09523 7.32892 1.81 −7.099 ± 0.045 −8.106 ± 0.054 2.92 ± 0.45 0.99<br />
NGC 4365 1085 186.08768 7.32041 2.17 −8.397 ± 0.035 −9.790 ± 0.019 2.20 ± 0.21 1.00<br />
NGC 4365 1087 186.09504 7.32931 1.83 −8.204 ± 0.024 −9.242 ± 0.031 2.83 ± 0.23 1.00<br />
NGC 4365 1088 186.08176 7.31375 2.60 −6.276 ± 0.072 −7.381 ± 0.238 5.74 ± 2.04 0.61<br />
NGC 4365 1089 186.10327 7.33924 1.87 −7.398 ± 0.039 −8.347 ± 0.041 2.25 ± 0.36 0.99<br />
NGC 4365 1091 186.10727 7.34407 2.05 −5.628 ± 0.356 −7.209 ± 0.075 4.46 ± 1.69 0.84<br />
NGC 4365 1092 186.08158 7.31373 2.61 −6.747 ± 0.058 −7.588 ± 0.075 5.67 ± 0.45 0.70<br />
NGC 4365 1093 186.08261 7.31508 2.53 −7.491 ± 0.041 −8.793 ± 0.028 2.72 ± 0.29 1.00<br />
NGC 4365 1094 186.10603 7.34280 2.00 −7.685 ± 0.121 −8.720 ± 0.068 8.15 ± 0.92 0.79<br />
NGC 4365 1095 186.10317 7.33954 1.89 −7.137 ± 0.039 −8.330 ± 0.044 3.51 ± 0.30 0.99<br />
NGC 4365 1098 186.09859 7.33429 1.82 −7.598 ± 0.623 −9.069 ± 0.113 2.02 ± 0.40 0.99<br />
NGC 4365 1101 186.08102 7.31419 2.65 −8.449 ± 0.056 −9.333 ± 0.022 3.74 ± 0.33 1.00<br />
NGC 4365 1102 186.10495 7.34268 2.02 −5.872 ± 0.829 −7.423 ± 0.133 5.19 ± 1.04 0.74<br />
NGC 4365 1103 186.08082 7.31416 2.66 −5.650 ± 0.290 −7.032 ± 0.101 2.93 ± 0.69 0.95<br />
NGC 4365 1104 186.09926 7.33604 1.87 −6.502 ± 0.093 −7.387 ± 0.073 5.25 ± 0.67 0.72<br />
NGC 4365 1105 186.08573 7.32017 2.30 −6.051 ± 0.108 −6.936 ± 0.696 2.49 ± 0.86 0.96<br />
NGC 4365 1106 186.09584 7.33217 1.89 −8.247 ± 0.035 −9.628 ± 0.015 1.90 ± 0.17 0.98<br />
NGC 4365 1111 186.07992 7.31364 2.73 −8.073 ± 0.042 −9.497 ± 0.022 2.31 ± 0.26 1.00<br />
NGC 4365 1113 186.09226 7.32835 1.98 −6.953 ± 0.078 −8.428 ± 0.056 3.36 ± 0.54 1.00<br />
NGC 4365 1114 186.08395 7.31868 2.43 −9.259 ± 0.019 −10.127 ± 0.014 3.11 ± 0.18 1.00<br />
NGC 4365 1115 186.10106 7.33838 1.91 −6.078 ± 0.102 −7.604 ± 0.094 3.33 ± 0.76 0.98<br />
NGC 4365 1116 186.10124 7.33964 1.98 −9.216 ± 0.023 −10.208 ± 0.019 2.14 ± 0.17 0.99<br />
NGC 4365 1117 186.09436 7.33152 1.95 −6.895 ± 0.073 −7.889 ± 0.121 3.65 ± 0.78 0.98<br />
NGC 4365 1118 186.11075 7.35109 2.46 −7.533 ± 0.031 −8.790 ± 0.072 2.32 ± 0.40 0.99<br />
NGC 4365 1121 186.10106 7.34010 2.01 −6.955 ± 0.041 −8.261 ± 0.038 2.43 ± 0.35 0.99<br />
NGC 4365 1123 186.08412 7.32033 2.42 −7.665 ± 0.030 −9.055 ± 0.024 3.72 ± 0.24 1.00<br />
NGC 4365 1125 186.10504 7.34562 2.21 −6.439 ± 0.230 −7.997 ± 0.046 2.58 ± 0.53 0.99<br />
NGC 4365 1126 186.09448 7.33318 2.01 −6.797 ± 0.053 −7.936 ± 0.240 3.24 ± 0.40 0.99<br />
NGC 4365 1129 186.10535 7.34633 2.25 −8.621 ± 0.035 −9.476 ± 0.015 2.52 ± 0.27 1.00<br />
NGC 4365 1130 186.10006 7.34011 2.05 −8.404 ± 0.017 −9.453 ± 0.021 2.38 ± 0.23 1.00<br />
Continued on Next Page. . .<br />
309
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4365 1131 186.09660 7.33599 2.01 −6.619 ± 0.057 −8.072 ± 0.044 3.60 ± 0.46 0.99<br />
NGC 4365 1132 186.08566 7.32325 2.34 −7.094 ± 0.052 −8.149 ± 0.069 2.94 ± 0.42 0.99<br />
NGC 4365 1133 186.11079 7.35343 2.63 −10.158 ± 0.011 −11.498 ± 0.027 4.30 ± 0.25 1.00<br />
NGC 4365 1136 186.10849 7.35088 2.48 −8.668 ± 0.266 −10.159 ± 0.439 3.22 ± 0.69 1.00<br />
NGC 4365 1137 186.07787 7.31463 2.87 −6.643 ± 0.116 −7.820 ± 0.091 6.04 ± 0.65 0.73<br />
NGC 4365 1138 186.10432 7.34538 2.22 −6.828 ± 0.040 −7.668 ± 0.067 2.53 ± 0.38 0.98<br />
NGC 4365 1142 186.09213 7.33187 2.10 −7.924 ± 0.029 −8.929 ± 0.023 2.97 ± 0.19 1.00<br />
NGC 4365 1146 186.11197 7.35549 2.76 −7.071 ± 0.025 −8.436 ± 0.037 3.05 ± 0.34 1.00<br />
NGC 4365 1147 186.10174 7.34345 2.18 −7.804 ± 0.029 −8.576 ± 0.028 2.37 ± 0.21 0.99<br />
NGC 4365 1149 186.08470 7.32347 2.41 −9.440 ± 0.017 −10.507 ± 0.019 1.86 ± 0.18 0.98<br />
NGC 4365 1151 186.08046 7.31861 2.68 −7.498 ± 0.028 −8.572 ± 0.037 3.77 ± 0.38 0.99<br />
NGC 4365 1153 186.09177 7.33207 2.13 −7.310 ± 0.038 −8.514 ± 0.026 2.24 ± 0.34 0.99<br />
NGC 4365 1156 186.09989 7.34190 2.17 −7.478 ± 0.041 −8.350 ± 0.034 3.39 ± 0.28 0.99<br />
NGC 4365 1159 186.09992 7.34149 2.14 −7.972 ± 0.018 −9.263 ± 0.030 1.94 ± 0.24 0.99<br />
NGC 4365 1163 186.08086 7.32000 2.65 −9.487 ± 0.024 −10.860 ± 0.014 2.65 ± 0.13 1.00<br />
NGC 4365 1169 186.10634 7.35052 2.51 −7.314 ± 0.093 −8.630 ± 0.185 7.68 ± 2.01 0.83<br />
NGC 4365 1172 186.08837 7.32926 2.27 −5.677 ± 0.075 −7.254 ± 0.195 5.67 ± 1.40 0.58<br />
NGC 4365 1174 186.09479 7.33710 2.16 −6.345 ± 0.080 −7.567 ± 0.107 2.86 ± 0.70 0.98<br />
NGC 4365 1178 186.09355 7.33609 2.18 −9.352 ± 0.022 −10.641 ± 0.040 2.61 ± 0.32 1.00<br />
NGC 4365 1181 186.09122 7.33341 2.21 −8.926 ± 0.012 −10.316 ± 0.018 2.06 ± 0.13 0.99<br />
NGC 4365 1183 186.09542 7.33851 2.19 −8.393 ± 0.030 −9.631 ± 0.019 1.89 ± 0.22 0.98<br />
NGC 4365 1184 186.10721 7.35252 2.62 −8.079 ± 0.029 −9.354 ± 0.021 1.81 ± 0.20 0.98<br />
NGC 4365 1187 186.09091 7.33356 2.24 −8.741 ± 0.018 −10.067 ± 0.018 2.86 ± 0.14 1.00<br />
NGC 4365 1188 186.08519 7.32690 2.43 −7.751 ± 0.029 −9.237 ± 0.017 2.46 ± 0.15 1.00<br />
NGC 4365 1189 186.08183 7.32286 2.60 −5.762 ± 0.087 −7.179 ± 0.105 3.13 ± 0.65 0.96<br />
NGC 4365 1190 186.07596 7.31631 3.00 −7.246 ± 0.056 −8.310 ± 0.108 5.13 ± 0.64 0.94<br />
NGC 4365 1194 186.07629 7.31739 2.97 −9.027 ± 0.022 −10.153 ± 0.017 2.72 ± 0.16 1.00<br />
NGC 4365 1195 186.07647 7.31768 2.96 −6.258 ± 0.084 −7.326 ± 0.060 3.88 ± 0.35 0.93<br />
NGC 4365 1198 186.09471 7.33948 2.28 −7.404 ± 0.048 −8.079 ± 0.022 3.20 ± 0.30 0.99<br />
NGC 4365 1199 186.09364 7.33828 2.28 −6.819 ± 0.043 −8.155 ± 0.046 3.26 ± 0.38 0.99<br />
NGC 4365 1202 186.10912 7.35691 2.90 −8.929 ± 0.040 −9.913 ± 0.037 5.01 ± 0.33 1.00<br />
NGC 4365 1204 186.08281 7.32584 2.57 −7.744 ± 0.027 −8.976 ± 0.041 2.34 ± 0.33 1.00<br />
NGC 4365 1205 186.09940 7.34547 2.40 −7.278 ± 0.033 −8.487 ± 0.040 2.77 ± 0.39 1.00<br />
NGC 4365 1206 186.09996 7.34628 2.42 −7.035 ± 0.029 −8.024 ± 0.178 2.72 ± 0.36 0.99<br />
NGC 4365 1207 186.09442 7.34003 2.32 −7.626 ± 0.047 −8.917 ± 0.026 2.70 ± 0.35 1.00<br />
NGC 4365 1208 186.07434 7.31628 3.12 −7.570 ± 0.040 −8.468 ± 0.044 4.09 ± 0.33 0.99<br />
NGC 4365 1209 186.09293 7.33833 2.32 −8.198 ± 0.025 −9.060 ± 0.024 2.92 ± 0.33 1.00<br />
NGC 4365 1214 186.10021 7.34726 2.48 −7.277 ± 1.075 −8.522 ± 0.037 1.99 ± 0.48 0.99<br />
NGC 4365 1216 186.10849 7.35775 2.97 −8.693 ± 0.032 −9.807 ± 0.027 2.74 ± 0.31 1.00<br />
NGC 4365 1218 186.08717 7.33302 2.46 −7.304 ± 0.079 −8.681 ± 0.050 2.33 ± 0.43 0.99<br />
NGC 4365 1219 186.08969 7.33619 2.41 −9.215 ± 0.027 −10.219 ± 0.035 7.02 ± 0.21 1.00<br />
NGC 4365 1221 186.08433 7.32991 2.55 −9.141 ± 0.044 −10.012 ± 0.042 9.60 ± 0.34 0.96<br />
NGC 4365 1223 186.07395 7.31773 3.14 −5.936 ± 0.447 −7.122 ± 0.249 4.05 ± 1.07 0.89<br />
NGC 4365 1226 186.10727 7.35744 2.97 −7.186 ± 0.040 −8.020 ± 0.052 3.22 ± 0.41 0.99<br />
NGC 4365 1228 186.08293 7.32877 2.62 −5.738 ± 0.862 −7.349 ± 0.078 2.97 ± 0.89 0.97<br />
NGC 4365 1230 186.10112 7.35055 2.65 −7.644 ± 0.028 −8.461 ± 0.032 2.05 ± 0.34 0.99<br />
NGC 4365 1231 186.08499 7.33183 2.56 −8.956 ± 0.084 −10.571 ± 0.069 11.26 ± 0.88 0.84<br />
NGC 4365 1233 186.07754 7.32317 2.91 −8.653 ± 0.020 −9.735 ± 0.027 3.91 ± 0.25 1.00<br />
NGC 4365 1234 186.07272 7.31746 3.23 −7.194 ± 0.076 −8.610 ± 0.033 3.66 ± 0.38 0.99<br />
NGC 4365 1235 186.09387 7.34270 2.49 −7.356 ± 0.031 −8.448 ± 0.361 2.58 ± 0.42 1.00<br />
NGC 4365 1236 186.08116 7.32775 2.72 −8.902 ± 0.025 −10.151 ± 0.018 3.29 ± 0.20 1.00<br />
NGC 4365 1238 186.07922 7.32629 2.83 −7.430 ± 1.363 −8.783 ± 0.432 1.78 ± 0.50 0.98<br />
NGC 4374 4 186.24051 12.88323 1.75 −8.499 ± 0.015 −9.375 ± 0.027 2.83 ± 0.14 1.00<br />
NGC 4374 5 186.24088 12.88349 1.72 −9.610 ± 0.021 −10.604 ± 0.022 3.39 ± 0.12 1.00<br />
NGC 4374 7 186.24109 12.88295 1.71 −6.067 ± 0.222 −7.333 ± 0.720 0.90 ± 0.36 0.65<br />
NGC 4374 10 186.23960 12.87709 1.92 −9.479 ± 0.032 −10.420 ± 0.040 6.86 ± 0.23 1.00<br />
NGC 4374 11 186.24707 12.90006 1.58 −8.057 ± 0.027 −8.835 ± 0.029 3.30 ± 0.17 1.00<br />
NGC 4374 13 186.23711 12.86857 2.36 −7.628 ± 0.033 −8.574 ± 0.036 2.88 ± 0.19 1.00<br />
NGC 4374 14 186.23966 12.87347 2.03 −5.706 ± 0.115 −6.892 ± 0.358 1.66 ± 0.50 0.91<br />
NGC 4374 18 186.23877 12.86886 2.25 −7.207 ± 0.045 −7.938 ± 0.032 3.40 ± 0.24 0.98<br />
NGC 4374 19 186.24130 12.87751 1.80 −6.981 ± 0.048 −7.860 ± 0.051 3.00 ± 0.28 0.99<br />
Continued on Next Page. . .<br />
310
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4374 20 186.24498 12.88983 1.43 −6.634 ± 0.068 −7.867 ± 0.065 3.16 ± 0.35 0.99<br />
NGC 4374 22 186.24132 12.87659 1.83 −9.179 ± 0.018 −10.565 ± 0.015 2.26 ± 0.14 1.00<br />
NGC 4374 23 186.24378 12.88512 1.51 −5.390 ± 0.433 −7.124 ± 0.472 1.43 ± 0.66 0.87<br />
NGC 4374 26 186.24090 12.87385 1.94 −9.529 ± 0.012 −10.462 ± 0.015 3.67 ± 0.11 1.00<br />
NGC 4374 27 186.24481 12.88656 1.43 −8.740 ± 0.025 −9.693 ± 0.021 2.69 ± 0.14 1.00<br />
NGC 4374 29 186.24434 12.88532 1.47 −7.682 ± 0.069 −8.731 ± 0.030 1.86 ± 0.23 1.00<br />
NGC 4374 30 186.24141 12.87409 1.90 −7.092 ± 0.034 −8.333 ± 0.056 3.05 ± 0.35 0.99<br />
NGC 4374 32 186.24036 12.87030 2.10 −7.817 ± 0.019 −8.779 ± 0.025 2.77 ± 0.16 1.00<br />
NGC 4374 37 186.24997 12.90129 1.48 −7.820 ± 0.021 −9.036 ± 0.034 1.87 ± 0.18 1.00<br />
NGC 4374 38 186.23989 12.86590 2.32 −5.627 ± 0.083 −6.988 ± 0.105 3.20 ± 0.59 0.93<br />
NGC 4374 39 186.24606 12.88682 1.35 −6.620 ± 0.084 −7.985 ± 0.052 1.58 ± 0.46 0.96<br />
NGC 4374 41 186.25108 12.90333 1.53 −7.104 ± 0.030 −8.028 ± 0.045 2.34 ± 0.24 1.00<br />
NGC 4374 42 186.24297 12.87461 1.79 −9.794 ± 0.021 −10.886 ± 0.019 3.79 ± 0.15 1.00<br />
NGC 4374 44 186.25261 12.90774 1.72 −6.605 ± 0.139 −7.642 ± 0.097 1.98 ± 0.39 0.98<br />
NGC 4374 45 186.24582 12.88361 1.38 −10.665 ± 0.011 −11.806 ± 0.025 4.93 ± 0.11 0.92<br />
NGC 4374 46 186.24790 12.89063 1.25 −5.530 ± 0.596 −6.603 ± 0.103 3.14 ± 0.98 0.92<br />
NGC 4374 48 186.24706 12.88738 1.28 −8.970 ± 0.019 −9.822 ± 0.012 2.93 ± 0.11 1.00<br />
NGC 4374 49 186.25110 12.90152 1.43 −7.648 ± 0.025 −8.698 ± 0.027 2.85 ± 0.21 1.00<br />
NGC 4374 50 186.24164 12.86841 2.11 −6.183 ± 0.289 −7.120 ± 0.133 3.12 ± 1.01 0.95<br />
NGC 4374 51 186.24849 12.89209 1.23 −6.797 ± 0.034 −7.849 ± 0.055 2.67 ± 0.34 0.99<br />
NGC 4374 53 186.25183 12.90320 1.49 −7.931 ± 0.034 −9.160 ± 0.022 1.75 ± 0.15 0.98<br />
NGC 4374 54 186.25410 12.91119 1.88 −6.158 ± 0.073 −7.480 ± 0.191 5.20 ± 1.23 0.71<br />
NGC 4374 55 186.25516 12.91408 2.04 −8.365 ± 0.014 −9.580 ± 0.019 2.96 ± 0.11 1.00<br />
NGC 4374 58 186.24585 12.88158 1.41 −7.818 ± 0.043 −8.588 ± 0.059 5.48 ± 0.28 0.96<br />
NGC 4374 60 186.24965 12.89465 1.22 −7.477 ± 0.485 −8.762 ± 0.021 1.81 ± 0.29 1.00<br />
NGC 4374 61 186.25577 12.91594 2.15 −6.813 ± 0.082 −7.619 ± 0.094 4.17 ± 0.47 0.91<br />
NGC 4374 63 186.24285 12.87050 1.95 −6.371 ± 0.589 −7.723 ± 0.053 2.15 ± 1.05 0.99<br />
NGC 4374 67 186.25336 12.90455 1.50 −6.566 ± 0.069 −7.301 ± 0.518 1.60 ± 0.51 0.92<br />
NGC 4374 68 186.24866 12.88809 1.17 −8.315 ± 0.017 −9.093 ± 0.027 2.82 ± 0.17 1.00<br />
NGC 4374 73 186.25592 12.91163 1.86 −6.666 ± 0.045 −8.076 ± 0.046 2.91 ± 0.36 0.99<br />
NGC 4374 74 186.25655 12.91311 1.95 −7.212 ± 0.038 −8.201 ± 0.056 3.40 ± 0.26 0.99<br />
NGC 4374 75 186.24501 12.87308 1.73 −7.078 ± 0.256 −7.589 ± 0.093 2.50 ± 0.49 0.99<br />
NGC 4374 76 186.24701 12.88002 1.37 −5.994 ± 0.080 −7.383 ± 0.066 3.03 ± 0.39 0.97<br />
NGC 4374 77 186.25044 12.89165 1.10 −6.841 ± 0.036 −7.865 ± 0.393 2.38 ± 0.39 0.99<br />
NGC 4374 79 186.24738 12.88036 1.34 −8.496 ± 0.026 −9.366 ± 0.024 2.49 ± 0.24 1.00<br />
NGC 4374 80 186.24994 12.88916 1.09 −8.066 ± 0.022 −9.371 ± 0.020 1.67 ± 0.10 0.97<br />
NGC 4374 81 186.24958 12.88726 1.10 −10.514 ± 0.013 −11.631 ± 0.017 3.91 ± 0.08 1.00<br />
NGC 4374 82 186.24314 12.86467 2.21 −8.581 ± 0.025 −9.511 ± 0.025 3.58 ± 0.19 1.00<br />
NGC 4374 83 186.24496 12.87074 1.83 −7.990 ± 0.021 −8.810 ± 0.033 2.65 ± 0.23 1.00<br />
NGC 4374 84 186.24660 12.87618 1.52 −9.403 ± 0.010 −10.792 ± 0.019 2.07 ± 0.12 1.00<br />
NGC 4374 86 186.25110 12.89179 1.06 −6.573 ± 0.391 −7.594 ± 0.059 2.70 ± 0.50 0.99<br />
NGC 4374 89 186.24765 12.87872 1.37 −9.447 ± 0.018 −10.355 ± 0.024 3.64 ± 0.15 1.00<br />
NGC 4374 90 186.24853 12.88098 1.25 −9.656 ± 0.026 −10.576 ± 0.013 4.06 ± 0.17 1.00<br />
NGC 4374 91 186.24425 12.86586 2.10 −8.700 ± 0.018 −10.026 ± 0.016 2.76 ± 0.14 1.00<br />
NGC 4374 92 186.25504 12.91156 1.88 −6.855 ± 0.049 −7.757 ± 0.080 4.12 ± 0.44 0.93<br />
NGC 4374 93 186.24848 12.88062 1.26 −5.859 ± 0.762 −7.234 ± 0.048 1.61 ± 0.53 0.92<br />
NGC 4374 95 186.24498 12.86782 1.96 −7.265 ± 0.046 −8.583 ± 0.029 3.27 ± 0.20 1.00<br />
NGC 4374 96 186.25401 12.89924 1.18 −6.347 ± 0.059 −7.478 ± 0.163 3.39 ± 0.90 0.96<br />
NGC 4374 98 186.24990 12.88453 1.10 −7.117 ± 0.030 −8.099 ± 0.118 2.73 ± 0.41 0.99<br />
NGC 4374 100 186.25168 12.88947 0.97 −7.732 ± 0.037 −8.581 ± 0.045 2.46 ± 0.34 1.00<br />
NGC 4374 101 186.25205 12.89063 0.97 −7.940 ± 0.058 −8.696 ± 0.085 5.73 ± 0.48 0.95<br />
NGC 4374 102 186.25147 12.88852 0.98 −7.642 ± 0.018 −8.464 ± 0.031 1.58 ± 0.19 0.96<br />
NGC 4374 103 186.24459 12.86411 2.17 −7.205 ± 0.037 −8.450 ± 0.037 2.36 ± 0.24 1.00<br />
NGC 4374 105 186.24924 12.87986 1.24 −5.711 ± 1.385 −6.687 ± 0.236 2.11 ± 0.71 0.94<br />
NGC 4374 106 186.24495 12.86465 2.13 −8.646 ± 0.009 −9.684 ± 0.018 2.31 ± 0.11 1.00<br />
NGC 4374 107 186.25110 12.88612 1.00 −6.084 ± 0.258 −7.198 ± 0.134 5.19 ± 2.31 0.58<br />
NGC 4374 108 186.25681 12.90578 1.46 −8.522 ± 0.028 −9.357 ± 0.025 2.37 ± 0.22 1.00<br />
NGC 4374 109 186.25063 12.88376 1.06 −8.752 ± 0.015 −9.830 ± 0.019 2.52 ± 0.15 1.00<br />
NGC 4374 111 186.24939 12.87930 1.24 −6.910 ± 0.186 −7.564 ± 0.343 2.49 ± 0.37 0.99<br />
NGC 4374 112 186.25063 12.88356 1.06 −7.185 ± 1.028 −8.115 ± 0.074 1.58 ± 0.39 0.96<br />
NGC 4374 113 186.25766 12.90786 1.57 −7.998 ± 0.032 −9.506 ± 0.023 2.78 ± 0.16 1.00<br />
NGC 4374 114 186.24513 12.86410 2.15 −7.005 ± 0.051 −7.868 ± 0.055 2.66 ± 0.25 0.99<br />
Continued on Next Page. . .<br />
311
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4374 116 186.24880 12.87656 1.37 −7.757 ± 0.027 −8.570 ± 0.023 3.10 ± 0.23 1.00<br />
NGC 4374 117 186.25935 12.91296 1.88 −6.564 ± 0.101 −7.089 ± 0.074 3.12 ± 0.71 0.95<br />
NGC 4374 118 186.25298 12.89073 0.91 −7.474 ± 0.025 −8.811 ± 0.034 2.21 ± 0.22 1.00<br />
NGC 4374 120 186.24971 12.87910 1.23 −7.417 ± 0.037 −8.394 ± 0.076 3.88 ± 0.38 1.00<br />
NGC 4374 121 186.25450 12.89513 0.96 −8.452 ± 0.021 −9.735 ± 0.015 1.78 ± 0.11 1.00<br />
NGC 4374 122 186.25900 12.91049 1.72 −8.278 ± 0.025 −9.034 ± 0.046 4.18 ± 0.23 1.00<br />
NGC 4374 123 186.25560 12.89863 1.07 −8.517 ± 0.018 −9.606 ± 0.019 2.47 ± 0.20 1.00<br />
NGC 4374 124 186.24916 12.87617 1.37 −6.416 ± 0.034 −7.253 ± 0.142 1.80 ± 0.42 0.95<br />
NGC 4374 126 186.25238 12.88703 0.91 −9.019 ± 0.020 −10.008 ± 0.023 3.09 ± 0.14 1.00<br />
NGC 4374 129 186.25609 12.89874 1.06 −7.094 ± 0.026 −8.228 ± 0.037 2.71 ± 0.26 1.00<br />
NGC 4374 130 186.25835 12.90614 1.44 −6.501 ± 0.066 −7.646 ± 0.052 3.03 ± 0.31 0.98<br />
NGC 4374 131 186.24941 12.87439 1.43 −8.062 ± 0.019 −9.266 ± 0.026 1.74 ± 0.17 0.98<br />
NGC 4374 132 186.25578 12.89642 0.95 −6.310 ± 0.575 −6.822 ± 0.322 1.34 ± 0.47 0.83<br />
NGC 4374 134 186.25521 12.89227 0.81 −9.310 ± 0.020 −10.228 ± 0.027 10.32 ± 0.16 0.86<br />
NGC 4374 135 186.25890 12.90507 1.36 −7.838 ± 0.040 −8.844 ± 0.048 5.19 ± 0.21 0.99<br />
NGC 4374 136 186.25070 12.87655 1.26 −7.573 ± 0.023 −8.472 ± 0.061 2.93 ± 0.51 1.00<br />
NGC 4374 138 186.25667 12.89688 0.93 −8.783 ± 0.021 −9.706 ± 0.018 2.04 ± 0.14 1.00<br />
NGC 4374 139 186.25573 12.89432 0.85 −7.871 ± 0.018 −8.948 ± 0.339 2.03 ± 0.26 1.00<br />
NGC 4374 140 186.25465 12.88963 0.78 −6.643 ± 0.326 −8.261 ± 0.069 1.80 ± 0.37 0.98<br />
NGC 4374 142 186.25606 12.89417 0.83 −8.013 ± 0.017 −9.325 ± 0.023 2.92 ± 0.16 1.00<br />
NGC 4374 145 186.25321 12.88361 0.89 −8.345 ± 0.026 −9.593 ± 0.014 2.28 ± 0.26 1.00<br />
NGC 4374 147 186.25513 12.89010 0.75 −6.825 ± 0.062 −7.761 ± 0.204 3.73 ± 1.08 0.96<br />
NGC 4374 148 186.25859 12.90155 1.14 −8.769 ± 0.021 −9.641 ± 0.022 2.84 ± 0.16 1.00<br />
NGC 4374 150 186.25891 12.90240 1.18 −7.397 ± 0.030 −8.684 ± 0.028 2.28 ± 0.17 1.00<br />
NGC 4374 153 186.25001 12.87103 1.56 −7.046 ± 0.076 −7.769 ± 0.058 3.73 ± 0.44 0.96<br />
NGC 4374 154 186.25506 12.88847 0.73 −6.544 ± 0.054 −7.751 ± 0.065 2.80 ± 0.43 0.99<br />
NGC 4374 155 186.26057 12.90731 1.48 −7.851 ± 0.028 −9.197 ± 0.028 2.77 ± 0.17 1.00<br />
NGC 4374 156 186.25743 12.89634 0.87 −8.017 ± 0.021 −9.532 ± 0.029 2.32 ± 0.18 1.00<br />
NGC 4374 157 186.26290 12.91530 2.01 −7.521 ± 0.027 −8.890 ± 0.022 2.01 ± 0.17 1.00<br />
NGC 4374 158 186.25966 12.90356 1.24 −8.678 ± 0.017 −9.618 ± 0.016 2.30 ± 0.13 1.00<br />
NGC 4374 163 186.25509 12.88706 0.72 −7.564 ± 0.094 −8.952 ± 0.054 1.80 ± 0.39 1.00<br />
NGC 4374 165 186.25833 12.89814 0.93 −6.301 ± 0.106 −7.511 ± 0.172 3.85 ± 0.91 0.92<br />
NGC 4374 166 186.25104 12.87212 1.45 −8.745 ± 0.021 −9.887 ± 0.019 2.40 ± 0.20 1.00<br />
NGC 4374 167 186.25261 12.87745 1.12 −6.329 ± 0.374 −7.775 ± 0.096 3.49 ± 0.60 0.97<br />
NGC 4374 172 186.26154 12.90726 1.46 −7.789 ± 0.030 −8.811 ± 0.026 2.94 ± 0.17 1.00<br />
NGC 4374 173 186.25575 12.88707 0.68 −7.271 ± 0.043 −8.206 ± 1.109 1.48 ± 0.31 0.95<br />
NGC 4374 174 186.25703 12.89121 0.66 −7.882 ± 0.026 −9.346 ± 0.196 1.59 ± 0.23 0.96<br />
NGC 4374 175 186.25690 12.89031 0.64 −8.277 ± 0.020 −9.076 ± 0.025 2.22 ± 0.21 1.00<br />
NGC 4374 176 186.25607 12.88750 0.66 −6.595 ± 0.181 −7.591 ± 0.054 1.79 ± 0.40 0.96<br />
NGC 4374 177 186.25639 12.88847 0.64 −6.447 ± 0.058 −7.583 ± 0.076 2.34 ± 0.39 0.99<br />
NGC 4374 179 186.25292 12.87549 1.19 −7.209 ± 0.039 −8.171 ± 0.062 4.29 ± 0.33 0.97<br />
NGC 4374 181 186.25780 12.89173 0.63 −7.656 ± 0.027 −8.987 ± 0.031 1.69 ± 0.22 0.98<br />
NGC 4374 182 186.24958 12.86292 2.03 −7.783 ± 0.025 −8.903 ± 0.039 3.43 ± 0.26 1.00<br />
NGC 4374 183 186.25885 12.89512 0.74 −8.526 ± 0.026 −9.529 ± 0.018 2.12 ± 0.13 1.00<br />
NGC 4374 187 186.26088 12.90178 1.09 −9.098 ± 0.024 −10.626 ± 0.021 2.47 ± 0.27 1.00<br />
NGC 4374 188 186.26282 12.90865 1.54 −6.849 ± 0.087 −7.986 ± 0.118 5.63 ± 0.63 0.82<br />
NGC 4374 189 186.24966 12.86274 2.04 −7.485 ± 0.030 −8.527 ± 0.040 3.33 ± 0.26 1.00<br />
NGC 4374 190 186.26323 12.90901 1.56 −8.562 ± 0.027 −9.575 ± 0.043 5.63 ± 0.17 0.99<br />
NGC 4374 192 186.26135 12.90219 1.11 −6.727 ± 0.040 −8.162 ± 0.055 1.77 ± 0.33 0.98<br />
NGC 4374 193 186.26103 12.90096 1.04 −6.776 ± 0.116 −7.570 ± 0.538 3.60 ± 1.12 0.95<br />
NGC 4374 194 186.25009 12.86284 2.01 −7.214 ± 0.029 −8.189 ± 0.054 2.56 ± 0.26 1.00<br />
NGC 4374 197 186.25227 12.86989 1.52 −6.536 ± 0.033 −7.896 ± 0.097 3.75 ± 0.36 0.97<br />
NGC 4374 199 186.25230 12.86960 1.53 −8.709 ± 0.020 −9.908 ± 0.023 3.77 ± 0.15 1.00<br />
NGC 4374 200 186.26116 12.89964 0.94 −8.526 ± 0.015 −9.520 ± 0.020 2.50 ± 0.09 1.00<br />
NGC 4374 201 186.26311 12.90644 1.38 −5.511 ± 0.271 −6.493 ± 0.431 2.06 ± 1.54 0.93<br />
NGC 4374 202 186.25191 12.86724 1.69 −8.004 ± 0.029 −8.855 ± 0.029 2.88 ± 0.23 1.00<br />
NGC 4374 203 186.26393 12.90906 1.56 −6.883 ± 0.057 −7.707 ± 0.047 3.22 ± 0.35 0.98<br />
NGC 4374 204 186.25083 12.86320 1.97 −8.266 ± 0.016 −9.142 ± 0.025 3.31 ± 0.17 1.00<br />
NGC 4374 205 186.26123 12.89953 0.93 −6.669 ± 0.036 −7.658 ± 0.049 2.64 ± 0.22 0.99<br />
NGC 4374 206 186.25742 12.88595 0.57 −7.630 ± 0.032 −9.017 ± 0.065 2.69 ± 0.36 1.00<br />
NGC 4374 207 186.25994 12.89455 0.66 −6.426 ± 0.117 −7.431 ± 0.182 3.67 ± 1.44 0.93<br />
NGC 4374 208 186.25725 12.88449 0.60 −8.184 ± 0.079 −9.457 ± 0.021 1.43 ± 0.20 0.94<br />
Continued on Next Page. . .<br />
312
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4374 209 186.25836 12.88820 0.51 −7.900 ± 0.026 −8.898 ± 0.046 3.21 ± 0.20 1.00<br />
NGC 4374 210 186.26601 12.91482 1.97 −6.687 ± 0.035 −7.806 ± 0.045 2.33 ± 0.33 0.99<br />
NGC 4374 211 186.25620 12.87992 0.82 −6.576 ± 0.223 −7.774 ± 0.170 6.39 ± 2.28 0.61<br />
NGC 4374 212 186.26073 12.89554 0.69 −6.300 ± 0.113 −7.979 ± 0.133 3.90 ± 0.84 0.97<br />
NGC 4374 213 186.25769 12.88489 0.57 −7.834 ± 0.021 −8.772 ± 0.053 2.59 ± 0.26 1.00<br />
NGC 4374 217 186.25791 12.88421 0.57 −8.030 ± 0.152 −9.354 ± 0.250 1.47 ± 0.30 0.95<br />
NGC 4374 218 186.25899 12.88788 0.46 −7.253 ± 0.090 −8.409 ± 0.095 6.87 ± 0.59 0.74<br />
NGC 4374 219 186.25975 12.89045 0.47 −8.184 ± 0.029 −9.612 ± 0.024 1.85 ± 0.20 1.00<br />
NGC 4374 222 186.25893 12.88705 0.46 −6.161 ± 1.161 −7.494 ± 0.164 1.82 ± 0.51 0.96<br />
NGC 4374 223 186.26421 12.90509 1.28 −7.308 ± 0.053 −8.099 ± 0.072 2.77 ± 0.30 0.99<br />
NGC 4374 224 186.25702 12.87962 0.79 −8.199 ± 0.052 −9.359 ± 0.059 1.40 ± 0.30 0.94<br />
NGC 4374 225 186.25968 12.88881 0.43 −8.665 ± 0.030 −9.713 ± 0.030 2.42 ± 0.19 1.00<br />
NGC 4374 226 186.25894 12.88607 0.46 −7.969 ± 0.020 −8.882 ± 0.052 2.98 ± 0.22 1.00<br />
NGC 4374 227 186.25861 12.88465 0.51 −7.903 ± 0.054 −9.003 ± 0.093 5.53 ± 0.49 0.98<br />
NGC 4374 228 186.25824 12.88335 0.57 −8.046 ± 0.021 −9.017 ± 0.032 1.89 ± 0.24 1.00<br />
NGC 4374 229 186.25838 12.88336 0.56 −8.845 ± 0.020 −10.066 ± 0.021 2.17 ± 0.15 1.00<br />
NGC 4374 230 186.26070 12.89203 0.49 −7.616 ± 0.045 −9.296 ± 0.034 1.90 ± 0.32 1.00<br />
NGC 4374 231 186.26003 12.88936 0.42 −8.350 ± 0.022 −9.787 ± 0.019 2.06 ± 0.24 1.00<br />
NGC 4374 232 186.25593 12.87469 1.10 −6.170 ± 0.078 −7.318 ± 0.372 1.28 ± 0.41 0.85<br />
NGC 4374 233 186.26126 12.89311 0.53 −9.268 ± 0.017 −10.202 ± 0.019 2.70 ± 0.21 1.00<br />
NGC 4374 234 186.26071 12.89083 0.43 −8.480 ± 0.027 −9.437 ± 0.031 2.94 ± 0.29 1.00<br />
NGC 4374 235 186.26244 12.89696 0.74 −9.841 ± 0.012 −10.922 ± 0.011 2.89 ± 0.13 1.00<br />
NGC 4374 236 186.26227 12.89605 0.68 −8.676 ± 0.023 −9.882 ± 0.020 2.35 ± 0.16 1.00<br />
NGC 4374 237 186.25822 12.88189 0.62 −5.326 ± 0.691 −7.088 ± 0.157 3.03 ± 1.77 0.95<br />
NGC 4374 238 186.26462 12.90317 1.14 −6.581 ± 0.199 −7.498 ± 0.097 2.85 ± 0.46 0.98<br />
NGC 4374 239 186.26520 12.90510 1.28 −6.490 ± 0.052 −7.693 ± 0.039 2.29 ± 0.34 0.99<br />
NGC 4374 240 186.26566 12.90658 1.38 −6.339 ± 0.060 −7.947 ± 0.067 2.61 ± 0.37 0.99<br />
NGC 4374 241 186.26253 12.89558 0.64 −9.132 ± 0.020 −9.968 ± 0.044 3.90 ± 0.21 1.00<br />
NGC 4374 242 186.25464 12.86735 1.58 −9.121 ± 0.040 −10.067 ± 0.052 6.74 ± 0.35 1.00<br />
NGC 4374 243 186.25600 12.87168 1.27 −7.451 ± 0.034 −8.620 ± 0.034 3.29 ± 0.31 1.00<br />
NGC 4374 244 186.25972 12.88484 0.43 −10.076 ± 0.013 −11.557 ± 0.021 2.55 ± 0.09 1.00<br />
NGC 4374 245 186.25386 12.86401 1.82 −7.429 ± 0.035 −8.530 ± 0.044 3.12 ± 0.23 1.00<br />
NGC 4374 246 186.26437 12.90031 0.94 −6.156 ± 0.095 −7.854 ± 0.139 5.68 ± 1.07 0.77<br />
NGC 4374 247 186.25733 12.87515 1.01 −9.816 ± 0.023 −10.688 ± 0.026 3.93 ± 0.13 1.00<br />
NGC 4374 250 186.26653 12.90691 1.41 −7.443 ± 0.019 −8.760 ± 0.022 2.39 ± 0.17 1.00<br />
NGC 4374 252 186.26667 12.90728 1.43 −5.498 ± 0.110 −6.688 ± 0.300 4.74 ± 3.22 0.53<br />
NGC 4374 254 186.25528 12.86694 1.59 −6.302 ± 0.118 −7.530 ± 0.047 2.53 ± 0.37 0.99<br />
NGC 4374 255 186.26876 12.91387 1.91 −5.386 ± 0.441 −6.812 ± 0.069 2.09 ± 0.71 0.95<br />
NGC 4374 257 186.25607 12.86938 1.41 −5.948 ± 0.057 −6.577 ± 0.763 1.43 ± 0.49 0.84<br />
NGC 4374 259 186.26901 12.91431 1.94 −6.085 ± 0.919 −7.800 ± 0.151 4.04 ± 40.80 0.94<br />
NGC 4374 260 186.25963 12.88130 0.58 −7.694 ± 0.027 −8.548 ± 0.048 2.55 ± 0.19 1.00<br />
NGC 4374 261 186.26225 12.89029 0.33 −8.149 ± 0.021 −9.122 ± 0.281 2.33 ± 0.24 1.00<br />
NGC 4374 264 186.26684 12.90554 1.31 −6.694 ± 0.041 −7.638 ± 0.099 1.98 ± 0.53 0.98<br />
NGC 4374 266 186.26067 12.88359 0.42 −9.400 ± 0.020 −10.364 ± 0.016 1.87 ± 0.18 1.00<br />
NGC 4374 267 186.26342 12.89318 0.46 −8.692 ± 0.015 −9.712 ± 0.026 2.79 ± 0.21 1.00<br />
NGC 4374 269 186.25614 12.86764 1.52 −6.656 ± 0.064 −7.614 ± 0.046 2.98 ± 0.32 0.98<br />
NGC 4374 270 186.26137 12.88514 0.32 −8.923 ± 0.026 −10.007 ± 0.023 2.81 ± 0.19 1.00<br />
NGC 4374 271 186.26920 12.91249 1.82 −7.027 ± 0.046 −8.095 ± 0.047 3.05 ± 0.32 0.99<br />
NGC 4374 272 186.26415 12.89427 0.52 −8.573 ± 0.018 −9.580 ± 0.028 2.50 ± 0.20 1.00<br />
NGC 4374 275 186.26762 12.90526 1.30 −6.265 ± 0.072 −7.531 ± 0.061 2.19 ± 0.49 0.98<br />
NGC 4374 276 186.25669 12.86679 1.55 −7.149 ± 0.025 −8.119 ± 0.317 1.50 ± 0.32 0.95<br />
NGC 4374 277 186.26810 12.90629 1.37 −9.101 ± 0.022 −10.074 ± 0.012 2.46 ± 0.12 1.00<br />
NGC 4374 278 186.26987 12.91257 1.83 −7.046 ± 0.045 −8.006 ± 0.079 3.69 ± 0.46 0.98<br />
NGC 4374 279 186.25568 12.86262 1.85 −5.296 ± 0.583 −6.217 ± 0.519 1.84 ± 1.31 0.91<br />
NGC 4374 280 186.26907 12.90906 1.58 −5.787 ± 0.064 −7.163 ± 0.247 2.39 ± 0.60 0.98<br />
NGC 4374 281 186.26357 12.88994 0.25 −7.750 ± 0.029 −8.742 ± 0.042 2.22 ± 0.22 1.00<br />
NGC 4374 282 186.26028 12.87795 0.74 −7.144 ± 0.050 −8.148 ± 0.041 2.12 ± 0.29 0.99<br />
NGC 4374 283 186.26578 12.89705 0.71 −8.108 ± 0.029 −8.822 ± 0.027 3.25 ± 0.16 1.00<br />
NGC 4374 284 186.26378 12.88955 0.22 −9.089 ± 0.064 −9.878 ± 0.030 2.88 ± 0.26 1.00<br />
NGC 4374 285 186.25981 12.87571 0.89 −8.131 ± 0.056 −9.494 ± 0.022 2.59 ± 0.31 1.00<br />
NGC 4374 286 186.26372 12.88936 0.21 −8.655 ± 0.022 −9.999 ± 0.032 2.68 ± 0.17 1.00<br />
NGC 4374 288 186.26132 12.88044 0.55 −6.165 ± 0.671 −7.117 ± 0.151 1.64 ± 0.62 0.92<br />
Continued on Next Page. . .<br />
313
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4374 291 186.26706 12.89966 0.90 −5.926 ± 0.084 −7.038 ± 0.128 2.46 ± 0.59 0.97<br />
NGC 4374 292 186.26350 12.88709 0.15 −8.314 ± 0.028 −9.525 ± 0.077 3.35 ± 0.30 1.00<br />
NGC 4374 293 186.26818 12.90330 1.16 −6.557 ± 0.063 −7.877 ± 0.061 2.79 ± 0.39 0.99<br />
NGC 4374 294 186.26595 12.89525 0.58 −8.479 ± 0.028 −10.060 ± 0.040 2.88 ± 0.22 1.00<br />
NGC 4374 295 186.26373 12.88682 0.13 −8.100 ± 0.394 −9.490 ± 1.031 1.21 ± 0.31 0.88<br />
NGC 4374 297 186.26653 12.89582 0.63 −7.466 ± 0.029 −8.450 ± 0.061 3.23 ± 0.31 1.00<br />
NGC 4374 298 186.25992 12.87256 1.09 −8.740 ± 0.019 −9.785 ± 0.020 3.08 ± 0.16 1.00<br />
NGC 4374 299 186.26422 12.88729 0.10 −9.776 ± 0.038 −10.837 ± 0.049 5.70 ± 0.20 1.00<br />
NGC 4374 300 186.26404 12.88678 0.11 −8.462 ± 0.014 −9.288 ± 0.082 2.26 ± 0.25 1.00<br />
NGC 4374 301 186.26198 12.87945 0.59 −8.944 ± 0.028 −9.854 ± 0.023 4.68 ± 0.13 1.00<br />
NGC 4374 302 186.26332 12.88383 0.27 −7.055 ± 0.160 −8.239 ± 0.171 3.49 ± 1.00 0.99<br />
NGC 4374 303 186.26870 12.90170 1.06 −8.801 ± 0.243 −9.693 ± 0.017 3.00 ± 0.49 1.00<br />
NGC 4374 304 186.25992 12.87094 1.20 −6.230 ± 0.092 −7.676 ± 0.200 5.02 ± 1.32 0.82<br />
NGC 4374 305 186.26639 12.89299 0.43 −5.906 ± 0.625 −7.713 ± 0.065 1.54 ± 0.56 0.94<br />
NGC 4374 306 186.26591 12.89110 0.29 −7.409 ± 0.697 −8.240 ± 0.356 2.06 ± 0.48 0.99<br />
NGC 4374 307 186.25892 12.86649 1.52 −8.450 ± 0.018 −9.729 ± 0.028 2.92 ± 0.16 1.00<br />
NGC 4374 308 186.26144 12.87486 0.90 −6.740 ± 0.137 −7.927 ± 0.056 2.73 ± 0.41 0.99<br />
NGC 4374 309 186.26077 12.87231 1.09 −8.817 ± 0.015 −9.953 ± 0.021 2.55 ± 0.10 1.00<br />
NGC 4374 311 186.26448 12.88540 0.14 −6.546 ± 0.320 −8.417 ± 0.160 3.83 ± 1.13 1.00<br />
NGC 4374 313 186.26584 12.88984 0.20 −7.999 ± 0.024 −9.003 ± 0.072 2.54 ± 0.34 1.00<br />
NGC 4374 314 186.26688 12.89227 0.38 −6.842 ± 0.138 −8.092 ± 0.167 3.80 ± 1.16 0.97<br />
NGC 4374 317 186.26869 12.89841 0.83 −7.333 ± 0.026 −8.897 ± 0.058 3.55 ± 0.20 1.00<br />
NGC 4374 318 186.25969 12.86615 1.53 −8.463 ± 0.019 −9.261 ± 0.019 2.27 ± 0.12 1.00<br />
NGC 4374 319 186.26547 12.88570 0.09 −8.880 ± 0.031 −10.047 ± 0.044 2.28 ± 0.25 1.00<br />
NGC 4374 321 186.27324 12.91255 1.88 −6.355 ± 0.075 −7.718 ± 0.164 6.47 ± 1.11 0.56<br />
NGC 4374 322 186.26321 12.87731 0.70 −9.744 ± 0.011 −10.753 ± 0.018 1.99 ± 0.11 1.00<br />
NGC 4374 323 186.26084 12.86862 1.34 −7.676 ± 0.023 −8.890 ± 0.023 1.83 ± 0.19 1.00<br />
NGC 4374 325 186.26706 12.88962 0.21 −7.056 ± 0.263 −7.940 ± 0.087 3.58 ± 0.52 0.98<br />
NGC 4374 326 186.26504 12.88237 0.33 −9.264 ± 0.023 −10.506 ± 0.016 1.60 ± 0.19 0.96<br />
NGC 4374 327 186.27294 12.90982 1.69 −6.887 ± 0.032 −7.811 ± 0.062 2.37 ± 0.39 0.99<br />
NGC 4374 328 186.26087 12.86769 1.40 −6.182 ± 0.063 −7.480 ± 0.067 3.34 ± 0.44 0.96<br />
NGC 4374 329 186.26869 12.89479 0.59 −6.230 ± 0.064 −7.932 ± 0.148 4.40 ± 1.00 0.94<br />
NGC 4374 331 186.26837 12.89327 0.48 −8.081 ± 0.029 −8.981 ± 0.029 3.36 ± 0.24 1.00<br />
NGC 4374 333 186.26705 12.88841 0.14 −7.657 ± 0.086 −8.453 ± 0.054 2.17 ± 0.35 1.00<br />
NGC 4374 334 186.26459 12.87973 0.52 −8.530 ± 0.015 −9.421 ± 0.027 2.83 ± 0.30 1.00<br />
NGC 4374 335 186.26600 12.88453 0.18 −7.899 ± 0.030 −8.713 ± 0.186 2.25 ± 0.43 1.00<br />
NGC 4374 336 186.26670 12.88606 0.10 −7.892 ± 0.520 −9.544 ± 0.037 2.15 ± 0.37 1.00<br />
NGC 4374 338 186.26678 12.88594 0.11 −6.349 ± 0.677 −7.986 ± 0.477 1.84 ± 0.65 0.98<br />
NGC 4374 339 186.26366 12.87490 0.87 −8.173 ± 0.023 −9.126 ± 0.030 2.23 ± 0.23 1.00<br />
NGC 4374 341 186.26773 12.88906 0.21 −7.140 ± 0.439 −8.320 ± 0.064 1.43 ± 0.41 0.94<br />
NGC 4374 342 186.26099 12.86547 1.55 −6.123 ± 0.074 −6.917 ± 0.086 2.94 ± 0.50 0.95<br />
NGC 4374 343 186.27360 12.90907 1.65 −7.678 ± 0.045 −8.485 ± 0.060 4.67 ± 0.26 1.00<br />
NGC 4374 344 186.26596 12.88242 0.32 −8.439 ± 0.033 −9.385 ± 0.039 3.76 ± 0.20 1.00<br />
NGC 4374 345 186.26801 12.88936 0.23 −8.156 ± 0.041 −9.085 ± 0.059 3.13 ± 0.26 1.00<br />
NGC 4374 346 186.26037 12.86244 1.77 −6.512 ± 0.094 −7.923 ± 0.054 2.52 ± 0.44 0.99<br />
NGC 4374 348 186.27109 12.89897 0.93 −7.475 ± 0.392 −8.979 ± 1.127 2.31 ± 0.59 1.00<br />
NGC 4374 349 186.26643 12.88251 0.32 −9.820 ± 0.012 −11.012 ± 0.018 2.41 ± 0.08 1.00<br />
NGC 4374 351 186.27217 12.90221 1.17 −7.341 ± 0.033 −8.572 ± 0.042 2.52 ± 0.28 1.00<br />
NGC 4374 352 186.26757 12.88609 0.15 −8.479 ± 0.041 −9.826 ± 0.085 3.79 ± 0.39 1.00<br />
NGC 4374 353 186.27321 12.90509 1.38 −9.646 ± 0.014 −10.724 ± 0.018 4.88 ± 0.12 1.00<br />
NGC 4374 355 186.26683 12.88230 0.34 −7.372 ± 0.046 −8.689 ± 0.248 2.52 ± 0.30 1.00<br />
NGC 4374 358 186.26801 12.88527 0.21 −7.264 ± 0.255 −8.618 ± 0.049 2.07 ± 0.37 1.00<br />
NGC 4374 359 186.26866 12.88696 0.21 −7.839 ± 0.044 −8.928 ± 0.051 2.57 ± 0.26 1.00<br />
NGC 4374 360 186.26889 12.88775 0.23 −6.798 ± 0.078 −7.812 ± 0.169 1.78 ± 0.39 0.97<br />
NGC 4374 361 186.27118 12.89564 0.72 −6.522 ± 0.085 −7.423 ± 0.423 3.83 ± 0.71 0.91<br />
NGC 4374 362 186.27237 12.89945 1.00 −6.477 ± 0.191 −7.441 ± 0.119 4.94 ± 1.29 0.75<br />
NGC 4374 363 186.26954 12.88967 0.33 −5.909 ± 1.145 −7.672 ± 0.285 1.84 ± 0.66 0.97<br />
NGC 4374 367 186.27000 12.89035 0.38 −7.882 ± 0.035 −9.394 ± 0.038 3.52 ± 0.20 1.00<br />
NGC 4374 369 186.27444 12.90543 1.44 −6.501 ± 0.114 −7.500 ± 0.182 5.32 ± 0.97 0.69<br />
NGC 4374 370 186.27337 12.90148 1.15 −6.700 ± 0.043 −8.284 ± 0.035 2.15 ± 0.26 0.99<br />
NGC 4374 371 186.27391 12.90339 1.29 −6.847 ± 0.020 −8.019 ± 0.038 2.08 ± 0.26 0.99<br />
NGC 4374 372 186.27030 12.89040 0.40 −7.271 ± 0.352 −8.585 ± 0.309 1.99 ± 0.35 1.00<br />
Continued on Next Page. . .<br />
314
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4374 374 186.27107 12.89237 0.53 −6.604 ± 0.090 −7.948 ± 0.288 1.85 ± 0.44 0.98<br />
NGC 4374 375 186.27190 12.89497 0.71 −7.094 ± 0.052 −8.082 ± 0.130 4.27 ± 0.57 0.96<br />
NGC 4374 376 186.27016 12.88885 0.34 −7.649 ± 0.087 −8.991 ± 2.064 1.63 ± 0.39 0.97<br />
NGC 4374 378 186.26563 12.87265 1.01 −7.153 ± 0.276 −8.512 ± 0.057 2.59 ± 0.42 1.00<br />
NGC 4374 379 186.26973 12.88601 0.29 −7.479 ± 0.098 −8.879 ± 0.200 5.80 ± 1.35 0.95<br />
NGC 4374 380 186.26748 12.87826 0.63 −6.171 ± 0.108 −7.421 ± 0.694 3.33 ± 41.63 0.96<br />
NGC 4374 383 186.26604 12.87264 1.02 −7.678 ± 0.035 −9.189 ± 0.024 2.08 ± 0.18 1.00<br />
NGC 4374 385 186.27236 12.89448 0.70 −7.281 ± 0.048 −8.398 ± 0.029 2.63 ± 0.28 1.00<br />
NGC 4374 386 186.26894 12.88232 0.40 −7.652 ± 0.261 −8.541 ± 0.044 1.61 ± 0.36 0.97<br />
NGC 4374 387 186.27107 12.88938 0.41 −6.643 ± 0.058 −8.009 ± 0.408 2.11 ± 0.42 0.99<br />
NGC 4374 389 186.26747 12.87654 0.75 −8.721 ± 0.035 −9.860 ± 0.021 1.93 ± 0.19 1.00<br />
NGC 4374 390 186.27307 12.89569 0.80 −7.401 ± 0.055 −8.490 ± 0.072 4.92 ± 0.42 0.98<br />
NGC 4374 391 186.26927 12.88218 0.42 −9.420 ± 0.027 −10.926 ± 0.017 1.56 ± 0.15 0.92<br />
NGC 4374 392 186.27269 12.89251 0.62 −9.502 ± 0.026 −10.432 ± 0.023 4.35 ± 0.17 1.00<br />
NGC 4374 393 186.27358 12.89571 0.82 −8.412 ± 0.025 −9.610 ± 0.033 3.27 ± 0.17 1.00<br />
NGC 4374 394 186.26987 12.88272 0.42 −7.308 ± 0.054 −8.678 ± 0.068 2.32 ± 0.45 1.00<br />
NGC 4374 396 186.27646 12.90517 1.49 −6.211 ± 0.095 −7.451 ± 0.131 4.69 ± 0.66 0.80<br />
NGC 4374 397 186.26488 12.86377 1.64 −10.186 ± 0.016 −11.199 ± 0.030 3.47 ± 0.16 1.00<br />
NGC 4374 398 186.26708 12.87108 1.13 −6.652 ± 0.061 −8.053 ± 0.049 2.56 ± 0.36 1.00<br />
NGC 4374 399 186.26738 12.87197 1.07 −5.853 ± 0.070 −7.261 ± 0.889 1.98 ± 0.62 0.96<br />
NGC 4374 400 186.27671 12.90415 1.43 −6.563 ± 0.037 −7.644 ± 0.055 2.08 ± 0.24 0.98<br />
NGC 4374 401 186.26833 12.87480 0.88 −9.357 ± 0.016 −10.233 ± 0.014 2.77 ± 0.13 1.00<br />
NGC 4374 402 186.27787 12.90778 1.69 −9.398 ± 0.021 −10.300 ± 0.028 4.38 ± 0.17 1.00<br />
NGC 4374 405 186.27356 12.89080 0.61 −8.694 ± 0.023 −9.691 ± 0.020 2.87 ± 0.18 1.00<br />
NGC 4374 406 186.27408 12.89200 0.68 −8.484 ± 0.017 −9.897 ± 0.016 2.83 ± 0.16 1.00<br />
NGC 4374 407 186.27144 12.88251 0.51 −8.274 ± 0.021 −9.674 ± 0.032 2.24 ± 0.21 1.00<br />
NGC 4374 408 186.27446 12.89286 0.74 −8.088 ± 0.026 −9.183 ± 0.042 3.62 ± 0.27 1.00<br />
NGC 4374 409 186.26669 12.86540 1.53 −7.307 ± 0.020 −8.216 ± 0.041 1.76 ± 0.20 0.98<br />
NGC 4374 411 186.27571 12.89632 0.96 −7.355 ± 0.070 −8.227 ± 0.053 4.65 ± 0.34 0.96<br />
NGC 4374 413 186.27321 12.88737 0.52 −8.351 ± 0.026 −9.183 ± 0.270 2.55 ± 0.26 1.00<br />
NGC 4374 414 186.26756 12.86721 1.41 −7.378 ± 0.040 −8.254 ± 0.054 2.83 ± 0.40 1.00<br />
NGC 4374 415 186.27928 12.90797 1.76 −5.573 ± 0.427 −6.656 ± 0.647 1.21 ± 0.59 0.78<br />
NGC 4374 416 186.27060 12.87724 0.77 −9.671 ± 0.014 −10.992 ± 0.027 2.65 ± 0.29 1.00<br />
NGC 4374 419 186.27160 12.88028 0.63 −7.478 ± 0.067 −8.590 ± 0.080 1.84 ± 0.31 1.00<br />
NGC 4374 420 186.26842 12.86911 1.28 −7.765 ± 0.026 −8.970 ± 0.039 2.13 ± 0.24 1.00<br />
NGC 4374 421 186.28065 12.91168 2.03 −6.575 ± 0.044 −7.922 ± 0.097 6.02 ± 0.59 0.76<br />
NGC 4374 422 186.27447 12.88988 0.64 −7.857 ± 0.019 −9.154 ± 0.025 1.66 ± 0.20 0.97<br />
NGC 4374 423 186.27187 12.88074 0.62 −8.984 ± 0.023 −10.058 ± 0.030 2.28 ± 0.17 1.00<br />
NGC 4374 424 186.27153 12.87934 0.68 −6.472 ± 0.176 −7.814 ± 0.090 2.59 ± 0.59 0.99<br />
NGC 4374 425 186.26927 12.87126 1.14 −8.505 ± 0.027 −9.515 ± 0.022 3.10 ± 0.15 1.00<br />
NGC 4374 428 186.27683 12.89690 1.04 −6.854 ± 0.041 −8.159 ± 0.035 2.59 ± 0.29 1.00<br />
NGC 4374 430 186.27350 12.88490 0.56 −6.738 ± 0.084 −7.945 ± 0.141 2.60 ± 0.67 0.99<br />
NGC 4374 431 186.26717 12.86245 1.74 −7.851 ± 0.020 −8.681 ± 0.032 2.15 ± 0.20 1.00<br />
NGC 4374 432 186.27980 12.90623 1.67 −7.186 ± 0.037 −8.420 ± 0.060 4.07 ± 0.25 1.00<br />
NGC 4374 433 186.27492 12.88908 0.66 −6.829 ± 0.048 −8.160 ± 0.156 4.52 ± 1.05 0.96<br />
NGC 4374 436 186.26804 12.86471 1.58 −8.221 ± 0.038 −9.069 ± 0.030 3.89 ± 0.20 1.00<br />
NGC 4374 438 186.27500 12.88874 0.66 −7.849 ± 0.021 −8.848 ± 0.056 3.53 ± 0.23 1.00<br />
NGC 4374 440 186.27086 12.87402 0.99 −8.678 ± 0.015 −9.640 ± 0.017 2.75 ± 0.13 1.00<br />
NGC 4374 441 186.27588 12.89114 0.77 −9.868 ± 0.014 −11.025 ± 0.011 3.33 ± 0.10 1.00<br />
NGC 4374 442 186.27792 12.89801 1.15 −6.894 ± 0.040 −7.738 ± 0.508 2.57 ± 0.47 0.99<br />
NGC 4374 443 186.27375 12.88349 0.61 −6.660 ± 0.044 −8.108 ± 0.072 2.62 ± 0.34 1.00<br />
NGC 4374 444 186.27893 12.90125 1.36 −6.950 ± 0.050 −7.868 ± 0.066 2.95 ± 0.36 0.99<br />
NGC 4374 446 186.26952 12.86793 1.37 −8.319 ± 0.027 −9.292 ± 0.024 2.73 ± 0.25 1.00<br />
NGC 4374 447 186.27144 12.87459 0.96 −7.294 ± 0.033 −8.734 ± 0.048 3.35 ± 0.32 1.00<br />
NGC 4374 448 186.26708 12.85866 2.00 −6.427 ± 0.136 −8.249 ± 0.112 7.06 ± 0.84 0.65<br />
NGC 4374 449 186.27563 12.88759 0.69 −7.616 ± 0.055 −8.763 ± 0.150 6.36 ± 1.13 0.86<br />
NGC 4374 451 186.27364 12.88042 0.72 −8.704 ± 0.020 −10.190 ± 0.016 2.06 ± 0.16 1.00<br />
NGC 4374 452 186.27647 12.88980 0.77 −8.226 ± 0.185 −9.199 ± 0.029 2.25 ± 0.31 1.00<br />
NGC 4374 453 186.27841 12.89647 1.11 −8.127 ± 0.019 −9.297 ± 0.021 2.44 ± 0.21 1.00<br />
NGC 4374 454 186.26966 12.86613 1.50 −5.621 ± 0.643 −7.119 ± 0.341 3.42 ± 0.86 0.92<br />
NGC 4374 455 186.28041 12.90297 1.52 −8.231 ± 0.023 −9.720 ± 0.020 2.22 ± 0.21 1.00<br />
NGC 4374 457 186.27639 12.88854 0.75 −10.582 ± 0.031 −11.602 ± 0.025 7.53 ± 0.17 1.00<br />
Continued on Next Page. . .<br />
315
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4374 458 186.27441 12.88174 0.71 −7.338 ± 0.036 −8.343 ± 0.053 2.77 ± 0.34 1.00<br />
NGC 4374 459 186.27247 12.87425 1.02 −8.372 ± 0.026 −9.606 ± 0.022 2.50 ± 0.22 1.00<br />
NGC 4374 460 186.28004 12.90038 1.37 −9.406 ± 0.014 −10.332 ± 0.021 2.88 ± 0.14 1.00<br />
NGC 4374 461 186.27273 12.87510 0.97 −7.541 ± 0.030 −8.902 ± 0.033 2.52 ± 0.19 1.00<br />
NGC 4374 462 186.27099 12.86899 1.33 −7.826 ± 0.027 −8.732 ± 0.036 2.47 ± 0.28 1.00<br />
NGC 4374 463 186.27404 12.87907 0.81 −8.496 ± 0.118 −9.669 ± 0.086 2.72 ± 0.80 1.00<br />
NGC 4374 464 186.27384 12.87836 0.83 −7.336 ± 0.045 −8.521 ± 0.074 3.09 ± 0.48 1.00<br />
NGC 4374 465 186.28104 12.90300 1.55 −7.364 ± 0.037 −8.692 ± 0.023 2.09 ± 0.21 1.00<br />
NGC 4374 466 186.27326 12.87590 0.95 −7.734 ± 0.042 −8.551 ± 0.045 3.40 ± 0.25 1.00<br />
NGC 4374 469 186.27427 12.87845 0.85 −9.650 ± 0.013 −10.565 ± 0.021 2.71 ± 0.12 1.00<br />
NGC 4374 470 186.28277 12.90865 1.93 −9.250 ± 0.029 −10.521 ± 0.018 3.62 ± 0.16 1.00<br />
NGC 4374 471 186.27506 12.88083 0.78 −6.743 ± 0.075 −7.730 ± 0.129 1.58 ± 0.34 0.95<br />
NGC 4374 472 186.27285 12.87300 1.11 −5.740 ± 0.091 −7.396 ± 0.052 2.59 ± 0.43 0.98<br />
NGC 4374 473 186.27527 12.88110 0.79 −7.492 ± 0.032 −8.584 ± 0.042 2.65 ± 0.25 1.00<br />
NGC 4374 475 186.27895 12.89387 1.04 −6.028 ± 0.054 −7.719 ± 0.218 5.62 ± 1.35 0.73<br />
NGC 4374 476 186.27815 12.89094 0.91 −5.445 ± 0.227 −6.419 ± 0.552 2.79 ± 1.25 0.93<br />
NGC 4374 480 186.27466 12.87819 0.88 −8.162 ± 0.025 −9.481 ± 0.028 2.17 ± 0.14 1.00<br />
NGC 4374 482 186.27605 12.88274 0.78 −7.449 ± 0.043 −9.003 ± 0.051 4.72 ± 0.26 1.00<br />
NGC 4374 483 186.27599 12.88213 0.79 −7.787 ± 0.032 −8.626 ± 0.031 1.84 ± 0.22 1.00<br />
NGC 4374 484 186.27820 12.88994 0.89 −7.939 ± 0.025 −9.300 ± 0.027 2.08 ± 0.17 1.00<br />
NGC 4374 485 186.26973 12.86011 1.92 −7.143 ± 0.141 −8.118 ± 0.549 2.33 ± 0.36 1.00<br />
NGC 4374 486 186.27486 12.87792 0.90 −7.163 ± 0.080 −8.800 ± 0.027 1.65 ± 0.21 0.97<br />
NGC 4374 487 186.27730 12.88637 0.81 −7.821 ± 0.034 −8.868 ± 0.043 3.06 ± 0.33 1.00<br />
NGC 4374 488 186.28024 12.89635 1.21 −7.398 ± 0.032 −8.216 ± 0.051 2.22 ± 0.40 1.00<br />
NGC 4374 489 186.27837 12.88963 0.90 −7.131 ± 0.040 −8.087 ± 0.040 3.36 ± 0.19 0.99<br />
NGC 4374 490 186.27580 12.88078 0.83 −5.658 ± 0.913 −6.797 ± 0.197 1.29 ± 0.49 0.81<br />
NGC 4374 492 186.28212 12.90252 1.58 −6.960 ± 0.039 −8.216 ± 0.056 2.30 ± 0.28 1.00<br />
NGC 4374 494 186.28327 12.90619 1.82 −8.206 ± 0.019 −9.111 ± 0.030 2.38 ± 0.16 1.00<br />
NGC 4374 496 186.28084 12.89703 1.27 −6.874 ± 0.060 −7.846 ± 0.048 3.08 ± 0.32 0.99<br />
NGC 4374 498 186.28053 12.89589 1.20 −7.730 ± 0.021 −8.739 ± 0.035 2.34 ± 0.26 1.00<br />
NGC 4374 501 186.27060 12.86092 1.87 −7.627 ± 0.032 −9.081 ± 0.027 2.13 ± 0.32 1.00<br />
NGC 4374 503 186.28064 12.89516 1.18 −6.021 ± 0.089 −7.513 ± 0.215 5.82 ± 1.58 0.59<br />
NGC 4374 504 186.27622 12.87870 0.94 −8.059 ± 0.031 −9.331 ± 0.017 1.68 ± 0.18 0.97<br />
NGC 4374 505 186.27527 12.87489 1.08 −6.372 ± 0.220 −7.424 ± 0.314 2.40 ± 4.85 0.99<br />
NGC 4374 507 186.27749 12.88146 0.91 −7.237 ± 0.065 −8.049 ± 0.370 4.41 ± 0.50 0.95<br />
NGC 4374 508 186.27486 12.87221 1.22 −7.626 ± 0.027 −8.655 ± 0.047 2.27 ± 0.30 1.00<br />
NGC 4374 509 186.28251 12.89867 1.43 −6.969 ± 0.042 −8.245 ± 0.032 2.87 ± 0.35 0.99<br />
NGC 4374 512 186.28414 12.90249 1.68 −5.483 ± 0.079 −6.240 ± 0.107 3.01 ± 0.51 0.93<br />
NGC 4374 513 186.28052 12.88958 1.04 −7.904 ± 0.014 −8.792 ± 0.019 2.26 ± 0.20 1.00<br />
NGC 4374 514 186.28279 12.89726 1.39 −8.781 ± 0.024 −9.749 ± 0.023 2.87 ± 0.22 1.00<br />
NGC 4374 517 186.28499 12.90467 1.83 −8.061 ± 0.023 −9.093 ± 0.027 2.77 ± 0.19 1.00<br />
NGC 4374 518 186.27345 12.86422 1.70 −6.158 ± 0.110 −7.042 ± 0.227 4.85 ± 1.60 0.60<br />
NGC 4374 519 186.27842 12.88144 0.97 −8.235 ± 0.026 −9.546 ± 0.026 1.84 ± 0.15 1.00<br />
NGC 4374 520 186.27563 12.87152 1.29 −5.200 ± 0.333 −6.619 ± 0.274 3.78 ± 2.14 0.83<br />
NGC 4374 521 186.27933 12.88427 0.96 −6.676 ± 0.090 −7.802 ± 0.214 2.94 ± 0.69 0.99<br />
NGC 4374 523 186.27766 12.87734 1.08 −6.977 ± 0.085 −7.701 ± 0.087 4.47 ± 0.58 0.90<br />
NGC 4374 524 186.27978 12.88439 0.99 −8.421 ± 0.018 −9.327 ± 0.033 2.40 ± 0.21 1.00<br />
NGC 4374 525 186.27919 12.88229 0.99 −6.182 ± 0.502 −7.404 ± 0.129 4.85 ± 2.04 0.75<br />
NGC 4374 526 186.27846 12.87909 1.05 −7.628 ± 0.317 −9.059 ± 0.252 2.02 ± 0.41 1.00<br />
NGC 4374 527 186.28295 12.89381 1.29 −9.732 ± 0.011 −10.690 ± 0.019 3.55 ± 0.09 1.00<br />
NGC 4374 528 186.28445 12.89856 1.53 −7.638 ± 0.016 −8.542 ± 0.035 2.69 ± 0.17 1.00<br />
NGC 4374 529 186.27559 12.86675 1.59 −8.000 ± 0.027 −9.356 ± 0.024 2.06 ± 0.28 1.00<br />
NGC 4374 530 186.28164 12.88619 1.11 −6.852 ± 0.236 −8.158 ± 0.340 1.07 ± 0.27 0.82<br />
NGC 4374 533 186.27596 12.86567 1.67 −7.099 ± 0.030 −8.159 ± 0.047 2.04 ± 0.33 0.99<br />
NGC 4374 535 186.27875 12.87521 1.23 −8.500 ± 0.030 −9.815 ± 0.024 4.11 ± 0.14 1.00<br />
NGC 4374 537 186.27510 12.86212 1.88 −8.240 ± 0.038 −9.092 ± 0.034 2.65 ± 0.20 1.00<br />
NGC 4374 538 186.27829 12.87300 1.32 −6.376 ± 0.055 −7.853 ± 0.053 2.81 ± 0.33 0.99<br />
NGC 4374 541 186.28028 12.87952 1.14 −6.142 ± 0.067 −6.991 ± 0.117 3.82 ± 0.51 0.85<br />
NGC 4374 543 186.28350 12.89011 1.25 −6.805 ± 0.038 −8.250 ± 0.037 3.08 ± 0.23 0.99<br />
NGC 4374 544 186.28465 12.89513 1.43 −5.497 ± 0.854 −6.871 ± 0.526 2.40 ± 24.74 0.96<br />
NGC 4374 545 186.28055 12.87928 1.16 −7.095 ± 0.034 −8.336 ± 0.069 2.80 ± 0.43 1.00<br />
NGC 4374 550 186.28639 12.89783 1.62 −8.120 ± 0.024 −8.949 ± 0.032 2.56 ± 0.17 1.00<br />
Continued on Next Page. . .<br />
316
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4374 551 186.28586 12.89552 1.52 −7.379 ± 0.026 −8.502 ± 0.038 2.06 ± 0.18 1.00<br />
NGC 4374 552 186.28554 12.89426 1.47 −8.766 ± 0.023 −10.103 ± 0.017 2.37 ± 0.18 1.00<br />
NGC 4374 554 186.27744 12.86585 1.70 −8.028 ± 0.078 −8.717 ± 0.106 6.98 ± 0.74 0.79<br />
NGC 4374 556 186.28918 12.90667 2.14 −5.282 ± 0.180 −6.299 ± 0.180 3.81 ± 1.03 0.82<br />
NGC 4374 557 186.27550 12.85849 2.13 −7.627 ± 0.038 −8.868 ± 0.047 4.03 ± 0.23 1.00<br />
NGC 4374 558 186.28411 12.88736 1.27 −6.405 ± 0.050 −7.848 ± 0.053 1.87 ± 0.37 0.98<br />
NGC 4374 559 186.27609 12.85900 2.11 −9.254 ± 0.017 −10.156 ± 0.012 2.54 ± 0.11 1.00<br />
NGC 4374 560 186.28143 12.87780 1.27 −5.776 ± 0.174 −6.960 ± 0.141 3.65 ± 0.92 0.87<br />
NGC 4374 561 186.27585 12.85802 2.17 −7.570 ± 0.059 −8.254 ± 0.073 6.52 ± 0.35 0.77<br />
NGC 4374 562 186.28847 12.90166 1.88 −6.096 ± 0.355 −7.316 ± 0.057 1.80 ± 0.35 0.95<br />
NGC 4374 563 186.28864 12.90228 1.92 −7.291 ± 0.034 −8.650 ± 0.038 1.47 ± 0.13 0.95<br />
NGC 4374 564 186.27989 12.87116 1.49 −7.706 ± 0.051 −8.567 ± 0.055 4.83 ± 0.24 0.98<br />
NGC 4374 565 186.28499 12.88862 1.34 −6.752 ± 0.137 −8.175 ± 0.052 2.08 ± 0.28 0.99<br />
NGC 4374 566 186.28500 12.88830 1.34 −7.050 ± 0.048 −8.537 ± 0.034 1.10 ± 0.23 0.83<br />
NGC 4374 567 186.28691 12.89470 1.56 −6.069 ± 0.072 −7.330 ± 0.115 3.41 ± 0.57 0.94<br />
NGC 4374 568 186.28671 12.89384 1.53 −8.445 ± 0.017 −9.910 ± 0.022 1.83 ± 0.12 1.00<br />
NGC 4374 569 186.28024 12.87053 1.54 −9.084 ± 0.029 −10.212 ± 0.018 2.42 ± 0.29 1.00<br />
NGC 4374 570 186.28830 12.89875 1.77 −5.488 ± 0.443 −6.399 ± 0.129 2.36 ± 0.69 0.94<br />
NGC 4374 571 186.28444 12.88517 1.30 −6.047 ± 1.654 −7.097 ± 0.876 1.25 ± 0.43 0.82<br />
NGC 4374 573 186.28845 12.89889 1.78 −5.768 ± 0.098 −6.954 ± 0.127 4.37 ± 0.69 0.72<br />
NGC 4374 574 186.28859 12.89925 1.80 −7.601 ± 0.018 −8.436 ± 0.037 3.97 ± 0.13 1.00<br />
NGC 4374 576 186.27683 12.85801 2.19 −8.576 ± 0.028 −9.538 ± 0.016 3.22 ± 0.19 1.00<br />
NGC 4374 577 186.27911 12.86598 1.75 −5.408 ± 0.495 −6.234 ± 0.715 1.10 ± 0.98 0.73<br />
NGC 4374 578 186.28489 12.88542 1.33 −6.885 ± 0.024 −8.328 ± 0.042 1.62 ± 0.25 0.97<br />
NGC 4374 581 186.28903 12.89952 1.84 −5.582 ± 0.738 −7.031 ± 0.152 2.07 ± 0.47 0.96<br />
NGC 4374 587 186.28006 12.86628 1.77 −9.714 ± 0.014 −10.933 ± 0.012 5.02 ± 0.07 1.00<br />
NGC 4374 588 186.27899 12.86238 1.97 −6.682 ± 0.059 −8.217 ± 0.056 2.06 ± 0.37 0.99<br />
NGC 4374 589 186.28566 12.88533 1.39 −7.138 ± 0.032 −8.317 ± 0.115 4.75 ± 0.59 0.97<br />
NGC 4374 590 186.28714 12.89030 1.50 −7.750 ± 0.027 −8.689 ± 0.025 2.09 ± 0.18 1.00<br />
NGC 4374 591 186.28435 12.88060 1.37 −7.864 ± 0.024 −8.872 ± 0.028 2.85 ± 0.25 1.00<br />
NGC 4374 593 186.28019 12.86578 1.80 −5.528 ± 0.398 −6.435 ± 0.447 3.59 ± 2.48 0.86<br />
NGC 4374 596 186.29190 12.90599 2.25 −8.925 ± 0.016 −9.810 ± 0.020 2.86 ± 0.17 1.00<br />
NGC 4374 597 186.28226 12.87237 1.54 −7.671 ± 0.243 −9.088 ± 0.026 1.55 ± 0.23 0.96<br />
NGC 4374 601 186.28089 12.86698 1.76 −6.553 ± 0.079 −7.543 ± 0.163 5.47 ± 1.17 0.68<br />
NGC 4374 603 186.28389 12.87688 1.45 −6.975 ± 0.048 −8.480 ± 0.062 2.64 ± 0.33 1.00<br />
NGC 4374 606 186.28482 12.87767 1.48 −9.132 ± 0.014 −10.170 ± 0.011 4.57 ± 0.08 1.00<br />
NGC 4374 608 186.28387 12.87335 1.59 −7.351 ± 0.021 −8.778 ± 0.024 2.36 ± 0.22 1.00<br />
NGC 4374 609 186.28493 12.87669 1.52 −8.209 ± 0.017 −9.788 ± 0.023 3.96 ± 0.16 1.00<br />
NGC 4374 611 186.27992 12.85781 2.29 −9.220 ± 0.011 −10.007 ± 0.015 2.49 ± 0.08 1.00<br />
NGC 4374 612 186.28746 12.88405 1.52 −6.854 ± 0.193 −8.189 ± 0.030 1.83 ± 0.33 0.98<br />
NGC 4374 613 186.28883 12.88866 1.60 −8.001 ± 0.031 −9.261 ± 0.021 1.88 ± 0.16 1.00<br />
NGC 4374 614 186.28475 12.87456 1.58 −6.934 ± 0.094 −8.169 ± 0.059 4.94 ± 0.47 0.94<br />
NGC 4374 615 186.28715 12.88261 1.52 −8.375 ± 0.023 −9.334 ± 0.024 2.19 ± 0.18 1.00<br />
NGC 4374 620 186.28328 12.86693 1.87 −6.788 ± 0.036 −7.981 ± 0.033 2.82 ± 0.26 0.99<br />
NGC 4374 625 186.29519 12.90642 2.46 −6.510 ± 0.641 −7.986 ± 0.477 2.03 ± 0.68 0.99<br />
NGC 4374 626 186.29106 12.89164 1.78 −6.871 ± 0.783 −7.661 ± 0.053 2.15 ± 0.38 0.99<br />
NGC 4374 627 186.29195 12.89465 1.89 −6.479 ± 0.069 −7.378 ± 0.048 2.48 ± 0.35 0.99<br />
NGC 4374 629 186.28912 12.88417 1.63 −5.664 ± 0.204 −6.609 ± 0.102 2.73 ± 0.66 0.94<br />
NGC 4374 630 186.29532 12.90542 2.43 −6.462 ± 0.079 −7.758 ± 0.078 6.42 ± 0.63 0.59<br />
NGC 4374 631 186.29249 12.89621 1.96 −8.958 ± 0.034 −9.879 ± 0.014 2.55 ± 0.17 1.00<br />
NGC 4374 635 186.29101 12.88989 1.76 −8.592 ± 0.030 −9.721 ± 0.022 2.52 ± 0.22 1.00<br />
NGC 4374 637 186.28904 12.88161 1.66 −7.954 ± 0.030 −8.806 ± 0.029 2.82 ± 0.22 1.00<br />
NGC 4374 639 186.28838 12.87899 1.67 −6.695 ± 0.112 −7.710 ± 0.073 4.59 ± 0.71 0.89<br />
NGC 4374 640 186.29486 12.90172 2.27 −6.679 ± 0.050 −7.769 ± 0.071 3.14 ± 0.41 0.98<br />
NGC 4374 641 186.28412 12.86392 2.07 −9.056 ± 0.018 −10.075 ± 0.072 2.91 ± 0.28 1.00<br />
NGC 4374 644 186.29035 12.88400 1.72 −10.323 ± 0.012 −11.445 ± 0.011 2.57 ± 0.09 1.00<br />
NGC 4374 646 186.28221 12.85428 2.58 −8.468 ± 0.023 −9.946 ± 0.037 3.70 ± 0.18 1.00<br />
NGC 4374 647 186.29357 12.89386 1.99 −7.900 ± 0.020 −8.781 ± 0.031 2.78 ± 0.15 1.00<br />
NGC 4374 651 186.28949 12.87798 1.76 −7.853 ± 0.032 −8.704 ± 0.031 3.05 ± 0.25 1.00<br />
NGC 4374 652 186.28946 12.87606 1.82 −8.439 ± 0.020 −9.297 ± 0.013 2.20 ± 0.20 1.00<br />
NGC 4374 656 186.29879 12.90756 2.71 −6.755 ± 0.055 −8.068 ± 0.038 2.51 ± 0.28 1.00<br />
NGC 4374 657 186.28919 12.87276 1.91 −8.208 ± 0.019 −9.189 ± 0.029 2.97 ± 0.19 1.00<br />
Continued on Next Page. . .<br />
317
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4374 662 186.28939 12.87370 1.89 −9.371 ± 0.007 −10.254 ± 0.014 3.39 ± 0.07 1.00<br />
NGC 4374 663 186.28460 12.85511 2.61 −6.859 ± 0.075 −7.429 ± 0.082 4.34 ± 0.31 0.85<br />
NGC 4374 665 186.29480 12.88955 2.02 −8.662 ± 0.026 −9.548 ± 0.024 2.49 ± 0.18 1.00<br />
NGC 4374 670 186.29577 12.89099 2.10 −9.002 ± 0.021 −10.321 ± 0.018 2.97 ± 0.17 1.00<br />
NGC 4374 671 186.29256 12.87984 1.92 −8.661 ± 0.012 −9.665 ± 0.015 2.26 ± 0.10 1.00<br />
NGC 4374 672 186.29523 12.88893 2.04 −8.331 ± 0.025 −9.522 ± 0.027 2.82 ± 0.18 1.00<br />
NGC 4374 673 186.29026 12.87155 2.02 −6.676 ± 0.073 −7.602 ± 0.104 3.91 ± 0.55 0.93<br />
NGC 4374 674 186.28713 12.86035 2.40 −7.010 ± 0.026 −8.211 ± 0.063 3.00 ± 0.35 0.99<br />
NGC 4374 678 186.29575 12.88841 2.08 −8.943 ± 0.065 −10.234 ± 0.065 7.73 ± 0.50 1.00<br />
NGC 4374 680 186.29251 12.87716 1.98 −7.561 ± 0.052 −8.739 ± 0.041 3.26 ± 0.23 1.00<br />
NGC 4374 681 186.29811 12.89664 2.34 −6.195 ± 0.135 −6.833 ± 0.121 3.12 ± 0.75 0.93<br />
NGC 4374 682 186.29005 12.86762 2.17 −7.633 ± 0.028 −8.546 ± 0.036 2.53 ± 0.26 1.00<br />
NGC 4374 683 186.29872 12.89750 2.40 −5.437 ± 0.151 −6.859 ± 0.061 3.47 ± 0.67 0.89<br />
NGC 4374 684 186.28937 12.86457 2.28 −9.001 ± 0.027 −10.069 ± 0.020 2.83 ± 0.26 1.00<br />
NGC 4374 686 186.29351 12.87898 2.00 −6.597 ± 0.049 −7.697 ± 0.096 4.70 ± 0.46 0.87<br />
NGC 4374 687 186.28926 12.86415 2.29 −7.086 ± 0.032 −8.354 ± 0.033 2.96 ± 0.30 0.99<br />
NGC 4374 690 186.29236 12.87413 2.06 −8.182 ± 0.019 −9.587 ± 0.019 2.83 ± 0.12 1.00<br />
NGC 4374 693 186.29000 12.86541 2.27 −6.846 ± 0.048 −8.116 ± 0.081 4.17 ± 0.41 0.97<br />
NGC 4374 699 186.29937 12.89505 2.39 −6.271 ± 0.063 −7.429 ± 0.080 2.34 ± 0.38 0.99<br />
NGC 4374 700 186.29694 12.88636 2.16 −7.889 ± 0.019 −9.273 ± 0.020 2.09 ± 0.12 1.00<br />
NGC 4374 702 186.28924 12.85819 2.61 −9.139 ± 0.015 −10.006 ± 0.012 3.11 ± 0.08 1.00<br />
NGC 4374 703 186.29259 12.86937 2.24 −6.941 ± 0.076 −7.624 ± 0.064 2.61 ± 0.36 0.99<br />
NGC 4374 705 186.30008 12.89480 2.44 −8.089 ± 0.020 −9.018 ± 0.023 2.27 ± 0.17 1.00<br />
NGC 4374 708 186.30207 12.90080 2.69 −7.711 ± 0.032 −8.675 ± 0.023 2.93 ± 0.22 1.00<br />
NGC 4374 709 186.29091 12.86165 2.50 −7.417 ± 0.028 −8.629 ± 0.027 2.34 ± 0.22 1.00<br />
NGC 4374 711 186.29467 12.87406 2.20 −7.180 ± 0.138 −8.786 ± 0.092 5.92 ± 0.88 0.93<br />
NGC 4374 712 186.30395 12.90605 2.96 −9.432 ± 0.022 −10.421 ± 0.022 3.20 ± 0.14 1.00<br />
NGC 4374 716 186.29439 12.87168 2.26 −8.684 ± 0.023 −9.685 ± 0.023 3.30 ± 0.18 1.00<br />
NGC 4374 717 186.29331 12.86750 2.35 −6.232 ± 0.107 −7.333 ± 0.131 3.10 ± 0.88 0.96<br />
NGC 4374 722 186.29513 12.87303 2.26 −6.506 ± 1.015 −8.248 ± 0.267 1.27 ± 0.35 0.90<br />
NGC 4374 723 186.29337 12.86623 2.41 −6.850 ± 0.062 −7.880 ± 0.086 4.22 ± 0.43 0.94<br />
NGC 4374 729 186.29716 12.87792 2.27 −7.528 ± 0.030 −8.986 ± 0.016 2.60 ± 0.17 1.00<br />
NGC 4374 731 186.29600 12.87267 2.33 −7.380 ± 0.037 −8.226 ± 0.030 2.83 ± 0.24 0.99<br />
NGC 4374 732 186.29661 12.87438 2.31 −6.949 ± 0.056 −8.293 ± 0.044 3.21 ± 0.27 0.99<br />
NGC 4374 735 186.29624 12.87224 2.35 −9.106 ± 0.030 −10.383 ± 0.018 2.95 ± 0.17 1.00<br />
NGC 4374 738 186.29950 12.88328 2.35 −7.533 ± 0.029 −8.293 ± 0.030 2.62 ± 0.20 1.00<br />
NGC 4374 742 186.30232 12.89234 2.56 −7.610 ± 0.036 −8.657 ± 0.031 3.70 ± 0.25 1.00<br />
NGC 4374 743 186.30498 12.90161 2.90 −6.065 ± 0.086 −6.727 ± 0.076 3.33 ± 0.48 0.90<br />
NGC 4374 744 186.29115 12.85388 2.93 −5.224 ± 0.276 −6.701 ± 0.236 3.68 ± 1.40 0.85<br />
NGC 4374 746 186.29975 12.88283 2.37 −6.050 ± 0.105 −7.723 ± 0.293 6.01 ± 3.63 0.67<br />
NGC 4374 749 186.30388 12.89600 2.71 −7.613 ± 0.025 −8.596 ± 0.035 4.14 ± 0.22 1.00<br />
NGC 4374 756 186.30460 12.89570 2.76 −7.347 ± 0.034 −8.381 ± 0.045 4.54 ± 0.31 1.00<br />
NGC 4374 757 186.30033 12.88078 2.43 −7.679 ± 0.037 −9.052 ± 0.021 2.66 ± 0.22 1.00<br />
NGC 4374 760 186.30600 12.89909 2.91 −6.982 ± 0.047 −7.834 ± 0.076 3.59 ± 0.46 0.97<br />
NGC 4374 763 186.30638 12.89871 2.93 −7.399 ± 0.056 −8.530 ± 0.038 4.30 ± 0.28 1.00<br />
NGC 4382 1 186.32349 18.17222 2.09 −7.019 ± 0.057 −7.769 ± 0.074 2.66 ± 0.36 0.95<br />
NGC 4382 5 186.32552 18.18377 1.62 −5.328 ± 0.131 −6.231 ± 0.703 2.91 ± 0.71 0.80<br />
NGC 4382 6 186.32346 18.16755 2.29 −5.236 ± 0.182 −6.829 ± 0.151 4.03 ± 1.17 0.59<br />
NGC 4382 7 186.32457 18.17407 1.96 −7.725 ± 0.033 −8.607 ± 0.040 3.94 ± 0.22 1.00<br />
NGC 4382 10 186.32678 18.18902 1.48 −5.807 ± 0.083 −7.212 ± 0.074 3.24 ± 0.32 0.84<br />
NGC 4382 11 186.32636 18.18449 1.56 −6.827 ± 0.049 −7.951 ± 0.036 2.71 ± 0.26 0.97<br />
NGC 4382 12 186.32697 18.18784 1.47 −6.762 ± 0.036 −7.891 ± 0.058 3.04 ± 0.24 0.95<br />
NGC 4382 17 186.32550 18.17319 1.95 −5.931 ± 0.106 −7.207 ± 0.172 4.47 ± 0.93 0.54<br />
NGC 4382 19 186.32725 18.18584 1.48 −8.245 ± 0.080 −9.149 ± 0.074 3.22 ± 0.39 1.00<br />
NGC 4382 20 186.32805 18.19185 1.39 −6.362 ± 0.073 −7.569 ± 0.096 4.09 ± 0.51 0.80<br />
NGC 4382 24 186.32683 18.18070 1.62 −7.384 ± 0.063 −8.042 ± 0.100 5.79 ± 0.59 0.62<br />
NGC 4382 28 186.32555 18.16897 2.13 −7.923 ± 0.030 −8.791 ± 0.027 3.26 ± 0.14 1.00<br />
NGC 4382 30 186.32598 18.16923 2.09 −6.444 ± 0.081 −7.379 ± 0.042 3.13 ± 0.38 0.89<br />
NGC 4382 31 186.33126 18.20877 1.67 −8.954 ± 0.014 −10.187 ± 0.015 3.13 ± 0.12 1.00<br />
NGC 4382 33 186.32938 18.19357 1.32 −7.800 ± 0.029 −8.978 ± 0.026 1.83 ± 0.20 1.00<br />
NGC 4382 34 186.32642 18.17048 2.02 −7.790 ± 0.031 −8.722 ± 0.023 2.74 ± 0.21 1.00<br />
Continued on Next Page. . .<br />
318
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4382 35 186.32901 18.19044 1.33 −7.412 ± 0.046 −9.057 ± 0.064 4.72 ± 0.47 1.00<br />
NGC 4382 44 186.32986 18.19240 1.28 −6.999 ± 0.053 −8.136 ± 0.067 2.76 ± 0.40 0.97<br />
NGC 4382 49 186.33157 18.20371 1.43 −6.355 ± 0.071 −7.774 ± 0.058 5.44 ± 0.31 0.55<br />
NGC 4382 56 186.32767 18.17000 1.98 −8.090 ± 0.070 −9.104 ± 0.101 2.65 ± 0.45 1.00<br />
NGC 4382 57 186.33335 18.21380 1.83 −9.044 ± 0.013 −10.462 ± 0.016 3.21 ± 0.08 1.00<br />
NGC 4382 63 186.32950 18.18295 1.41 −8.291 ± 0.027 −9.122 ± 0.033 2.87 ± 0.17 1.00<br />
NGC 4382 66 186.33179 18.19938 1.28 −8.290 ± 0.036 −9.221 ± 0.082 8.28 ± 0.58 0.52<br />
NGC 4382 70 186.33111 18.19347 1.21 −5.007 ± 0.487 −6.215 ± 0.443 3.55 ± 1.49 0.76<br />
NGC 4382 72 186.33208 18.19994 1.28 −9.379 ± 0.027 −10.225 ± 0.017 3.73 ± 0.12 1.00<br />
NGC 4382 77 186.33045 18.18627 1.28 −8.687 ± 0.017 −9.749 ± 0.020 2.60 ± 0.16 1.00<br />
NGC 4382 78 186.33208 18.19753 1.21 −5.599 ± 0.199 −6.388 ± 0.128 3.74 ± 1.43 0.69<br />
NGC 4382 84 186.33416 18.21128 1.67 −5.718 ± 0.074 −6.451 ± 0.606 2.24 ± 0.47 0.76<br />
NGC 4382 85 186.33357 18.20601 1.43 −8.129 ± 0.051 −8.992 ± 0.052 5.08 ± 0.29 0.98<br />
NGC 4382 87 186.33350 18.20501 1.39 −5.570 ± 0.121 −7.016 ± 0.120 3.77 ± 0.63 0.69<br />
NGC 4382 90 186.33058 18.18057 1.41 −7.518 ± 0.037 −9.028 ± 0.027 3.06 ± 0.18 1.00<br />
NGC 4382 93 186.33152 18.18719 1.20 −6.422 ± 0.093 −7.529 ± 0.095 3.96 ± 0.49 0.80<br />
NGC 4382 97 186.33325 18.19896 1.18 −5.714 ± 0.470 −7.091 ± 0.132 3.58 ± 1.47 0.75<br />
NGC 4382 98 186.33502 18.21245 1.70 −7.648 ± 0.024 −8.909 ± 0.034 2.83 ± 0.16 1.00<br />
NGC 4382 100 186.33017 18.17461 1.66 −5.832 ± 0.122 −7.492 ± 0.144 4.66 ± 0.83 0.62<br />
NGC 4382 101 186.33228 18.19088 1.13 −7.137 ± 0.043 −8.372 ± 0.045 3.20 ± 0.23 1.00<br />
NGC 4382 102 186.33331 18.19858 1.17 −7.108 ± 0.060 −8.062 ± 0.029 2.50 ± 0.26 0.97<br />
NGC 4382 103 186.33185 18.18706 1.18 −6.830 ± 0.050 −8.203 ± 0.030 1.41 ± 0.31 0.51<br />
NGC 4382 104 186.33327 18.19817 1.16 −5.105 ± 0.106 −6.581 ± 0.123 3.05 ± 0.59 0.79<br />
NGC 4382 105 186.33220 18.18834 1.14 −6.940 ± 0.038 −8.204 ± 0.048 1.44 ± 0.22 0.54<br />
NGC 4382 107 186.33331 18.19592 1.11 −9.772 ± 0.020 −10.918 ± 0.011 2.38 ± 0.10 1.00<br />
NGC 4382 108 186.32957 18.16710 2.04 −6.882 ± 0.062 −8.048 ± 0.059 3.60 ± 0.32 0.94<br />
NGC 4382 111 186.33594 18.21313 1.71 −5.136 ± 0.163 −6.361 ± 0.275 3.58 ± 1.94 0.73<br />
NGC 4382 113 186.33579 18.21132 1.61 −8.165 ± 0.034 −9.075 ± 0.042 4.70 ± 0.19 1.00<br />
NGC 4382 115 186.33532 18.20830 1.47 −6.988 ± 0.036 −7.949 ± 0.035 2.13 ± 0.29 0.95<br />
NGC 4382 116 186.33376 18.19469 1.06 −5.218 ± 0.727 −6.361 ± 0.162 2.43 ± 0.64 0.78<br />
NGC 4382 120 186.33087 18.16964 1.86 −7.445 ± 0.056 −8.648 ± 0.043 4.01 ± 0.23 1.00<br />
NGC 4382 125 186.33153 18.17278 1.68 −7.682 ± 0.027 −8.854 ± 0.348 1.79 ± 0.23 1.00<br />
NGC 4382 126 186.33613 18.20866 1.46 −6.000 ± 0.089 −7.453 ± 0.131 3.95 ± 0.49 0.78<br />
NGC 4382 129 186.33458 18.19567 1.03 −5.339 ± 0.116 −6.672 ± 0.221 3.49 ± 1.18 0.72<br />
NGC 4382 131 186.33261 18.17919 1.36 −7.442 ± 0.041 −8.721 ± 0.031 2.50 ± 0.17 1.00<br />
NGC 4382 132 186.33410 18.19102 1.01 −6.062 ± 0.109 −7.109 ± 0.085 3.08 ± 0.51 0.85<br />
NGC 4382 133 186.33272 18.17975 1.33 −5.062 ± 0.578 −6.870 ± 0.279 4.03 ± 5.29 0.60<br />
NGC 4382 135 186.33106 18.16635 2.03 −8.286 ± 0.046 −9.331 ± 0.036 6.78 ± 0.18 0.86<br />
NGC 4382 136 186.33505 18.19753 1.04 −5.523 ± 0.080 −7.191 ± 0.106 4.33 ± 0.43 0.58<br />
NGC 4382 138 186.33545 18.19987 1.09 −8.242 ± 0.055 −9.129 ± 0.021 2.34 ± 0.21 1.00<br />
NGC 4382 140 186.33385 18.18673 1.07 −7.698 ± 0.020 −8.641 ± 0.031 2.48 ± 0.20 1.00<br />
NGC 4382 142 186.33653 18.20678 1.34 −8.226 ± 0.021 −9.417 ± 0.016 2.86 ± 0.15 1.00<br />
NGC 4382 148 186.33412 18.18479 1.09 −8.411 ± 0.027 −9.325 ± 0.029 4.13 ± 0.15 1.00<br />
NGC 4382 151 186.33305 18.17528 1.50 −7.913 ± 0.022 −8.965 ± 0.023 2.71 ± 0.20 1.00<br />
NGC 4382 152 186.33439 18.18539 1.06 −9.213 ± 0.013 −10.142 ± 0.023 3.80 ± 0.13 1.00<br />
NGC 4382 154 186.33714 18.20703 1.33 −5.471 ± 0.474 −6.724 ± 0.116 3.73 ± 1.02 0.67<br />
NGC 4382 155 186.33352 18.17839 1.34 −5.646 ± 0.233 −6.793 ± 0.146 3.47 ± 0.81 0.73<br />
NGC 4382 156 186.33209 18.16708 1.95 −5.021 ± 0.372 −6.229 ± 0.563 2.18 ± 0.69 0.74<br />
NGC 4382 157 186.33371 18.17944 1.29 −5.421 ± 0.149 −6.293 ± 0.187 4.02 ± 0.77 0.60<br />
NGC 4382 161 186.33449 18.18314 1.12 −5.976 ± 0.091 −7.186 ± 0.140 3.54 ± 0.73 0.78<br />
NGC 4382 162 186.33580 18.19281 0.91 −5.260 ± 0.453 −6.715 ± 0.220 3.71 ± 0.90 0.68<br />
NGC 4382 167 186.33755 18.20369 1.15 −9.008 ± 0.021 −10.115 ± 0.027 2.98 ± 0.13 1.00<br />
NGC 4382 169 186.33326 18.17046 1.73 −5.432 ± 0.511 −7.298 ± 0.222 3.99 ± 1.74 0.72<br />
NGC 4382 171 186.33769 18.20466 1.19 −6.752 ± 0.047 −7.775 ± 0.047 2.03 ± 0.27 0.91<br />
NGC 4382 176 186.33795 18.20490 1.19 −7.869 ± 0.026 −8.599 ± 0.039 3.78 ± 0.14 1.00<br />
NGC 4382 177 186.33492 18.18145 1.15 −6.345 ± 0.051 −7.336 ± 0.049 2.29 ± 0.31 0.92<br />
NGC 4382 178 186.33832 18.20801 1.34 −5.828 ± 0.063 −6.717 ± 0.155 3.32 ± 0.64 0.76<br />
NGC 4382 179 186.33746 18.20118 1.04 −5.674 ± 0.144 −7.167 ± 0.307 3.36 ± 1.01 0.81<br />
NGC 4382 181 186.33324 18.16784 1.87 −7.217 ± 0.040 −8.527 ± 0.034 3.68 ± 0.19 1.00<br />
NGC 4382 190 186.33605 18.18676 0.93 −9.352 ± 0.016 −10.535 ± 0.013 2.61 ± 0.11 1.00<br />
NGC 4382 192 186.33732 18.19634 0.88 −5.767 ± 0.085 −7.095 ± 0.115 3.62 ± 0.63 0.74<br />
NGC 4382 193 186.33536 18.18053 1.16 −9.088 ± 0.018 −10.218 ± 0.018 2.82 ± 0.15 1.00<br />
Continued on Next Page. . .<br />
319
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4382 194 186.33574 18.18305 1.05 −6.509 ± 0.069 −7.359 ± 0.070 3.13 ± 0.41 0.88<br />
NGC 4382 195 186.33844 18.20412 1.13 −6.702 ± 0.040 −8.182 ± 0.047 3.13 ± 0.37 0.96<br />
NGC 4382 197 186.33495 18.17605 1.38 −8.781 ± 0.019 −9.571 ± 0.026 3.51 ± 0.14 1.00<br />
NGC 4382 198 186.33638 18.18839 0.89 −9.201 ± 0.048 −10.151 ± 0.016 2.58 ± 0.24 1.00<br />
NGC 4382 204 186.33863 18.20355 1.10 −8.456 ± 0.021 −9.476 ± 0.020 2.35 ± 0.14 1.00<br />
NGC 4382 205 186.33804 18.19915 0.93 −6.481 ± 0.044 −7.833 ± 0.100 4.47 ± 0.53 0.82<br />
NGC 4382 208 186.33968 18.20998 1.41 −8.632 ± 0.020 −9.552 ± 0.020 2.74 ± 0.13 1.00<br />
NGC 4382 210 186.33727 18.19017 0.82 −6.112 ± 0.118 −7.296 ± 0.099 3.64 ± 0.59 0.79<br />
NGC 4382 212 186.33435 18.16705 1.87 −6.775 ± 0.084 −8.245 ± 0.045 3.36 ± 0.32 0.96<br />
NGC 4382 214 186.33797 18.19488 0.81 −6.224 ± 0.339 −7.354 ± 1.064 2.33 ± 0.62 0.92<br />
NGC 4382 215 186.34079 18.21640 1.77 −7.725 ± 0.037 −9.039 ± 0.024 3.03 ± 0.14 1.00<br />
NGC 4382 217 186.33681 18.18454 0.95 −9.432 ± 0.023 −10.389 ± 0.013 2.76 ± 0.14 1.00<br />
NGC 4382 218 186.33795 18.19355 0.79 −6.495 ± 0.064 −7.982 ± 0.047 2.01 ± 0.27 0.93<br />
NGC 4382 219 186.33950 18.20564 1.17 −6.111 ± 0.087 −7.644 ± 0.127 4.64 ± 0.70 0.70<br />
NGC 4382 220 186.34075 18.21491 1.68 −4.958 ± 1.124 −6.634 ± 0.120 3.36 ± 0.87 0.75<br />
NGC 4382 223 186.34101 18.21535 1.70 −6.168 ± 0.052 −7.552 ± 0.067 3.09 ± 0.34 0.92<br />
NGC 4382 225 186.33894 18.19838 0.86 −8.680 ± 0.022 −9.751 ± 0.014 2.62 ± 0.13 1.00<br />
NGC 4382 230 186.33641 18.17429 1.41 −7.461 ± 0.037 −8.558 ± 0.055 2.87 ± 0.26 1.00<br />
NGC 4382 231 186.33586 18.17007 1.65 −6.373 ± 0.065 −7.258 ± 0.242 2.60 ± 0.37 0.92<br />
NGC 4382 233 186.33606 18.17072 1.61 −8.404 ± 0.038 −9.536 ± 0.026 6.64 ± 0.17 0.96<br />
NGC 4382 234 186.33867 18.19130 0.72 −5.691 ± 0.115 −6.845 ± 0.179 3.04 ± 0.50 0.81<br />
NGC 4382 235 186.34193 18.21632 1.74 −6.050 ± 0.117 −7.043 ± 0.085 3.56 ± 0.54 0.74<br />
NGC 4382 236 186.34082 18.20703 1.21 −8.268 ± 0.032 −9.382 ± 0.027 2.66 ± 0.19 1.00<br />
NGC 4382 238 186.33896 18.19042 0.71 −7.211 ± 0.028 −8.222 ± 0.066 2.96 ± 0.37 0.97<br />
NGC 4382 239 186.33664 18.17148 1.55 −8.719 ± 0.021 −9.643 ± 0.023 4.16 ± 0.15 1.00<br />
NGC 4382 240 186.34003 18.19820 0.79 −6.755 ± 0.067 −7.740 ± 0.068 3.20 ± 0.41 0.94<br />
NGC 4382 241 186.33717 18.17575 1.30 −5.421 ± 0.198 −6.857 ± 0.192 4.03 ± 1.45 0.59<br />
NGC 4382 242 186.33973 18.19557 0.72 −8.011 ± 0.023 −9.051 ± 0.028 2.28 ± 0.17 1.00<br />
NGC 4382 243 186.33877 18.18771 0.75 −6.620 ± 0.130 −7.829 ± 0.092 5.83 ± 0.84 0.51<br />
NGC 4382 246 186.33943 18.19198 0.68 −7.504 ± 0.037 −8.128 ± 0.056 2.84 ± 0.27 0.97<br />
NGC 4382 248 186.33731 18.17523 1.32 −5.714 ± 0.105 −7.134 ± 0.097 3.81 ± 0.59 0.71<br />
NGC 4382 250 186.34223 18.21264 1.51 −9.494 ± 0.020 −10.582 ± 0.016 2.76 ± 0.16 1.00<br />
NGC 4382 253 186.33779 18.17628 1.25 −8.723 ± 0.023 −9.656 ± 0.022 2.97 ± 0.19 1.00<br />
NGC 4382 255 186.34139 18.20425 1.03 −6.539 ± 0.139 −7.979 ± 0.030 1.51 ± 0.28 0.62<br />
NGC 4382 256 186.33936 18.18825 0.71 −6.848 ± 0.087 −7.520 ± 0.146 4.57 ± 0.73 0.66<br />
NGC 4382 257 186.34290 18.21560 1.68 −5.708 ± 0.096 −6.794 ± 0.127 3.56 ± 0.55 0.71<br />
NGC 4382 258 186.33893 18.18421 0.84 −7.257 ± 0.079 −8.653 ± 0.086 5.80 ± 0.64 0.78<br />
NGC 4382 259 186.34178 18.20537 1.08 −8.734 ± 0.020 −9.653 ± 0.027 3.82 ± 0.14 1.00<br />
NGC 4382 262 186.33794 18.17419 1.36 −8.803 ± 0.020 −9.743 ± 0.030 5.22 ± 0.11 1.00<br />
NGC 4382 264 186.34076 18.19727 0.72 −10.151 ± 0.029 −11.315 ± 0.420 1.77 ± 0.24 1.00<br />
NGC 4382 265 186.34179 18.20349 0.97 −5.032 ± 0.250 −6.218 ± 0.236 3.50 ± 0.74 0.77<br />
NGC 4382 267 186.34187 18.20368 0.98 −8.061 ± 0.031 −9.000 ± 0.026 2.53 ± 0.23 1.00<br />
NGC 4382 268 186.33968 18.18598 0.74 −6.945 ± 0.059 −7.695 ± 1.737 1.83 ± 0.45 0.81<br />
NGC 4382 269 186.33871 18.17788 1.13 −6.572 ± 0.060 −7.803 ± 0.079 4.11 ± 0.39 0.87<br />
NGC 4382 270 186.34335 18.21371 1.55 −5.182 ± 0.072 −6.163 ± 0.572 2.06 ± 0.54 0.71<br />
NGC 4382 271 186.34115 18.19555 0.64 −7.444 ± 0.031 −8.778 ± 0.030 2.37 ± 0.21 1.00<br />
NGC 4382 282 186.33878 18.17316 1.38 −5.738 ± 0.310 −6.731 ± 0.111 2.90 ± 0.58 0.81<br />
NGC 4382 283 186.34254 18.20246 0.89 −4.930 ± 0.745 −6.439 ± 0.549 3.27 ± 16.09 0.77<br />
NGC 4382 284 186.34199 18.19744 0.67 −8.025 ± 0.031 −9.079 ± 0.027 1.79 ± 0.17 1.00<br />
NGC 4382 285 186.34284 18.20418 0.98 −7.040 ± 0.048 −8.191 ± 0.044 2.50 ± 0.26 0.98<br />
NGC 4382 286 186.33867 18.17113 1.50 −8.140 ± 0.029 −9.409 ± 0.029 4.32 ± 0.20 1.00<br />
NGC 4382 287 186.34259 18.20149 0.84 −6.952 ± 0.052 −8.169 ± 0.078 4.06 ± 0.48 0.94<br />
NGC 4382 288 186.34033 18.18341 0.80 −6.208 ± 0.167 −7.509 ± 0.074 2.17 ± 0.43 0.91<br />
NGC 4382 290 186.34317 18.20552 1.05 −7.877 ± 0.033 −9.185 ± 0.041 2.98 ± 0.19 1.00<br />
NGC 4382 292 186.34240 18.19881 0.71 −8.093 ± 0.026 −9.058 ± 0.021 3.27 ± 0.12 1.00<br />
NGC 4382 296 186.33884 18.16860 1.65 −5.459 ± 0.107 −6.459 ± 0.444 3.14 ± 0.41 0.78<br />
NGC 4382 297 186.33925 18.17101 1.49 −7.938 ± 0.033 −9.217 ± 0.037 3.99 ± 0.25 1.00<br />
NGC 4382 300 186.34358 18.20457 0.98 −5.843 ± 0.106 −6.847 ± 0.107 3.46 ± 0.47 0.74<br />
NGC 4382 303 186.34197 18.19072 0.52 −6.782 ± 0.099 −7.866 ± 0.164 5.16 ± 0.89 0.65<br />
NGC 4382 304 186.33916 18.16859 1.64 −5.804 ± 0.069 −7.501 ± 0.059 2.66 ± 0.34 0.93<br />
NGC 4382 305 186.33930 18.16906 1.61 −6.720 ± 0.062 −7.823 ± 0.054 2.85 ± 0.30 0.95<br />
NGC 4382 306 186.34218 18.19124 0.51 −7.625 ± 0.039 −8.859 ± 0.028 3.13 ± 0.17 1.00<br />
Continued on Next Page. . .<br />
320
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4382 308 186.34001 18.17332 1.34 −8.283 ± 0.032 −9.509 ± 0.040 3.90 ± 0.28 1.00<br />
NGC 4382 309 186.34032 18.17601 1.17 −5.940 ± 0.108 −7.419 ± 0.115 4.47 ± 0.68 0.64<br />
NGC 4382 315 186.34014 18.17479 1.25 −5.495 ± 0.232 −6.375 ± 0.257 2.47 ± 1.27 0.79<br />
NGC 4382 317 186.34062 18.17566 1.18 −6.161 ± 0.097 −7.767 ± 0.120 4.77 ± 0.64 0.72<br />
NGC 4382 318 186.34316 18.19572 0.54 −5.238 ± 0.582 −6.876 ± 0.156 3.74 ± 0.89 0.68<br />
NGC 4382 321 186.34166 18.18281 0.77 −6.891 ± 0.145 −8.148 ± 0.324 6.20 ± 1.31 0.55<br />
NGC 4382 326 186.34085 18.17463 1.24 −5.435 ± 0.143 −6.830 ± 0.156 2.84 ± 0.67 0.84<br />
NGC 4382 327 186.34450 18.20282 0.85 −7.717 ± 0.030 −8.737 ± 0.029 2.45 ± 0.18 1.00<br />
NGC 4382 329 186.34062 18.17123 1.44 −6.578 ± 0.072 −7.600 ± 0.053 3.74 ± 0.32 0.86<br />
NGC 4382 331 186.34609 18.21294 1.46 −5.479 ± 0.169 −7.177 ± 0.205 3.68 ± 1.19 0.74<br />
NGC 4382 332 186.33975 18.16308 1.96 −5.254 ± 0.280 −6.569 ± 0.594 2.21 ± 0.75 0.78<br />
NGC 4382 336 186.34443 18.19793 0.58 −7.873 ± 0.035 −8.933 ± 0.031 2.62 ± 0.22 1.00<br />
NGC 4382 337 186.34399 18.19404 0.44 −6.815 ± 0.035 −8.185 ± 0.080 3.30 ± 0.38 0.96<br />
NGC 4382 338 186.34494 18.20119 0.74 −8.335 ± 0.031 −9.358 ± 0.033 3.25 ± 0.20 1.00<br />
NGC 4382 339 186.34270 18.18364 0.68 −8.187 ± 0.026 −9.449 ± 0.028 1.82 ± 0.18 1.00<br />
NGC 4382 340 186.34176 18.17613 1.12 −5.766 ± 0.072 −7.048 ± 0.755 3.78 ± 0.77 0.69<br />
NGC 4382 342 186.34259 18.18192 0.77 −6.866 ± 0.043 −7.926 ± 0.049 1.86 ± 0.29 0.87<br />
NGC 4382 344 186.34270 18.18249 0.74 −7.115 ± 0.037 −8.050 ± 0.056 2.45 ± 0.25 0.97<br />
NGC 4382 346 186.34245 18.18020 0.87 −6.694 ± 0.065 −8.149 ± 0.064 2.49 ± 0.31 0.98<br />
NGC 4382 347 186.34448 18.19565 0.47 −6.586 ± 0.044 −7.437 ± 0.086 2.08 ± 0.53 0.88<br />
NGC 4382 348 186.34131 18.17062 1.46 −8.291 ± 0.018 −9.397 ± 0.026 3.01 ± 0.15 1.00<br />
NGC 4382 349 186.34285 18.18476 0.62 −6.213 ± 0.079 −7.551 ± 0.099 3.78 ± 0.59 0.84<br />
NGC 4382 351 186.34052 18.16411 1.88 −6.638 ± 0.053 −8.114 ± 0.037 2.39 ± 0.34 0.97<br />
NGC 4382 353 186.34372 18.18743 0.47 −7.657 ± 0.047 −8.866 ± 0.035 2.22 ± 0.29 1.00<br />
NGC 4382 354 186.34333 18.18436 0.62 −7.137 ± 0.107 −8.407 ± 0.038 2.53 ± 0.29 1.00<br />
NGC 4382 355 186.34335 18.18394 0.64 −7.454 ± 0.070 −8.479 ± 0.069 3.60 ± 0.39 1.00<br />
NGC 4382 357 186.34517 18.19662 0.48 −8.672 ± 0.028 −9.570 ± 0.046 4.27 ± 0.19 1.00<br />
NGC 4382 359 186.34167 18.16911 1.55 −7.294 ± 0.044 −8.193 ± 0.051 2.83 ± 0.32 0.97<br />
NGC 4382 360 186.34270 18.17716 1.03 −7.255 ± 0.031 −8.126 ± 0.085 3.24 ± 0.39 0.96<br />
NGC 4382 361 186.34413 18.18780 0.44 −6.007 ± 0.287 −6.873 ± 1.496 1.87 ± 1.34 0.67<br />
NGC 4382 364 186.34351 18.18140 0.77 −7.300 ± 0.032 −8.845 ± 0.062 3.13 ± 0.33 1.00<br />
NGC 4382 367 186.34487 18.18874 0.37 −9.326 ± 0.026 −10.757 ± 0.015 2.16 ± 0.14 1.00<br />
NGC 4382 369 186.34713 18.20720 1.08 −6.180 ± 0.067 −7.516 ± 0.157 3.32 ± 0.78 0.89<br />
NGC 4382 373 186.34757 18.20809 1.13 −6.903 ± 0.060 −8.343 ± 0.053 3.41 ± 0.34 1.00<br />
NGC 4382 377 186.34832 18.21199 1.38 −5.306 ± 0.255 −7.015 ± 0.204 4.07 ± 1.57 0.61<br />
NGC 4382 380 186.34647 18.19704 0.46 −9.017 ± 0.026 −9.910 ± 0.029 2.88 ± 0.17 1.00<br />
NGC 4382 381 186.34369 18.17482 1.15 −8.756 ± 0.018 −9.982 ± 0.027 3.18 ± 0.16 1.00<br />
NGC 4382 382 186.34566 18.19047 0.29 −7.172 ± 0.073 −8.016 ± 0.063 4.01 ± 0.38 0.92<br />
NGC 4382 383 186.34603 18.19238 0.28 −7.126 ± 0.069 −8.595 ± 0.065 4.21 ± 0.28 1.00<br />
NGC 4382 384 186.34613 18.19246 0.27 −9.026 ± 0.029 −10.015 ± 0.030 3.68 ± 0.19 1.00<br />
NGC 4382 389 186.34740 18.20205 0.74 −5.872 ± 0.166 −6.993 ± 0.216 4.18 ± 1.20 0.57<br />
NGC 4382 392 186.34902 18.21407 1.52 −6.192 ± 0.128 −7.105 ± 0.123 4.17 ± 0.67 0.60<br />
NGC 4382 393 186.34535 18.18487 0.51 −9.150 ± 0.025 −10.558 ± 0.020 2.54 ± 0.21 1.00<br />
NGC 4382 394 186.34511 18.18321 0.61 −5.363 ± 0.218 −7.234 ± 0.245 3.55 ± 1.86 0.79<br />
NGC 4382 396 186.34659 18.19423 0.31 −7.366 ± 0.044 −8.608 ± 0.080 3.70 ± 0.29 1.00<br />
NGC 4382 401 186.34723 18.19770 0.47 −7.219 ± 0.065 −7.915 ± 0.082 6.06 ± 0.42 0.51<br />
NGC 4382 403 186.34482 18.17825 0.91 −8.783 ± 0.023 −10.072 ± 0.024 2.15 ± 0.12 1.00<br />
NGC 4382 404 186.34650 18.19135 0.23 −6.848 ± 0.060 −8.198 ± 0.098 2.42 ± 0.37 0.98<br />
NGC 4382 407 186.34493 18.17817 0.92 −6.374 ± 0.088 −7.614 ± 0.343 1.72 ± 0.47 0.71<br />
NGC 4382 408 186.34684 18.19246 0.23 −5.918 ± 0.215 −7.559 ± 0.122 2.24 ± 0.79 0.93<br />
NGC 4382 409 186.34954 18.21225 1.40 −6.838 ± 0.096 −7.848 ± 0.057 4.90 ± 0.45 0.71<br />
NGC 4382 410 186.34711 18.19290 0.23 −8.716 ± 0.030 −9.617 ± 0.038 4.05 ± 0.27 1.00<br />
NGC 4382 411 186.35002 18.21522 1.59 −5.484 ± 0.166 −6.735 ± 0.539 3.99 ± 1.05 0.60<br />
NGC 4382 414 186.34909 18.20737 1.08 −6.463 ± 0.099 −7.673 ± 0.295 3.02 ± 0.55 0.94<br />
NGC 4382 415 186.34375 18.16527 1.75 −8.646 ± 0.024 −9.665 ± 0.012 2.41 ± 0.12 1.00<br />
NGC 4382 416 186.34593 18.18241 0.63 −6.656 ± 0.121 −7.694 ± 0.165 3.96 ± 0.99 0.86<br />
NGC 4382 417 186.34752 18.19448 0.28 −5.556 ± 0.864 −7.144 ± 0.189 2.44 ± 0.85 0.91<br />
NGC 4382 418 186.34622 18.18406 0.53 −7.813 ± 0.023 −8.792 ± 0.040 2.03 ± 0.22 1.00<br />
NGC 4382 423 186.34786 18.19466 0.28 −7.297 ± 0.066 −8.627 ± 0.048 2.71 ± 0.27 1.00<br />
NGC 4382 424 186.34700 18.18775 0.30 −7.938 ± 0.040 −8.953 ± 0.079 3.69 ± 0.38 1.00<br />
NGC 4382 425 186.34682 18.18609 0.39 −6.320 ± 0.446 −7.635 ± 0.095 2.89 ± 0.51 0.93<br />
NGC 4382 426 186.34854 18.19907 0.54 −8.481 ± 0.055 −9.274 ± 0.032 6.07 ± 0.22 0.91<br />
Continued on Next Page. . .<br />
321
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4382 427 186.34732 18.18906 0.23 −6.980 ± 0.077 −8.387 ± 0.061 3.22 ± 0.41 1.00<br />
NGC 4382 430 186.34500 18.17019 1.42 −5.319 ± 0.319 −6.124 ± 0.172 1.87 ± 0.67 0.62<br />
NGC 4382 431 186.34565 18.17497 1.10 −5.385 ± 0.076 −7.016 ± 0.346 2.92 ± 2.75 0.86<br />
NGC 4382 432 186.34589 18.17632 1.01 −7.051 ± 0.112 −8.096 ± 0.081 5.05 ± 0.64 0.79<br />
NGC 4382 434 186.34718 18.18620 0.38 −7.495 ± 0.048 −8.570 ± 0.045 2.69 ± 0.29 1.00<br />
NGC 4382 435 186.34867 18.19748 0.43 −6.976 ± 0.055 −8.326 ± 0.049 2.76 ± 0.32 1.00<br />
NGC 4382 438 186.34691 18.18236 0.61 −6.684 ± 0.056 −7.909 ± 0.047 4.27 ± 0.23 0.88<br />
NGC 4382 442 186.34633 18.17712 0.95 −7.544 ± 0.026 −8.341 ± 0.072 2.50 ± 0.39 1.00<br />
NGC 4382 446 186.34877 18.19540 0.30 −8.208 ± 0.042 −9.397 ± 0.021 2.49 ± 0.23 1.00<br />
NGC 4382 447 186.35022 18.20645 1.01 −8.116 ± 0.037 −9.213 ± 0.038 4.12 ± 0.23 1.00<br />
NGC 4382 448 186.34676 18.17983 0.77 −7.346 ± 0.027 −8.651 ± 0.035 1.44 ± 0.27 0.55<br />
NGC 4382 449 186.34807 18.18988 0.16 −6.597 ± 0.239 −7.972 ± 0.874 1.76 ± 1.67 0.82<br />
NGC 4382 454 186.34613 18.17183 1.30 −8.817 ± 0.021 −9.816 ± 0.015 2.60 ± 0.13 1.00<br />
NGC 4382 456 186.35039 18.20499 0.92 −6.614 ± 0.052 −7.952 ± 0.065 2.68 ± 0.28 0.97<br />
NGC 4382 457 186.35132 18.21209 1.39 −7.952 ± 0.042 −9.353 ± 0.016 1.87 ± 0.22 1.00<br />
NGC 4382 458 186.34847 18.18917 0.17 −7.243 ± 0.112 −8.103 ± 0.126 5.11 ± 0.61 0.78<br />
NGC 4382 459 186.35047 18.20461 0.89 −7.304 ± 0.036 −8.830 ± 0.345 1.67 ± 0.29 0.78<br />
NGC 4382 462 186.34768 18.18226 0.60 −7.619 ± 0.045 −8.818 ± 0.082 4.34 ± 0.36 1.00<br />
NGC 4382 463 186.34804 18.18418 0.48 −6.807 ± 0.078 −7.751 ± 0.076 4.29 ± 0.37 0.83<br />
NGC 4382 464 186.34892 18.19110 0.08 −7.548 ± 0.232 −9.272 ± 0.134 2.24 ± 0.63 1.00<br />
NGC 4382 465 186.35115 18.20856 1.15 −5.115 ± 0.429 −6.243 ± 0.303 2.67 ± 1.80 0.79<br />
NGC 4382 466 186.34808 18.18363 0.51 −7.799 ± 0.030 −9.090 ± 0.020 1.51 ± 0.19 0.61<br />
NGC 4382 467 186.34799 18.18210 0.61 −8.396 ± 0.083 −9.467 ± 0.066 6.58 ± 0.47 0.95<br />
NGC 4382 468 186.35178 18.21134 1.34 −7.738 ± 0.061 −9.004 ± 0.091 5.39 ± 0.52 0.93<br />
NGC 4382 470 186.34601 18.16529 1.72 −7.593 ± 0.103 −8.213 ± 0.205 5.96 ± 2.09 0.64<br />
NGC 4382 471 186.34996 18.19568 0.30 −7.898 ± 0.052 −8.925 ± 0.032 2.22 ± 0.22 1.00<br />
NGC 4382 474 186.35006 18.19612 0.33 −7.547 ± 0.035 −8.911 ± 0.029 4.36 ± 0.13 1.00<br />
NGC 4382 475 186.35123 18.20455 0.89 −7.339 ± 0.041 −8.530 ± 0.055 3.38 ± 0.20 1.00<br />
NGC 4382 476 186.34606 18.16419 1.79 −7.124 ± 0.059 −8.117 ± 0.067 3.64 ± 0.39 0.94<br />
NGC 4382 477 186.34665 18.16761 1.56 −7.118 ± 0.051 −7.952 ± 0.044 3.04 ± 0.26 0.96<br />
NGC 4382 482 186.35211 18.20847 1.15 −5.148 ± 1.717 −7.036 ± 0.790 3.10 ± 1.51 0.83<br />
NGC 4382 484 186.35147 18.20266 0.77 −6.350 ± 0.075 −8.134 ± 0.151 4.69 ± 1.08 0.87<br />
NGC 4382 485 186.34912 18.18426 0.46 −9.289 ± 0.182 −10.502 ± 0.187 2.32 ± 0.40 1.00<br />
NGC 4382 491 186.35327 18.21473 1.57 −6.580 ± 0.100 −7.920 ± 0.089 5.60 ± 0.55 0.59<br />
NGC 4382 492 186.34880 18.18380 0.49 −7.937 ± 0.035 −9.320 ± 0.028 2.27 ± 0.25 1.00<br />
NGC 4382 497 186.34848 18.17585 1.01 −9.395 ± 0.018 −10.445 ± 0.023 2.73 ± 0.15 1.00<br />
NGC 4382 498 186.35133 18.19765 0.44 −8.072 ± 0.045 −9.231 ± 0.047 2.19 ± 0.26 1.00<br />
NGC 4382 501 186.35115 18.19533 0.28 −7.932 ± 0.043 −9.040 ± 0.063 3.86 ± 0.44 1.00<br />
NGC 4382 503 186.34960 18.18090 0.67 −6.630 ± 0.082 −7.554 ± 0.342 2.55 ± 0.41 0.94<br />
NGC 4382 504 186.35018 18.18512 0.39 −7.296 ± 0.071 −8.094 ± 0.104 3.53 ± 0.48 0.94<br />
NGC 4382 505 186.34783 18.16697 1.60 −5.570 ± 0.207 −7.058 ± 0.090 3.98 ± 1.02 0.65<br />
NGC 4382 506 186.34990 18.18225 0.58 −7.827 ± 0.040 −9.231 ± 0.060 4.59 ± 0.36 1.00<br />
NGC 4382 507 186.34969 18.18048 0.70 −6.192 ± 0.074 −7.422 ± 0.170 2.72 ± 0.75 0.92<br />
NGC 4382 508 186.35082 18.18814 0.20 −8.844 ± 0.021 −10.323 ± 0.015 2.00 ± 0.20 1.00<br />
NGC 4382 510 186.35115 18.18961 0.11 −8.862 ± 0.018 −9.983 ± 0.448 1.80 ± 0.26 1.00<br />
NGC 4382 511 186.35192 18.19581 0.33 −8.296 ± 0.045 −9.349 ± 0.062 4.35 ± 0.38 1.00<br />
NGC 4382 512 186.34797 18.16478 1.74 −6.954 ± 0.044 −8.198 ± 0.053 5.11 ± 0.20 0.82<br />
NGC 4382 513 186.35247 18.19928 0.56 −10.894 ± 0.026 −12.076 ± 0.008 1.86 ± 0.18 1.00<br />
NGC 4382 514 186.34772 18.16255 1.89 −5.438 ± 0.199 −6.368 ± 0.355 2.91 ± 0.95 0.79<br />
NGC 4382 516 186.35358 18.20611 1.01 −8.133 ± 0.030 −9.364 ± 0.032 3.11 ± 0.17 1.00<br />
NGC 4382 520 186.35199 18.19302 0.17 −8.230 ± 0.036 −9.890 ± 0.146 6.09 ± 1.10 1.00<br />
NGC 4382 522 186.35226 18.19386 0.22 −7.261 ± 0.062 −8.846 ± 0.108 3.58 ± 0.49 1.00<br />
NGC 4382 524 186.35059 18.18070 0.69 −7.405 ± 0.106 −8.675 ± 0.333 1.46 ± 0.25 0.57<br />
NGC 4382 527 186.35268 18.19587 0.35 −8.245 ± 0.030 −9.604 ± 0.031 2.01 ± 0.14 1.00<br />
NGC 4382 530 186.35338 18.19845 0.52 −8.287 ± 0.022 −9.269 ± 0.279 2.26 ± 0.43 1.00<br />
NGC 4382 532 186.35544 18.21437 1.57 −7.302 ± 0.039 −8.566 ± 0.041 2.59 ± 0.27 1.00<br />
NGC 4382 533 186.35210 18.18757 0.26 −7.671 ± 0.043 −8.934 ± 0.059 2.93 ± 0.30 1.00<br />
NGC 4382 535 186.35030 18.17256 1.22 −6.537 ± 0.075 −7.612 ± 0.078 3.71 ± 0.46 0.87<br />
NGC 4382 538 186.35222 18.18704 0.29 −6.902 ± 0.051 −7.882 ± 0.628 2.58 ± 0.47 0.96<br />
NGC 4382 540 186.34957 18.16352 1.82 −8.140 ± 0.030 −9.314 ± 0.019 3.12 ± 0.15 1.00<br />
NGC 4382 541 186.35339 18.19375 0.26 −8.672 ± 0.033 −9.886 ± 0.017 2.19 ± 0.20 1.00<br />
NGC 4382 542 186.35332 18.19282 0.22 −8.544 ± 0.031 −9.526 ± 0.033 2.97 ± 0.19 1.00<br />
Continued on Next Page. . .<br />
322
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4382 543 186.35374 18.19611 0.40 −8.336 ± 0.044 −9.353 ± 0.039 3.75 ± 0.25 1.00<br />
NGC 4382 544 186.35349 18.19360 0.26 −7.055 ± 0.124 −7.694 ± 0.092 4.29 ± 0.53 0.81<br />
NGC 4382 549 186.35330 18.19051 0.20 −8.829 ± 0.026 −9.720 ± 0.028 2.36 ± 0.13 1.00<br />
NGC 4382 551 186.35211 18.18075 0.69 −9.264 ± 0.022 −10.449 ± 0.016 2.03 ± 0.13 1.00<br />
NGC 4382 555 186.35052 18.17126 1.31 −5.752 ± 0.159 −7.296 ± 0.108 3.25 ± 0.82 0.86<br />
NGC 4382 558 186.35557 18.20399 0.91 −8.504 ± 0.074 −9.827 ± 0.081 8.57 ± 0.56 0.62<br />
NGC 4382 559 186.35558 18.20424 0.93 −7.625 ± 0.039 −9.008 ± 0.052 3.88 ± 0.20 1.00<br />
NGC 4382 560 186.35327 18.18622 0.37 −8.615 ± 0.025 −10.064 ± 0.022 1.97 ± 0.11 1.00<br />
NGC 4382 561 186.35193 18.17504 1.06 −6.240 ± 0.119 −7.004 ± 0.122 2.35 ± 0.64 0.89<br />
NGC 4382 562 186.35312 18.18414 0.49 −5.822 ± 0.080 −6.958 ± 0.259 2.57 ± 1.36 0.88<br />
NGC 4382 563 186.35617 18.20786 1.17 −8.029 ± 0.021 −9.173 ± 0.030 2.52 ± 0.18 1.00<br />
NGC 4382 564 186.35094 18.16659 1.62 −7.852 ± 0.022 −8.652 ± 0.029 2.94 ± 0.13 1.00<br />
NGC 4382 566 186.35670 18.21197 1.44 −7.708 ± 0.056 −8.983 ± 0.142 6.83 ± 1.00 0.66<br />
NGC 4382 567 186.35423 18.19149 0.25 −6.919 ± 0.073 −8.238 ± 1.164 2.02 ± 0.48 0.94<br />
NGC 4382 569 186.35284 18.17949 0.78 −7.454 ± 0.057 −8.941 ± 0.032 3.05 ± 0.26 1.00<br />
NGC 4382 570 186.35359 18.18490 0.46 −7.978 ± 0.031 −8.934 ± 0.020 2.40 ± 0.20 1.00<br />
NGC 4382 572 186.35083 18.16276 1.87 −8.171 ± 0.048 −9.315 ± 0.047 5.18 ± 0.29 0.98<br />
NGC 4382 574 186.35113 18.16361 1.81 −7.873 ± 0.032 −8.799 ± 0.024 3.55 ± 0.15 1.00<br />
NGC 4382 575 186.35781 18.21594 1.71 −5.334 ± 0.186 −6.334 ± 0.671 3.24 ± 13.72 0.79<br />
NGC 4382 579 186.35374 18.18366 0.54 −8.629 ± 0.034 −9.620 ± 0.028 2.36 ± 0.19 1.00<br />
NGC 4382 584 186.35629 18.20124 0.77 −5.788 ± 0.269 −6.862 ± 0.195 3.85 ± 1.53 0.65<br />
NGC 4382 585 186.35548 18.19396 0.38 −8.517 ± 0.026 −9.841 ± 0.014 2.37 ± 0.13 1.00<br />
NGC 4382 588 186.35659 18.20209 0.83 −7.797 ± 0.026 −8.836 ± 0.024 2.58 ± 0.22 1.00<br />
NGC 4382 590 186.35433 18.18422 0.52 −8.077 ± 0.026 −9.049 ± 0.029 2.68 ± 0.20 1.00<br />
NGC 4382 592 186.35506 18.18965 0.32 −7.462 ± 0.068 −8.253 ± 0.326 2.15 ± 0.51 0.96<br />
NGC 4382 594 186.35563 18.19304 0.36 −9.536 ± 0.020 −10.737 ± 0.017 2.62 ± 0.11 1.00<br />
NGC 4382 596 186.35380 18.17782 0.90 −7.064 ± 0.026 −8.168 ± 0.031 2.02 ± 0.26 0.94<br />
NGC 4382 597 186.35402 18.17941 0.81 −5.997 ± 0.096 −7.047 ± 0.157 2.34 ± 0.53 0.90<br />
NGC 4382 599 186.35701 18.20137 0.80 −8.357 ± 0.031 −9.527 ± 0.029 3.08 ± 0.19 1.00<br />
NGC 4382 601 186.35568 18.19126 0.34 −6.655 ± 0.080 −7.213 ± 0.088 3.48 ± 0.53 0.80<br />
NGC 4382 603 186.35625 18.19421 0.43 −6.888 ± 0.056 −7.640 ± 0.096 3.29 ± 0.38 0.92<br />
NGC 4382 604 186.35675 18.19768 0.60 −7.118 ± 0.038 −8.041 ± 0.041 2.41 ± 0.28 0.97<br />
NGC 4382 607 186.35646 18.19362 0.42 −6.427 ± 0.111 −7.259 ± 0.446 4.64 ± 1.86 0.51<br />
NGC 4382 609 186.35823 18.20569 1.08 −8.682 ± 0.022 −10.136 ± 0.016 2.67 ± 0.14 1.00<br />
NGC 4382 610 186.35836 18.20618 1.12 −4.929 ± 0.308 −6.411 ± 0.813 3.04 ± 1.67 0.79<br />
NGC 4382 611 186.35765 18.20030 0.76 −6.007 ± 0.196 −7.297 ± 0.292 2.34 ± 0.89 0.92<br />
NGC 4382 612 186.35344 18.16689 1.61 −5.627 ± 0.071 −6.754 ± 0.279 3.71 ± 0.66 0.67<br />
NGC 4382 619 186.35397 18.16819 1.53 −7.745 ± 0.047 −8.803 ± 0.036 3.02 ± 0.20 1.00<br />
NGC 4382 621 186.36025 18.21556 1.73 −5.060 ± 0.126 −6.681 ± 0.354 3.60 ± 2.91 0.70<br />
NGC 4382 624 186.35486 18.17180 1.30 −7.532 ± 0.043 −8.833 ± 0.050 3.63 ± 0.29 1.00<br />
NGC 4382 627 186.35558 18.17622 1.04 −7.502 ± 0.067 −8.853 ± 0.068 6.01 ± 0.33 0.77<br />
NGC 4382 628 186.35605 18.17986 0.83 −5.531 ± 0.362 −6.727 ± 0.555 3.40 ± 2.01 0.74<br />
NGC 4382 631 186.35558 18.17477 1.13 −7.545 ± 0.064 −9.096 ± 0.021 2.31 ± 0.31 1.00<br />
NGC 4382 632 186.35716 18.18649 0.53 −8.381 ± 0.027 −9.134 ± 0.023 2.62 ± 0.14 1.00<br />
NGC 4382 633 186.35784 18.19254 0.49 −6.731 ± 0.052 −7.459 ± 0.319 1.84 ± 0.41 0.76<br />
NGC 4382 635 186.35653 18.18042 0.81 −8.895 ± 0.028 −9.718 ± 0.026 3.01 ± 0.19 1.00<br />
NGC 4382 636 186.35733 18.18710 0.52 −7.293 ± 0.078 −8.221 ± 0.044 2.49 ± 0.37 0.98<br />
NGC 4382 640 186.35734 18.18566 0.57 −6.597 ± 0.061 −8.219 ± 0.176 5.48 ± 1.52 0.76<br />
NGC 4382 642 186.35625 18.17557 1.09 −5.075 ± 0.163 −6.547 ± 0.101 3.06 ± 0.70 0.79<br />
NGC 4382 643 186.35698 18.18128 0.77 −5.755 ± 0.150 −6.653 ± 0.117 3.77 ± 0.82 0.66<br />
NGC 4382 644 186.35939 18.19937 0.79 −8.594 ± 0.018 −9.466 ± 0.022 2.09 ± 0.19 1.00<br />
NGC 4382 645 186.35675 18.17853 0.92 −5.957 ± 0.080 −7.078 ± 0.077 2.86 ± 0.64 0.87<br />
NGC 4382 649 186.35914 18.19624 0.65 −6.760 ± 0.056 −8.287 ± 0.088 3.68 ± 0.51 1.00<br />
NGC 4382 650 186.35933 18.19704 0.69 −7.175 ± 0.083 −7.968 ± 0.097 3.25 ± 0.49 0.95<br />
NGC 4382 651 186.35631 18.17246 1.29 −9.822 ± 0.014 −10.738 ± 0.022 5.57 ± 0.11 1.00<br />
NGC 4382 654 186.35936 18.19656 0.68 −7.791 ± 0.041 −9.206 ± 0.065 3.98 ± 0.41 1.00<br />
NGC 4382 655 186.36077 18.20659 1.22 −9.425 ± 0.020 −10.440 ± 0.011 3.02 ± 0.11 1.00<br />
NGC 4382 656 186.36173 18.21466 1.71 −5.702 ± 0.121 −6.848 ± 0.103 2.73 ± 0.62 0.85<br />
NGC 4382 657 186.35898 18.19301 0.56 −8.843 ± 0.025 −9.793 ± 0.017 2.83 ± 0.22 1.00<br />
NGC 4382 658 186.35530 18.16455 1.78 −5.741 ± 0.118 −7.213 ± 0.097 4.34 ± 0.62 0.58<br />
NGC 4382 659 186.35991 18.19939 0.82 −6.338 ± 0.104 −7.063 ± 0.216 2.29 ± 0.52 0.90<br />
NGC 4382 660 186.36123 18.20870 1.35 −7.686 ± 0.042 −8.846 ± 0.067 4.43 ± 0.29 1.00<br />
Continued on Next Page. . .<br />
323
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4382 662 186.35991 18.19759 0.74 −8.586 ± 0.052 −9.546 ± 0.110 9.14 ± 0.77 0.51<br />
NGC 4382 665 186.36098 18.20393 1.08 −5.284 ± 0.739 −6.511 ± 0.196 2.96 ± 0.93 0.79<br />
NGC 4382 666 186.36127 18.20611 1.21 −6.151 ± 0.103 −7.112 ± 0.157 3.42 ± 0.75 0.79<br />
NGC 4382 671 186.35833 18.18253 0.76 −5.236 ± 0.194 −6.622 ± 0.106 3.57 ± 0.71 0.71<br />
NGC 4382 673 186.35614 18.16372 1.84 −6.858 ± 0.030 −8.107 ± 0.090 4.18 ± 0.32 0.92<br />
NGC 4382 674 186.35701 18.17038 1.43 −5.759 ± 0.139 −7.030 ± 0.159 3.76 ± 0.79 0.69<br />
NGC 4382 677 186.35990 18.19112 0.60 −8.213 ± 0.031 −9.578 ± 0.023 3.21 ± 0.18 1.00<br />
NGC 4382 680 186.36062 18.19669 0.75 −8.165 ± 0.030 −9.330 ± 0.024 3.63 ± 0.14 1.00<br />
NGC 4382 681 186.36198 18.20656 1.26 −6.333 ± 0.115 −7.035 ± 0.214 3.71 ± 1.01 0.71<br />
NGC 4382 682 186.36184 18.20584 1.21 −4.953 ± 0.210 −6.351 ± 0.268 2.58 ± 0.81 0.79<br />
NGC 4382 685 186.36238 18.20762 1.33 −6.595 ± 0.052 −8.001 ± 0.061 2.56 ± 0.36 0.97<br />
NGC 4382 687 186.35759 18.17048 1.44 −5.447 ± 0.144 −6.559 ± 0.317 1.91 ± 1.26 0.65<br />
NGC 4382 690 186.35675 18.16338 1.87 −5.079 ± 1.000 −6.675 ± 0.849 3.96 ± 27.04 0.60<br />
NGC 4382 691 186.36313 18.21195 1.59 −8.352 ± 0.040 −9.698 ± 0.073 6.10 ± 0.40 0.98<br />
NGC 4382 693 186.35918 18.18005 0.92 −5.490 ± 0.181 −6.817 ± 0.198 3.22 ± 0.79 0.78<br />
NGC 4382 694 186.35905 18.17852 1.00 −6.470 ± 0.074 −7.566 ± 0.055 4.28 ± 0.21 0.76<br />
NGC 4382 695 186.36234 18.20331 1.11 −7.279 ± 0.037 −8.668 ± 0.063 4.01 ± 0.21 1.00<br />
NGC 4382 698 186.35809 18.16998 1.48 −5.372 ± 0.163 −6.276 ± 0.145 4.09 ± 0.86 0.56<br />
NGC 4382 699 186.36345 18.21138 1.57 −6.438 ± 0.071 −7.398 ± 0.347 4.39 ± 0.41 0.66<br />
NGC 4382 701 186.35961 18.18085 0.89 −8.158 ± 0.027 −9.233 ± 0.031 2.10 ± 0.25 1.00<br />
NGC 4382 702 186.36226 18.20167 1.03 −7.698 ± 0.048 −8.585 ± 0.045 4.30 ± 0.23 1.00<br />
NGC 4382 703 186.36306 18.20773 1.36 −6.612 ± 0.128 −7.976 ± 0.162 5.67 ± 1.18 0.61<br />
NGC 4382 706 186.35938 18.17689 1.10 −7.536 ± 0.029 −8.443 ± 0.034 2.18 ± 0.26 1.00<br />
NGC 4382 710 186.36139 18.19151 0.70 −5.835 ± 1.971 −7.261 ± 0.716 2.31 ± 0.79 0.92<br />
NGC 4382 711 186.36005 18.18089 0.91 −6.293 ± 0.119 −7.303 ± 0.082 4.41 ± 1.10 0.60<br />
NGC 4382 715 186.36153 18.19102 0.71 −6.543 ± 0.109 −7.909 ± 0.059 1.92 ± 0.39 0.89<br />
NGC 4382 718 186.36096 18.18593 0.75 −6.950 ± 0.072 −7.723 ± 0.056 2.40 ± 0.32 0.95<br />
NGC 4382 719 186.36197 18.19326 0.75 −7.492 ± 0.040 −8.651 ± 0.064 3.27 ± 0.34 1.00<br />
NGC 4382 720 186.36180 18.19075 0.72 −7.748 ± 0.018 −9.013 ± 0.028 3.00 ± 0.22 1.00<br />
NGC 4382 722 186.36433 18.20936 1.49 −9.805 ± 0.044 −10.663 ± 0.038 6.82 ± 0.29 1.00<br />
NGC 4382 727 186.36293 18.19709 0.89 −7.494 ± 0.028 −8.774 ± 0.025 2.18 ± 0.25 1.00<br />
NGC 4382 730 186.36386 18.20413 1.21 −7.207 ± 0.034 −8.298 ± 0.038 2.71 ± 0.28 1.00<br />
NGC 4382 731 186.36345 18.20072 1.04 −5.963 ± 0.137 −7.026 ± 0.241 2.90 ± 0.56 0.86<br />
NGC 4382 732 186.36359 18.20178 1.09 −6.404 ± 0.066 −7.237 ± 0.424 2.15 ± 0.46 0.88<br />
NGC 4382 739 186.36073 18.17807 1.08 −5.989 ± 0.135 −7.216 ± 0.070 2.87 ± 0.66 0.89<br />
NGC 4382 740 186.36117 18.18151 0.93 −6.203 ± 0.142 −7.453 ± 0.121 4.63 ± 0.85 0.61<br />
NGC 4382 741 186.36173 18.18566 0.80 −5.261 ± 0.292 −6.648 ± 0.409 2.31 ± 1.14 0.81<br />
NGC 4382 743 186.36327 18.19704 0.91 −7.041 ± 0.034 −8.245 ± 0.061 3.71 ± 0.28 0.95<br />
NGC 4382 744 186.36287 18.19338 0.81 −8.396 ± 0.031 −9.394 ± 0.020 2.55 ± 0.17 1.00<br />
NGC 4382 745 186.36275 18.19183 0.79 −7.541 ± 0.025 −8.519 ± 0.039 2.25 ± 0.23 1.00<br />
NGC 4382 749 186.36177 18.18356 0.88 −6.572 ± 0.106 −7.803 ± 1.005 1.99 ± 0.52 0.90<br />
NGC 4382 750 186.36199 18.18451 0.85 −7.357 ± 0.064 −8.223 ± 0.088 5.62 ± 0.59 0.73<br />
NGC 4382 752 186.36153 18.18069 0.99 −8.391 ± 0.054 −9.239 ± 0.047 5.76 ± 0.26 0.90<br />
NGC 4382 753 186.36274 18.19016 0.79 −7.145 ± 0.041 −8.269 ± 0.041 2.82 ± 0.28 0.98<br />
NGC 4382 757 186.36026 18.16985 1.54 −8.004 ± 0.036 −9.083 ± 0.037 4.37 ± 0.19 1.00<br />
NGC 4382 767 186.36559 18.20768 1.46 −6.086 ± 0.389 −7.167 ± 0.316 2.62 ± 0.65 0.91<br />
NGC 4382 768 186.36363 18.19162 0.84 −8.309 ± 0.027 −9.530 ± 0.021 2.85 ± 0.16 1.00<br />
NGC 4382 769 186.36499 18.20233 1.18 −5.633 ± 0.114 −7.162 ± 0.080 4.28 ± 0.64 0.58<br />
NGC 4382 770 186.36139 18.17411 1.32 −4.965 ± 0.161 −6.278 ± 0.191 3.22 ± 0.93 0.79<br />
NGC 4382 778 186.36032 18.16292 1.96 −5.012 ± 0.561 −6.252 ± 0.157 3.09 ± 1.20 0.80<br />
NGC 4382 781 186.36496 18.19652 0.99 −5.587 ± 0.203 −6.594 ± 0.106 3.75 ± 0.86 0.67<br />
NGC 4382 782 186.36375 18.18438 0.96 −5.844 ± 0.159 −6.910 ± 0.102 4.26 ± 0.91 0.51<br />
NGC 4382 783 186.36104 18.16294 1.98 −6.459 ± 0.067 −7.873 ± 0.058 2.63 ± 0.38 0.96<br />
NGC 4382 786 186.36178 18.16721 1.73 −6.338 ± 0.122 −7.383 ± 0.189 4.82 ± 1.28 0.52<br />
NGC 4382 789 186.36719 18.20823 1.55 −7.423 ± 0.028 −8.193 ± 0.042 2.55 ± 0.26 0.98<br />
NGC 4382 794 186.36484 18.18800 0.94 −6.682 ± 0.051 −7.542 ± 0.052 1.82 ± 0.30 0.77<br />
NGC 4382 795 186.36854 18.21674 2.04 −6.064 ± 0.077 −7.238 ± 0.191 4.07 ± 1.07 0.68<br />
NGC 4382 798 186.36751 18.20735 1.52 −7.878 ± 0.020 −9.229 ± 0.028 3.06 ± 0.22 1.00<br />
NGC 4382 800 186.36679 18.20145 1.24 −7.198 ± 0.033 −8.591 ± 0.033 2.01 ± 0.24 1.00<br />
NGC 4382 801 186.36670 18.20096 1.22 −5.273 ± 0.619 −6.152 ± 0.279 1.85 ± 0.83 0.61<br />
NGC 4382 804 186.36769 18.20854 1.59 −5.717 ± 0.814 −6.717 ± 0.102 2.19 ± 0.49 0.80<br />
NGC 4382 806 186.36850 18.21423 1.91 −5.883 ± 0.102 −6.624 ± 0.590 2.85 ± 0.57 0.81<br />
Continued on Next Page. . .<br />
324
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4382 807 186.36884 18.21672 2.05 −8.309 ± 0.031 −9.131 ± 0.022 2.74 ± 0.16 1.00<br />
NGC 4382 808 186.36579 18.19268 0.98 −8.766 ± 0.040 −9.979 ± 0.019 3.04 ± 0.21 1.00<br />
NGC 4382 809 186.36191 18.16251 2.02 −5.413 ± 0.126 −6.867 ± 0.216 4.20 ± 1.26 0.53<br />
NGC 4382 814 186.36562 18.18813 0.98 −7.436 ± 0.032 −8.476 ± 0.045 3.95 ± 0.36 1.00<br />
NGC 4382 816 186.36571 18.18655 1.01 −9.548 ± 0.016 −10.680 ± 0.019 2.89 ± 0.17 1.00<br />
NGC 4382 817 186.36580 18.18754 1.00 −6.156 ± 0.047 −7.169 ± 0.415 2.35 ± 1.43 0.91<br />
NGC 4382 818 186.36274 18.16371 1.97 −5.255 ± 0.101 −6.361 ± 0.420 2.78 ± 0.72 0.79<br />
NGC 4382 821 186.36494 18.17724 1.30 −5.898 ± 0.111 −6.779 ± 0.440 2.51 ± 0.55 0.85<br />
NGC 4382 822 186.36526 18.17920 1.23 −7.348 ± 0.058 −8.576 ± 0.144 6.38 ± 1.06 0.56<br />
NGC 4382 832 186.36940 18.20941 1.70 −5.597 ± 0.195 −6.829 ± 0.090 3.34 ± 1.17 0.76<br />
NGC 4382 833 186.36531 18.17729 1.31 −7.490 ± 0.059 −8.250 ± 0.049 4.16 ± 0.42 0.94<br />
NGC 4382 840 186.36701 18.18725 1.08 −6.437 ± 0.054 −7.481 ± 0.055 4.88 ± 0.23 0.55<br />
NGC 4382 841 186.36601 18.17974 1.24 −6.677 ± 0.039 −7.893 ± 0.064 3.22 ± 0.35 0.95<br />
NGC 4382 842 186.36526 18.17349 1.49 −7.667 ± 0.034 −9.093 ± 0.024 2.37 ± 0.27 1.00<br />
NGC 4382 843 186.36945 18.20598 1.55 −8.126 ± 0.028 −9.588 ± 0.027 3.51 ± 0.18 1.00<br />
NGC 4382 845 186.36705 18.18686 1.09 −7.661 ± 0.025 −8.788 ± 0.064 4.24 ± 0.22 1.00<br />
NGC 4382 846 186.36899 18.20208 1.38 −7.201 ± 0.039 −8.215 ± 0.053 3.21 ± 0.26 0.96<br />
NGC 4382 854 186.36970 18.20207 1.42 −7.564 ± 0.038 −8.872 ± 0.054 4.87 ± 0.21 0.98<br />
NGC 4382 856 186.36910 18.19632 1.23 −7.285 ± 0.068 −8.077 ± 0.064 4.74 ± 0.34 0.84<br />
NGC 4382 858 186.36602 18.17185 1.61 −5.667 ± 0.120 −6.656 ± 0.168 3.69 ± 0.82 0.68<br />
NGC 4382 860 186.36701 18.17821 1.35 −8.223 ± 0.044 −9.025 ± 0.041 6.82 ± 0.24 0.68<br />
NGC 4382 861 186.36815 18.18727 1.15 −7.083 ± 0.079 −8.280 ± 0.034 5.32 ± 0.26 0.81<br />
NGC 4382 863 186.36941 18.19616 1.25 −7.026 ± 0.034 −7.901 ± 0.146 2.27 ± 1.49 0.96<br />
NGC 4382 864 186.36807 18.18547 1.18 −5.630 ± 0.062 −6.678 ± 0.053 2.03 ± 0.38 0.74<br />
NGC 4382 865 186.36734 18.17994 1.30 −8.230 ± 0.026 −9.106 ± 0.021 3.13 ± 0.16 1.00<br />
NGC 4382 866 186.37149 18.21078 1.86 −8.967 ± 0.023 −10.312 ± 0.012 2.33 ± 0.16 1.00<br />
NGC 4382 869 186.36727 18.17705 1.41 −6.245 ± 0.730 −7.622 ± 0.310 2.83 ± 0.61 0.93<br />
NGC 4382 872 186.36937 18.19099 1.20 −7.529 ± 0.035 −8.292 ± 0.024 2.17 ± 0.18 1.00<br />
NGC 4382 875 186.36887 18.18596 1.22 −10.339 ± 0.027 −11.190 ± 0.017 4.07 ± 0.13 1.00<br />
NGC 4382 877 186.36783 18.17819 1.39 −6.908 ± 0.039 −8.167 ± 0.039 3.92 ± 0.22 0.94<br />
NGC 4382 879 186.36699 18.17056 1.71 −5.954 ± 0.072 −7.100 ± 0.111 3.19 ± 0.50 0.83<br />
NGC 4382 882 186.36952 18.18989 1.21 −7.012 ± 0.076 −8.332 ± 0.045 4.43 ± 0.27 1.00<br />
NGC 4382 883 186.37276 18.21457 2.09 −8.758 ± 0.027 −9.965 ± 0.019 3.12 ± 0.15 1.00<br />
NGC 4382 886 186.36943 18.18726 1.23 −8.350 ± 0.022 −9.548 ± 0.022 3.99 ± 0.15 1.00<br />
NGC 4382 888 186.36784 18.17544 1.51 −8.615 ± 0.021 −9.864 ± 0.018 2.17 ± 0.20 1.00<br />
NGC 4382 889 186.36970 18.18991 1.22 −7.626 ± 0.029 −9.016 ± 0.035 2.46 ± 0.20 1.00<br />
NGC 4382 890 186.36875 18.18206 1.30 −5.331 ± 0.323 −6.676 ± 0.186 3.68 ± 1.82 0.68<br />
NGC 4382 891 186.37079 18.19775 1.36 −6.002 ± 0.142 −7.053 ± 0.195 3.89 ± 1.27 0.67<br />
NGC 4382 892 186.37218 18.20822 1.78 −6.349 ± 0.050 −7.941 ± 0.141 6.09 ± 0.94 0.51<br />
NGC 4382 898 186.37301 18.21162 1.97 −5.265 ± 0.193 −7.095 ± 0.086 4.08 ± 0.57 0.63<br />
NGC 4382 901 186.36745 18.16692 1.92 −5.361 ± 0.186 −6.301 ± 0.186 3.82 ± 0.90 0.67<br />
NGC 4382 910 186.37224 18.19936 1.48 −8.834 ± 0.023 −9.736 ± 0.015 2.62 ± 0.13 1.00<br />
NGC 4382 917 186.37073 18.18366 1.37 −5.463 ± 0.162 −6.679 ± 0.157 4.08 ± 0.95 0.56<br />
NGC 4382 921 186.37306 18.20036 1.55 −8.814 ± 0.022 −9.674 ± 0.017 2.56 ± 0.12 1.00<br />
NGC 4382 923 186.36923 18.16999 1.83 −8.183 ± 0.022 −9.210 ± 0.018 2.39 ± 0.16 1.00<br />
NGC 4382 927 186.37173 18.18571 1.39 −8.223 ± 0.022 −9.371 ± 0.017 1.92 ± 0.14 1.00<br />
NGC 4382 928 186.37294 18.19532 1.45 −6.850 ± 0.075 −8.033 ± 0.053 5.93 ± 0.39 0.59<br />
NGC 4382 941 186.37340 18.19398 1.46 −9.662 ± 0.049 −10.629 ± 0.104 7.31 ± 0.58 1.00<br />
NGC 4382 945 186.37118 18.17488 1.69 −5.172 ± 0.420 −6.854 ± 0.198 4.12 ± 1.65 0.56<br />
NGC 4382 946 186.37566 18.20973 2.01 −6.646 ± 0.051 −7.653 ± 0.042 3.05 ± 0.29 0.93<br />
NGC 4382 947 186.37493 18.20366 1.75 −8.829 ± 0.017 −9.975 ± 0.016 2.34 ± 0.14 1.00<br />
NGC 4382 953 186.37172 18.17584 1.68 −8.444 ± 0.018 −9.353 ± 0.027 2.58 ± 0.20 1.00<br />
NGC 4382 959 186.37292 18.18357 1.51 −7.166 ± 0.065 −8.530 ± 0.142 6.03 ± 0.94 0.67<br />
NGC 4382 961 186.37432 18.19385 1.52 −5.914 ± 0.075 −7.521 ± 0.100 4.52 ± 0.58 0.68<br />
NGC 4382 963 186.37657 18.20974 2.06 −6.501 ± 0.069 −7.456 ± 0.127 4.67 ± 0.93 0.60<br />
NGC 4382 966 186.37670 18.20866 2.02 −5.198 ± 0.368 −6.897 ± 0.114 3.32 ± 0.63 0.77<br />
NGC 4382 977 186.37454 18.18501 1.57 −7.136 ± 0.053 −8.280 ± 0.100 5.36 ± 0.51 0.81<br />
NGC 4382 979 186.37253 18.16802 2.07 −5.039 ± 0.139 −6.447 ± 0.136 3.14 ± 0.65 0.78<br />
NGC 4382 981 186.37295 18.16946 2.02 −5.599 ± 0.081 −6.750 ± 0.070 2.79 ± 0.57 0.83<br />
NGC 4382 987 186.37672 18.19253 1.66 −7.938 ± 0.083 −8.730 ± 0.047 4.02 ± 0.37 1.00<br />
NGC 4382 988 186.37551 18.18255 1.68 −7.728 ± 0.015 −8.570 ± 0.028 2.11 ± 0.15 1.00<br />
NGC 4382 991 186.37317 18.16363 2.31 −5.520 ± 0.057 −6.936 ± 0.157 3.19 ± 0.73 0.80<br />
Continued on Next Page. . .<br />
325
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4382 992 186.37930 18.21057 2.23 −9.434 ± 0.025 −10.647 ± 0.014 2.75 ± 0.25 1.00<br />
NGC 4382 993 186.37766 18.19741 1.77 −5.919 ± 0.211 −7.142 ± 0.065 3.71 ± 1.14 0.73<br />
NGC 4382 998 186.37917 18.20559 2.05 −7.018 ± 0.036 −8.227 ± 0.027 3.06 ± 0.24 0.97<br />
NGC 4382 1008 186.37846 18.19338 1.77 −7.838 ± 0.031 −9.321 ± 0.024 2.85 ± 0.22 1.00<br />
NGC 4382 1011 186.37969 18.20232 1.99 −5.777 ± 0.081 −6.767 ± 0.141 3.76 ± 0.66 0.66<br />
NGC 4382 1014 186.37825 18.19018 1.76 −5.359 ± 0.764 −6.746 ± 0.150 1.81 ± 1.87 0.61<br />
NGC 4382 1017 186.37857 18.19099 1.78 −5.549 ± 0.063 −6.766 ± 0.474 1.87 ± 0.45 0.66<br />
NGC 4382 1019 186.38182 18.21517 2.54 −7.852 ± 0.028 −8.599 ± 0.025 2.86 ± 0.17 1.00<br />
NGC 4382 1023 186.37848 18.18688 1.79 −9.817 ± 0.015 −10.897 ± 0.027 3.30 ± 0.12 1.00<br />
NGC 4382 1033 186.37762 18.17217 2.12 −8.346 ± 0.025 −9.320 ± 0.038 3.92 ± 0.19 1.00<br />
NGC 4382 1035 186.37920 18.18323 1.89 −7.859 ± 0.026 −8.831 ± 0.024 3.16 ± 0.18 1.00<br />
NGC 4382 1037 186.38104 18.19726 1.97 −5.145 ± 0.461 −6.127 ± 0.352 2.55 ± 4.79 0.79<br />
NGC 4382 1038 186.37694 18.16498 2.40 −4.997 ± 0.119 −6.669 ± 0.093 3.37 ± 0.53 0.75<br />
NGC 4382 1039 186.37721 18.16649 2.34 −8.315 ± 0.018 −9.366 ± 0.018 3.53 ± 0.12 1.00<br />
NGC 4382 1041 186.37654 18.16053 2.60 −8.213 ± 0.039 −9.454 ± 0.021 3.30 ± 0.15 1.00<br />
NGC 4382 1046 186.38030 18.18776 1.90 −7.858 ± 0.032 −8.809 ± 0.033 3.63 ± 0.24 1.00<br />
NGC 4382 1050 186.38048 18.18695 1.91 −5.400 ± 0.404 −6.609 ± 0.113 3.95 ± 9.74 0.60<br />
NGC 4382 1054 186.38107 18.19057 1.93 −7.588 ± 0.037 −8.469 ± 0.034 3.53 ± 0.23 1.00<br />
NGC 4382 1055 186.38225 18.19920 2.08 −5.654 ± 0.135 −6.749 ± 0.168 3.15 ± 0.79 0.79<br />
NGC 4382 1056 186.37865 18.17084 2.23 −7.323 ± 0.042 −8.179 ± 0.030 2.31 ± 0.22 0.97<br />
NGC 4382 1058 186.38252 18.19923 2.09 −7.921 ± 0.029 −8.810 ± 0.050 4.22 ± 0.22 1.00<br />
NGC 4382 1060 186.37999 18.17900 2.03 −5.361 ± 0.127 −6.786 ± 0.122 2.91 ± 0.60 0.82<br />
NGC 4382 1062 186.38373 18.20677 2.34 −7.872 ± 0.024 −8.888 ± 0.031 2.84 ± 0.19 1.00<br />
NGC 4382 1063 186.37892 18.16909 2.31 −6.058 ± 0.095 −7.307 ± 0.107 4.73 ± 0.77 0.51<br />
NGC 4382 1064 186.38489 18.21372 2.63 −10.055 ± 0.018 −11.016 ± 0.022 5.30 ± 0.10 0.96<br />
NGC 4382 1066 186.38496 18.21404 2.65 −5.884 ± 0.055 −7.376 ± 0.074 3.20 ± 0.55 0.88<br />
NGC 4382 1067 186.38002 18.17502 2.15 −7.693 ± 0.039 −8.892 ± 0.036 3.55 ± 0.23 1.00<br />
NGC 4382 1074 186.38019 18.17183 2.27 −8.497 ± 0.030 −9.462 ± 0.038 4.19 ± 0.19 1.00<br />
NGC 4382 1077 186.38426 18.20061 2.22 −4.974 ± 0.116 −6.402 ± 0.300 3.58 ± 2.89 0.73<br />
NGC 4382 1079 186.38219 18.18295 2.07 −6.602 ± 0.072 −7.438 ± 0.078 2.46 ± 0.59 0.93<br />
NGC 4382 1084 186.38429 18.19652 2.16 −6.659 ± 0.057 −7.592 ± 0.054 3.23 ± 0.40 0.92<br />
NGC 4382 1086 186.38353 18.18887 2.09 −8.854 ± 0.020 −9.811 ± 0.018 3.34 ± 0.14 1.00<br />
NGC 4382 1090 186.38132 18.17047 2.38 −6.082 ± 0.071 −6.784 ± 0.062 3.43 ± 0.35 0.74<br />
NGC 4382 1093 186.38305 18.18257 2.13 −7.804 ± 0.033 −8.632 ± 0.027 2.86 ± 0.17 1.00<br />
NGC 4382 1096 186.38075 18.16328 2.65 −8.029 ± 0.030 −9.280 ± 0.029 2.78 ± 0.28 1.00<br />
NGC 4382 1097 186.38654 18.20710 2.51 −8.654 ± 0.020 −9.488 ± 0.016 2.89 ± 0.10 1.00<br />
NGC 4382 1103 186.38727 18.20949 2.62 −7.245 ± 0.035 −7.997 ± 0.039 2.77 ± 0.31 0.97<br />
NGC 4382 1109 186.38737 18.20592 2.52 −5.277 ± 0.220 −6.300 ± 0.692 2.22 ± 1.04 0.75<br />
NGC 4382 1111 186.38776 18.20787 2.60 −6.524 ± 0.071 −7.721 ± 0.025 2.66 ± 0.28 0.95<br />
NGC 4382 1114 186.38344 18.17327 2.39 −6.940 ± 0.033 −8.101 ± 0.026 2.63 ± 0.27 0.97<br />
NGC 4382 1117 186.38504 18.18473 2.22 −5.243 ± 0.193 −6.723 ± 0.057 2.96 ± 0.46 0.81<br />
NGC 4382 1121 186.39016 18.21470 2.95 −6.586 ± 0.063 −7.161 ± 0.109 3.77 ± 0.59 0.72<br />
NGC 4382 1122 186.38945 18.20686 2.67 −9.125 ± 0.049 −9.983 ± 0.025 4.98 ± 0.24 1.00<br />
NGC 4406 1 186.58181 12.94307 1.11 −5.392 ± 0.127 −6.206 ± 0.379 3.20 ± 1.42 0.86<br />
NGC 4406 4 186.56871 12.93331 0.80 −7.600 ± 0.022 −8.376 ± 0.046 3.99 ± 0.19 1.00<br />
NGC 4406 8 186.56587 12.93146 0.77 −8.682 ± 0.016 −9.752 ± 0.025 2.62 ± 0.11 1.00<br />
NGC 4406 11 186.57129 12.93645 0.83 −8.062 ± 0.020 −9.120 ± 0.027 2.85 ± 0.15 1.00<br />
NGC 4406 12 186.56331 12.92991 0.74 −5.304 ± 0.451 −6.737 ± 0.099 3.17 ± 0.56 0.86<br />
NGC 4406 13 186.56346 12.93020 0.74 −7.718 ± 0.021 −8.749 ± 0.036 3.15 ± 0.21 1.00<br />
NGC 4406 14 186.57475 12.93966 0.90 −8.543 ± 0.015 −9.697 ± 0.016 2.09 ± 0.09 1.00<br />
NGC 4406 15 186.56741 12.93385 0.76 −7.529 ± 0.060 −8.571 ± 0.075 5.88 ± 0.53 0.82<br />
NGC 4406 16 186.56939 12.93556 0.78 −8.551 ± 0.013 −9.503 ± 0.015 2.51 ± 0.10 1.00<br />
NGC 4406 17 186.56365 12.93116 0.72 −9.585 ± 0.018 −10.693 ± 0.016 2.71 ± 0.10 1.00<br />
NGC 4406 18 186.56550 12.93281 0.73 −8.546 ± 0.031 −9.325 ± 0.028 4.23 ± 0.12 1.00<br />
NGC 4406 19 186.55429 12.92373 0.80 −7.219 ± 0.033 −8.434 ± 0.029 2.34 ± 0.23 1.00<br />
NGC 4406 22 186.57644 12.94248 0.94 −8.997 ± 0.035 −10.264 ± 0.052 11.24 ± 0.43 1.00<br />
NGC 4406 23 186.55252 12.92306 0.81 −7.101 ± 0.033 −8.426 ± 0.037 2.57 ± 0.27 1.00<br />
NGC 4406 25 186.58162 12.94689 1.10 −7.907 ± 0.038 −9.013 ± 0.028 3.17 ± 0.17 1.00<br />
NGC 4406 26 186.56961 12.93714 0.77 −6.826 ± 0.074 −8.001 ± 0.054 4.22 ± 0.24 0.93<br />
NGC 4406 31 186.55336 12.92481 0.76 −7.477 ± 0.023 −8.269 ± 0.042 2.86 ± 0.25 0.99<br />
NGC 4406 32 186.57580 12.94314 0.91 −8.140 ± 0.023 −9.274 ± 0.015 2.56 ± 0.11 1.00<br />
Continued on Next Page. . .<br />
326
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4406 36 186.55378 12.92576 0.73 −6.860 ± 0.040 −7.759 ± 0.104 3.29 ± 0.50 0.96<br />
NGC 4406 38 186.56345 12.93415 0.64 −7.312 ± 0.031 −8.610 ± 0.031 2.01 ± 0.22 1.00<br />
NGC 4406 42 186.54069 12.91604 1.08 −5.845 ± 0.150 −7.396 ± 0.459 2.22 ± 0.68 0.96<br />
NGC 4406 43 186.56214 12.93356 0.63 −7.935 ± 0.063 −8.537 ± 0.143 6.00 ± 1.03 0.78<br />
NGC 4406 45 186.56762 12.93793 0.69 −6.678 ± 0.035 −7.984 ± 0.039 1.83 ± 0.20 0.95<br />
NGC 4406 49 186.55436 12.92782 0.66 −5.761 ± 0.342 −6.929 ± 0.403 1.60 ± 0.65 0.75<br />
NGC 4406 50 186.55542 12.92893 0.64 −7.037 ± 0.041 −8.014 ± 0.053 1.75 ± 0.23 0.94<br />
NGC 4406 51 186.56172 12.93438 0.60 −9.509 ± 0.022 −10.612 ± 0.019 1.98 ± 0.23 1.00<br />
NGC 4406 52 186.57824 12.94789 0.99 −5.569 ± 0.074 −7.450 ± 0.122 5.27 ± 0.53 0.53<br />
NGC 4406 54 186.56384 12.93654 0.60 −8.344 ± 0.022 −9.685 ± 0.027 3.16 ± 0.14 1.00<br />
NGC 4406 55 186.56607 12.93850 0.64 −8.871 ± 0.018 −9.853 ± 0.020 2.69 ± 0.12 1.00<br />
NGC 4406 58 186.54919 12.92502 0.73 −8.534 ± 0.029 −9.535 ± 0.014 2.66 ± 0.19 1.00<br />
NGC 4406 60 186.54394 12.92109 0.89 −8.102 ± 0.018 −9.115 ± 0.024 2.33 ± 0.14 1.00<br />
NGC 4406 62 186.55828 12.93336 0.55 −9.313 ± 0.018 −10.188 ± 0.017 4.24 ± 0.10 1.00<br />
NGC 4406 63 186.54953 12.92625 0.69 −6.716 ± 0.062 −7.923 ± 0.051 2.04 ± 0.33 0.98<br />
NGC 4406 65 186.54622 12.92397 0.78 −7.523 ± 0.038 −8.621 ± 0.050 3.40 ± 0.25 1.00<br />
NGC 4406 71 186.56124 12.93663 0.53 −7.553 ± 0.030 −8.524 ± 0.023 3.41 ± 0.19 1.00<br />
NGC 4406 72 186.55630 12.93268 0.53 −5.211 ± 0.152 −6.321 ± 0.135 2.53 ± 0.59 0.88<br />
NGC 4406 74 186.55887 12.93522 0.51 −7.694 ± 0.037 −8.578 ± 0.261 3.22 ± 0.34 1.00<br />
NGC 4406 75 186.55870 12.93557 0.49 −6.877 ± 0.056 −8.365 ± 0.062 2.72 ± 0.33 1.00<br />
NGC 4406 77 186.57706 12.95064 0.96 −6.237 ± 0.068 −7.475 ± 0.054 3.52 ± 0.31 0.91<br />
NGC 4406 78 186.54563 12.92535 0.73 −8.799 ± 0.023 −9.866 ± 0.014 2.10 ± 0.09 1.00<br />
NGC 4406 81 186.54817 12.92758 0.65 −7.017 ± 0.047 −8.125 ± 0.065 3.06 ± 0.34 0.98<br />
NGC 4406 82 186.56286 12.93953 0.52 −6.297 ± 0.181 −7.545 ± 0.052 2.22 ± 0.30 0.97<br />
NGC 4406 84 186.57489 12.94978 0.88 −7.792 ± 0.036 −8.630 ± 0.031 3.82 ± 0.20 1.00<br />
NGC 4406 85 186.54715 12.92729 0.66 −5.746 ± 0.179 −6.504 ± 0.426 2.10 ± 0.65 0.87<br />
NGC 4406 86 186.56297 12.94059 0.51 −9.640 ± 0.027 −10.737 ± 0.032 3.58 ± 0.27 1.00<br />
NGC 4406 87 186.55843 12.93689 0.46 −7.788 ± 0.027 −8.673 ± 0.044 2.23 ± 0.25 1.00<br />
NGC 4406 91 186.54633 12.92778 0.65 −8.448 ± 0.022 −9.761 ± 0.024 1.95 ± 0.20 1.00<br />
NGC 4406 92 186.56731 12.94494 0.62 −7.566 ± 0.028 −8.833 ± 0.036 2.72 ± 0.16 1.00<br />
NGC 4406 93 186.54273 12.92509 0.76 −8.475 ± 0.026 −9.327 ± 0.026 2.94 ± 0.14 1.00<br />
NGC 4406 94 186.54260 12.92508 0.76 −7.608 ± 0.030 −8.510 ± 0.031 2.17 ± 0.21 1.00<br />
NGC 4406 95 186.57254 12.94934 0.80 −7.120 ± 0.029 −8.444 ± 0.022 2.06 ± 0.14 1.00<br />
NGC 4406 98 186.55672 12.93676 0.42 −6.799 ± 0.333 −7.890 ± 0.188 1.23 ± 0.34 0.70<br />
NGC 4406 100 186.56397 12.94299 0.52 −5.599 ± 0.581 −6.824 ± 0.225 2.13 ± 1.19 0.90<br />
NGC 4406 101 186.55205 12.93346 0.45 −8.696 ± 0.057 −9.518 ± 0.039 3.13 ± 0.35 1.00<br />
NGC 4406 102 186.57832 12.95484 1.03 −7.768 ± 0.083 −9.121 ± 0.060 5.92 ± 0.45 0.91<br />
NGC 4406 103 186.55105 12.93275 0.47 −6.763 ± 0.030 −8.235 ± 0.042 2.23 ± 0.25 0.99<br />
NGC 4406 104 186.55530 12.93626 0.41 −7.431 ± 0.042 −8.345 ± 0.069 2.99 ± 0.33 1.00<br />
NGC 4406 107 186.55311 12.93460 0.43 −5.964 ± 0.076 −6.557 ± 0.348 1.72 ± 0.59 0.79<br />
NGC 4406 108 186.55881 12.93932 0.41 −8.013 ± 0.030 −9.023 ± 0.040 3.45 ± 0.25 1.00<br />
NGC 4406 109 186.56647 12.94554 0.59 −8.343 ± 0.021 −9.825 ± 0.018 2.16 ± 0.16 1.00<br />
NGC 4406 110 186.54006 12.92421 0.82 −7.178 ± 0.060 −8.089 ± 0.049 3.88 ± 0.25 0.95<br />
NGC 4406 111 186.54651 12.92964 0.58 −8.634 ± 0.023 −10.000 ± 0.021 1.98 ± 0.15 1.00<br />
NGC 4406 112 186.56673 12.94627 0.60 −9.344 ± 0.026 −10.554 ± 0.017 2.53 ± 0.22 1.00<br />
NGC 4406 113 186.56018 12.94130 0.42 −9.192 ± 0.026 −10.637 ± 0.033 2.27 ± 0.21 1.00<br />
NGC 4406 114 186.53796 12.92329 0.88 −8.136 ± 0.033 −9.195 ± 0.019 1.97 ± 0.10 1.00<br />
NGC 4406 115 186.55496 12.93723 0.37 −10.444 ± 0.019 −11.569 ± 0.015 3.42 ± 0.11 1.00<br />
NGC 4406 116 186.55630 12.93831 0.37 −7.214 ± 0.044 −8.248 ± 0.068 2.37 ± 0.36 0.99<br />
NGC 4406 117 186.55076 12.93397 0.43 −6.837 ± 0.033 −8.146 ± 0.049 2.87 ± 0.31 0.99<br />
NGC 4406 121 186.55780 12.94017 0.37 −7.566 ± 0.037 −8.632 ± 0.034 1.92 ± 0.28 1.00<br />
NGC 4406 122 186.56093 12.94278 0.42 −9.078 ± 0.019 −10.123 ± 0.014 2.57 ± 0.11 1.00<br />
NGC 4406 125 186.53571 12.92245 0.94 −5.015 ± 0.155 −6.322 ± 0.142 2.90 ± 0.77 0.88<br />
NGC 4406 128 186.56421 12.94624 0.51 −9.084 ± 0.026 −10.134 ± 0.016 2.49 ± 0.12 1.00<br />
NGC 4406 129 186.55444 12.93905 0.31 −6.853 ± 0.068 −7.967 ± 0.083 1.87 ± 0.51 0.96<br />
NGC 4406 133 186.55563 12.94074 0.30 −6.048 ± 0.056 −7.351 ± 0.073 3.18 ± 0.28 0.93<br />
NGC 4406 134 186.57431 12.95594 0.92 −6.909 ± 0.046 −8.057 ± 0.057 3.51 ± 0.34 0.96<br />
NGC 4406 137 186.55257 12.93835 0.30 −7.351 ± 0.038 −8.415 ± 0.078 4.22 ± 0.37 1.00<br />
NGC 4406 138 186.54666 12.93362 0.44 −6.853 ± 0.085 −8.092 ± 0.078 3.80 ± 0.42 0.95<br />
NGC 4406 140 186.53325 12.92286 0.97 −7.691 ± 0.035 −8.601 ± 0.028 2.53 ± 0.19 1.00<br />
NGC 4406 142 186.54195 12.93008 0.61 −8.249 ± 0.028 −9.570 ± 0.019 1.80 ± 0.16 1.00<br />
NGC 4406 144 186.53860 12.92762 0.73 −6.861 ± 0.022 −7.920 ± 0.022 2.87 ± 0.19 0.98<br />
Continued on Next Page. . .<br />
327
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4406 145 186.57525 12.95752 0.97 −6.523 ± 0.067 −7.786 ± 0.029 2.70 ± 0.38 0.98<br />
NGC 4406 146 186.56539 12.94964 0.57 −6.215 ± 0.068 −7.348 ± 0.368 2.25 ± 0.37 0.96<br />
NGC 4406 147 186.55329 12.94017 0.26 −7.231 ± 0.077 −8.445 ± 0.053 2.95 ± 0.26 1.00<br />
NGC 4406 149 186.57465 12.95840 0.96 −6.546 ± 0.097 −7.500 ± 0.100 4.21 ± 0.61 0.81<br />
NGC 4406 151 186.56833 12.95349 0.70 −9.263 ± 0.028 −10.152 ± 0.031 8.61 ± 0.17 0.61<br />
NGC 4406 153 186.56651 12.95216 0.63 −10.305 ± 0.023 −11.432 ± 0.015 2.88 ± 0.16 1.00<br />
NGC 4406 155 186.56087 12.94753 0.40 −5.278 ± 1.302 −6.225 ± 0.940 2.29 ± 43.58 0.88<br />
NGC 4406 157 186.53813 12.92923 0.69 −6.514 ± 0.063 −7.663 ± 0.060 3.22 ± 0.32 0.96<br />
NGC 4406 159 186.56948 12.95473 0.75 −5.778 ± 0.068 −6.371 ± 0.120 3.27 ± 0.37 0.84<br />
NGC 4406 162 186.54872 12.93759 0.30 −7.347 ± 0.046 −8.432 ± 0.075 4.13 ± 0.38 1.00<br />
NGC 4406 163 186.56021 12.94730 0.38 −7.103 ± 0.056 −8.286 ± 0.077 3.11 ± 0.49 1.00<br />
NGC 4406 165 186.57521 12.95974 1.00 −9.690 ± 0.049 −10.573 ± 0.051 8.27 ± 0.31 0.78<br />
NGC 4406 166 186.56035 12.94783 0.39 −8.758 ± 0.027 −9.539 ± 0.018 2.00 ± 0.22 1.00<br />
NGC 4406 167 186.54259 12.93361 0.49 −8.475 ± 0.025 −9.353 ± 0.021 3.09 ± 0.16 1.00<br />
NGC 4406 168 186.56103 12.94858 0.42 −5.877 ± 0.127 −7.518 ± 0.165 4.89 ± 1.04 0.67<br />
NGC 4406 169 186.54240 12.93357 0.49 −7.617 ± 0.032 −8.851 ± 0.027 2.79 ± 0.19 1.00<br />
NGC 4406 170 186.56085 12.94864 0.41 −8.901 ± 0.024 −10.125 ± 0.014 1.66 ± 0.15 0.92<br />
NGC 4406 171 186.54924 12.93920 0.24 −8.064 ± 0.024 −9.246 ± 0.019 2.51 ± 0.22 1.00<br />
NGC 4406 173 186.54985 12.93983 0.22 −7.525 ± 0.045 −8.162 ± 0.048 3.15 ± 0.35 0.98<br />
NGC 4406 174 186.54936 12.93953 0.23 −9.445 ± 0.015 −10.458 ± 0.031 2.56 ± 0.18 1.00<br />
NGC 4406 176 186.54348 12.93496 0.43 −7.636 ± 0.034 −8.693 ± 0.036 2.53 ± 0.27 1.00<br />
NGC 4406 178 186.56824 12.95533 0.72 −7.468 ± 0.061 −8.157 ± 0.035 4.78 ± 0.32 0.90<br />
NGC 4406 180 186.55751 12.94680 0.29 −6.322 ± 0.077 −7.889 ± 0.073 4.25 ± 0.35 0.91<br />
NGC 4406 183 186.54745 12.93875 0.26 −7.041 ± 0.061 −7.724 ± 0.044 2.34 ± 0.33 0.98<br />
NGC 4406 184 186.55888 12.94834 0.34 −8.632 ± 0.025 −9.457 ± 0.036 4.58 ± 0.14 1.00<br />
NGC 4406 185 186.53760 12.93108 0.65 −5.437 ± 0.229 −6.154 ± 0.938 1.46 ± 39.95 0.72<br />
NGC 4406 186 186.57053 12.95788 0.83 −8.706 ± 0.024 −9.809 ± 0.018 1.79 ± 0.15 1.00<br />
NGC 4406 188 186.54860 12.94009 0.21 −7.683 ± 0.044 −9.118 ± 0.048 4.62 ± 0.25 1.00<br />
NGC 4406 190 186.55392 12.94472 0.18 −7.727 ± 0.039 −8.819 ± 0.062 2.66 ± 0.33 1.00<br />
NGC 4406 193 186.56948 12.95755 0.80 −7.157 ± 0.047 −8.231 ± 0.045 3.45 ± 0.27 0.97<br />
NGC 4406 195 186.56011 12.95003 0.40 −8.308 ± 0.021 −9.352 ± 0.046 3.31 ± 0.27 1.00<br />
NGC 4406 196 186.54437 12.93729 0.35 −5.330 ± 0.706 −7.175 ± 0.584 1.38 ± 0.95 0.67<br />
NGC 4406 197 186.53358 12.92870 0.80 −7.143 ± 0.040 −8.268 ± 0.038 2.26 ± 0.22 0.99<br />
NGC 4406 199 186.56313 12.95292 0.53 −7.091 ± 0.030 −8.333 ± 0.207 2.39 ± 0.30 1.00<br />
NGC 4406 200 186.55539 12.94672 0.22 −9.351 ± 0.019 −10.315 ± 0.022 2.38 ± 0.13 1.00<br />
NGC 4406 201 186.53826 12.93276 0.59 −6.924 ± 0.029 −8.375 ± 0.035 1.90 ± 0.17 1.00<br />
NGC 4406 202 186.53444 12.92979 0.75 −8.474 ± 0.023 −9.383 ± 0.017 2.10 ± 0.14 1.00<br />
NGC 4406 203 186.56158 12.95204 0.47 −7.161 ± 0.059 −8.326 ± 0.073 3.33 ± 0.34 1.00<br />
NGC 4406 204 186.56537 12.95535 0.64 −8.266 ± 0.052 −9.112 ± 0.032 4.90 ± 0.23 1.00<br />
NGC 4406 205 186.54350 12.93766 0.35 −8.110 ± 0.021 −9.270 ± 0.020 2.58 ± 0.14 1.00<br />
NGC 4406 206 186.55186 12.94449 0.12 −7.075 ± 0.613 −8.335 ± 0.270 1.50 ± 0.52 0.87<br />
NGC 4406 207 186.56895 12.95847 0.80 −9.288 ± 0.022 −10.317 ± 0.027 3.51 ± 0.20 1.00<br />
NGC 4406 209 186.54694 12.94087 0.20 −9.908 ± 0.020 −10.798 ± 0.014 4.08 ± 0.09 1.00<br />
NGC 4406 210 186.55604 12.94834 0.25 −7.081 ± 0.061 −8.060 ± 0.093 4.55 ± 0.51 0.91<br />
NGC 4406 211 186.52918 12.92668 0.95 −7.212 ± 0.042 −8.525 ± 0.045 2.90 ± 0.31 1.00<br />
NGC 4406 212 186.55699 12.94933 0.29 −7.566 ± 0.031 −8.477 ± 0.047 2.35 ± 0.31 1.00<br />
NGC 4406 214 186.53579 12.93216 0.66 −7.408 ± 0.044 −8.251 ± 0.049 3.12 ± 0.26 0.98<br />
NGC 4406 215 186.54971 12.94351 0.10 −8.777 ± 0.031 −9.731 ± 0.028 2.19 ± 0.27 1.00<br />
NGC 4406 216 186.54030 12.93602 0.46 −7.392 ± 0.038 −8.442 ± 0.026 2.09 ± 0.22 1.00<br />
NGC 4406 218 186.54443 12.93958 0.28 −11.520 ± 0.034 −13.051 ± 0.016 8.11 ± 0.23 1.00<br />
NGC 4406 220 186.55468 12.94797 0.20 −9.360 ± 0.017 −10.351 ± 0.016 2.51 ± 0.20 1.00<br />
NGC 4406 221 186.55048 12.94459 0.08 −8.470 ± 0.022 −9.537 ± 0.029 2.29 ± 0.18 1.00<br />
NGC 4406 222 186.55565 12.94884 0.24 −7.012 ± 0.106 −8.046 ± 0.132 2.12 ± 0.43 0.98<br />
NGC 4406 223 186.53602 12.93294 0.63 −9.300 ± 0.026 −10.512 ± 0.014 2.46 ± 0.12 1.00<br />
NGC 4406 225 186.55932 12.95201 0.40 −6.511 ± 0.107 −7.783 ± 0.189 5.67 ± 1.22 0.62<br />
NGC 4406 228 186.53757 12.93473 0.55 −8.208 ± 0.081 −9.408 ± 0.052 2.63 ± 0.34 1.00<br />
NGC 4406 229 186.56192 12.95474 0.53 −8.787 ± 0.019 −9.677 ± 0.023 2.84 ± 0.14 1.00<br />
NGC 4406 230 186.56750 12.95928 0.77 −5.594 ± 0.173 −7.446 ± 0.283 5.02 ± 5.84 0.60<br />
NGC 4406 231 186.56505 12.95748 0.67 −8.770 ± 0.021 −9.595 ± 0.027 3.02 ± 0.14 1.00<br />
NGC 4406 232 186.54766 12.94352 0.10 −7.299 ± 0.066 −8.663 ± 0.085 3.51 ± 0.47 1.00<br />
NGC 4406 235 186.55847 12.95266 0.39 −9.349 ± 0.023 −10.532 ± 0.018 2.31 ± 0.13 1.00<br />
NGC 4406 236 186.55176 12.94717 0.10 −7.345 ± 0.067 −8.354 ± 0.107 2.57 ± 0.63 1.00<br />
Continued on Next Page. . .<br />
328
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4406 237 186.56647 12.95917 0.74 −7.950 ± 0.082 −9.377 ± 0.038 6.30 ± 0.46 0.96<br />
NGC 4406 244 186.53182 12.93145 0.77 −7.067 ± 0.047 −8.261 ± 0.034 2.24 ± 0.25 0.99<br />
NGC 4406 246 186.53380 12.93277 0.69 −8.299 ± 0.034 −9.623 ± 0.023 2.32 ± 0.18 1.00<br />
NGC 4406 248 186.56770 12.96085 0.81 −6.229 ± 0.051 −7.362 ± 0.121 3.78 ± 0.47 0.84<br />
NGC 4406 249 186.56959 12.96248 0.90 −6.864 ± 0.039 −7.934 ± 0.044 3.00 ± 0.22 0.98<br />
NGC 4406 251 186.55893 12.95401 0.43 −6.399 ± 0.059 −7.869 ± 0.081 3.34 ± 0.43 0.96<br />
NGC 4406 252 186.55861 12.95380 0.42 −8.457 ± 0.033 −9.486 ± 0.023 1.84 ± 0.21 1.00<br />
NGC 4406 253 186.52973 12.93048 0.85 −8.678 ± 0.032 −10.030 ± 0.018 2.27 ± 0.18 1.00<br />
NGC 4406 254 186.55764 12.95307 0.38 −5.105 ± 0.157 −6.735 ± 0.179 3.94 ± 0.95 0.68<br />
NGC 4406 256 186.56221 12.95714 0.59 −7.186 ± 0.053 −8.065 ± 0.116 5.13 ± 0.72 0.82<br />
NGC 4406 258 186.55413 12.95099 0.24 −9.868 ± 0.016 −10.871 ± 0.024 3.44 ± 0.17 1.00<br />
NGC 4406 260 186.54738 12.94571 0.06 −6.995 ± 0.271 −8.235 ± 0.268 4.56 ± 2.42 0.94<br />
NGC 4406 261 186.56712 12.96200 0.82 −8.476 ± 0.042 −9.316 ± 0.031 3.59 ± 0.26 1.00<br />
NGC 4406 262 186.54107 12.94067 0.33 −7.941 ± 0.024 −8.856 ± 0.037 2.95 ± 0.18 1.00<br />
NGC 4406 263 186.56178 12.95766 0.59 −6.489 ± 0.051 −7.468 ± 0.073 2.07 ± 0.51 0.95<br />
NGC 4406 264 186.56485 12.96037 0.73 −7.039 ± 0.126 −7.884 ± 0.320 2.92 ± 0.51 0.98<br />
NGC 4406 265 186.55315 12.95092 0.22 −8.082 ± 0.021 −9.021 ± 0.279 1.33 ± 0.25 0.77<br />
NGC 4406 266 186.55057 12.94897 0.11 −7.893 ± 0.273 −8.891 ± 0.041 1.35 ± 0.24 0.78<br />
NGC 4406 267 186.54145 12.94170 0.30 −7.201 ± 0.055 −8.145 ± 0.063 3.15 ± 0.35 0.98<br />
NGC 4406 268 186.54974 12.94843 0.08 −7.677 ± 0.071 −8.813 ± 0.047 2.80 ± 0.31 1.00<br />
NGC 4406 269 186.56149 12.95809 0.59 −9.290 ± 0.029 −10.189 ± 0.023 3.44 ± 0.22 1.00<br />
NGC 4406 270 186.55139 12.94998 0.15 −7.456 ± 0.049 −8.820 ± 0.048 3.18 ± 0.22 1.00<br />
NGC 4406 272 186.53662 12.93820 0.50 −7.719 ± 0.050 −9.118 ± 0.118 7.23 ± 0.69 0.75<br />
NGC 4406 273 186.56235 12.95919 0.64 −8.305 ± 0.019 −9.468 ± 0.020 2.22 ± 0.18 1.00<br />
NGC 4406 275 186.53917 12.94048 0.39 −6.484 ± 0.078 −7.532 ± 0.193 3.20 ± 0.41 0.95<br />
NGC 4406 276 186.56583 12.96216 0.79 −5.706 ± 0.540 −6.532 ± 0.439 3.36 ± 2.36 0.82<br />
NGC 4406 277 186.54796 12.94783 0.06 −8.154 ± 0.043 −9.563 ± 0.051 2.44 ± 0.25 1.00<br />
NGC 4406 278 186.56819 12.96446 0.90 −6.217 ± 0.052 −7.466 ± 0.601 2.19 ± 0.61 0.96<br />
NGC 4406 279 186.54130 12.94266 0.29 −6.614 ± 0.066 −7.562 ± 0.089 3.79 ± 0.56 0.89<br />
NGC 4406 283 186.53171 12.93543 0.69 −9.345 ± 0.026 −10.338 ± 0.012 3.06 ± 0.16 1.00<br />
NGC 4406 284 186.55191 12.95198 0.22 −10.499 ± 0.031 −11.481 ± 0.022 5.32 ± 0.10 0.82<br />
NGC 4406 287 186.53605 12.93924 0.50 −5.903 ± 0.091 −7.487 ± 0.072 3.32 ± 0.47 0.93<br />
NGC 4406 288 186.53667 12.94002 0.47 −8.319 ± 0.023 −9.164 ± 0.025 2.80 ± 0.14 1.00<br />
NGC 4406 289 186.56913 12.96648 0.98 −8.823 ± 0.036 −9.702 ± 0.055 5.74 ± 0.28 0.99<br />
NGC 4406 290 186.55577 12.95563 0.40 −6.610 ± 0.057 −7.725 ± 0.080 2.97 ± 0.38 0.97<br />
NGC 4406 292 186.54317 12.94546 0.20 −8.410 ± 0.026 −9.256 ± 0.028 2.91 ± 0.13 1.00<br />
NGC 4406 293 186.56590 12.96414 0.84 −6.566 ± 0.068 −7.277 ± 0.379 1.48 ± 0.37 0.74<br />
NGC 4406 294 186.54892 12.95044 0.15 −7.216 ± 0.082 −7.720 ± 0.398 3.41 ± 2.83 0.95<br />
NGC 4406 295 186.56355 12.96213 0.74 −6.102 ± 0.121 −6.746 ± 0.094 4.37 ± 0.53 0.52<br />
NGC 4406 296 186.54267 12.94545 0.21 −8.329 ± 0.054 −9.141 ± 0.058 3.91 ± 0.33 1.00<br />
NGC 4406 298 186.55986 12.95947 0.59 −8.645 ± 0.022 −9.924 ± 0.020 1.97 ± 0.20 1.00<br />
NGC 4406 299 186.54861 12.95039 0.14 −9.018 ± 0.041 −10.165 ± 0.032 4.44 ± 0.18 1.00<br />
NGC 4406 300 186.54631 12.94848 0.12 −8.352 ± 0.032 −9.419 ± 0.024 2.38 ± 0.20 1.00<br />
NGC 4406 303 186.56102 12.96056 0.64 −8.160 ± 0.022 −8.977 ± 0.026 2.67 ± 0.20 1.00<br />
NGC 4406 305 186.54456 12.94746 0.15 −8.032 ± 0.037 −9.117 ± 0.038 3.95 ± 0.29 1.00<br />
NGC 4406 306 186.55069 12.95265 0.23 −5.335 ± 0.303 −7.149 ± 0.186 4.08 ± 0.93 0.73<br />
NGC 4406 307 186.55954 12.95994 0.59 −5.188 ± 0.171 −6.386 ± 0.534 2.60 ± 0.80 0.88<br />
NGC 4406 309 186.56268 12.96264 0.73 −7.520 ± 0.062 −8.715 ± 0.116 5.46 ± 1.06 0.93<br />
NGC 4406 310 186.55733 12.95835 0.51 −6.865 ± 0.233 −8.229 ± 0.289 1.57 ± 0.30 0.90<br />
NGC 4406 311 186.55531 12.95677 0.42 −7.959 ± 0.042 −9.056 ± 0.017 1.95 ± 0.19 1.00<br />
NGC 4406 315 186.54831 12.95139 0.18 −7.338 ± 0.029 −8.375 ± 0.076 3.34 ± 0.37 1.00<br />
NGC 4406 316 186.56076 12.96173 0.67 −7.168 ± 0.191 −7.988 ± 0.108 6.15 ± 1.20 0.64<br />
NGC 4406 317 186.56469 12.96497 0.84 −7.206 ± 0.060 −8.009 ± 0.042 2.72 ± 0.34 0.99<br />
NGC 4406 318 186.56001 12.96113 0.64 −6.127 ± 0.087 −7.555 ± 0.056 5.55 ± 0.35 0.52<br />
NGC 4406 319 186.55895 12.96029 0.59 −5.061 ± 0.339 −6.356 ± 0.173 4.01 ± 1.66 0.64<br />
NGC 4406 321 186.56517 12.96545 0.86 −8.109 ± 0.038 −8.981 ± 0.038 3.35 ± 0.24 1.00<br />
NGC 4406 322 186.54612 12.94930 0.14 −6.541 ± 0.286 −7.832 ± 0.162 2.03 ± 0.39 0.97<br />
NGC 4406 323 186.56251 12.96344 0.75 −8.925 ± 0.026 −9.732 ± 0.023 3.58 ± 0.12 1.00<br />
NGC 4406 327 186.52663 12.93447 0.86 −7.727 ± 0.042 −8.854 ± 0.027 2.35 ± 0.26 1.00<br />
NGC 4406 332 186.53366 12.94126 0.54 −7.546 ± 0.055 −8.828 ± 0.031 1.91 ± 0.31 1.00<br />
NGC 4406 334 186.56038 12.96352 0.71 −7.804 ± 0.028 −8.759 ± 0.037 3.63 ± 0.25 1.00<br />
NGC 4406 336 186.56221 12.96524 0.80 −6.906 ± 0.460 −8.241 ± 0.044 3.13 ± 0.54 0.98<br />
Continued on Next Page. . .<br />
329
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4406 337 186.54494 12.95142 0.22 −6.897 ± 0.048 −8.193 ± 0.081 2.24 ± 0.36 0.99<br />
NGC 4406 341 186.55365 12.95924 0.48 −7.753 ± 0.029 −9.043 ± 0.021 1.92 ± 0.19 1.00<br />
NGC 4406 342 186.55574 12.96131 0.57 −6.658 ± 0.084 −7.726 ± 0.113 3.34 ± 0.60 0.95<br />
NGC 4406 343 186.56032 12.96516 0.76 −7.443 ± 0.074 −8.223 ± 0.069 4.91 ± 0.37 0.90<br />
NGC 4406 345 186.53398 12.94388 0.51 −6.310 ± 0.057 −7.340 ± 0.059 2.56 ± 0.37 0.96<br />
NGC 4406 346 186.54581 12.95366 0.28 −6.557 ± 0.050 −7.634 ± 0.090 2.77 ± 0.43 0.97<br />
NGC 4406 349 186.53238 12.94309 0.57 −9.258 ± 0.021 −10.407 ± 0.013 3.33 ± 0.14 1.00<br />
NGC 4406 352 186.56074 12.96624 0.80 −8.634 ± 0.035 −9.433 ± 0.018 2.85 ± 0.18 1.00<br />
NGC 4406 353 186.53658 12.94690 0.42 −9.367 ± 0.030 −10.191 ± 0.030 6.86 ± 0.15 1.00<br />
NGC 4406 354 186.52382 12.93664 0.91 −6.942 ± 0.055 −7.911 ± 0.100 4.27 ± 0.51 0.91<br />
NGC 4406 356 186.56056 12.96657 0.81 −7.216 ± 0.051 −8.004 ± 0.057 4.38 ± 0.28 0.92<br />
NGC 4406 358 186.52829 12.94070 0.72 −6.465 ± 0.055 −7.242 ± 0.046 2.66 ± 0.36 0.95<br />
NGC 4406 360 186.53552 12.94658 0.45 −6.297 ± 0.057 −7.187 ± 0.118 2.79 ± 0.67 0.94<br />
NGC 4406 361 186.55870 12.96548 0.74 −8.223 ± 0.030 −9.094 ± 0.019 2.72 ± 0.14 1.00<br />
NGC 4406 364 186.55139 12.95983 0.48 −8.551 ± 0.024 −10.065 ± 0.037 2.06 ± 0.26 1.00<br />
NGC 4406 365 186.52885 12.94147 0.70 −5.341 ± 0.099 −6.709 ± 0.090 2.98 ± 0.53 0.88<br />
NGC 4406 366 186.55932 12.96637 0.78 −5.200 ± 0.103 −6.515 ± 0.207 4.05 ± 0.70 0.62<br />
NGC 4406 369 186.53953 12.95051 0.35 −8.129 ± 0.030 −9.111 ± 0.044 3.38 ± 0.25 1.00<br />
NGC 4406 370 186.56065 12.96801 0.85 −8.573 ± 0.025 −9.757 ± 0.023 2.73 ± 0.21 1.00<br />
NGC 4406 371 186.55788 12.96596 0.75 −10.752 ± 0.086 −11.684 ± 0.023 6.57 ± 0.68 1.00<br />
NGC 4406 372 186.55371 12.96241 0.58 −6.971 ± 0.031 −8.162 ± 0.023 2.03 ± 0.26 0.98<br />
NGC 4406 373 186.53483 12.94729 0.48 −9.102 ± 0.015 −10.052 ± 0.016 3.43 ± 0.11 1.00<br />
NGC 4406 374 186.52126 12.93626 1.00 −8.739 ± 0.021 −9.897 ± 0.028 1.83 ± 0.25 1.00<br />
NGC 4406 375 186.54035 12.95188 0.35 −8.566 ± 0.024 −9.465 ± 0.031 3.02 ± 0.17 1.00<br />
NGC 4406 377 186.54272 12.95381 0.34 −7.552 ± 0.145 −8.717 ± 0.289 2.16 ± 0.40 1.00<br />
NGC 4406 378 186.54217 12.95351 0.34 −9.347 ± 0.055 −10.233 ± 0.069 10.25 ± 0.54 0.87<br />
NGC 4406 379 186.55450 12.96341 0.62 −5.782 ± 0.674 −6.847 ± 0.820 1.27 ± 0.70 0.56<br />
NGC 4406 380 186.54968 12.95964 0.46 −7.464 ± 0.066 −8.380 ± 0.069 5.18 ± 0.33 0.91<br />
NGC 4406 381 186.54164 12.95316 0.34 −8.153 ± 0.023 −9.590 ± 0.022 2.10 ± 0.13 1.00<br />
NGC 4406 382 186.55476 12.96386 0.64 −6.677 ± 0.095 −7.682 ± 0.050 5.75 ± 0.37 0.56<br />
NGC 4406 383 186.53107 12.94472 0.60 −6.004 ± 0.228 −7.005 ± 0.119 3.64 ± 0.63 0.79<br />
NGC 4406 384 186.54096 12.95287 0.35 −6.567 ± 0.113 −7.715 ± 0.042 2.22 ± 0.39 0.98<br />
NGC 4406 385 186.53595 12.94885 0.45 −7.767 ± 0.052 −8.631 ± 0.049 1.98 ± 0.37 1.00<br />
NGC 4406 386 186.54081 12.95292 0.36 −7.036 ± 0.090 −8.049 ± 0.086 3.48 ± 0.39 0.96<br />
NGC 4406 387 186.54541 12.95667 0.38 −6.979 ± 0.034 −8.074 ± 0.091 3.53 ± 0.44 0.96<br />
NGC 4406 388 186.55259 12.96266 0.58 −7.791 ± 0.022 −8.600 ± 0.024 2.48 ± 0.24 1.00<br />
NGC 4406 389 186.52855 12.94320 0.70 −9.030 ± 0.020 −10.320 ± 0.015 1.81 ± 0.10 1.00<br />
NGC 4406 390 186.53542 12.94876 0.46 −5.358 ± 0.293 −7.063 ± 0.228 2.49 ± 2.14 0.95<br />
NGC 4406 392 186.54523 12.95690 0.39 −8.858 ± 0.017 −9.874 ± 0.018 2.20 ± 0.16 1.00<br />
NGC 4406 393 186.54203 12.95436 0.37 −7.006 ± 0.048 −8.209 ± 0.042 2.50 ± 0.31 0.99<br />
NGC 4406 394 186.56100 12.97000 0.92 −7.898 ± 0.038 −8.702 ± 0.037 3.93 ± 0.28 1.00<br />
NGC 4406 396 186.56353 12.97242 1.03 −6.405 ± 0.054 −7.305 ± 0.088 2.55 ± 0.46 0.96<br />
NGC 4406 397 186.55601 12.96633 0.74 −7.073 ± 0.048 −7.950 ± 0.044 2.54 ± 0.27 0.99<br />
NGC 4406 398 186.54700 12.95906 0.45 −5.761 ± 0.106 −7.046 ± 0.523 1.86 ± 2.69 0.87<br />
NGC 4406 399 186.54105 12.95473 0.40 −7.760 ± 0.046 −8.522 ± 0.064 3.27 ± 0.47 1.00<br />
NGC 4406 402 186.55349 12.96557 0.69 −5.104 ± 0.493 −6.156 ± 0.120 4.06 ± 2.68 0.65<br />
NGC 4406 403 186.54544 12.95923 0.46 −8.584 ± 0.021 −9.355 ± 0.018 2.21 ± 0.19 1.00<br />
NGC 4406 404 186.56224 12.97295 1.03 −8.173 ± 0.038 −9.190 ± 0.044 4.96 ± 0.24 1.00<br />
NGC 4406 405 186.54892 12.96212 0.55 −7.384 ± 0.085 −8.906 ± 0.082 6.69 ± 0.51 0.76<br />
NGC 4406 406 186.55760 12.96924 0.85 −7.674 ± 0.033 −8.592 ± 0.038 3.87 ± 0.25 1.00<br />
NGC 4406 407 186.53839 12.95365 0.44 −7.196 ± 0.029 −8.523 ± 0.023 2.38 ± 0.28 1.00<br />
NGC 4406 409 186.53866 12.95403 0.44 −6.972 ± 0.052 −8.047 ± 0.064 2.48 ± 0.32 0.99<br />
NGC 4406 410 186.53709 12.95304 0.46 −6.326 ± 0.123 −7.370 ± 0.148 5.05 ± 1.06 0.55<br />
NGC 4406 412 186.52769 12.94553 0.72 −7.576 ± 0.027 −8.688 ± 0.041 2.91 ± 0.23 1.00<br />
NGC 4406 413 186.53444 12.95129 0.52 −7.648 ± 0.025 −8.531 ± 0.051 3.39 ± 0.28 1.00<br />
NGC 4406 414 186.52621 12.94471 0.77 −7.440 ± 0.081 −8.899 ± 0.099 6.42 ± 0.67 0.80<br />
NGC 4406 415 186.53264 12.94995 0.56 −6.439 ± 0.072 −7.275 ± 0.062 2.03 ± 0.46 0.93<br />
NGC 4406 416 186.53165 12.94919 0.59 −6.603 ± 0.044 −7.580 ± 0.075 2.98 ± 0.29 0.96<br />
NGC 4406 417 186.55400 12.96742 0.75 −7.686 ± 0.057 −8.696 ± 0.035 3.25 ± 0.31 1.00<br />
NGC 4406 418 186.55379 12.96734 0.75 −6.185 ± 0.059 −7.766 ± 0.053 2.45 ± 0.46 0.98<br />
NGC 4406 419 186.55113 12.96560 0.67 −6.310 ± 0.090 −7.174 ± 0.149 3.93 ± 0.69 0.77<br />
NGC 4406 420 186.55316 12.96740 0.75 −8.025 ± 0.043 −8.847 ± 0.041 4.56 ± 0.20 1.00<br />
Continued on Next Page. . .<br />
330
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4406 421 186.55383 12.96823 0.78 −6.143 ± 0.055 −7.564 ± 0.087 5.60 ± 0.38 0.52<br />
NGC 4406 427 186.55484 12.96999 0.85 −7.725 ± 0.023 −9.081 ± 0.053 5.11 ± 0.35 0.99<br />
NGC 4406 430 186.52487 12.94611 0.81 −6.328 ± 0.065 −7.496 ± 0.057 2.43 ± 0.31 0.97<br />
NGC 4406 431 186.52973 12.95020 0.66 −8.323 ± 0.030 −9.217 ± 0.030 3.60 ± 0.19 1.00<br />
NGC 4406 432 186.54635 12.96408 0.62 −7.545 ± 0.045 −8.202 ± 0.034 2.66 ± 0.24 0.99<br />
NGC 4406 435 186.53378 12.95427 0.58 −6.979 ± 0.336 −8.184 ± 0.347 1.68 ± 0.42 0.93<br />
NGC 4406 437 186.53777 12.95773 0.55 −7.304 ± 0.089 −8.712 ± 0.106 7.57 ± 0.71 0.50<br />
NGC 4406 439 186.55446 12.97139 0.89 −8.827 ± 0.029 −9.893 ± 0.023 2.12 ± 0.23 1.00<br />
NGC 4406 440 186.53458 12.95525 0.58 −6.741 ± 0.055 −7.459 ± 0.259 2.06 ± 0.38 0.95<br />
NGC 4406 442 186.53339 12.95455 0.60 −6.977 ± 0.034 −8.443 ± 0.058 3.18 ± 0.30 1.00<br />
NGC 4406 443 186.54091 12.96072 0.57 −7.506 ± 0.976 −9.057 ± 1.047 1.06 ± 0.31 0.53<br />
NGC 4406 444 186.53984 12.95987 0.56 −7.970 ± 0.022 −8.873 ± 0.046 2.22 ± 0.21 1.00<br />
NGC 4406 445 186.52591 12.94874 0.78 −5.511 ± 0.196 −7.299 ± 0.153 4.98 ± 0.93 0.53<br />
NGC 4406 446 186.53282 12.95442 0.61 −8.111 ± 0.030 −9.111 ± 0.027 2.45 ± 0.18 1.00<br />
NGC 4406 449 186.52156 12.94555 0.92 −6.020 ± 0.040 −7.371 ± 0.050 1.58 ± 0.34 0.81<br />
NGC 4406 450 186.54945 12.96837 0.77 −7.965 ± 0.027 −8.875 ± 0.023 2.54 ± 0.17 1.00<br />
NGC 4406 455 186.51648 12.94242 1.10 −7.764 ± 0.030 −8.569 ± 0.023 2.34 ± 0.20 1.00<br />
NGC 4406 459 186.52362 12.94869 0.86 −7.757 ± 0.034 −8.809 ± 0.029 2.78 ± 0.26 1.00<br />
NGC 4406 460 186.54309 12.96453 0.66 −7.342 ± 0.043 −8.541 ± 0.050 3.96 ± 0.25 1.00<br />
NGC 4406 464 186.53210 12.95598 0.66 −7.152 ± 0.033 −7.925 ± 0.029 1.72 ± 0.22 0.93<br />
NGC 4406 465 186.52679 12.95164 0.77 −4.978 ± 0.186 −6.296 ± 0.147 3.85 ± 0.97 0.71<br />
NGC 4406 469 186.55551 12.97565 1.04 −5.272 ± 0.171 −6.323 ± 0.140 3.26 ± 0.80 0.85<br />
NGC 4406 471 186.52396 12.95085 0.86 −8.248 ± 0.017 −9.178 ± 0.028 2.09 ± 0.16 1.00<br />
NGC 4406 475 186.55428 12.97572 1.04 −7.385 ± 0.044 −8.676 ± 0.034 2.81 ± 0.25 1.00<br />
NGC 4406 478 186.52325 12.95104 0.88 −5.716 ± 0.101 −7.257 ± 0.180 4.52 ± 1.08 0.64<br />
NGC 4406 481 186.53952 12.96457 0.71 −6.259 ± 0.048 −7.532 ± 0.088 3.02 ± 0.34 0.95<br />
NGC 4406 483 186.51961 12.94882 0.99 −7.774 ± 0.025 −9.112 ± 0.018 2.34 ± 0.12 1.00<br />
NGC 4406 484 186.51877 12.94825 1.02 −5.697 ± 0.813 −6.601 ± 0.145 2.52 ± 0.54 0.90<br />
NGC 4406 485 186.52860 12.95637 0.77 −5.957 ± 0.158 −7.535 ± 0.145 3.96 ± 0.89 0.86<br />
NGC 4406 487 186.52519 12.95369 0.84 −6.582 ± 0.058 −8.117 ± 0.044 6.34 ± 0.27 0.62<br />
NGC 4406 488 186.51671 12.94688 1.09 −8.013 ± 0.023 −9.290 ± 0.021 2.83 ± 0.18 1.00<br />
NGC 4406 489 186.54848 12.97265 0.91 −7.133 ± 0.070 −8.388 ± 0.032 4.00 ± 0.28 1.00<br />
NGC 4406 490 186.52664 12.95513 0.81 −5.677 ± 0.592 −6.807 ± 0.094 2.37 ± 0.76 0.92<br />
NGC 4406 491 186.51378 12.94492 1.19 −8.267 ± 0.034 −9.298 ± 0.019 2.64 ± 0.17 1.00<br />
NGC 4406 492 186.53282 12.96043 0.73 −7.958 ± 0.024 −9.203 ± 0.025 1.83 ± 0.16 1.00<br />
NGC 4406 493 186.55128 12.97584 1.03 −7.099 ± 0.035 −7.941 ± 0.069 3.22 ± 0.34 0.97<br />
NGC 4406 494 186.53190 12.96012 0.75 −5.948 ± 0.084 −7.219 ± 0.069 3.19 ± 0.37 0.91<br />
NGC 4406 495 186.54189 12.96829 0.80 −8.695 ± 0.018 −9.723 ± 0.019 2.35 ± 0.12 1.00<br />
NGC 4406 496 186.55618 12.97990 1.19 −6.155 ± 0.088 −7.386 ± 0.048 3.10 ± 0.41 0.94<br />
NGC 4406 497 186.54741 12.97285 0.92 −7.497 ± 0.041 −8.616 ± 0.022 2.79 ± 0.23 1.00<br />
NGC 4406 501 186.54718 12.97309 0.93 −7.960 ± 0.026 −9.177 ± 0.022 2.67 ± 0.18 1.00<br />
NGC 4406 504 186.55409 12.97887 1.14 −8.109 ± 0.765 −9.243 ± 0.836 1.63 ± 0.66 0.90<br />
NGC 4406 507 186.54118 12.96881 0.82 −5.571 ± 0.112 −6.773 ± 0.153 3.80 ± 0.78 0.73<br />
NGC 4406 508 186.53537 12.96420 0.77 −9.657 ± 0.022 −11.048 ± 0.021 2.28 ± 0.13 1.00<br />
NGC 4406 511 186.52158 12.95327 0.95 −6.272 ± 0.062 −7.685 ± 0.060 1.94 ± 0.42 0.95<br />
NGC 4406 512 186.54817 12.97488 0.99 −6.270 ± 0.062 −7.475 ± 0.055 2.39 ± 0.34 0.97<br />
NGC 4406 513 186.54766 12.97472 0.99 −10.865 ± 0.015 −11.893 ± 0.015 4.10 ± 0.14 1.00<br />
NGC 4406 514 186.54359 12.97124 0.88 −7.347 ± 0.030 −8.401 ± 0.055 3.14 ± 0.25 1.00<br />
NGC 4406 516 186.55498 12.98076 1.21 −7.563 ± 0.037 −8.426 ± 0.032 2.85 ± 0.20 1.00<br />
NGC 4406 518 186.54530 12.97316 0.94 −8.995 ± 0.020 −10.200 ± 0.014 2.29 ± 0.11 1.00<br />
NGC 4406 519 186.53880 12.96816 0.83 −7.570 ± 0.033 −9.006 ± 0.034 2.24 ± 0.23 1.00<br />
NGC 4406 521 186.53578 12.96592 0.81 −7.612 ± 0.040 −8.629 ± 0.039 3.52 ± 0.21 1.00<br />
NGC 4406 523 186.53108 12.96237 0.82 −7.755 ± 0.052 −9.237 ± 0.026 3.35 ± 0.30 1.00<br />
NGC 4406 526 186.52115 12.95464 0.98 −8.302 ± 0.026 −9.334 ± 0.020 2.43 ± 0.19 1.00<br />
NGC 4406 531 186.52179 12.95632 0.98 −6.947 ± 0.062 −7.989 ± 0.077 3.94 ± 0.46 0.94<br />
NGC 4406 532 186.52463 12.95875 0.93 −6.797 ± 0.153 −7.820 ± 0.288 1.67 ± 0.35 0.91<br />
NGC 4406 533 186.53215 12.96494 0.86 −8.232 ± 0.041 −9.647 ± 0.021 1.74 ± 0.23 1.00<br />
NGC 4406 534 186.52889 12.96236 0.88 −7.147 ± 0.041 −8.186 ± 0.056 3.58 ± 0.28 0.97<br />
NGC 4406 535 186.52775 12.96156 0.89 −7.073 ± 0.048 −8.307 ± 0.026 2.35 ± 0.20 1.00<br />
NGC 4406 536 186.51360 12.95011 1.20 −5.413 ± 0.195 −6.533 ± 0.370 3.24 ± 1.07 0.84<br />
NGC 4406 537 186.54111 12.97290 0.96 −5.690 ± 0.147 −7.411 ± 0.154 3.99 ± 0.86 0.82<br />
NGC 4406 541 186.54435 12.97604 1.04 −7.816 ± 0.035 −8.790 ± 0.027 4.46 ± 0.15 1.00<br />
Continued on Next Page. . .<br />
331
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4406 547 186.54585 12.97801 1.10 −7.485 ± 0.034 −8.273 ± 0.025 3.20 ± 0.26 0.98<br />
NGC 4406 548 186.51021 12.94911 1.31 −7.390 ± 0.062 −8.173 ± 0.077 5.26 ± 0.34 0.85<br />
NGC 4406 550 186.55092 12.98236 1.25 −6.168 ± 0.052 −6.868 ± 0.056 2.32 ± 0.36 0.93<br />
NGC 4406 551 186.53384 12.96876 0.93 −8.622 ± 0.016 −9.518 ± 0.022 2.89 ± 0.12 1.00<br />
NGC 4406 553 186.52317 12.96020 0.99 −9.639 ± 0.012 −10.589 ± 0.015 2.28 ± 0.10 1.00<br />
NGC 4406 554 186.53742 12.97201 0.97 −6.955 ± 0.035 −7.993 ± 0.065 2.63 ± 0.40 0.99<br />
NGC 4406 555 186.53640 12.97122 0.96 −7.096 ± 0.059 −7.799 ± 0.061 4.24 ± 0.28 0.89<br />
NGC 4406 557 186.51588 12.95501 1.16 −9.396 ± 0.019 −10.293 ± 0.019 2.62 ± 0.15 1.00<br />
NGC 4406 559 186.52699 12.96467 0.98 −5.984 ± 0.076 −7.614 ± 0.152 5.74 ± 0.71 0.52<br />
NGC 4406 560 186.53191 12.96951 0.99 −9.588 ± 0.016 −10.526 ± 0.024 2.92 ± 0.15 1.00<br />
NGC 4406 561 186.51769 12.95798 1.13 −8.245 ± 0.018 −9.354 ± 0.017 2.22 ± 0.14 1.00<br />
NGC 4406 562 186.53520 12.97232 1.01 −5.979 ± 0.090 −7.167 ± 0.061 3.10 ± 0.50 0.91<br />
NGC 4406 563 186.52121 12.96110 1.07 −6.975 ± 0.092 −7.673 ± 0.054 5.25 ± 0.51 0.65<br />
NGC 4406 566 186.52881 12.96776 1.01 −8.618 ± 0.018 −9.526 ± 0.018 3.48 ± 0.16 1.00<br />
NGC 4406 567 186.52894 12.96788 1.01 −7.517 ± 0.040 −8.458 ± 0.041 4.18 ± 0.15 1.00<br />
NGC 4406 568 186.54808 12.98337 1.29 −6.650 ± 0.057 −7.427 ± 0.048 2.69 ± 0.30 0.96<br />
NGC 4406 571 186.54248 12.97959 1.17 −5.479 ± 0.571 −6.439 ± 0.867 3.67 ± 38.38 0.75<br />
NGC 4406 575 186.53681 12.97597 1.11 −6.851 ± 0.041 −7.944 ± 0.076 4.32 ± 0.40 0.91<br />
NGC 4406 578 186.52594 12.96758 1.07 −7.477 ± 0.024 −8.717 ± 0.028 2.67 ± 0.14 1.00<br />
NGC 4406 579 186.54765 12.98533 1.35 −6.838 ± 0.078 −8.371 ± 0.061 6.54 ± 0.41 0.58<br />
NGC 4406 580 186.51938 12.96281 1.15 −8.597 ± 0.028 −9.898 ± 0.018 2.52 ± 0.19 1.00<br />
NGC 4406 581 186.52222 12.96525 1.12 −6.840 ± 0.042 −7.809 ± 0.062 3.18 ± 0.24 0.97<br />
NGC 4406 584 186.53234 12.97446 1.13 −8.035 ± 0.017 −8.974 ± 0.024 2.68 ± 0.15 1.00<br />
NGC 4406 585 186.54246 12.98278 1.28 −8.290 ± 0.015 −9.504 ± 0.016 2.40 ± 0.14 1.00<br />
NGC 4406 586 186.51894 12.96375 1.18 −7.398 ± 0.111 −8.869 ± 0.125 7.94 ± 0.92 0.53<br />
NGC 4406 591 186.51157 12.95874 1.33 −7.904 ± 0.026 −8.919 ± 0.029 3.36 ± 0.16 1.00<br />
NGC 4406 593 186.52128 12.96679 1.17 −5.942 ± 0.421 −6.789 ± 0.114 2.66 ± 0.73 0.91<br />
NGC 4406 596 186.52268 12.96897 1.18 −7.709 ± 0.026 −8.673 ± 0.019 2.16 ± 0.22 1.00<br />
NGC 4406 600 186.52543 12.97170 1.19 −5.974 ± 0.085 −7.314 ± 0.110 1.66 ± 0.36 0.84<br />
NGC 4406 601 186.51347 12.96217 1.32 −8.439 ± 0.018 −9.588 ± 0.028 2.87 ± 0.17 1.00<br />
NGC 4406 602 186.53148 12.97706 1.22 −9.204 ± 0.022 −10.134 ± 0.014 3.31 ± 0.16 1.00<br />
NGC 4406 604 186.51624 12.96509 1.28 −8.720 ± 0.040 −9.997 ± 0.037 4.77 ± 0.19 1.00<br />
NGC 4406 606 186.50763 12.95867 1.46 −7.368 ± 0.072 −8.249 ± 0.064 5.05 ± 0.44 0.90<br />
NGC 4472 3 187.47752 8.01730 1.26 −8.349 ± 0.052 −9.476 ± 0.023 3.58 ± 0.20 1.00<br />
NGC 4472 4 187.46965 8.00037 0.85 −6.214 ± 0.051 −7.085 ± 0.061 2.54 ± 0.41 0.98<br />
NGC 4472 5 187.47403 8.00980 1.05 −5.381 ± 0.056 −6.824 ± 0.176 3.88 ± 1.19 0.86<br />
NGC 4472 7 187.46917 7.99987 0.83 −6.745 ± 0.032 −8.167 ± 0.265 1.78 ± 0.27 1.00<br />
NGC 4472 9 187.47252 8.00762 0.98 −6.134 ± 0.085 −7.227 ± 0.099 3.45 ± 0.58 0.95<br />
NGC 4472 11 187.46522 7.99190 0.76 −7.235 ± 0.030 −8.645 ± 0.022 1.66 ± 0.15 1.00<br />
NGC 4472 13 187.46486 7.99192 0.75 −8.919 ± 0.013 −9.887 ± 0.026 3.20 ± 0.13 1.00<br />
NGC 4472 14 187.46158 7.98474 0.79 −5.632 ± 0.102 −7.373 ± 0.225 5.99 ± 1.60 0.58<br />
NGC 4472 15 187.47543 8.01474 1.16 −8.820 ± 0.020 −9.844 ± 0.021 3.56 ± 0.13 1.00<br />
NGC 4472 17 187.46831 7.99978 0.80 −7.463 ± 0.036 −8.452 ± 0.036 2.34 ± 0.18 1.00<br />
NGC 4472 18 187.46681 7.99685 0.76 −9.523 ± 0.019 −10.885 ± 0.022 2.55 ± 0.14 1.00<br />
NGC 4472 19 187.46245 7.98732 0.76 −7.338 ± 0.040 −8.251 ± 0.065 4.52 ± 0.39 0.98<br />
NGC 4472 20 187.45854 7.97883 0.88 −8.140 ± 0.035 −9.402 ± 0.023 2.54 ± 0.23 1.00<br />
NGC 4472 21 187.46768 7.99791 0.79 −5.908 ± 0.058 −7.061 ± 0.137 3.87 ± 0.75 0.89<br />
NGC 4472 22 187.46765 7.99879 0.78 −8.065 ± 0.099 −8.919 ± 0.192 7.48 ± 1.53 0.83<br />
NGC 4472 23 187.47343 8.01131 1.05 −5.567 ± 0.172 −6.746 ± 0.142 3.64 ± 0.76 0.91<br />
NGC 4472 27 187.46290 7.98895 0.74 −5.940 ± 0.146 −7.075 ± 0.184 4.46 ± 0.96 0.78<br />
NGC 4472 28 187.46202 7.98729 0.74 −7.913 ± 0.025 −9.509 ± 0.033 4.37 ± 0.19 1.00<br />
NGC 4472 29 187.46956 8.00354 0.85 −6.888 ± 0.053 −7.734 ± 0.405 2.29 ± 0.49 1.00<br />
NGC 4472 30 187.47392 8.01303 1.09 −6.644 ± 0.079 −7.861 ± 0.044 3.43 ± 0.31 0.98<br />
NGC 4472 31 187.46440 7.99252 0.72 −7.237 ± 0.054 −8.730 ± 0.030 2.10 ± 0.23 1.00<br />
NGC 4472 32 187.46844 8.00131 0.81 −5.917 ± 0.188 −7.389 ± 0.084 2.24 ± 0.38 0.99<br />
NGC 4472 33 187.45670 7.97650 0.92 −5.046 ± 0.309 −6.619 ± 0.118 4.65 ± 1.49 0.65<br />
NGC 4472 34 187.46997 8.00532 0.88 −8.352 ± 0.018 −9.586 ± 0.015 2.89 ± 0.10 1.00<br />
NGC 4472 36 187.46584 7.99667 0.73 −7.202 ± 0.031 −8.729 ± 0.023 1.88 ± 0.16 1.00<br />
NGC 4472 37 187.45276 7.96881 1.13 −7.350 ± 0.032 −8.798 ± 0.039 2.58 ± 0.22 1.00<br />
NGC 4472 38 187.46969 8.00539 0.87 −7.304 ± 0.037 −8.539 ± 0.033 2.81 ± 0.23 1.00<br />
NGC 4472 39 187.46333 7.99174 0.70 −6.214 ± 0.105 −7.730 ± 0.141 5.55 ± 0.68 0.82<br />
Continued on Next Page. . .<br />
332
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4472 40 187.47049 8.00736 0.91 −6.680 ± 0.053 −8.227 ± 0.028 1.94 ± 0.23 1.00<br />
NGC 4472 43 187.45223 7.96911 1.11 −7.285 ± 0.036 −8.245 ± 0.039 3.35 ± 0.16 1.00<br />
NGC 4472 44 187.45488 7.97549 0.93 −7.775 ± 0.069 −9.177 ± 0.072 6.06 ± 0.44 0.98<br />
NGC 4472 45 187.45746 7.98125 0.79 −5.735 ± 0.150 −6.926 ± 0.117 3.58 ± 1.01 0.92<br />
NGC 4472 46 187.45626 7.97897 0.84 −8.564 ± 0.031 −9.482 ± 0.037 4.13 ± 0.20 1.00<br />
NGC 4472 47 187.47250 8.01419 1.06 −6.847 ± 0.049 −8.082 ± 0.048 3.15 ± 0.27 0.99<br />
NGC 4472 48 187.46530 7.99870 0.70 −6.849 ± 0.054 −7.633 ± 0.043 2.62 ± 0.25 0.99<br />
NGC 4472 49 187.45228 7.97090 1.06 −9.150 ± 0.018 −10.642 ± 0.016 4.05 ± 0.09 1.00<br />
NGC 4472 51 187.46959 8.00835 0.89 −7.392 ± 0.030 −8.849 ± 0.028 2.95 ± 0.16 1.00<br />
NGC 4472 52 187.46283 7.99385 0.66 −7.730 ± 0.034 −9.273 ± 0.029 2.38 ± 0.25 1.00<br />
NGC 4472 55 187.46299 7.99449 0.66 −8.643 ± 0.016 −9.613 ± 0.017 2.05 ± 0.14 1.00<br />
NGC 4472 56 187.46356 7.99590 0.66 −7.937 ± 0.024 −9.449 ± 0.020 2.18 ± 0.16 1.00<br />
NGC 4472 57 187.46349 7.99582 0.66 −5.470 ± 0.239 −7.169 ± 0.143 3.09 ± 0.88 0.97<br />
NGC 4472 58 187.46156 7.99202 0.64 −8.586 ± 0.016 −9.591 ± 0.025 2.10 ± 0.12 1.00<br />
NGC 4472 61 187.46753 8.00561 0.80 −5.421 ± 0.414 −6.912 ± 0.402 2.31 ± 0.82 0.99<br />
NGC 4472 62 187.46735 8.00545 0.79 −5.368 ± 0.129 −7.238 ± 0.126 2.66 ± 0.89 0.98<br />
NGC 4472 66 187.46045 7.99132 0.62 −9.363 ± 0.033 −10.359 ± 0.014 3.06 ± 0.14 1.00<br />
NGC 4472 68 187.47052 8.01439 1.00 −9.732 ± 0.019 −10.699 ± 0.026 3.48 ± 0.10 1.00<br />
NGC 4472 69 187.45908 7.98966 0.62 −7.229 ± 0.044 −8.747 ± 0.035 3.19 ± 0.18 1.00<br />
NGC 4472 70 187.46274 7.99757 0.62 −7.947 ± 0.032 −9.239 ± 0.026 2.17 ± 0.19 1.00<br />
NGC 4472 73 187.46626 8.00532 0.75 −6.640 ± 0.036 −8.311 ± 0.035 2.40 ± 0.26 1.00<br />
NGC 4472 74 187.45472 7.98063 0.77 −8.061 ± 0.017 −9.486 ± 0.026 1.96 ± 0.11 1.00<br />
NGC 4472 75 187.47137 8.01682 1.07 −9.854 ± 0.020 −10.823 ± 0.011 3.93 ± 0.07 1.00<br />
NGC 4472 76 187.45291 7.97718 0.85 −6.623 ± 0.057 −7.661 ± 0.066 2.68 ± 0.26 0.99<br />
NGC 4472 77 187.45386 7.97938 0.79 −8.432 ± 0.018 −9.931 ± 0.013 1.96 ± 0.10 1.00<br />
NGC 4472 78 187.45589 7.98373 0.69 −7.429 ± 0.027 −8.888 ± 0.040 2.23 ± 0.25 1.00<br />
NGC 4472 79 187.45703 7.98636 0.64 −8.884 ± 0.017 −9.790 ± 0.023 2.11 ± 0.12 1.00<br />
NGC 4472 81 187.45920 7.99115 0.59 −5.980 ± 0.045 −7.346 ± 0.209 1.12 ± 0.38 0.85<br />
NGC 4472 82 187.45592 7.98417 0.68 −6.778 ± 0.060 −7.762 ± 0.051 4.36 ± 0.29 0.94<br />
NGC 4472 83 187.45749 7.98762 0.62 −8.780 ± 0.020 −10.037 ± 0.019 1.55 ± 0.09 0.97<br />
NGC 4472 84 187.46798 8.01027 0.86 −5.667 ± 0.093 −7.350 ± 0.090 2.16 ± 0.49 0.99<br />
NGC 4472 85 187.45877 7.99064 0.59 −6.776 ± 0.048 −8.405 ± 0.060 2.41 ± 0.33 1.00<br />
NGC 4472 86 187.45926 7.99195 0.58 −10.449 ± 0.017 −11.670 ± 0.013 3.20 ± 0.14 1.00<br />
NGC 4472 89 187.46809 8.01081 0.87 −5.382 ± 0.239 −6.658 ± 0.349 3.18 ± 0.67 0.95<br />
NGC 4472 91 187.46850 8.01212 0.91 −5.252 ± 0.233 −6.658 ± 0.421 4.93 ± 5.02 0.59<br />
NGC 4472 92 187.45288 7.97886 0.80 −7.230 ± 0.061 −8.011 ± 0.042 3.76 ± 0.20 0.98<br />
NGC 4472 93 187.45970 7.99356 0.56 −5.749 ± 0.066 −7.065 ± 0.080 1.68 ± 0.39 0.96<br />
NGC 4472 94 187.45035 7.97363 0.95 −7.815 ± 0.032 −9.121 ± 0.024 3.24 ± 0.17 1.00<br />
NGC 4472 95 187.44934 7.97175 1.01 −9.427 ± 0.018 −10.311 ± 0.018 5.53 ± 0.07 1.00<br />
NGC 4472 96 187.46840 8.01284 0.91 −6.275 ± 0.104 −7.092 ± 0.105 2.47 ± 0.59 0.99<br />
NGC 4472 97 187.46164 7.99841 0.58 −9.017 ± 0.020 −9.882 ± 0.015 2.04 ± 0.10 1.00<br />
NGC 4472 98 187.45044 7.97426 0.93 −5.394 ± 0.312 −7.067 ± 0.179 2.56 ± 0.92 0.98<br />
NGC 4472 99 187.45716 7.98874 0.59 −6.943 ± 0.052 −7.582 ± 0.086 2.41 ± 0.36 0.99<br />
NGC 4472 100 187.47046 8.01755 1.06 −6.220 ± 0.052 −7.921 ± 0.040 2.37 ± 0.41 1.00<br />
NGC 4472 101 187.45720 7.98923 0.58 −9.005 ± 0.022 −9.903 ± 0.022 3.93 ± 0.15 1.00<br />
NGC 4472 102 187.45706 7.98931 0.57 −7.894 ± 0.025 −9.149 ± 0.017 2.00 ± 0.11 1.00<br />
NGC 4472 103 187.45855 7.99219 0.55 −6.875 ± 0.043 −8.462 ± 0.026 1.72 ± 0.22 1.00<br />
NGC 4472 107 187.45833 7.99248 0.54 −7.817 ± 0.024 −8.747 ± 0.066 3.45 ± 0.21 1.00<br />
NGC 4472 109 187.46356 8.00398 0.65 −9.024 ± 0.016 −10.183 ± 0.018 3.84 ± 0.12 1.00<br />
NGC 4472 110 187.47076 8.01945 1.10 −7.126 ± 0.086 −8.084 ± 0.061 5.43 ± 0.51 0.91<br />
NGC 4472 112 187.46292 8.00342 0.63 −9.640 ± 0.015 −10.626 ± 0.014 2.93 ± 0.09 1.00<br />
NGC 4472 113 187.46421 8.00624 0.69 −8.868 ± 0.018 −10.232 ± 0.015 1.89 ± 0.14 1.00<br />
NGC 4472 114 187.45822 7.99316 0.52 −7.510 ± 0.033 −9.087 ± 0.039 1.99 ± 0.20 1.00<br />
NGC 4472 119 187.44992 7.97634 0.85 −9.432 ± 0.022 −10.723 ± 0.017 2.09 ± 0.09 1.00<br />
NGC 4472 122 187.45640 7.99097 0.51 −6.230 ± 0.509 −7.740 ± 0.382 4.36 ± 5.58 0.94<br />
NGC 4472 123 187.45836 7.99525 0.50 −8.698 ± 0.013 −10.066 ± 0.013 1.73 ± 0.08 1.00<br />
NGC 4472 124 187.46066 8.00036 0.54 −7.055 ± 0.030 −8.293 ± 0.044 2.17 ± 0.23 1.00<br />
NGC 4472 125 187.44936 7.97647 0.85 −6.497 ± 0.079 −7.643 ± 0.065 3.39 ± 0.39 0.98<br />
NGC 4472 126 187.45347 7.98538 0.60 −7.121 ± 0.066 −7.983 ± 0.179 4.00 ± 0.95 0.98<br />
NGC 4472 127 187.44696 7.97150 1.01 −7.547 ± 0.030 −8.404 ± 0.042 2.97 ± 0.20 1.00<br />
NGC 4472 132 187.45489 7.98869 0.53 −6.878 ± 0.149 −7.931 ± 0.086 2.30 ± 2.47 1.00<br />
NGC 4472 133 187.45169 7.98210 0.68 −7.861 ± 0.776 −8.867 ± 0.037 2.18 ± 0.48 1.00<br />
Continued on Next Page. . .<br />
333
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4472 134 187.46119 8.00266 0.57 −7.761 ± 0.028 −8.736 ± 0.037 2.81 ± 0.18 1.00<br />
NGC 4472 135 187.46664 8.01454 0.89 −7.773 ± 0.019 −9.160 ± 0.019 2.57 ± 0.12 1.00<br />
NGC 4472 136 187.44902 7.97653 0.84 −6.951 ± 0.076 −8.094 ± 0.035 1.85 ± 0.29 0.99<br />
NGC 4472 137 187.46741 8.01634 0.95 −5.550 ± 0.077 −6.466 ± 0.118 3.77 ± 0.60 0.89<br />
NGC 4472 138 187.45703 7.99421 0.47 −8.027 ± 0.037 −9.021 ± 0.073 4.09 ± 0.30 1.00<br />
NGC 4472 139 187.45288 7.98529 0.59 −7.335 ± 0.035 −8.563 ± 0.049 3.06 ± 0.23 1.00<br />
NGC 4472 140 187.45470 7.98927 0.51 −7.963 ± 0.025 −8.958 ± 0.031 2.36 ± 0.16 1.00<br />
NGC 4472 141 187.45879 7.99816 0.48 −8.488 ± 0.031 −9.311 ± 0.019 2.61 ± 0.15 1.00<br />
NGC 4472 142 187.45152 7.98252 0.66 −6.321 ± 0.059 −7.613 ± 0.258 2.34 ± 0.33 0.99<br />
NGC 4472 144 187.44666 7.97226 0.98 −5.498 ± 0.226 −6.835 ± 0.555 4.08 ± 1.58 0.81<br />
NGC 4472 145 187.44616 7.97144 1.01 −7.371 ± 0.054 −8.041 ± 0.068 4.28 ± 0.32 0.97<br />
NGC 4472 146 187.45577 7.99223 0.47 −8.115 ± 0.023 −9.539 ± 0.018 1.73 ± 0.14 1.00<br />
NGC 4472 150 187.45660 7.99444 0.45 −8.769 ± 0.021 −9.804 ± 0.022 2.63 ± 0.15 1.00<br />
NGC 4472 151 187.46714 8.01689 0.95 −5.736 ± 0.052 −7.508 ± 0.051 2.60 ± 0.37 0.99<br />
NGC 4472 153 187.45566 7.99269 0.46 −9.125 ± 0.016 −9.983 ± 0.019 2.73 ± 0.15 1.00<br />
NGC 4472 154 187.45300 7.98714 0.54 −6.222 ± 0.102 −7.784 ± 0.070 2.07 ± 0.55 1.00<br />
NGC 4472 156 187.44681 7.97400 0.92 −6.920 ± 0.039 −8.416 ± 0.039 2.41 ± 0.19 1.00<br />
NGC 4472 158 187.46402 8.01147 0.76 −7.963 ± 0.045 −9.300 ± 0.174 2.23 ± 0.37 1.00<br />
NGC 4472 159 187.46099 8.00499 0.57 −7.556 ± 0.027 −8.513 ± 0.058 2.87 ± 0.24 1.00<br />
NGC 4472 160 187.45233 7.98649 0.55 −7.996 ± 0.041 −8.921 ± 0.057 4.09 ± 0.31 1.00<br />
NGC 4472 161 187.44854 7.97824 0.78 −7.310 ± 0.024 −8.688 ± 0.025 1.91 ± 0.19 1.00<br />
NGC 4472 162 187.45506 7.99240 0.45 −6.962 ± 0.048 −8.010 ± 0.091 2.94 ± 0.43 0.99<br />
NGC 4472 163 187.45569 7.99383 0.44 −6.433 ± 0.042 −7.984 ± 0.084 2.62 ± 0.44 1.00<br />
NGC 4472 164 187.46451 8.01290 0.80 −6.121 ± 0.085 −7.173 ± 0.061 3.47 ± 0.41 0.94<br />
NGC 4472 165 187.44869 7.97893 0.76 −6.915 ± 0.040 −8.334 ± 0.043 1.72 ± 0.29 1.00<br />
NGC 4472 167 187.45075 7.98358 0.62 −6.450 ± 0.055 −7.896 ± 0.038 2.82 ± 0.30 0.99<br />
NGC 4472 170 187.45664 7.99655 0.43 −6.211 ± 0.038 −7.647 ± 0.143 2.23 ± 0.28 1.00<br />
NGC 4472 171 187.45774 7.99900 0.44 −8.034 ± 0.024 −9.506 ± 0.022 2.85 ± 0.12 1.00<br />
NGC 4472 172 187.44893 7.98022 0.71 −5.617 ± 0.776 −6.468 ± 0.183 2.98 ± 0.69 0.96<br />
NGC 4472 173 187.46338 8.01118 0.74 −5.927 ± 0.166 −7.565 ± 0.225 2.82 ± 1.47 0.99<br />
NGC 4472 174 187.46344 8.01207 0.75 −7.338 ± 0.020 −8.184 ± 0.036 2.95 ± 0.24 1.00<br />
NGC 4472 175 187.45030 7.98386 0.60 −7.738 ± 0.090 −9.261 ± 0.061 7.15 ± 0.49 0.96<br />
NGC 4472 177 187.45691 7.99829 0.42 −8.761 ± 0.016 −9.768 ± 0.019 3.51 ± 0.12 1.00<br />
NGC 4472 178 187.44925 7.98175 0.67 −6.830 ± 0.048 −8.331 ± 0.049 2.51 ± 0.22 1.00<br />
NGC 4472 181 187.44780 7.97901 0.75 −7.357 ± 0.033 −8.543 ± 0.045 2.82 ± 0.23 1.00<br />
NGC 4472 183 187.45566 7.99610 0.40 −9.403 ± 0.016 −10.298 ± 0.027 3.58 ± 0.14 1.00<br />
NGC 4472 184 187.45204 7.98854 0.48 −7.191 ± 0.043 −8.523 ± 0.046 2.51 ± 0.28 1.00<br />
NGC 4472 185 187.44606 7.97572 0.86 −5.325 ± 0.415 −7.071 ± 0.091 3.40 ± 1.22 0.94<br />
NGC 4472 187 187.44521 7.97414 0.91 −7.129 ± 0.045 −8.615 ± 0.037 2.75 ± 0.19 1.00<br />
NGC 4472 188 187.44634 7.97604 0.85 −8.885 ± 0.025 −10.542 ± 0.021 2.77 ± 0.12 1.00<br />
NGC 4472 189 187.46613 8.01950 0.98 −8.773 ± 0.028 −9.631 ± 0.027 3.77 ± 0.13 1.00<br />
NGC 4472 190 187.44392 7.97183 0.99 −8.270 ± 0.033 −9.184 ± 0.024 3.07 ± 0.16 1.00<br />
NGC 4472 191 187.45804 8.00232 0.46 −6.373 ± 0.060 −7.892 ± 0.058 2.54 ± 0.28 1.00<br />
NGC 4472 192 187.45845 8.00332 0.48 −6.950 ± 0.049 −7.780 ± 0.033 2.49 ± 0.24 1.00<br />
NGC 4472 195 187.45993 8.00671 0.56 −8.474 ± 0.064 −9.515 ± 0.069 6.54 ± 0.38 0.99<br />
NGC 4472 199 187.45831 8.00374 0.48 −5.503 ± 0.313 −6.328 ± 1.021 2.40 ± 1.50 0.98<br />
NGC 4472 201 187.45587 7.99850 0.38 −7.014 ± 0.045 −7.929 ± 0.041 1.72 ± 0.26 0.99<br />
NGC 4472 202 187.45494 7.99663 0.37 −6.879 ± 0.130 −8.210 ± 0.027 1.67 ± 0.24 1.00<br />
NGC 4472 203 187.45392 7.99447 0.37 −7.191 ± 0.129 −8.695 ± 0.039 2.36 ± 0.28 1.00<br />
NGC 4472 205 187.45957 8.00675 0.55 −6.956 ± 0.041 −8.676 ± 0.039 3.07 ± 0.20 1.00<br />
NGC 4472 207 187.45039 7.98720 0.50 −8.702 ± 0.027 −9.562 ± 0.018 2.09 ± 0.13 1.00<br />
NGC 4472 208 187.45137 7.98965 0.44 −6.566 ± 0.043 −7.814 ± 0.133 2.48 ± 0.46 1.00<br />
NGC 4472 209 187.45560 7.99887 0.37 −7.481 ± 0.026 −8.345 ± 0.070 2.26 ± 0.31 1.00<br />
NGC 4472 210 187.45593 7.99956 0.38 −6.283 ± 0.046 −7.346 ± 0.067 2.71 ± 0.41 0.99<br />
NGC 4472 211 187.44830 7.98331 0.61 −8.681 ± 0.015 −9.938 ± 0.015 1.86 ± 0.13 1.00<br />
NGC 4472 212 187.45171 7.98020 0.74 −6.838 ± 0.047 −7.719 ± 0.081 3.27 ± 0.32 0.98<br />
NGC 4472 213 187.46025 8.00961 0.62 −5.881 ± 0.344 −7.271 ± 1.362 1.54 ± 0.48 0.95<br />
NGC 4472 214 187.45883 8.00668 0.53 −5.794 ± 0.089 −6.585 ± 0.383 2.42 ± 0.48 0.98<br />
NGC 4472 215 187.46323 8.01612 0.83 −5.999 ± 0.111 −7.206 ± 0.088 4.10 ± 0.55 0.88<br />
NGC 4472 217 187.46326 8.00515 0.65 −5.784 ± 0.368 −6.754 ± 0.094 2.22 ± 0.47 0.99<br />
NGC 4472 218 187.45415 7.99680 0.34 −8.550 ± 0.035 −9.548 ± 0.038 4.20 ± 0.12 1.00<br />
NGC 4472 219 187.45275 7.99375 0.36 −7.171 ± 0.044 −8.015 ± 0.074 2.25 ± 0.29 1.00<br />
Continued on Next Page. . .<br />
334
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4472 220 187.46335 8.01698 0.85 −7.048 ± 0.032 −8.455 ± 0.038 2.49 ± 0.25 1.00<br />
NGC 4472 221 187.45727 8.00407 0.44 −8.543 ± 0.019 −9.590 ± 0.015 2.20 ± 0.16 1.00<br />
NGC 4472 224 187.46576 8.02243 1.04 −7.283 ± 0.059 −8.410 ± 0.079 4.81 ± 0.39 0.98<br />
NGC 4472 225 187.45440 7.99800 0.34 −8.938 ± 0.024 −10.416 ± 0.023 2.62 ± 0.13 1.00<br />
NGC 4472 226 187.44390 7.97565 0.86 −8.306 ± 0.028 −9.255 ± 0.024 2.81 ± 0.15 1.00<br />
NGC 4472 227 187.44380 7.97563 0.86 −7.777 ± 0.029 −8.849 ± 0.028 3.08 ± 0.20 1.00<br />
NGC 4472 228 187.46303 8.01719 0.85 −5.401 ± 0.201 −6.508 ± 0.102 3.58 ± 1.03 0.92<br />
NGC 4472 230 187.45203 7.99383 0.34 −6.624 ± 0.048 −7.929 ± 0.112 1.87 ± 0.91 0.99<br />
NGC 4472 233 187.45424 7.99911 0.33 −9.954 ± 0.030 −10.868 ± 0.023 2.90 ± 0.20 1.00<br />
NGC 4472 234 187.45068 7.99156 0.37 −6.495 ± 0.077 −7.741 ± 0.417 2.60 ± 0.47 0.99<br />
NGC 4472 235 187.44956 7.98924 0.42 −6.011 ± 0.146 −7.149 ± 0.196 2.58 ± 0.69 0.98<br />
NGC 4472 236 187.44829 7.98653 0.50 −7.187 ± 0.052 −8.255 ± 0.203 5.23 ± 1.03 0.94<br />
NGC 4472 239 187.46213 8.01665 0.81 −7.719 ± 0.036 −8.729 ± 0.056 3.61 ± 0.31 1.00<br />
NGC 4472 240 187.45532 8.00196 0.36 −7.937 ± 0.044 −8.897 ± 0.029 2.27 ± 0.25 1.00<br />
NGC 4472 241 187.45494 8.00127 0.35 −6.137 ± 0.122 −7.507 ± 0.081 6.32 ± 0.82 0.53<br />
NGC 4472 242 187.46100 8.01428 0.73 −7.305 ± 0.041 −8.815 ± 0.032 2.44 ± 0.21 1.00<br />
NGC 4472 243 187.45054 7.99181 0.36 −7.705 ± 0.028 −9.097 ± 0.032 2.38 ± 0.16 1.00<br />
NGC 4472 244 187.45468 8.00090 0.34 −8.224 ± 0.033 −9.188 ± 0.036 2.52 ± 0.22 1.00<br />
NGC 4472 245 187.44461 7.97930 0.73 −7.423 ± 0.069 −7.989 ± 0.100 4.51 ± 0.39 0.96<br />
NGC 4472 246 187.44808 7.98697 0.48 −6.659 ± 0.273 −8.037 ± 0.108 2.82 ± 0.47 0.99<br />
NGC 4472 247 187.44737 7.98547 0.53 −7.393 ± 0.063 −8.667 ± 0.040 4.02 ± 0.20 1.00<br />
NGC 4472 248 187.45485 8.00166 0.35 −6.955 ± 0.098 −7.641 ± 0.063 3.54 ± 0.46 0.97<br />
NGC 4472 249 187.46426 8.02198 1.00 −6.955 ± 0.054 −8.220 ± 0.042 2.99 ± 0.27 1.00<br />
NGC 4472 253 187.44736 7.98646 0.49 −8.486 ± 0.019 −9.871 ± 0.017 2.08 ± 0.16 1.00<br />
NGC 4472 254 187.44352 7.97822 0.77 −5.750 ± 0.426 −7.158 ± 0.143 2.48 ± 0.64 0.99<br />
NGC 4472 255 187.46388 8.02214 0.99 −7.652 ± 0.030 −8.521 ± 0.034 3.46 ± 0.15 1.00<br />
NGC 4472 256 187.44895 7.99013 0.38 −7.940 ± 0.039 −9.162 ± 0.030 2.59 ± 0.25 1.00<br />
NGC 4472 257 187.44406 7.98002 0.71 −7.822 ± 0.037 −8.829 ± 0.026 2.21 ± 0.15 1.00<br />
NGC 4472 258 187.44128 7.97405 0.92 −7.562 ± 0.032 −8.399 ± 0.044 3.87 ± 0.16 1.00<br />
NGC 4472 261 187.44849 7.99000 0.38 −6.343 ± 0.099 −7.454 ± 0.252 3.20 ± 0.51 0.98<br />
NGC 4472 262 187.44693 7.98676 0.48 −7.674 ± 0.032 −9.105 ± 0.024 2.03 ± 0.21 1.00<br />
NGC 4472 264 187.44551 7.98386 0.58 −6.108 ± 0.105 −7.224 ± 0.101 3.79 ± 0.51 0.92<br />
NGC 4472 265 187.45703 8.00869 0.51 −5.257 ± 0.594 −6.639 ± 0.797 1.36 ± 0.58 0.89<br />
NGC 4472 266 187.45801 8.01106 0.58 −6.912 ± 0.052 −8.644 ± 0.062 4.04 ± 0.25 1.00<br />
NGC 4472 267 187.45996 8.01540 0.73 −7.300 ± 0.043 −8.341 ± 0.079 5.30 ± 0.44 0.94<br />
NGC 4472 268 187.45686 8.00863 0.50 −6.445 ± 0.078 −7.464 ± 0.097 2.93 ± 0.39 0.98<br />
NGC 4472 269 187.45108 7.99624 0.26 −6.745 ± 0.438 −8.097 ± 0.571 1.44 ± 0.37 0.96<br />
NGC 4472 270 187.44568 7.98472 0.55 −5.691 ± 0.109 −7.325 ± 0.101 2.42 ± 0.63 0.99<br />
NGC 4472 271 187.45024 7.99478 0.27 −10.509 ± 0.015 −11.756 ± 0.011 3.74 ± 0.06 1.00<br />
NGC 4472 272 187.44533 7.98410 0.57 −5.899 ± 0.845 −7.406 ± 0.125 1.91 ± 0.67 0.99<br />
NGC 4472 273 187.45142 7.99739 0.25 −7.064 ± 0.128 −7.691 ± 0.123 5.55 ± 0.62 0.81<br />
NGC 4472 274 187.46322 8.02309 1.00 −8.197 ± 0.035 −9.179 ± 0.025 3.43 ± 0.19 1.00<br />
NGC 4472 276 187.44592 7.98607 0.50 −7.329 ± 0.047 −8.590 ± 0.108 4.75 ± 0.56 0.99<br />
NGC 4472 277 187.45152 7.99838 0.24 −9.893 ± 0.029 −10.732 ± 0.042 5.48 ± 0.18 1.00<br />
NGC 4472 278 187.45125 7.99761 0.24 −6.391 ± 0.095 −7.717 ± 0.215 3.16 ± 1.00 0.99<br />
NGC 4472 280 187.45175 7.99890 0.24 −7.695 ± 0.034 −8.905 ± 0.043 2.20 ± 0.19 1.00<br />
NGC 4472 281 187.46211 8.02130 0.93 −6.486 ± 0.052 −8.018 ± 0.037 1.83 ± 0.26 0.99<br />
NGC 4472 282 187.46133 8.01967 0.87 −6.796 ± 0.035 −8.443 ± 0.021 1.92 ± 0.19 1.00<br />
NGC 4472 284 187.46071 8.01841 0.83 −6.036 ± 0.097 −7.077 ± 0.070 2.64 ± 0.51 0.98<br />
NGC 4472 286 187.45119 7.99807 0.23 −6.420 ± 0.164 −7.260 ± 0.531 2.55 ± 0.82 0.99<br />
NGC 4472 287 187.44101 7.97616 0.85 −5.932 ± 0.092 −7.301 ± 0.323 2.40 ± 0.80 0.99<br />
NGC 4472 288 187.44517 7.98532 0.52 −7.044 ± 0.045 −8.122 ± 0.077 3.15 ± 0.39 0.99<br />
NGC 4472 290 187.44827 7.99206 0.31 −8.864 ± 0.017 −9.998 ± 0.024 2.44 ± 0.14 1.00<br />
NGC 4472 291 187.44129 7.97718 0.82 −6.647 ± 0.045 −8.215 ± 0.061 3.91 ± 0.28 1.00<br />
NGC 4472 292 187.45665 8.01084 0.54 −8.988 ± 0.023 −9.969 ± 0.015 2.13 ± 0.17 1.00<br />
NGC 4472 294 187.46182 8.02232 0.95 −7.110 ± 0.048 −8.615 ± 0.037 3.43 ± 0.20 1.00<br />
NGC 4472 295 187.44458 7.98531 0.52 −9.776 ± 0.017 −11.130 ± 0.019 2.34 ± 0.09 1.00<br />
NGC 4472 297 187.45566 8.00952 0.49 −6.911 ± 0.033 −8.343 ± 0.125 1.22 ± 0.20 0.91<br />
NGC 4472 298 187.45988 8.01867 0.81 −5.658 ± 0.064 −7.144 ± 0.033 2.71 ± 0.31 0.98<br />
NGC 4472 299 187.44902 7.99544 0.23 −7.199 ± 0.121 −8.949 ± 0.085 5.22 ± 0.61 0.98<br />
NGC 4472 300 187.44782 7.99315 0.27 −8.453 ± 0.015 −9.806 ± 0.022 2.01 ± 0.17 1.00<br />
NGC 4472 302 187.44580 7.98890 0.40 −6.940 ± 0.095 −7.730 ± 1.576 2.62 ± 0.59 0.99<br />
Continued on Next Page. . .<br />
335
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4472 303 187.45193 8.00218 0.25 −7.021 ± 0.044 −8.020 ± 0.182 2.33 ± 0.40 1.00<br />
NGC 4472 306 187.43919 7.97525 0.89 −5.456 ± 0.361 −7.267 ± 0.269 5.75 ± 3.10 0.60<br />
NGC 4472 307 187.44551 7.98917 0.39 −5.165 ± 0.159 −6.899 ± 0.107 3.45 ± 0.57 0.93<br />
NGC 4472 308 187.45214 8.00363 0.27 −7.168 ± 0.061 −8.036 ± 0.050 2.57 ± 0.32 1.00<br />
NGC 4472 310 187.45824 8.01692 0.73 −8.625 ± 0.044 −9.972 ± 0.032 4.74 ± 0.25 1.00<br />
NGC 4472 311 187.45632 8.01280 0.58 −6.387 ± 0.060 −7.625 ± 0.101 4.39 ± 0.47 0.92<br />
NGC 4472 312 187.45198 8.00366 0.27 −8.257 ± 0.027 −9.274 ± 0.033 3.36 ± 0.16 1.00<br />
NGC 4472 314 187.45769 8.01617 0.70 −7.469 ± 0.031 −8.662 ± 0.026 2.49 ± 0.15 1.00<br />
NGC 4472 315 187.43987 7.97781 0.80 −6.654 ± 0.052 −7.964 ± 0.041 2.10 ± 0.31 1.00<br />
NGC 4472 316 187.45444 8.00951 0.45 −8.163 ± 0.027 −9.743 ± 0.043 3.69 ± 0.17 1.00<br />
NGC 4472 317 187.44054 7.97967 0.73 −8.309 ± 0.024 −9.827 ± 0.012 2.00 ± 0.11 1.00<br />
NGC 4472 318 187.44672 7.99331 0.26 −7.264 ± 0.025 −8.759 ± 0.041 2.79 ± 0.26 1.00<br />
NGC 4472 319 187.44873 7.99762 0.17 −7.134 ± 1.213 −8.890 ± 0.358 2.10 ± 0.56 1.00<br />
NGC 4472 320 187.43958 7.97800 0.80 −6.048 ± 0.075 −7.213 ± 0.053 2.51 ± 0.34 0.99<br />
NGC 4472 321 187.45195 8.00473 0.28 −6.087 ± 0.128 −7.473 ± 0.093 3.53 ± 0.50 0.96<br />
NGC 4472 322 187.45952 8.02117 0.88 −6.339 ± 0.044 −7.821 ± 0.034 2.41 ± 0.26 1.00<br />
NGC 4472 323 187.44859 7.99800 0.15 −8.267 ± 0.028 −9.708 ± 0.024 1.33 ± 0.18 0.93<br />
NGC 4472 324 187.44240 7.98501 0.54 −7.361 ± 0.082 −8.172 ± 0.250 6.83 ± 1.81 0.64<br />
NGC 4472 325 187.45174 8.00523 0.29 −6.673 ± 0.469 −7.455 ± 0.062 1.28 ± 0.36 0.91<br />
NGC 4472 326 187.45389 8.01032 0.46 −7.203 ± 0.044 −8.532 ± 0.037 2.46 ± 0.25 1.00<br />
NGC 4472 327 187.45381 8.01024 0.46 −8.005 ± 0.019 −8.996 ± 0.037 2.85 ± 0.18 1.00<br />
NGC 4472 329 187.44946 8.00098 0.16 −6.783 ± 0.065 −7.879 ± 0.392 1.86 ± 0.39 0.99<br />
NGC 4472 330 187.44960 8.00144 0.17 −6.769 ± 0.086 −7.735 ± 0.104 2.24 ± 0.52 1.00<br />
NGC 4472 331 187.44690 7.99584 0.18 −9.623 ± 0.022 −11.187 ± 0.024 4.10 ± 0.15 1.00<br />
NGC 4472 332 187.45002 8.00265 0.19 −9.460 ± 0.021 −10.754 ± 0.021 3.47 ± 0.15 1.00<br />
NGC 4472 333 187.45776 8.01938 0.79 −9.094 ± 0.017 −10.382 ± 0.012 2.07 ± 0.09 1.00<br />
NGC 4472 334 187.45372 8.01059 0.46 −7.899 ± 0.028 −9.459 ± 0.020 1.88 ± 0.14 1.00<br />
NGC 4472 335 187.44972 8.00222 0.18 −10.310 ± 0.025 −11.717 ± 0.017 2.38 ± 0.15 1.00<br />
NGC 4472 337 187.43877 7.97880 0.78 −6.462 ± 0.070 −7.768 ± 0.041 2.41 ± 0.29 1.00<br />
NGC 4472 338 187.44794 7.99855 0.13 −7.869 ± 0.109 −9.105 ± 0.027 1.74 ± 0.24 1.00<br />
NGC 4472 339 187.45628 8.01675 0.69 −8.482 ± 0.024 −10.069 ± 0.012 2.85 ± 0.10 1.00<br />
NGC 4472 340 187.45779 8.02002 0.81 −7.807 ± 0.032 −8.817 ± 0.044 2.92 ± 0.20 1.00<br />
NGC 4472 342 187.44059 7.98377 0.60 −6.740 ± 0.056 −7.860 ± 0.060 2.87 ± 0.28 0.99<br />
NGC 4472 343 187.44182 7.98646 0.50 −8.219 ± 0.028 −9.460 ± 0.019 3.12 ± 0.16 1.00<br />
NGC 4472 344 187.44336 7.98980 0.37 −6.434 ± 0.083 −8.093 ± 0.103 4.04 ± 0.51 0.98<br />
NGC 4472 345 187.44948 8.00314 0.18 −8.617 ± 0.022 −9.654 ± 0.033 2.70 ± 0.12 1.00<br />
NGC 4472 347 187.45437 8.01406 0.57 −7.417 ± 0.035 −8.947 ± 0.027 2.88 ± 0.17 1.00<br />
NGC 4472 348 187.45493 8.01541 0.62 −9.265 ± 0.019 −10.759 ± 0.013 2.02 ± 0.10 1.00<br />
NGC 4472 349 187.45224 8.00956 0.40 −6.309 ± 0.080 −7.692 ± 0.109 2.92 ± 0.63 0.99<br />
NGC 4472 350 187.45037 8.00569 0.26 −8.423 ± 0.019 −9.997 ± 0.019 2.25 ± 0.14 1.00<br />
NGC 4472 351 187.44913 8.00304 0.17 −10.537 ± 0.012 −11.939 ± 0.022 2.39 ± 0.10 1.00<br />
NGC 4472 352 187.44687 7.99820 0.10 −9.842 ± 0.028 −11.241 ± 0.011 2.97 ± 0.10 1.00<br />
NGC 4472 354 187.43645 7.97587 0.90 −6.701 ± 0.042 −8.164 ± 0.037 1.71 ± 0.25 1.00<br />
NGC 4472 356 187.45361 8.01245 0.51 −7.731 ± 0.028 −8.967 ± 0.029 2.10 ± 0.22 1.00<br />
NGC 4472 357 187.44268 7.98947 0.39 −9.487 ± 0.016 −10.370 ± 0.018 3.48 ± 0.12 1.00<br />
NGC 4472 358 187.43956 7.98263 0.64 −7.619 ± 0.035 −8.925 ± 0.027 1.85 ± 0.23 1.00<br />
NGC 4472 359 187.45091 8.00718 0.31 −7.375 ± 0.052 −8.505 ± 0.043 3.41 ± 0.23 1.00<br />
NGC 4472 360 187.45143 8.00837 0.35 −7.195 ± 0.033 −8.582 ± 0.041 1.79 ± 0.18 1.00<br />
NGC 4472 361 187.44646 7.99796 0.10 −7.156 ± 0.512 −7.720 ± 0.578 1.78 ± 3.71 0.99<br />
NGC 4472 362 187.45023 8.00623 0.27 −6.369 ± 0.135 −8.144 ± 0.148 5.90 ± 0.80 0.83<br />
NGC 4472 364 187.44875 8.00333 0.17 −6.262 ± 0.590 −7.538 ± 0.090 1.77 ± 0.52 0.98<br />
NGC 4472 367 187.44223 7.98957 0.39 −7.373 ± 0.045 −7.909 ± 0.408 1.23 ± 0.30 0.91<br />
NGC 4472 368 187.44694 7.99978 0.08 −8.573 ± 0.029 −9.913 ± 0.031 2.11 ± 0.18 1.00<br />
NGC 4472 369 187.44749 8.00104 0.09 −7.629 ± 0.084 −8.821 ± 0.102 4.33 ± 0.51 1.00<br />
NGC 4472 370 187.44139 7.98796 0.45 −9.109 ± 0.020 −10.476 ± 0.016 2.31 ± 0.17 1.00<br />
NGC 4472 371 187.44197 7.98948 0.39 −8.788 ± 0.018 −10.025 ± 0.020 2.58 ± 0.08 1.00<br />
NGC 4472 372 187.45144 8.00989 0.40 −7.535 ± 0.038 −8.848 ± 0.042 2.59 ± 0.22 1.00<br />
NGC 4472 373 187.44287 7.99168 0.31 −7.955 ± 0.025 −8.617 ± 0.031 1.91 ± 0.19 1.00<br />
NGC 4472 374 187.44540 7.99656 0.14 −7.718 ± 0.053 −9.142 ± 0.036 2.29 ± 0.22 1.00<br />
NGC 4472 375 187.45726 8.02283 0.88 −7.768 ± 0.026 −9.069 ± 0.019 2.43 ± 0.14 1.00<br />
NGC 4472 377 187.44797 8.00295 0.14 −8.195 ± 0.038 −9.270 ± 0.079 4.16 ± 0.40 1.00<br />
NGC 4472 379 187.44388 7.99453 0.21 −10.884 ± 0.028 −12.442 ± 0.020 5.41 ± 0.19 1.00<br />
Continued on Next Page. . .<br />
336
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4472 380 187.44507 7.99698 0.12 −7.345 ± 0.050 −8.838 ± 0.048 1.69 ± 0.29 1.00<br />
NGC 4472 383 187.43834 7.98275 0.65 −7.246 ± 0.045 −9.020 ± 0.109 7.39 ± 0.73 0.88<br />
NGC 4472 386 187.44029 7.98740 0.48 −7.512 ± 0.061 −8.560 ± 0.062 3.47 ± 0.31 1.00<br />
NGC 4472 389 187.44064 7.98875 0.43 −7.118 ± 0.036 −8.477 ± 0.060 2.77 ± 0.29 1.00<br />
NGC 4472 390 187.44717 8.00275 0.11 −7.196 ± 0.055 −8.536 ± 0.080 1.68 ± 0.38 1.00<br />
NGC 4472 391 187.43429 7.97540 0.94 −7.587 ± 0.033 −8.959 ± 0.029 2.75 ± 0.17 1.00<br />
NGC 4472 392 187.43963 7.98693 0.50 −6.934 ± 0.156 −8.107 ± 0.037 2.98 ± 0.36 0.99<br />
NGC 4472 394 187.45466 8.01953 0.74 −7.736 ± 0.036 −8.680 ± 0.035 2.79 ± 0.22 1.00<br />
NGC 4472 395 187.45364 8.01739 0.66 −8.615 ± 0.015 −9.641 ± 0.018 2.71 ± 0.11 1.00<br />
NGC 4472 396 187.44161 7.99148 0.33 −5.587 ± 0.340 −7.280 ± 0.112 3.07 ± 0.78 0.97<br />
NGC 4472 397 187.45694 8.02449 0.93 −7.819 ± 0.032 −8.857 ± 0.016 2.36 ± 0.18 1.00<br />
NGC 4472 398 187.44852 8.00665 0.25 −8.870 ± 0.041 −9.869 ± 0.030 2.24 ± 0.19 1.00<br />
NGC 4472 399 187.44483 7.99868 0.06 −8.833 ± 0.032 −10.214 ± 0.046 2.15 ± 0.20 1.00<br />
NGC 4472 400 187.45595 8.02273 0.86 −8.190 ± 0.023 −9.122 ± 0.032 3.14 ± 0.16 1.00<br />
NGC 4472 401 187.45305 8.01663 0.63 −5.597 ± 0.111 −6.827 ± 0.083 2.77 ± 0.49 0.97<br />
NGC 4472 403 187.44888 8.00787 0.29 −6.188 ± 0.097 −7.770 ± 0.138 2.80 ± 0.66 0.99<br />
NGC 4472 404 187.44847 8.00705 0.26 −7.765 ± 0.028 −9.113 ± 0.027 2.01 ± 0.25 1.00<br />
NGC 4472 405 187.44551 8.00101 0.03 −7.333 ± 0.093 −8.430 ± 0.426 2.47 ± 0.82 1.00<br />
NGC 4472 407 187.44236 7.99449 0.22 −6.413 ± 0.142 −8.076 ± 0.297 6.85 ± 2.00 0.59<br />
NGC 4472 408 187.44847 8.00803 0.29 −5.721 ± 0.273 −6.770 ± 0.408 1.61 ± 2.54 0.95<br />
NGC 4472 410 187.45084 8.01333 0.49 −6.925 ± 0.072 −8.522 ± 0.124 4.38 ± 0.64 0.99<br />
NGC 4472 412 187.44547 8.00267 0.08 −8.057 ± 0.038 −9.005 ± 0.087 2.83 ± 0.37 1.00<br />
NGC 4472 414 187.44210 7.99567 0.19 −8.351 ± 0.029 −9.741 ± 0.025 2.86 ± 0.16 1.00<br />
NGC 4472 415 187.45407 8.02167 0.80 −6.758 ± 0.038 −8.005 ± 0.042 2.18 ± 0.28 1.00<br />
NGC 4472 416 187.45031 8.01354 0.49 −5.188 ± 0.464 −7.039 ± 0.186 3.27 ± 1.27 0.95<br />
NGC 4472 418 187.44518 8.00262 0.08 −7.519 ± 0.095 −8.360 ± 0.203 4.03 ± 1.02 1.00<br />
NGC 4472 419 187.44394 8.00003 0.03 −8.653 ± 0.057 −9.805 ± 0.050 2.75 ± 0.26 1.00<br />
NGC 4472 420 187.44258 7.99710 0.14 −7.078 ± 0.119 −8.639 ± 0.320 5.77 ± 2.74 0.91<br />
NGC 4472 422 187.44987 8.01307 0.47 −7.017 ± 0.057 −7.747 ± 0.099 2.87 ± 0.56 0.99<br />
NGC 4472 423 187.44834 8.01008 0.35 −7.993 ± 0.036 −9.084 ± 0.043 3.33 ± 0.24 1.00<br />
NGC 4472 424 187.43379 7.97873 0.84 −5.469 ± 0.098 −6.950 ± 0.328 2.65 ± 0.64 0.98<br />
NGC 4472 425 187.44597 8.00508 0.16 −8.877 ± 0.027 −9.813 ± 0.029 2.37 ± 0.16 1.00<br />
NGC 4472 426 187.44010 7.99248 0.32 −5.499 ± 0.363 −7.162 ± 0.370 1.97 ± 0.51 0.99<br />
NGC 4472 427 187.45285 8.01984 0.72 −6.428 ± 0.302 −8.248 ± 0.899 1.13 ± 0.35 0.87<br />
NGC 4472 429 187.44752 8.00874 0.30 −6.637 ± 0.054 −7.653 ± 0.133 3.52 ± 0.81 0.97<br />
NGC 4472 430 187.45059 8.01564 0.56 −8.317 ± 0.019 −9.378 ± 0.036 3.07 ± 0.17 1.00<br />
NGC 4472 431 187.44794 8.01002 0.35 −8.343 ± 0.025 −9.319 ± 0.036 3.35 ± 0.18 1.00<br />
NGC 4472 432 187.44483 8.00335 0.10 −8.237 ± 0.028 −9.632 ± 0.049 1.36 ± 0.26 0.94<br />
NGC 4472 433 187.43847 7.98984 0.43 −6.745 ± 0.055 −7.740 ± 0.094 2.59 ± 0.38 0.99<br />
NGC 4472 434 187.44658 8.00733 0.24 −8.130 ± 0.045 −9.041 ± 0.045 2.54 ± 0.24 1.00<br />
NGC 4472 435 187.44137 7.99605 0.19 −8.090 ± 0.028 −9.564 ± 0.024 2.99 ± 0.14 1.00<br />
NGC 4472 437 187.43901 7.99122 0.38 −8.415 ± 0.023 −9.689 ± 0.021 2.88 ± 0.14 1.00<br />
NGC 4472 438 187.44000 7.99333 0.30 −7.074 ± 0.050 −8.514 ± 0.035 2.12 ± 0.24 1.00<br />
NGC 4472 439 187.44679 8.00813 0.27 −8.760 ± 0.025 −9.814 ± 0.026 2.60 ± 0.21 1.00<br />
NGC 4472 440 187.44360 8.00117 0.05 −8.092 ± 0.046 −9.461 ± 0.043 1.86 ± 0.28 1.00<br />
NGC 4472 441 187.44239 7.99877 0.10 −9.028 ± 0.020 −9.959 ± 0.036 2.55 ± 0.15 1.00<br />
NGC 4472 443 187.44014 7.99453 0.26 −8.073 ± 0.024 −9.300 ± 0.037 2.22 ± 0.21 1.00<br />
NGC 4472 444 187.44448 8.00406 0.12 −7.884 ± 0.025 −9.370 ± 0.085 2.34 ± 0.27 1.00<br />
NGC 4472 445 187.44166 7.99806 0.14 −9.164 ± 0.044 −9.998 ± 0.022 2.05 ± 0.25 1.00<br />
NGC 4472 447 187.44409 8.00355 0.11 −7.041 ± 0.123 −7.756 ± 0.101 2.79 ± 0.51 0.99<br />
NGC 4472 449 187.43870 7.99239 0.35 −7.650 ± 0.260 −8.493 ± 0.099 6.33 ± 2.23 0.84<br />
NGC 4472 451 187.43707 7.98898 0.48 −6.772 ± 0.038 −7.749 ± 0.255 1.89 ± 0.45 0.99<br />
NGC 4472 452 187.45201 8.02117 0.76 −6.061 ± 0.151 −6.707 ± 0.076 3.46 ± 0.67 0.93<br />
NGC 4472 454 187.43768 7.99072 0.42 −7.774 ± 0.024 −9.369 ± 0.021 3.42 ± 0.11 1.00<br />
NGC 4472 455 187.43727 7.98991 0.45 −6.606 ± 0.048 −8.189 ± 0.033 2.37 ± 0.20 1.00<br />
NGC 4472 457 187.43231 7.97941 0.85 −7.919 ± 0.032 −8.816 ± 0.030 2.74 ± 0.20 1.00<br />
NGC 4472 459 187.43909 7.99416 0.29 −6.616 ± 0.094 −8.182 ± 0.034 2.10 ± 0.37 1.00<br />
NGC 4472 461 187.44333 8.00349 0.12 −7.638 ± 0.052 −9.040 ± 0.045 1.81 ± 0.27 1.00<br />
NGC 4472 462 187.44621 8.00994 0.33 −8.354 ± 0.051 −9.427 ± 0.047 2.87 ± 0.30 1.00<br />
NGC 4472 463 187.44472 8.00675 0.22 −8.848 ± 0.027 −10.375 ± 0.028 3.01 ± 0.14 1.00<br />
NGC 4472 464 187.43455 7.98501 0.64 −7.235 ± 0.033 −8.909 ± 0.260 1.47 ± 0.26 0.97<br />
NGC 4472 467 187.44752 8.01340 0.46 −8.801 ± 0.034 −9.613 ± 0.052 6.21 ± 0.22 1.00<br />
Continued on Next Page. . .<br />
337
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4472 469 187.43977 7.99705 0.21 −7.466 ± 0.024 −8.841 ± 0.044 1.56 ± 0.18 0.98<br />
NGC 4472 470 187.43830 7.99408 0.32 −7.857 ± 0.035 −8.621 ± 0.032 2.97 ± 0.20 1.00<br />
NGC 4472 471 187.44447 8.00738 0.24 −6.836 ± 0.078 −8.239 ± 0.062 1.95 ± 0.34 1.00<br />
NGC 4472 472 187.44005 7.99792 0.19 −7.762 ± 0.063 −8.607 ± 0.231 1.68 ± 0.41 1.00<br />
NGC 4472 474 187.43902 7.99586 0.26 −7.322 ± 0.333 −8.928 ± 0.040 2.28 ± 0.29 1.00<br />
NGC 4472 476 187.44408 8.00689 0.22 −6.644 ± 0.289 −8.352 ± 0.061 2.56 ± 0.45 1.00<br />
NGC 4472 478 187.43045 7.97780 0.93 −7.392 ± 0.035 −8.943 ± 0.025 2.28 ± 0.24 1.00<br />
NGC 4472 479 187.45268 8.02589 0.92 −6.967 ± 0.041 −8.411 ± 0.022 2.42 ± 0.22 1.00<br />
NGC 4472 480 187.43999 7.99853 0.18 −8.484 ± 0.021 −9.930 ± 0.021 2.06 ± 0.12 1.00<br />
NGC 4472 482 187.44632 8.01249 0.42 −6.094 ± 0.108 −6.779 ± 1.111 1.56 ± 0.47 0.94<br />
NGC 4472 483 187.43508 7.98864 0.53 −8.551 ± 0.026 −9.574 ± 0.014 2.77 ± 0.19 1.00<br />
NGC 4472 484 187.44854 8.01763 0.61 −5.884 ± 0.093 −7.541 ± 0.094 4.79 ± 0.43 0.85<br />
NGC 4472 485 187.44174 8.00302 0.14 −7.331 ± 0.189 −9.204 ± 0.157 2.50 ± 0.75 1.00<br />
NGC 4472 486 187.43057 7.97896 0.89 −5.439 ± 0.114 −6.887 ± 0.096 5.09 ± 0.51 0.59<br />
NGC 4472 487 187.44297 8.00610 0.20 −6.157 ± 0.081 −7.631 ± 0.093 2.77 ± 0.41 0.99<br />
NGC 4472 488 187.43190 7.98232 0.77 −5.590 ± 0.230 −6.746 ± 0.141 5.10 ± 1.84 0.56<br />
NGC 4472 490 187.43233 7.98371 0.72 −6.666 ± 0.112 −7.963 ± 0.168 5.94 ± 1.23 0.81<br />
NGC 4472 491 187.43948 7.99912 0.19 −7.582 ± 0.028 −9.147 ± 1.481 2.09 ± 0.20 1.00<br />
NGC 4472 492 187.43750 7.99495 0.32 −9.324 ± 0.028 −10.225 ± 0.033 4.55 ± 0.16 1.00<br />
NGC 4472 494 187.44441 8.00977 0.32 −7.337 ± 0.046 −8.856 ± 0.028 1.51 ± 0.20 0.97<br />
NGC 4472 495 187.44391 8.00918 0.30 −9.180 ± 0.019 −10.847 ± 0.025 2.67 ± 0.16 1.00<br />
NGC 4472 496 187.44701 8.01579 0.54 −9.514 ± 0.020 −10.717 ± 0.018 1.98 ± 0.08 1.00<br />
NGC 4472 497 187.42942 7.97814 0.94 −7.580 ± 0.027 −8.582 ± 0.040 2.88 ± 0.25 1.00<br />
NGC 4472 498 187.44864 8.01950 0.67 −6.690 ± 0.057 −8.153 ± 0.070 2.61 ± 0.36 1.00<br />
NGC 4472 499 187.44540 8.01320 0.44 −5.893 ± 0.442 −7.209 ± 0.661 1.69 ± 0.57 0.97<br />
NGC 4472 500 187.44076 8.00329 0.17 −6.706 ± 0.043 −7.618 ± 0.374 2.85 ± 0.41 0.99<br />
NGC 4472 501 187.43994 8.00170 0.17 −8.527 ± 0.024 −9.338 ± 0.024 2.01 ± 0.12 1.00<br />
NGC 4472 502 187.43175 7.98406 0.72 −6.177 ± 0.099 −7.137 ± 0.172 3.51 ± 0.81 0.94<br />
NGC 4472 503 187.44348 8.00937 0.31 −8.843 ± 0.028 −10.393 ± 0.016 1.69 ± 0.12 1.00<br />
NGC 4472 504 187.43252 7.98596 0.66 −7.981 ± 0.035 −9.035 ± 0.020 2.51 ± 0.16 1.00<br />
NGC 4472 506 187.44322 8.00915 0.31 −7.404 ± 0.048 −8.944 ± 0.066 2.65 ± 0.32 1.00<br />
NGC 4472 507 187.43065 7.98226 0.80 −7.122 ± 0.061 −8.319 ± 0.047 3.20 ± 0.31 1.00<br />
NGC 4472 508 187.43564 7.99310 0.41 −9.516 ± 0.014 −10.579 ± 0.022 2.78 ± 0.21 1.00<br />
NGC 4472 512 187.43329 7.98877 0.57 −5.302 ± 0.619 −6.867 ± 0.540 1.29 ± 0.57 0.87<br />
NGC 4472 516 187.44969 8.02573 0.89 −6.773 ± 0.054 −7.757 ± 0.069 2.84 ± 0.34 0.99<br />
NGC 4472 517 187.44319 8.01169 0.39 −6.030 ± 0.259 −7.588 ± 0.378 2.12 ± 0.45 0.99<br />
NGC 4472 518 187.44484 8.01565 0.53 −8.195 ± 0.014 −9.110 ± 0.022 2.11 ± 0.12 1.00<br />
NGC 4472 519 187.44434 8.01469 0.49 −6.045 ± 0.114 −7.590 ± 0.090 2.87 ± 0.52 0.99<br />
NGC 4472 520 187.44792 8.02261 0.77 −6.017 ± 0.069 −7.244 ± 0.444 1.66 ± 0.39 0.97<br />
NGC 4472 521 187.44774 8.02244 0.77 −7.086 ± 0.027 −8.096 ± 0.037 2.24 ± 0.18 1.00<br />
NGC 4472 523 187.44896 8.02539 0.87 −4.895 ± 0.350 −6.438 ± 0.187 3.52 ± 0.87 0.93<br />
NGC 4472 524 187.43471 7.99488 0.40 −7.601 ± 0.033 −9.246 ± 0.029 2.74 ± 0.21 1.00<br />
NGC 4472 527 187.43546 7.99676 0.35 −6.106 ± 0.298 −7.970 ± 0.214 4.49 ± 1.45 0.96<br />
NGC 4472 529 187.44479 8.01717 0.58 −5.613 ± 0.498 −7.290 ± 0.078 1.77 ± 0.49 0.98<br />
NGC 4472 530 187.43748 8.00162 0.26 −7.489 ± 0.029 −8.875 ± 0.031 1.77 ± 0.20 1.00<br />
NGC 4472 531 187.44530 8.01879 0.63 −7.495 ± 0.034 −8.935 ± 0.038 2.88 ± 0.21 1.00<br />
NGC 4472 534 187.44490 8.01807 0.61 −7.038 ± 0.035 −8.628 ± 0.034 2.42 ± 0.22 1.00<br />
NGC 4472 535 187.44043 8.00845 0.31 −5.774 ± 0.114 −7.113 ± 0.820 2.10 ± 0.56 0.99<br />
NGC 4472 536 187.43815 8.00363 0.25 −8.678 ± 0.029 −9.559 ± 0.031 2.33 ± 0.21 1.00<br />
NGC 4472 537 187.44277 8.01375 0.46 −7.333 ± 0.050 −8.487 ± 0.029 1.69 ± 0.23 1.00<br />
NGC 4472 538 187.43559 7.99830 0.33 −8.228 ± 0.024 −9.681 ± 0.015 2.34 ± 0.14 1.00<br />
NGC 4472 539 187.44286 8.01347 0.45 −5.272 ± 0.346 −6.925 ± 0.304 4.34 ± 2.71 0.76<br />
NGC 4472 540 187.44077 8.00954 0.34 −7.270 ± 0.057 −7.800 ± 0.078 2.96 ± 0.34 0.99<br />
NGC 4472 541 187.43716 8.00187 0.27 −7.435 ± 0.040 −8.861 ± 0.051 2.82 ± 0.29 1.00<br />
NGC 4472 542 187.42857 7.98373 0.80 −9.441 ± 0.020 −10.569 ± 0.023 4.39 ± 0.09 1.00<br />
NGC 4472 543 187.43568 7.99910 0.32 −7.691 ± 0.057 −8.303 ± 0.040 3.06 ± 0.29 1.00<br />
NGC 4472 544 187.44160 8.01232 0.42 −7.548 ± 0.043 −8.357 ± 0.054 2.05 ± 0.33 1.00<br />
NGC 4472 545 187.43200 7.99179 0.53 −6.995 ± 0.046 −8.735 ± 0.064 4.90 ± 0.28 0.99<br />
NGC 4472 546 187.43152 7.99076 0.57 −8.190 ± 0.024 −9.146 ± 0.020 2.41 ± 0.15 1.00<br />
NGC 4472 547 187.42786 7.98300 0.84 −7.171 ± 0.037 −8.584 ± 0.119 1.81 ± 0.27 1.00<br />
NGC 4472 548 187.42832 7.98402 0.80 −6.444 ± 0.082 −7.708 ± 0.382 3.65 ± 0.59 0.97<br />
NGC 4472 549 187.44850 8.02753 0.94 −6.296 ± 0.051 −7.891 ± 0.040 1.26 ± 0.23 0.92<br />
Continued on Next Page. . .<br />
338
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4472 550 187.43858 8.00632 0.29 −6.190 ± 0.200 −7.539 ± 0.836 1.65 ± 0.57 0.98<br />
NGC 4472 551 187.43960 8.00860 0.33 −6.521 ± 0.089 −7.139 ± 0.113 2.27 ± 0.45 0.99<br />
NGC 4472 552 187.44187 8.01359 0.47 −6.016 ± 0.091 −7.338 ± 0.202 3.91 ± 1.12 0.93<br />
NGC 4472 553 187.43996 8.00956 0.36 −6.181 ± 0.060 −7.646 ± 0.146 4.66 ± 0.81 0.89<br />
NGC 4472 554 187.44254 8.01522 0.52 −8.304 ± 0.019 −9.595 ± 0.020 1.89 ± 0.13 1.00<br />
NGC 4472 555 187.42894 7.98615 0.74 −8.393 ± 0.022 −9.798 ± 0.024 2.67 ± 0.14 1.00<br />
NGC 4472 556 187.42692 7.98179 0.89 −5.670 ± 0.092 −7.223 ± 0.078 3.26 ± 0.45 0.96<br />
NGC 4472 557 187.42969 7.98793 0.68 −7.317 ± 0.030 −8.734 ± 0.037 2.27 ± 0.29 1.00<br />
NGC 4472 559 187.44367 8.01808 0.61 −8.294 ± 0.022 −9.479 ± 0.024 2.92 ± 0.13 1.00<br />
NGC 4472 561 187.44678 8.02493 0.85 −7.649 ± 0.024 −8.597 ± 0.034 3.06 ± 0.18 1.00<br />
NGC 4472 562 187.44421 8.01941 0.66 −7.673 ± 0.029 −8.508 ± 0.042 2.56 ± 0.31 1.00<br />
NGC 4472 563 187.43987 8.01004 0.37 −5.654 ± 0.103 −6.855 ± 0.097 2.29 ± 0.67 0.99<br />
NGC 4472 565 187.44650 8.02507 0.85 −7.170 ± 0.041 −8.478 ± 0.030 2.21 ± 0.24 1.00<br />
NGC 4472 566 187.44763 8.02750 0.94 −7.405 ± 0.032 −8.397 ± 0.028 2.78 ± 0.20 1.00<br />
NGC 4472 567 187.43576 8.00229 0.32 −8.581 ± 0.055 −9.540 ± 0.043 3.12 ± 0.28 1.00<br />
NGC 4472 568 187.42856 7.98642 0.74 −7.888 ± 0.050 −9.247 ± 0.157 1.88 ± 0.35 1.00<br />
NGC 4472 569 187.44559 8.02349 0.80 −7.519 ± 0.025 −9.090 ± 0.024 1.89 ± 0.23 1.00<br />
NGC 4472 570 187.44224 8.01619 0.55 −5.694 ± 0.147 −6.791 ± 0.377 2.91 ± 0.94 0.96<br />
NGC 4472 572 187.42676 7.98319 0.86 −7.934 ± 0.035 −9.353 ± 0.016 2.23 ± 0.18 1.00<br />
NGC 4472 573 187.43909 8.00973 0.38 −7.125 ± 0.055 −8.628 ± 0.037 2.91 ± 0.26 1.00<br />
NGC 4472 574 187.44574 8.02413 0.82 −6.681 ± 0.036 −8.118 ± 0.024 1.65 ± 0.16 0.98<br />
NGC 4472 575 187.43009 7.99042 0.61 −5.208 ± 0.147 −6.421 ± 0.209 2.82 ± 0.75 0.96<br />
NGC 4472 576 187.43756 8.00656 0.33 −5.629 ± 0.306 −7.076 ± 0.294 4.08 ± 1.23 0.86<br />
NGC 4472 577 187.42730 7.98470 0.81 −6.892 ± 0.036 −7.906 ± 0.072 2.63 ± 0.28 1.00<br />
NGC 4472 580 187.44303 8.01873 0.63 −7.700 ± 0.676 −9.377 ± 0.028 1.92 ± 0.36 1.00<br />
NGC 4472 581 187.44128 8.01520 0.52 −7.231 ± 0.025 −8.200 ± 0.035 2.53 ± 0.22 1.00<br />
NGC 4472 582 187.43025 7.99150 0.59 −7.175 ± 1.317 −8.715 ± 0.705 1.81 ± 0.36 1.00<br />
NGC 4472 583 187.43451 8.00077 0.35 −6.267 ± 0.612 −7.099 ± 0.587 1.97 ± 0.75 0.99<br />
NGC 4472 584 187.44386 8.02104 0.71 −7.463 ± 0.024 −8.558 ± 0.186 2.08 ± 0.22 1.00<br />
NGC 4472 585 187.44390 8.02114 0.72 −6.212 ± 0.489 −7.877 ± 0.521 1.03 ± 0.31 0.83<br />
NGC 4472 586 187.43414 8.00013 0.37 −6.112 ± 0.142 −7.373 ± 0.155 3.92 ± 1.04 0.93<br />
NGC 4472 587 187.44275 8.01814 0.62 −5.463 ± 0.312 −6.803 ± 0.079 3.86 ± 0.85 0.87<br />
NGC 4472 589 187.43305 7.99694 0.42 −7.710 ± 0.032 −8.932 ± 0.034 2.30 ± 0.24 1.00<br />
NGC 4472 590 187.43973 8.01271 0.46 −7.631 ± 0.023 −9.055 ± 0.022 2.39 ± 0.19 1.00<br />
NGC 4472 591 187.43407 8.00062 0.37 −7.300 ± 0.032 −8.688 ± 0.356 1.75 ± 0.28 1.00<br />
NGC 4472 592 187.43549 8.00363 0.34 −6.480 ± 0.082 −8.093 ± 0.148 5.48 ± 0.83 0.90<br />
NGC 4472 593 187.44270 8.01947 0.66 −8.764 ± 0.033 −10.178 ± 0.024 1.79 ± 0.15 1.00<br />
NGC 4472 594 187.44386 8.02217 0.75 −7.172 ± 0.054 −8.372 ± 0.105 3.12 ± 0.37 1.00<br />
NGC 4472 595 187.43510 8.00328 0.35 −6.156 ± 0.530 −7.209 ± 0.788 2.08 ± 0.66 0.99<br />
NGC 4472 596 187.42988 7.99225 0.59 −6.181 ± 0.077 −7.639 ± 0.052 1.96 ± 0.35 0.99<br />
NGC 4472 598 187.43032 7.99333 0.56 −5.519 ± 0.391 −6.282 ± 0.243 3.69 ± 0.81 0.91<br />
NGC 4472 599 187.44433 8.02389 0.81 −7.138 ± 0.036 −8.253 ± 0.071 3.83 ± 0.35 1.00<br />
NGC 4472 600 187.43239 7.99768 0.44 −8.108 ± 0.022 −9.199 ± 0.030 2.84 ± 0.19 1.00<br />
NGC 4472 602 187.43461 8.00323 0.36 −7.609 ± 0.035 −9.218 ± 0.025 2.97 ± 0.14 1.00<br />
NGC 4472 603 187.44104 8.01712 0.59 −6.476 ± 0.438 −7.784 ± 0.047 1.18 ± 0.35 0.90<br />
NGC 4472 604 187.43910 8.01298 0.48 −6.087 ± 0.073 −7.426 ± 0.158 1.43 ± 0.43 0.94<br />
NGC 4472 606 187.43872 8.01237 0.46 −7.411 ± 0.034 −8.520 ± 0.029 2.21 ± 0.18 1.00<br />
NGC 4472 608 187.42905 7.99160 0.62 −5.517 ± 0.150 −6.753 ± 0.185 2.77 ± 0.89 0.97<br />
NGC 4472 610 187.43644 8.00790 0.39 −6.920 ± 0.083 −8.251 ± 0.070 2.61 ± 0.44 1.00<br />
NGC 4472 611 187.43257 7.99959 0.42 −5.913 ± 0.106 −7.259 ± 0.197 4.50 ± 0.94 0.82<br />
NGC 4472 612 187.43532 8.00566 0.37 −8.056 ± 0.021 −9.666 ± 0.016 1.61 ± 0.20 1.00<br />
NGC 4472 615 187.43515 8.00543 0.37 −7.330 ± 0.034 −8.286 ± 0.060 1.88 ± 0.42 1.00<br />
NGC 4472 616 187.42656 7.98700 0.78 −7.288 ± 0.043 −8.415 ± 0.071 4.10 ± 0.37 1.00<br />
NGC 4472 617 187.44032 8.01691 0.59 −8.564 ± 0.024 −9.547 ± 0.020 2.70 ± 0.14 1.00<br />
NGC 4472 618 187.42577 7.98556 0.83 −6.028 ± 0.082 −7.601 ± 0.177 4.24 ± 1.14 0.93<br />
NGC 4472 619 187.43895 8.01395 0.51 −7.995 ± 0.027 −9.392 ± 0.022 2.06 ± 0.12 1.00<br />
NGC 4472 620 187.43809 8.01229 0.47 −8.248 ± 0.019 −9.152 ± 0.030 2.66 ± 0.18 1.00<br />
NGC 4472 621 187.43099 7.99693 0.49 −8.325 ± 0.022 −9.830 ± 0.016 2.06 ± 0.12 1.00<br />
NGC 4472 622 187.44421 8.02553 0.87 −8.487 ± 0.030 −9.834 ± 0.022 2.36 ± 0.25 1.00<br />
NGC 4472 623 187.42781 7.99019 0.68 −5.496 ± 0.150 −6.887 ± 0.215 5.26 ± 1.38 0.55<br />
NGC 4472 625 187.42360 7.98156 0.98 −7.944 ± 0.028 −9.373 ± 0.016 1.98 ± 0.19 1.00<br />
NGC 4472 626 187.43226 8.00022 0.43 −7.266 ± 0.028 −8.732 ± 0.037 2.63 ± 0.22 1.00<br />
Continued on Next Page. . .<br />
339
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4472 627 187.43712 8.01076 0.44 −6.626 ± 0.046 −7.451 ± 0.114 2.57 ± 0.52 0.99<br />
NGC 4472 628 187.42818 7.99173 0.65 −6.966 ± 0.052 −8.052 ± 0.165 2.17 ± 0.29 1.00<br />
NGC 4472 629 187.43350 8.00328 0.40 −6.679 ± 0.054 −7.974 ± 0.063 2.23 ± 0.32 1.00<br />
NGC 4472 630 187.44168 8.02100 0.72 −7.639 ± 0.030 −9.002 ± 0.022 2.30 ± 0.25 1.00<br />
NGC 4472 633 187.43247 8.00135 0.43 −7.572 ± 0.044 −9.024 ± 0.030 3.50 ± 0.19 1.00<br />
NGC 4472 634 187.44244 8.02288 0.78 −6.432 ± 0.067 −7.817 ± 0.068 2.64 ± 0.50 0.99<br />
NGC 4472 635 187.43198 8.00040 0.44 −6.382 ± 0.061 −7.870 ± 0.038 2.70 ± 0.24 0.99<br />
NGC 4472 636 187.43487 8.00672 0.40 −8.535 ± 0.022 −10.010 ± 0.020 2.18 ± 0.14 1.00<br />
NGC 4472 639 187.42650 7.98892 0.75 −7.281 ± 0.049 −8.740 ± 0.049 3.70 ± 0.29 1.00<br />
NGC 4472 640 187.43536 8.00818 0.42 −10.116 ± 0.026 −11.001 ± 0.014 4.91 ± 0.09 0.98<br />
NGC 4472 641 187.43849 8.01516 0.55 −8.052 ± 0.029 −8.962 ± 0.038 3.80 ± 0.15 1.00<br />
NGC 4472 642 187.44214 8.02292 0.78 −7.600 ± 0.038 −9.008 ± 0.463 2.42 ± 0.34 1.00<br />
NGC 4472 643 187.44101 8.02043 0.70 −6.181 ± 0.097 −7.157 ± 0.129 3.13 ± 0.69 0.96<br />
NGC 4472 644 187.42565 7.98765 0.79 −5.516 ± 0.120 −7.181 ± 0.201 5.00 ± 1.52 0.71<br />
NGC 4472 645 187.44297 8.02522 0.86 −7.828 ± 0.025 −8.792 ± 0.045 3.13 ± 0.25 1.00<br />
NGC 4472 646 187.43882 8.01625 0.58 −8.086 ± 0.025 −9.105 ± 0.028 2.58 ± 0.17 1.00<br />
NGC 4472 647 187.42418 7.98472 0.89 −6.805 ± 0.059 −8.109 ± 0.049 2.76 ± 0.32 1.00<br />
NGC 4472 648 187.44028 8.01946 0.68 −8.326 ± 0.020 −9.311 ± 0.022 2.14 ± 0.17 1.00<br />
NGC 4472 649 187.43718 8.01337 0.52 −8.092 ± 0.027 −8.977 ± 0.032 2.36 ± 0.25 1.00<br />
NGC 4472 651 187.43164 8.00184 0.45 −8.012 ± 0.023 −9.139 ± 0.020 2.56 ± 0.16 1.00<br />
NGC 4472 653 187.44063 8.02139 0.74 −6.631 ± 0.051 −8.151 ± 0.031 2.19 ± 0.26 1.00<br />
NGC 4472 654 187.43667 8.01340 0.53 −8.071 ± 0.037 −9.170 ± 0.036 3.72 ± 0.24 1.00<br />
NGC 4472 655 187.42804 7.99481 0.61 −7.756 ± 0.042 −8.851 ± 0.239 2.49 ± 0.40 1.00<br />
NGC 4472 656 187.43194 8.00337 0.45 −6.259 ± 0.097 −7.250 ± 0.369 2.69 ± 1.52 0.98<br />
NGC 4472 657 187.43727 8.01489 0.56 −6.288 ± 0.096 −7.047 ± 0.395 3.12 ± 0.92 0.96<br />
NGC 4472 658 187.43809 8.01668 0.61 −5.560 ± 0.525 −6.355 ± 0.680 0.94 ± 0.54 0.74<br />
NGC 4472 659 187.42747 7.99404 0.64 −9.308 ± 0.026 −10.446 ± 0.010 2.45 ± 0.16 1.00<br />
NGC 4472 660 187.43303 8.00598 0.45 −5.401 ± 0.139 −7.044 ± 0.106 2.29 ± 0.57 0.99<br />
NGC 4472 661 187.43437 8.00899 0.46 −8.141 ± 0.027 −9.677 ± 0.018 2.28 ± 0.15 1.00<br />
NGC 4472 662 187.43097 8.00183 0.48 −8.486 ± 0.019 −9.842 ± 0.015 2.26 ± 0.10 1.00<br />
NGC 4472 663 187.43287 8.00602 0.45 −7.797 ± 0.036 −9.167 ± 0.021 2.39 ± 0.14 1.00<br />
NGC 4472 664 187.42643 7.99226 0.69 −7.272 ± 0.036 −8.396 ± 0.032 1.90 ± 0.27 1.00<br />
NGC 4472 666 187.43811 8.01758 0.64 −5.266 ± 0.248 −6.515 ± 0.773 1.43 ± 0.47 0.91<br />
NGC 4472 670 187.43127 8.00329 0.48 −7.918 ± 0.062 −9.415 ± 0.035 1.68 ± 0.27 1.00<br />
NGC 4472 671 187.42115 7.98157 1.04 −6.309 ± 0.097 −7.646 ± 0.067 5.55 ± 0.45 0.79<br />
NGC 4472 672 187.44111 8.02488 0.85 −8.326 ± 0.082 −9.153 ± 0.065 6.75 ± 0.44 0.93<br />
NGC 4472 674 187.43260 8.00657 0.47 −6.266 ± 0.076 −7.436 ± 0.108 3.61 ± 0.37 0.96<br />
NGC 4472 675 187.43519 8.01221 0.52 −5.696 ± 0.138 −6.980 ± 0.693 2.31 ± 0.73 0.99<br />
NGC 4472 676 187.42395 7.98818 0.83 −9.102 ± 0.020 −9.974 ± 0.018 2.82 ± 0.16 1.00<br />
NGC 4472 679 187.43187 8.00604 0.48 −7.459 ± 0.035 −8.711 ± 0.036 2.67 ± 0.21 1.00<br />
NGC 4472 680 187.42563 7.99291 0.71 −8.814 ± 0.018 −9.784 ± 0.018 1.89 ± 0.12 1.00<br />
NGC 4472 681 187.42452 7.99035 0.78 −4.973 ± 0.155 −6.728 ± 0.198 5.14 ± 1.24 0.54<br />
NGC 4472 682 187.42619 7.99413 0.68 −7.689 ± 0.034 −8.728 ± 0.020 2.23 ± 0.19 1.00<br />
NGC 4472 683 187.42113 7.98266 1.02 −7.185 ± 0.066 −7.859 ± 0.068 3.81 ± 0.39 0.98<br />
NGC 4472 684 187.42855 7.99914 0.56 −5.617 ± 0.308 −6.800 ± 0.066 2.78 ± 0.60 0.97<br />
NGC 4472 685 187.42636 7.99453 0.67 −7.120 ± 0.060 −8.291 ± 0.068 3.56 ± 0.41 1.00<br />
NGC 4472 686 187.43999 8.02395 0.83 −6.430 ± 0.044 −7.963 ± 0.044 2.09 ± 0.28 1.00<br />
NGC 4472 687 187.43685 8.01741 0.65 −6.594 ± 0.085 −8.433 ± 0.046 4.50 ± 0.32 0.99<br />
NGC 4472 690 187.42611 7.99467 0.67 −7.418 ± 0.017 −8.339 ± 0.019 2.03 ± 0.17 1.00<br />
NGC 4472 691 187.42891 8.00071 0.55 −7.383 ± 0.030 −8.560 ± 0.027 1.88 ± 0.22 1.00<br />
NGC 4472 692 187.43472 8.01333 0.56 −7.030 ± 2.772 −8.487 ± 0.029 1.07 ± 0.33 0.84<br />
NGC 4472 693 187.42673 7.99605 0.64 −5.967 ± 0.080 −7.124 ± 0.127 2.65 ± 0.70 0.98<br />
NGC 4472 694 187.43986 8.02447 0.85 −5.923 ± 0.077 −6.721 ± 0.313 5.25 ± 2.70 0.51<br />
NGC 4472 695 187.42914 8.00163 0.54 −7.502 ± 0.036 −8.892 ± 0.023 1.57 ± 0.19 0.98<br />
NGC 4472 696 187.43293 8.00985 0.52 −8.184 ± 0.017 −9.308 ± 0.037 2.68 ± 0.18 1.00<br />
NGC 4472 697 187.42932 8.00239 0.54 −7.543 ± 0.039 −9.001 ± 0.029 1.92 ± 0.24 1.00<br />
NGC 4472 699 187.42652 7.99644 0.64 −7.676 ± 0.028 −9.018 ± 0.038 3.47 ± 0.15 1.00<br />
NGC 4472 700 187.42464 7.99259 0.74 −8.396 ± 0.022 −9.164 ± 0.024 2.37 ± 0.13 1.00<br />
NGC 4472 703 187.43820 8.02246 0.79 −8.842 ± 0.028 −9.792 ± 0.018 2.42 ± 0.22 1.00<br />
NGC 4472 704 187.42489 7.99373 0.72 −5.948 ± 0.056 −7.198 ± 0.661 2.11 ± 0.44 0.99<br />
NGC 4472 707 187.43018 8.00591 0.54 −9.434 ± 0.023 −10.450 ± 0.014 3.71 ± 0.14 1.00<br />
NGC 4472 708 187.42049 7.98525 0.99 −7.522 ± 0.028 −9.055 ± 0.034 2.75 ± 0.16 1.00<br />
Continued on Next Page. . .<br />
340
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4472 709 187.43949 8.02626 0.91 −7.551 ± 0.038 −8.500 ± 0.036 2.46 ± 0.19 1.00<br />
NGC 4472 710 187.43910 8.02545 0.89 −5.888 ± 1.342 −7.768 ± 1.395 0.99 ± 0.31 0.81<br />
NGC 4472 711 187.44157 8.03093 1.06 −7.514 ± 0.038 −9.053 ± 0.027 2.90 ± 0.23 1.00<br />
NGC 4472 713 187.43474 8.01629 0.65 −5.765 ± 0.109 −7.058 ± 0.089 2.50 ± 0.45 0.99<br />
NGC 4472 714 187.42827 8.00253 0.57 −6.898 ± 0.111 −8.632 ± 0.096 7.51 ± 0.69 0.70<br />
NGC 4472 715 187.42758 8.00154 0.59 −7.010 ± 0.041 −7.830 ± 0.084 3.72 ± 0.30 0.98<br />
NGC 4472 716 187.43083 8.00878 0.56 −8.874 ± 0.021 −10.372 ± 0.023 2.88 ± 0.12 1.00<br />
NGC 4472 717 187.43326 8.01397 0.61 −5.470 ± 0.181 −6.610 ± 0.533 1.71 ± 0.60 0.96<br />
NGC 4472 718 187.42514 7.99673 0.69 −7.784 ± 0.027 −9.165 ± 0.026 2.80 ± 0.17 1.00<br />
NGC 4472 719 187.42102 7.98844 0.92 −7.111 ± 0.051 −8.548 ± 0.041 2.11 ± 0.23 1.00<br />
NGC 4472 720 187.44106 8.03159 1.08 −7.164 ± 1.142 −8.622 ± 0.047 2.34 ± 0.39 1.00<br />
NGC 4472 721 187.43464 8.01805 0.70 −9.049 ± 0.016 −10.150 ± 0.010 2.24 ± 0.08 1.00<br />
NGC 4472 722 187.42848 8.00476 0.58 −6.575 ± 0.544 −8.115 ± 0.048 1.65 ± 0.34 0.98<br />
NGC 4472 725 187.43674 8.02341 0.84 −6.148 ± 0.052 −7.731 ± 0.051 1.98 ± 0.31 0.99<br />
NGC 4472 726 187.42424 7.99655 0.72 −7.285 ± 0.025 −8.605 ± 0.028 1.58 ± 0.17 0.98<br />
NGC 4472 727 187.42664 8.00173 0.63 −6.485 ± 0.064 −7.702 ± 0.056 2.21 ± 0.44 1.00<br />
NGC 4472 728 187.43414 8.01795 0.71 −5.800 ± 0.108 −6.866 ± 0.145 2.99 ± 0.62 0.96<br />
NGC 4472 729 187.43457 8.01920 0.74 −5.299 ± 0.436 −6.727 ± 0.185 2.76 ± 0.95 0.97<br />
NGC 4472 730 187.42758 8.00418 0.61 −6.567 ± 0.048 −8.032 ± 0.068 2.48 ± 0.30 1.00<br />
NGC 4472 731 187.42717 8.00367 0.62 −8.533 ± 0.022 −9.947 ± 0.022 1.79 ± 0.15 1.00<br />
NGC 4472 732 187.43274 8.01578 0.67 −7.140 ± 0.303 −8.434 ± 0.097 2.82 ± 0.55 1.00<br />
NGC 4472 733 187.41785 7.98364 1.09 −6.754 ± 0.027 −8.013 ± 0.050 2.01 ± 0.28 1.00<br />
NGC 4472 734 187.42543 8.00013 0.67 −8.597 ± 0.031 −9.563 ± 0.030 3.11 ± 0.16 1.00<br />
NGC 4472 735 187.42588 8.00100 0.65 −7.008 ± 0.044 −8.155 ± 0.126 3.36 ± 0.70 1.00<br />
NGC 4472 736 187.42358 7.99602 0.74 −5.139 ± 1.099 −6.511 ± 0.328 3.42 ± 1.87 0.93<br />
NGC 4472 738 187.42046 7.98936 0.92 −5.399 ± 0.196 −6.254 ± 0.222 4.78 ± 1.54 0.64<br />
NGC 4472 739 187.43516 8.02146 0.80 −9.319 ± 0.020 −10.290 ± 0.016 2.19 ± 0.13 1.00<br />
NGC 4472 740 187.42400 7.99743 0.72 −6.971 ± 0.043 −8.069 ± 0.072 3.01 ± 0.28 0.99<br />
NGC 4472 741 187.43590 8.02330 0.85 −8.724 ± 0.026 −9.903 ± 0.016 2.69 ± 0.14 1.00<br />
NGC 4472 742 187.43822 8.02823 0.99 −6.054 ± 0.099 −7.175 ± 0.122 3.37 ± 0.90 0.95<br />
NGC 4472 743 187.43820 8.02845 0.99 −7.730 ± 0.027 −8.585 ± 0.026 1.99 ± 0.21 1.00<br />
NGC 4472 745 187.42273 7.99545 0.78 −6.368 ± 0.085 −7.642 ± 0.041 2.21 ± 0.39 0.99<br />
NGC 4472 746 187.42673 8.00432 0.63 −7.442 ± 0.047 −8.479 ± 0.056 3.64 ± 0.31 1.00<br />
NGC 4472 748 187.41780 7.98518 1.07 −8.580 ± 0.032 −9.523 ± 0.036 2.57 ± 0.26 1.00<br />
NGC 4472 749 187.43762 8.02793 0.98 −8.314 ± 0.022 −9.239 ± 0.033 2.74 ± 0.16 1.00<br />
NGC 4472 750 187.43274 8.01736 0.72 −7.154 ± 0.049 −8.311 ± 0.064 3.61 ± 0.27 1.00<br />
NGC 4472 751 187.42309 7.99687 0.76 −9.179 ± 0.023 −10.107 ± 0.015 3.05 ± 0.12 1.00<br />
NGC 4472 752 187.43134 8.01463 0.67 −8.816 ± 0.019 −10.063 ± 0.017 1.67 ± 0.13 1.00<br />
NGC 4472 756 187.43183 8.01647 0.71 −6.835 ± 0.050 −8.017 ± 0.051 2.45 ± 0.24 1.00<br />
NGC 4472 757 187.42331 7.99833 0.74 −8.475 ± 0.051 −9.403 ± 0.113 7.14 ± 0.70 0.98<br />
NGC 4472 759 187.43834 8.03081 1.07 −6.886 ± 0.041 −8.186 ± 0.183 2.24 ± 0.25 1.00<br />
NGC 4472 762 187.42618 8.00522 0.66 −6.290 ± 0.039 −7.740 ± 0.046 2.33 ± 0.35 1.00<br />
NGC 4472 763 187.43337 8.02090 0.81 −8.352 ± 0.018 −10.009 ± 0.020 1.88 ± 0.15 1.00<br />
NGC 4472 764 187.43268 8.01940 0.78 −6.819 ± 0.084 −7.757 ± 0.044 3.33 ± 0.27 0.98<br />
NGC 4472 768 187.43134 8.01652 0.72 −7.187 ± 0.039 −8.577 ± 0.082 2.34 ± 0.37 1.00<br />
NGC 4472 769 187.42352 8.00044 0.73 −9.623 ± 0.015 −11.291 ± 0.015 2.91 ± 0.08 1.00<br />
NGC 4472 770 187.43706 8.02965 1.04 −8.559 ± 0.017 −9.446 ± 0.018 2.56 ± 0.12 1.00<br />
NGC 4472 771 187.41523 7.98275 1.19 −6.391 ± 0.131 −7.709 ± 0.296 3.99 ± 3.51 0.96<br />
NGC 4472 772 187.41676 7.98627 1.08 −7.224 ± 0.034 −8.376 ± 0.035 3.09 ± 0.15 1.00<br />
NGC 4472 773 187.43302 8.02159 0.84 −8.274 ± 0.024 −9.774 ± 0.025 2.10 ± 0.11 1.00<br />
NGC 4472 774 187.41765 7.98855 1.02 −5.371 ± 0.173 −6.023 ± 0.237 4.48 ± 1.32 0.77<br />
NGC 4472 775 187.42935 8.01390 0.71 −7.102 ± 0.027 −8.546 ± 0.032 1.92 ± 0.21 1.00<br />
NGC 4472 776 187.42128 7.99710 0.82 −9.047 ± 0.037 −9.959 ± 0.020 2.88 ± 0.17 1.00<br />
NGC 4472 777 187.43771 8.03270 1.14 −7.644 ± 0.027 −9.171 ± 0.022 2.14 ± 0.21 1.00<br />
NGC 4472 778 187.42539 8.00642 0.70 −10.280 ± 0.031 −11.292 ± 0.031 3.81 ± 0.16 1.00<br />
NGC 4472 779 187.43743 8.03239 1.13 −8.117 ± 0.018 −9.514 ± 0.025 2.28 ± 0.14 1.00<br />
NGC 4472 780 187.42780 8.01176 0.70 −7.796 ± 0.038 −9.062 ± 0.055 4.65 ± 0.30 1.00<br />
NGC 4472 781 187.43666 8.03116 1.10 −10.506 ± 0.026 −11.748 ± 0.020 3.53 ± 0.12 1.00<br />
NGC 4472 783 187.42703 8.01046 0.70 −6.313 ± 0.072 −7.614 ± 1.195 1.43 ± 0.42 0.95<br />
NGC 4472 784 187.43429 8.02671 0.98 −7.372 ± 0.028 −8.584 ± 0.028 2.54 ± 0.17 1.00<br />
NGC 4472 786 187.42573 8.00861 0.71 −9.196 ± 0.019 −10.564 ± 0.016 3.27 ± 0.12 1.00<br />
NGC 4472 787 187.41661 7.98885 1.05 −7.072 ± 0.081 −8.658 ± 0.065 6.11 ± 0.40 0.88<br />
Continued on Next Page. . .<br />
341
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4472 788 187.42961 8.01681 0.77 −6.992 ± 0.039 −8.299 ± 0.025 2.77 ± 0.16 1.00<br />
NGC 4472 789 187.42238 8.00123 0.77 −7.525 ± 0.034 −8.916 ± 0.021 1.34 ± 0.11 0.95<br />
NGC 4472 790 187.42256 8.00194 0.77 −6.046 ± 0.155 −6.976 ± 0.316 2.69 ± 0.73 0.98<br />
NGC 4472 791 187.42138 7.99935 0.80 −6.013 ± 0.840 −6.996 ± 0.476 1.14 ± 0.73 0.82<br />
NGC 4472 792 187.41670 7.98958 1.04 −7.017 ± 0.046 −8.333 ± 0.027 1.41 ± 0.24 0.96<br />
NGC 4472 793 187.42898 8.01599 0.76 −5.143 ± 0.311 −6.999 ± 0.174 2.87 ± 1.01 0.97<br />
NGC 4472 794 187.41439 7.98462 1.18 −4.822 ± 0.446 −6.126 ± 0.192 2.36 ± 0.98 0.98<br />
NGC 4472 795 187.43512 8.02941 1.06 −7.937 ± 0.019 −8.805 ± 0.035 2.48 ± 0.15 1.00<br />
NGC 4472 796 187.42872 8.01559 0.76 −5.868 ± 0.181 −6.583 ± 0.066 2.94 ± 0.49 0.96<br />
NGC 4472 798 187.41781 7.99248 0.97 −7.062 ± 0.025 −8.275 ± 0.032 1.54 ± 0.17 0.98<br />
NGC 4472 801 187.41664 7.99008 1.03 −7.518 ± 0.035 −8.415 ± 0.037 2.30 ± 0.25 1.00<br />
NGC 4472 803 187.42743 8.01354 0.75 −8.511 ± 0.015 −9.865 ± 0.023 2.13 ± 0.13 1.00<br />
NGC 4472 804 187.43520 8.03035 1.09 −7.857 ± 0.021 −8.990 ± 0.016 2.32 ± 0.18 1.00<br />
NGC 4472 807 187.43335 8.02684 0.99 −9.207 ± 0.018 −10.314 ± 0.017 2.02 ± 0.11 1.00<br />
NGC 4472 808 187.42653 8.01225 0.75 −8.237 ± 0.020 −9.723 ± 0.018 2.23 ± 0.12 1.00<br />
NGC 4472 809 187.41776 7.99338 0.96 −6.180 ± 0.065 −7.243 ± 0.105 2.52 ± 0.41 0.99<br />
NGC 4472 810 187.43121 8.02248 0.89 −9.045 ± 0.023 −10.102 ± 0.025 3.74 ± 0.16 1.00<br />
NGC 4472 812 187.42453 8.00852 0.75 −8.692 ± 0.033 −10.295 ± 0.044 4.97 ± 0.27 1.00<br />
NGC 4472 813 187.41918 7.99700 0.89 −7.234 ± 0.028 −8.314 ± 0.038 1.63 ± 0.24 1.00<br />
NGC 4472 815 187.41826 7.99520 0.93 −6.771 ± 0.054 −7.968 ± 0.057 3.51 ± 0.29 0.98<br />
NGC 4472 817 187.42857 8.01747 0.81 −6.123 ± 0.096 −7.479 ± 0.123 3.94 ± 0.64 0.94<br />
NGC 4472 818 187.43192 8.02496 0.96 −8.236 ± 0.022 −9.623 ± 0.019 1.80 ± 0.10 1.00<br />
NGC 4472 819 187.41916 7.99755 0.89 −7.640 ± 0.029 −9.048 ± 0.018 2.55 ± 0.17 1.00<br />
NGC 4472 820 187.42410 8.00824 0.76 −6.482 ± 0.078 −7.976 ± 0.062 4.96 ± 0.30 0.93<br />
NGC 4472 821 187.42322 8.00646 0.77 −8.656 ± 0.020 −9.659 ± 0.014 2.17 ± 0.10 1.00<br />
NGC 4472 823 187.41850 7.99620 0.91 −5.491 ± 0.064 −6.530 ± 0.092 2.03 ± 0.42 0.98<br />
NGC 4472 824 187.43044 8.02205 0.90 −8.214 ± 0.027 −9.343 ± 0.033 3.42 ± 0.13 1.00<br />
NGC 4472 825 187.41603 7.99107 1.04 −5.275 ± 0.430 −6.233 ± 0.361 1.73 ± 0.72 0.96<br />
NGC 4472 826 187.42882 8.01874 0.84 −6.340 ± 0.058 −7.690 ± 0.077 3.29 ± 0.40 0.98<br />
NGC 4472 827 187.41646 7.99220 1.01 −6.613 ± 0.039 −8.217 ± 0.027 1.95 ± 0.23 1.00<br />
NGC 4472 828 187.41513 7.98995 1.08 −5.449 ± 0.513 −6.568 ± 0.072 1.83 ± 0.37 0.97<br />
NGC 4472 829 187.43207 8.02675 1.01 −7.108 ± 0.026 −8.627 ± 0.028 1.97 ± 0.18 1.00<br />
NGC 4472 830 187.41869 7.99799 0.90 −7.879 ± 0.024 −8.894 ± 0.034 2.84 ± 0.25 1.00<br />
NGC 4472 831 187.41379 7.98739 1.16 −5.827 ± 0.452 −7.235 ± 0.061 2.29 ± 0.55 0.99<br />
NGC 4472 832 187.43015 8.02273 0.92 −6.038 ± 0.316 −7.459 ± 0.031 1.61 ± 0.23 0.97<br />
NGC 4472 833 187.41283 7.98562 1.21 −8.221 ± 0.026 −9.599 ± 0.023 2.34 ± 0.14 1.00<br />
NGC 4472 837 187.41312 7.98630 1.19 −7.272 ± 0.022 −8.693 ± 0.021 1.90 ± 0.11 1.00<br />
NGC 4472 838 187.43358 8.03040 1.11 −5.183 ± 0.408 −6.408 ± 0.324 2.18 ± 0.69 0.98<br />
NGC 4472 839 187.41510 7.99117 1.07 −8.521 ± 0.024 −9.703 ± 0.023 2.45 ± 0.17 1.00<br />
NGC 4472 840 187.43403 8.03196 1.15 −6.290 ± 0.074 −7.515 ± 0.085 3.70 ± 0.48 0.96<br />
NGC 4472 841 187.42488 8.01255 0.80 −10.381 ± 0.017 −11.583 ± 0.015 4.10 ± 0.14 1.00<br />
NGC 4472 842 187.42326 8.00938 0.80 −7.864 ± 0.025 −9.378 ± 0.018 1.67 ± 0.13 1.00<br />
NGC 4472 843 187.42447 8.01239 0.81 −6.560 ± 0.062 −7.301 ± 0.259 2.27 ± 0.38 0.99<br />
NGC 4472 844 187.43338 8.03120 1.13 −7.442 ± 0.028 −9.066 ± 0.025 1.85 ± 0.19 1.00<br />
NGC 4472 846 187.41611 7.99467 1.01 −6.447 ± 0.067 −7.625 ± 0.054 2.61 ± 0.28 0.99<br />
NGC 4472 847 187.42787 8.02026 0.90 −7.149 ± 0.025 −8.415 ± 0.037 2.57 ± 0.21 1.00<br />
NGC 4472 851 187.42449 8.01348 0.83 −7.641 ± 0.052 −8.437 ± 0.054 4.26 ± 0.34 0.99<br />
NGC 4472 852 187.42679 8.01864 0.88 −6.319 ± 0.056 −7.932 ± 0.046 2.23 ± 0.25 1.00<br />
NGC 4472 854 187.42652 8.01844 0.88 −6.609 ± 0.120 −7.564 ± 0.074 2.90 ± 0.41 0.99<br />
NGC 4472 855 187.42370 8.01235 0.83 −5.854 ± 0.242 −7.427 ± 0.071 5.25 ± 1.46 0.76<br />
NGC 4472 856 187.42827 8.02229 0.94 −8.569 ± 0.016 −10.070 ± 0.011 1.91 ± 0.11 1.00<br />
NGC 4472 858 187.42551 8.01726 0.88 −5.905 ± 0.176 −7.064 ± 0.107 4.61 ± 0.84 0.75<br />
NGC 4472 860 187.42242 8.01146 0.86 −9.082 ± 0.013 −10.181 ± 0.021 2.27 ± 0.12 1.00<br />
NGC 4472 862 187.42291 8.01253 0.86 −8.113 ± 0.040 −9.703 ± 0.041 5.57 ± 0.26 1.00<br />
NGC 4472 863 187.42340 8.01364 0.86 −8.796 ± 0.018 −9.831 ± 0.020 1.81 ± 0.13 1.00<br />
NGC 4472 864 187.42979 8.02764 1.07 −6.267 ± 0.080 −7.959 ± 0.071 2.80 ± 0.41 0.99<br />
NGC 4472 865 187.41483 7.99542 1.04 −7.030 ± 0.032 −8.235 ± 0.026 1.70 ± 0.20 1.00<br />
NGC 4472 867 187.42461 8.01689 0.90 −8.370 ± 0.014 −9.429 ± 0.017 2.18 ± 0.06 1.00<br />
NGC 4472 869 187.41424 7.99511 1.06 −7.571 ± 0.027 −9.143 ± 0.021 2.20 ± 0.17 1.00<br />
NGC 4472 870 187.41228 7.99106 1.16 −7.244 ± 0.040 −8.120 ± 0.035 2.71 ± 0.16 1.00<br />
NGC 4472 871 187.42351 8.01548 0.90 −8.710 ± 0.014 −9.575 ± 0.027 2.38 ± 0.14 1.00<br />
NGC 4472 872 187.41463 7.99633 1.05 −6.870 ± 0.046 −7.848 ± 0.041 2.18 ± 0.22 1.00<br />
Continued on Next Page. . .<br />
342
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4472 875 187.42155 8.01169 0.89 −6.301 ± 0.076 −6.822 ± 0.191 2.55 ± 0.99 0.98<br />
NGC 4472 879 187.41996 8.00911 0.90 −6.355 ± 0.035 −7.600 ± 0.483 1.94 ± 0.35 0.99<br />
NGC 4472 882 187.41401 7.99694 1.06 −7.873 ± 0.039 −9.051 ± 0.070 5.46 ± 0.44 0.97<br />
NGC 4472 883 187.40901 7.98694 1.31 −9.166 ± 0.016 −10.245 ± 0.013 2.90 ± 0.09 1.00<br />
NGC 4472 884 187.42366 8.01861 0.96 −4.840 ± 0.356 −6.322 ± 0.099 2.41 ± 1.00 0.98<br />
NGC 4472 885 187.42034 8.01162 0.92 −6.635 ± 0.034 −8.058 ± 0.046 2.12 ± 0.31 1.00<br />
NGC 4472 887 187.42945 8.03134 1.19 −7.929 ± 0.030 −9.453 ± 0.022 2.13 ± 0.18 1.00<br />
NGC 4472 888 187.42708 8.02629 1.08 −6.646 ± 0.050 −8.141 ± 0.061 3.62 ± 0.22 1.00<br />
NGC 4472 889 187.43138 8.03566 1.30 −5.686 ± 0.208 −6.875 ± 0.144 5.44 ± 1.15 0.51<br />
NGC 4472 891 187.43112 8.03547 1.30 −7.881 ± 0.030 −8.711 ± 0.048 4.60 ± 0.18 1.00<br />
NGC 4472 893 187.42369 8.01958 0.98 −6.851 ± 0.040 −8.592 ± 0.024 1.48 ± 0.17 0.97<br />
NGC 4472 894 187.42518 8.02300 1.03 −9.168 ± 0.022 −10.099 ± 0.015 2.74 ± 0.16 1.00<br />
NGC 4472 895 187.40823 7.98672 1.34 −6.012 ± 0.049 −7.416 ± 0.046 3.05 ± 0.23 0.98<br />
NGC 4472 897 187.42682 8.02692 1.10 −5.602 ± 0.414 −7.035 ± 0.134 3.62 ± 1.04 0.92<br />
NGC 4472 901 187.41357 7.99862 1.07 −7.604 ± 0.025 −8.812 ± 0.035 2.47 ± 0.30 1.00<br />
NGC 4472 903 187.41127 7.99414 1.17 −7.169 ± 0.035 −8.219 ± 0.057 2.96 ± 0.41 1.00<br />
NGC 4472 904 187.42169 8.01673 0.97 −6.245 ± 0.045 −7.714 ± 0.061 2.60 ± 0.34 0.99<br />
NGC 4472 905 187.41928 8.01161 0.96 −5.854 ± 0.070 −7.081 ± 0.389 3.75 ± 0.65 0.91<br />
NGC 4472 907 187.42891 8.03257 1.24 −6.139 ± 0.035 −7.651 ± 0.032 3.04 ± 0.25 0.99<br />
NGC 4472 910 187.42258 8.01917 1.00 −6.859 ± 0.057 −7.603 ± 0.074 2.82 ± 0.39 0.99<br />
NGC 4472 911 187.41558 8.00411 1.01 −6.271 ± 0.059 −6.998 ± 0.096 2.00 ± 0.38 0.99<br />
NGC 4472 912 187.41556 8.00426 1.01 −6.501 ± 0.081 −7.747 ± 0.033 3.30 ± 0.31 0.98<br />
NGC 4472 915 187.42024 8.01468 0.98 −6.247 ± 0.054 −7.644 ± 0.042 1.46 ± 0.25 0.96<br />
NGC 4472 916 187.41372 8.00067 1.07 −5.654 ± 0.068 −7.244 ± 0.053 2.90 ± 0.33 0.98<br />
NGC 4472 917 187.41205 7.99713 1.13 −5.565 ± 0.186 −6.760 ± 0.306 4.31 ± 0.95 0.74<br />
NGC 4472 918 187.42323 8.02126 1.03 −6.655 ± 0.034 −7.523 ± 0.087 2.46 ± 0.39 0.99<br />
NGC 4472 922 187.40764 7.98811 1.34 −9.135 ± 0.026 −10.020 ± 0.016 2.88 ± 0.14 1.00<br />
NGC 4472 923 187.42009 8.01488 0.98 −6.269 ± 0.058 −7.770 ± 0.067 1.95 ± 0.30 0.99<br />
NGC 4472 926 187.41290 8.00034 1.09 −6.965 ± 0.033 −8.342 ± 0.031 1.96 ± 0.13 1.00<br />
NGC 4472 927 187.42697 8.03081 1.22 −5.487 ± 0.185 −6.922 ± 0.444 1.66 ± 0.56 0.96<br />
NGC 4472 928 187.42865 8.03472 1.31 −7.855 ± 0.027 −9.065 ± 0.025 3.21 ± 0.15 1.00<br />
NGC 4472 929 187.42945 8.03665 1.36 −7.453 ± 0.021 −8.760 ± 0.027 1.90 ± 0.16 1.00<br />
NGC 4472 931 187.42795 8.03372 1.29 −7.358 ± 0.042 −8.261 ± 0.041 2.82 ± 0.32 1.00<br />
NGC 4472 933 187.41652 8.00937 1.02 −7.146 ± 0.046 −7.958 ± 0.052 2.74 ± 0.23 0.99<br />
NGC 4472 934 187.42357 8.02449 1.11 −7.238 ± 0.024 −8.648 ± 0.021 2.02 ± 0.17 1.00<br />
NGC 4472 937 187.41693 8.01086 1.02 −5.515 ± 0.069 −6.992 ± 0.068 2.81 ± 0.42 0.97<br />
NGC 4472 939 187.42345 8.02538 1.13 −9.457 ± 0.040 −10.327 ± 0.041 2.90 ± 0.39 1.00<br />
NGC 4472 940 187.41008 7.99677 1.20 −7.097 ± 0.031 −8.605 ± 0.050 2.68 ± 0.22 1.00<br />
NGC 4472 943 187.42861 8.03690 1.38 −7.397 ± 0.027 −8.356 ± 0.052 2.73 ± 0.32 1.00<br />
NGC 4472 945 187.40759 7.99175 1.31 −6.755 ± 0.045 −7.594 ± 0.054 3.79 ± 0.17 0.96<br />
NGC 4472 946 187.42014 8.01903 1.06 −7.649 ± 0.041 −8.724 ± 0.077 5.17 ± 0.37 0.97<br />
NGC 4472 947 187.41874 8.01632 1.05 −7.260 ± 0.038 −8.502 ± 0.026 1.93 ± 0.17 1.00<br />
NGC 4472 950 187.42274 8.02603 1.16 −8.033 ± 0.055 −9.414 ± 0.093 4.83 ± 0.56 1.00<br />
NGC 4472 951 187.41437 8.00793 1.08 −7.546 ± 0.020 −8.483 ± 0.035 2.70 ± 0.14 1.00<br />
NGC 4472 952 187.42735 8.03584 1.36 −5.054 ± 1.436 −6.574 ± 0.139 1.84 ± 0.73 0.97<br />
NGC 4472 953 187.41714 8.01426 1.06 −9.432 ± 0.012 −10.627 ± 0.013 2.32 ± 0.07 1.00<br />
NGC 4472 954 187.41339 8.00630 1.10 −7.696 ± 0.027 −8.955 ± 0.023 1.82 ± 0.15 1.00<br />
NGC 4472 956 187.41011 7.99958 1.19 −7.398 ± 0.029 −8.431 ± 0.041 2.97 ± 0.16 1.00<br />
NGC 4472 960 187.41609 8.01291 1.08 −6.474 ± 0.048 −7.679 ± 0.032 2.59 ± 0.29 0.99<br />
NGC 4472 962 187.41209 8.00447 1.13 −6.928 ± 0.039 −8.315 ± 0.039 2.15 ± 0.25 1.00<br />
NGC 4472 963 187.41032 8.00073 1.18 −8.749 ± 0.031 −10.118 ± 0.023 2.07 ± 0.18 1.00<br />
NGC 4472 964 187.42482 8.03203 1.29 −8.782 ± 0.023 −9.714 ± 0.025 2.71 ± 0.18 1.00<br />
NGC 4472 966 187.40867 7.99752 1.24 −7.133 ± 0.040 −8.541 ± 0.032 2.20 ± 0.17 1.00<br />
NGC 4472 967 187.41182 8.00447 1.14 −6.125 ± 0.176 −7.825 ± 0.086 4.72 ± 0.62 0.92<br />
NGC 4472 968 187.41770 8.01751 1.10 −7.399 ± 0.029 −8.700 ± 0.039 2.57 ± 0.21 1.00<br />
NGC 4472 969 187.40816 7.99738 1.26 −7.867 ± 0.017 −9.304 ± 0.020 2.43 ± 0.10 1.00<br />
NGC 4472 971 187.41274 8.00771 1.13 −6.423 ± 0.045 −7.897 ± 0.067 3.13 ± 0.26 0.99<br />
NGC 4472 972 187.40983 8.00145 1.20 −7.674 ± 0.021 −8.632 ± 0.014 2.48 ± 0.21 1.00<br />
NGC 4472 973 187.41774 8.01876 1.12 −6.783 ± 0.197 −8.339 ± 0.057 7.17 ± 1.27 0.62<br />
NGC 4472 974 187.41788 8.01935 1.13 −8.027 ± 0.027 −9.053 ± 0.020 2.85 ± 0.15 1.00<br />
NGC 4472 975 187.42669 8.03848 1.46 −9.443 ± 0.020 −10.324 ± 0.014 2.79 ± 0.14 1.00<br />
NGC 4472 977 187.40981 8.00213 1.20 −6.182 ± 0.063 −6.925 ± 0.055 3.61 ± 0.27 0.91<br />
Continued on Next Page. . .<br />
343
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4472 978 187.40755 7.99770 1.28 −8.538 ± 0.024 −9.996 ± 0.019 3.18 ± 0.16 1.00<br />
NGC 4472 985 187.40715 7.99817 1.29 −8.886 ± 0.011 −10.049 ± 0.013 3.13 ± 0.07 1.00<br />
NGC 4472 986 187.41251 8.00970 1.15 −8.389 ± 0.038 −9.360 ± 0.021 3.01 ± 0.19 1.00<br />
NGC 4472 987 187.40754 7.99920 1.28 −7.552 ± 0.062 −8.822 ± 0.032 4.23 ± 0.28 1.00<br />
NGC 4472 990 187.40488 7.99389 1.39 −8.163 ± 0.024 −9.145 ± 0.021 3.16 ± 0.12 1.00<br />
NGC 4472 992 187.41269 8.01074 1.16 −6.268 ± 0.045 −7.147 ± 0.089 2.53 ± 0.42 0.99<br />
NGC 4472 994 187.41657 8.01934 1.17 −8.170 ± 0.021 −9.051 ± 0.023 2.70 ± 0.15 1.00<br />
NGC 4472 996 187.41036 8.00685 1.20 −6.045 ± 0.078 −7.715 ± 0.039 3.36 ± 0.31 0.98<br />
NGC 4472 1000 187.40319 7.99198 1.46 −5.623 ± 0.129 −7.390 ± 0.137 4.45 ± 0.81 0.87<br />
NGC 4472 1001 187.40446 7.99474 1.40 −5.090 ± 0.302 −6.041 ± 0.333 4.67 ± 3.40 0.72<br />
NGC 4472 1002 187.42402 8.03669 1.44 −6.997 ± 0.030 −7.849 ± 0.116 5.93 ± 0.64 0.79<br />
NGC 4472 1003 187.42363 8.03634 1.44 −5.800 ± 0.304 −6.449 ± 1.355 2.13 ± 0.71 0.98<br />
NGC 4486 1 187.74225 12.41903 1.71 −6.459 ± 0.101 −7.812 ± 0.106 5.97 ± 0.64 0.88<br />
NGC 4486 3 187.68294 12.36655 1.26 −5.646 ± 0.075 −7.398 ± 0.035 3.42 ± 0.30 0.98<br />
NGC 4486 4 187.68315 12.38098 0.93 −6.650 ± 0.059 −7.468 ± 0.036 3.19 ± 0.27 0.99<br />
NGC 4486 5 187.68324 12.38300 0.90 −7.806 ± 0.039 −8.660 ± 0.029 3.09 ± 0.17 1.00<br />
NGC 4486 6 187.68334 12.38080 0.92 −5.380 ± 0.127 −6.322 ± 0.119 3.21 ± 0.51 0.97<br />
NGC 4486 7 187.68343 12.36415 1.32 −7.169 ± 0.035 −8.129 ± 0.049 5.10 ± 0.21 0.97<br />
NGC 4486 8 187.68354 12.38576 0.85 −7.059 ± 0.044 −8.449 ± 0.023 1.80 ± 0.24 1.00<br />
NGC 4486 9 187.68365 12.39014 0.83 −6.887 ± 0.044 −8.158 ± 0.042 2.80 ± 0.26 1.00<br />
NGC 4486 10 187.68366 12.37576 1.01 −7.421 ± 0.044 −8.408 ± 0.046 3.86 ± 0.25 1.00<br />
NGC 4486 11 187.68377 12.39295 0.82 −6.913 ± 0.058 −8.533 ± 0.066 3.92 ± 0.32 1.00<br />
NGC 4486 12 187.68381 12.37787 0.96 −6.781 ± 0.047 −7.736 ± 0.052 2.31 ± 0.28 1.00<br />
NGC 4486 13 187.68390 12.38992 0.82 −7.156 ± 0.033 −8.499 ± 0.107 2.21 ± 0.23 1.00<br />
NGC 4486 14 187.68396 12.38629 0.83 −6.428 ± 0.124 −7.216 ± 0.051 2.63 ± 0.27 0.99<br />
NGC 4486 15 187.68403 12.39262 0.81 −6.985 ± 0.033 −7.727 ± 0.038 2.79 ± 0.18 1.00<br />
NGC 4486 16 187.68413 12.38592 0.83 −6.798 ± 0.042 −7.958 ± 0.041 2.36 ± 0.27 1.00<br />
NGC 4486 17 187.68418 12.37002 1.14 −6.754 ± 0.058 −7.644 ± 0.088 3.09 ± 0.42 0.99<br />
NGC 4486 18 187.68419 12.38682 0.82 −7.931 ± 0.031 −9.396 ± 0.021 1.77 ± 0.15 1.00<br />
NGC 4486 19 187.68435 12.37475 1.01 −7.225 ± 0.034 −8.390 ± 0.032 3.01 ± 0.20 1.00<br />
NGC 4486 20 187.68434 12.40713 1.00 −6.877 ± 0.038 −8.569 ± 0.051 3.34 ± 0.23 1.00<br />
NGC 4486 21 187.68444 12.36463 1.28 −6.557 ± 0.035 −8.020 ± 0.042 3.30 ± 0.25 0.99<br />
NGC 4486 23 187.68451 12.38204 0.87 −7.052 ± 0.043 −7.939 ± 0.041 2.40 ± 0.25 1.00<br />
NGC 4486 24 187.68453 12.37982 0.90 −7.287 ± 0.101 −8.773 ± 0.039 2.58 ± 0.31 1.00<br />
NGC 4486 25 187.68453 12.38134 0.88 −8.202 ± 0.015 −9.425 ± 0.017 2.31 ± 0.09 1.00<br />
NGC 4486 26 187.68451 12.37013 1.12 −5.000 ± 0.141 −6.076 ± 0.097 1.51 ± 0.63 0.96<br />
NGC 4486 27 187.68456 12.39895 0.85 −8.669 ± 0.021 −10.029 ± 0.009 2.11 ± 0.12 1.00<br />
NGC 4486 28 187.68456 12.40980 1.06 −8.287 ± 0.037 −9.531 ± 0.023 2.65 ± 0.21 1.00<br />
NGC 4486 29 187.68460 12.37604 0.98 −7.819 ± 0.027 −8.848 ± 0.024 3.16 ± 0.17 1.00<br />
NGC 4486 30 187.68456 12.38060 0.89 −7.402 ± 0.040 −8.314 ± 0.034 2.64 ± 0.18 1.00<br />
NGC 4486 31 187.68462 12.39019 0.79 −7.938 ± 0.024 −9.349 ± 0.025 2.57 ± 0.17 1.00<br />
NGC 4486 32 187.68468 12.37483 1.00 −8.752 ± 0.019 −9.723 ± 0.027 3.80 ± 0.16 1.00<br />
NGC 4486 33 187.68466 12.40012 0.86 −7.310 ± 0.034 −8.268 ± 0.037 2.53 ± 0.18 1.00<br />
NGC 4486 34 187.68471 12.40466 0.94 −7.583 ± 0.020 −8.990 ± 0.026 2.66 ± 0.11 1.00<br />
NGC 4486 35 187.68466 12.38580 0.81 −7.020 ± 0.203 −8.483 ± 0.027 1.13 ± 0.19 0.94<br />
NGC 4486 36 187.68490 12.38916 0.78 −6.424 ± 0.038 −7.900 ± 0.047 2.19 ± 0.26 1.00<br />
NGC 4486 37 187.68490 12.40223 0.89 −6.663 ± 0.048 −8.142 ± 0.043 2.11 ± 0.28 1.00<br />
NGC 4486 38 187.68493 12.40344 0.91 −7.964 ± 0.028 −9.340 ± 0.018 2.50 ± 0.14 1.00<br />
NGC 4486 40 187.68495 12.39694 0.81 −5.892 ± 0.144 −7.426 ± 0.188 6.10 ± 1.43 0.73<br />
NGC 4486 41 187.68507 12.37861 0.91 −8.357 ± 0.015 −9.763 ± 0.017 2.27 ± 0.10 1.00<br />
NGC 4486 42 187.68526 12.38329 0.82 −5.189 ± 0.483 −6.239 ± 0.483 1.79 ± 0.88 0.98<br />
NGC 4486 43 187.68537 12.41710 1.25 −5.772 ± 0.129 −7.251 ± 0.068 1.73 ± 0.42 0.99<br />
NGC 4486 44 187.68544 12.40953 1.03 −6.311 ± 0.052 −7.575 ± 0.044 2.08 ± 0.28 1.00<br />
NGC 4486 45 187.68554 12.39527 0.77 −8.715 ± 0.018 −9.714 ± 0.017 3.69 ± 0.08 1.00<br />
NGC 4486 46 187.68553 12.40173 0.86 −8.396 ± 0.019 −9.358 ± 0.042 3.63 ± 0.22 1.00<br />
NGC 4486 48 187.68557 12.39950 0.82 −8.797 ± 0.016 −9.849 ± 0.020 2.72 ± 0.11 1.00<br />
NGC 4486 49 187.68556 12.37088 1.08 −6.140 ± 0.060 −7.703 ± 0.061 2.59 ± 0.31 1.00<br />
NGC 4486 50 187.68576 12.39088 0.75 −8.127 ± 0.021 −9.173 ± 0.021 2.62 ± 0.12 1.00<br />
NGC 4486 52 187.68586 12.40671 0.95 −7.200 ± 0.039 −8.314 ± 0.038 3.15 ± 0.23 1.00<br />
NGC 4486 53 187.68584 12.40290 0.87 −7.420 ± 0.030 −8.753 ± 0.032 2.73 ± 0.18 1.00<br />
NGC 4486 54 187.68586 12.36574 1.22 −5.940 ± 1.395 −6.572 ± 0.596 1.00 ± 0.91 0.86<br />
Continued on Next Page. . .<br />
344
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4486 55 187.68595 12.38170 0.82 −9.517 ± 0.016 −10.629 ± 0.016 8.51 ± 0.10 0.87<br />
NGC 4486 56 187.68593 12.39914 0.80 −7.571 ± 0.060 −8.496 ± 0.056 3.94 ± 0.28 1.00<br />
NGC 4486 57 187.68595 12.41606 1.20 −9.526 ± 0.024 −10.569 ± 0.028 4.16 ± 0.12 1.00<br />
NGC 4486 58 187.68591 12.39411 0.75 −6.719 ± 0.054 −7.273 ± 0.062 2.67 ± 0.29 0.99<br />
NGC 4486 59 187.68592 12.40028 0.82 −6.425 ± 0.046 −7.957 ± 0.033 1.41 ± 0.29 0.98<br />
NGC 4486 60 187.68599 12.36948 1.10 −8.412 ± 0.025 −10.033 ± 0.017 2.64 ± 0.18 1.00<br />
NGC 4486 61 187.68600 12.38544 0.77 −8.599 ± 0.018 −9.804 ± 0.017 1.90 ± 0.14 1.00<br />
NGC 4486 62 187.68603 12.39477 0.75 −8.492 ± 0.054 −10.012 ± 0.014 2.94 ± 0.29 1.00<br />
NGC 4486 64 187.68601 12.37244 1.02 −7.134 ± 0.037 −8.576 ± 0.023 2.55 ± 0.19 1.00<br />
NGC 4486 66 187.68632 12.38425 0.77 −9.093 ± 0.015 −10.082 ± 0.015 3.20 ± 0.16 1.00<br />
NGC 4486 67 187.68625 12.40321 0.86 −6.814 ± 0.033 −8.225 ± 0.036 1.54 ± 0.24 0.99<br />
NGC 4486 68 187.68619 12.39168 0.73 −9.094 ± 0.016 −10.206 ± 0.014 2.71 ± 0.11 1.00<br />
NGC 4486 70 187.68629 12.39695 0.76 −6.856 ± 0.039 −8.219 ± 0.025 2.03 ± 0.24 1.00<br />
NGC 4486 71 187.68634 12.38406 0.77 −7.804 ± 0.030 −9.058 ± 0.030 2.94 ± 0.19 1.00<br />
NGC 4486 72 187.68633 12.39435 0.74 −8.108 ± 0.022 −9.701 ± 0.022 2.44 ± 0.10 1.00<br />
NGC 4486 74 187.68642 12.38926 0.73 −9.055 ± 0.016 −10.009 ± 0.013 2.55 ± 0.09 1.00<br />
NGC 4486 77 187.68612 12.39014 0.74 −6.992 ± 0.072 −8.399 ± 0.050 2.87 ± 0.32 1.00<br />
NGC 4486 78 187.68650 12.38876 0.73 −6.904 ± 0.053 −8.344 ± 0.040 2.46 ± 0.20 1.00<br />
NGC 4486 80 187.68656 12.40785 0.96 −8.028 ± 0.023 −8.866 ± 0.035 2.74 ± 0.14 1.00<br />
NGC 4486 81 187.68657 12.41385 1.12 −6.450 ± 0.063 −8.143 ± 0.057 3.95 ± 0.32 1.00<br />
NGC 4486 82 187.68668 12.41247 1.08 −6.951 ± 0.041 −7.952 ± 0.031 2.20 ± 0.24 1.00<br />
NGC 4486 83 187.68672 12.41538 1.16 −6.650 ± 0.042 −7.969 ± 0.022 2.33 ± 0.31 1.00<br />
NGC 4486 84 187.68695 12.37574 0.91 −9.252 ± 0.021 −10.173 ± 0.016 4.07 ± 0.09 1.00<br />
NGC 4486 86 187.68703 12.40251 0.82 −7.310 ± 0.042 −8.867 ± 0.022 2.43 ± 0.15 1.00<br />
NGC 4486 88 187.68714 12.38966 0.70 −8.309 ± 0.025 −9.242 ± 0.031 2.69 ± 0.15 1.00<br />
NGC 4486 89 187.68712 12.40365 0.84 −6.308 ± 0.055 −7.187 ± 0.177 2.92 ± 0.86 0.99<br />
NGC 4486 90 187.68715 12.37508 0.92 −6.605 ± 0.035 −7.645 ± 0.050 2.27 ± 0.28 1.00<br />
NGC 4486 92 187.68726 12.36935 1.08 −8.082 ± 0.050 −9.144 ± 0.026 3.49 ± 0.26 1.00<br />
NGC 4486 93 187.68725 12.40004 0.77 −5.116 ± 0.507 −6.083 ± 0.624 4.47 ± 6.47 0.82<br />
NGC 4486 94 187.68726 12.39688 0.73 −7.221 ± 0.027 −8.208 ± 0.044 2.63 ± 0.31 1.00<br />
NGC 4486 95 187.68738 12.39583 0.71 −8.861 ± 0.014 −9.889 ± 0.015 3.06 ± 0.08 1.00<br />
NGC 4486 96 187.68750 12.39544 0.70 −9.091 ± 0.013 −9.998 ± 0.022 4.27 ± 0.08 1.00<br />
NGC 4486 97 187.68739 12.36460 1.22 −8.087 ± 0.023 −9.631 ± 0.022 2.72 ± 0.15 1.00<br />
NGC 4486 98 187.68752 12.41015 0.99 −9.584 ± 0.021 −11.125 ± 0.014 3.54 ± 0.11 1.00<br />
NGC 4486 99 187.68750 12.38753 0.70 −7.921 ± 0.025 −9.000 ± 0.031 2.74 ± 0.13 1.00<br />
NGC 4486 100 187.68750 12.37094 1.03 −4.786 ± 0.214 −6.436 ± 0.165 4.63 ± 1.00 0.77<br />
NGC 4486 101 187.68608 12.41581 1.19 −6.264 ± 0.394 −7.509 ± 0.117 3.42 ± 0.57 0.99<br />
NGC 4486 103 187.68758 12.38509 0.72 −8.982 ± 0.016 −10.014 ± 0.013 2.45 ± 0.11 1.00<br />
NGC 4486 104 187.68762 12.40417 0.84 −9.204 ± 0.012 −10.181 ± 0.014 2.29 ± 0.07 1.00<br />
NGC 4486 105 187.68756 12.39664 0.71 −5.990 ± 0.089 −6.716 ± 0.098 4.34 ± 0.52 0.84<br />
NGC 4486 106 187.68758 12.40589 0.88 −6.707 ± 0.038 −7.925 ± 0.244 4.81 ± 3.35 0.97<br />
NGC 4486 107 187.68774 12.37978 0.80 −9.385 ± 0.019 −10.405 ± 0.019 2.43 ± 0.14 1.00<br />
NGC 4486 108 187.68768 12.40961 0.97 −5.242 ± 0.465 −6.697 ± 0.793 2.69 ± 0.76 0.99<br />
NGC 4486 109 187.68772 12.40974 0.98 −7.755 ± 0.030 −8.695 ± 0.055 3.49 ± 0.25 1.00<br />
NGC 4486 110 187.68779 12.37269 0.97 −8.317 ± 0.012 −9.122 ± 0.026 2.99 ± 0.12 1.00<br />
NGC 4486 113 187.68777 12.40481 0.85 −6.424 ± 0.060 −7.878 ± 0.053 1.93 ± 0.30 1.00<br />
NGC 4486 114 187.68783 12.36292 1.26 −7.787 ± 0.026 −8.860 ± 0.023 3.11 ± 0.13 1.00<br />
NGC 4486 116 187.68785 12.40967 0.97 −7.056 ± 0.035 −8.421 ± 0.051 2.64 ± 0.25 1.00<br />
NGC 4486 117 187.68767 12.41558 1.15 −6.074 ± 0.065 −7.340 ± 0.034 1.51 ± 0.25 0.98<br />
NGC 4486 118 187.68791 12.37095 1.02 −6.579 ± 0.057 −7.931 ± 0.053 3.55 ± 0.31 0.99<br />
NGC 4486 119 187.68793 12.36950 1.06 −5.916 ± 0.327 −6.931 ± 0.058 3.11 ± 0.88 0.98<br />
NGC 4486 121 187.68799 12.40011 0.75 −6.676 ± 0.060 −7.990 ± 0.060 2.70 ± 0.27 1.00<br />
NGC 4486 122 187.68805 12.41241 1.04 −8.118 ± 0.026 −9.545 ± 0.015 2.20 ± 0.12 1.00<br />
NGC 4486 123 187.68618 12.39520 0.75 −7.930 ± 0.024 −9.383 ± 0.021 2.45 ± 0.11 1.00<br />
NGC 4486 124 187.68616 12.40050 0.81 −5.832 ± 0.074 −7.490 ± 0.117 3.43 ± 0.62 0.99<br />
NGC 4486 125 187.68810 12.39095 0.66 −7.859 ± 0.037 −9.164 ± 0.020 2.27 ± 0.15 1.00<br />
NGC 4486 126 187.68809 12.41410 1.09 −7.349 ± 0.029 −8.257 ± 0.037 2.76 ± 0.19 1.00<br />
NGC 4486 128 187.68811 12.41034 0.98 −6.103 ± 0.104 −6.849 ± 0.141 3.41 ± 0.67 0.96<br />
NGC 4486 129 187.68814 12.38374 0.72 −6.546 ± 0.049 −8.013 ± 0.040 2.34 ± 0.27 1.00<br />
NGC 4486 130 187.68620 12.40664 0.94 −6.825 ± 0.050 −8.061 ± 0.041 2.42 ± 0.22 1.00<br />
NGC 4486 131 187.68822 12.40798 0.92 −7.121 ± 0.036 −8.597 ± 0.027 2.64 ± 0.15 1.00<br />
NGC 4486 134 187.68833 12.41091 0.99 −5.901 ± 0.108 −7.113 ± 0.077 2.40 ± 0.48 0.99<br />
Continued on Next Page. . .<br />
345
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4486 135 187.68635 12.40673 0.94 −8.421 ± 0.013 −9.695 ± 0.014 1.87 ± 0.11 1.00<br />
NGC 4486 136 187.68841 12.37975 0.78 −9.169 ± 0.015 −10.089 ± 0.014 2.13 ± 0.10 1.00<br />
NGC 4486 138 187.68837 12.40562 0.85 −6.277 ± 0.117 −7.275 ± 0.194 4.41 ± 0.94 0.93<br />
NGC 4486 139 187.68843 12.41751 1.19 −6.786 ± 0.175 −7.726 ± 0.085 3.34 ± 0.44 0.99<br />
NGC 4486 140 187.68846 12.37602 0.86 −6.925 ± 0.040 −7.732 ± 1.240 2.64 ± 0.31 1.00<br />
NGC 4486 141 187.68845 12.38348 0.71 −6.952 ± 0.035 −7.887 ± 0.048 2.86 ± 0.33 1.00<br />
NGC 4486 142 187.68846 12.38410 0.70 −8.208 ± 0.021 −9.189 ± 0.038 2.81 ± 0.15 1.00<br />
NGC 4486 144 187.68847 12.40405 0.81 −7.504 ± 0.031 −8.710 ± 0.032 2.32 ± 0.22 1.00<br />
NGC 4486 145 187.68848 12.37419 0.91 −5.597 ± 0.453 −6.795 ± 0.302 1.89 ± 0.45 0.99<br />
NGC 4486 146 187.68857 12.37621 0.86 −7.055 ± 0.024 −8.531 ± 0.028 2.46 ± 0.21 1.00<br />
NGC 4486 147 187.68857 12.39465 0.66 −7.476 ± 0.030 −8.714 ± 0.021 2.34 ± 0.29 1.00<br />
NGC 4486 148 187.68878 12.38744 0.65 −6.799 ± 0.039 −8.155 ± 0.052 2.43 ± 0.22 1.00<br />
NGC 4486 149 187.68884 12.40277 0.77 −9.971 ± 0.013 −10.991 ± 0.014 2.66 ± 0.14 1.00<br />
NGC 4486 150 187.68882 12.40808 0.90 −7.496 ± 0.022 −8.411 ± 0.027 2.77 ± 0.13 1.00<br />
NGC 4486 151 187.68880 12.41463 1.10 −5.725 ± 0.133 −7.128 ± 0.040 1.97 ± 0.39 0.99<br />
NGC 4486 152 187.68889 12.38839 0.64 −8.191 ± 0.023 −9.096 ± 0.037 2.66 ± 0.22 1.00<br />
NGC 4486 153 187.68897 12.37560 0.86 −7.477 ± 0.031 −8.231 ± 0.039 2.61 ± 0.19 1.00<br />
NGC 4486 154 187.68900 12.38770 0.64 −7.975 ± 0.033 −9.311 ± 0.020 2.46 ± 0.17 1.00<br />
NGC 4486 155 187.68905 12.39807 0.68 −8.993 ± 0.024 −10.466 ± 0.016 2.26 ± 0.12 1.00<br />
NGC 4486 156 187.68905 12.37512 0.87 −8.079 ± 0.020 −9.501 ± 0.019 2.43 ± 0.10 1.00<br />
NGC 4486 157 187.68908 12.38234 0.71 −7.245 ± 0.022 −8.779 ± 0.027 2.38 ± 0.19 1.00<br />
NGC 4486 158 187.68906 12.39029 0.63 −5.330 ± 0.278 −7.114 ± 0.084 3.06 ± 0.50 0.99<br />
NGC 4486 159 187.68915 12.39417 0.63 −8.482 ± 0.016 −9.885 ± 0.014 2.05 ± 0.08 1.00<br />
NGC 4486 160 187.68918 12.36736 1.09 −9.246 ± 0.018 −10.514 ± 0.014 2.78 ± 0.12 1.00<br />
NGC 4486 161 187.68914 12.41707 1.16 −5.379 ± 0.459 −7.008 ± 0.072 2.13 ± 0.47 1.00<br />
NGC 4486 162 187.68915 12.39999 0.71 −5.929 ± 0.139 −7.785 ± 0.132 4.53 ± 0.84 0.97<br />
NGC 4486 163 187.68921 12.39703 0.66 −8.585 ± 0.022 −10.000 ± 0.021 2.48 ± 0.10 1.00<br />
NGC 4486 164 187.68920 12.38874 0.63 −5.197 ± 0.109 −6.797 ± 0.074 1.76 ± 0.44 0.98<br />
NGC 4486 165 187.68920 12.38141 0.72 −5.317 ± 0.193 −7.017 ± 0.977 1.12 ± 0.55 0.91<br />
NGC 4486 166 187.68929 12.36933 1.03 −6.648 ± 0.095 −7.931 ± 0.258 7.33 ± 2.57 0.61<br />
NGC 4486 168 187.68927 12.37668 0.83 −7.940 ± 0.024 −8.903 ± 0.015 2.38 ± 0.14 1.00<br />
NGC 4486 169 187.68927 12.40642 0.85 −6.070 ± 0.073 −6.882 ± 0.309 1.83 ± 0.54 0.99<br />
NGC 4486 170 187.68928 12.39064 0.62 −6.833 ± 0.028 −7.752 ± 0.073 2.52 ± 0.32 1.00<br />
NGC 4486 171 187.68929 12.41623 1.13 −7.581 ± 0.039 −9.096 ± 0.022 2.74 ± 0.17 1.00<br />
NGC 4486 172 187.68930 12.38000 0.75 −6.595 ± 0.037 −8.159 ± 0.038 1.89 ± 0.21 1.00<br />
NGC 4486 174 187.68932 12.41315 1.04 −5.816 ± 0.074 −7.442 ± 0.370 2.83 ± 0.54 0.99<br />
NGC 4486 175 187.68939 12.40072 0.71 −6.358 ± 0.048 −7.230 ± 0.056 2.21 ± 0.30 1.00<br />
NGC 4486 176 187.68942 12.41296 1.03 −6.859 ± 0.042 −8.212 ± 0.047 2.61 ± 0.28 1.00<br />
NGC 4486 177 187.68952 12.40530 0.81 −10.167 ± 0.015 −11.218 ± 0.017 3.62 ± 0.08 1.00<br />
NGC 4486 178 187.68952 12.39654 0.64 −8.891 ± 0.012 −10.036 ± 0.024 2.78 ± 0.15 1.00<br />
NGC 4486 180 187.68958 12.38566 0.64 −9.570 ± 0.011 −10.711 ± 0.014 3.43 ± 0.09 1.00<br />
NGC 4486 181 187.68959 12.38684 0.63 −8.554 ± 0.020 −9.508 ± 0.027 3.39 ± 0.14 1.00<br />
NGC 4486 182 187.68952 12.38874 0.62 −5.016 ± 0.124 −6.240 ± 0.261 2.94 ± 0.56 0.98<br />
NGC 4486 183 187.68959 12.39740 0.65 −6.927 ± 0.062 −7.647 ± 0.039 3.14 ± 0.23 0.99<br />
NGC 4486 185 187.68962 12.39886 0.67 −6.377 ± 0.130 −6.946 ± 0.190 5.17 ± 1.29 0.73<br />
NGC 4486 186 187.68969 12.40338 0.76 −6.157 ± 0.043 −7.502 ± 0.378 1.91 ± 0.33 1.00<br />
NGC 4486 187 187.68973 12.39013 0.60 −6.025 ± 0.066 −7.518 ± 0.150 4.56 ± 0.86 0.94<br />
NGC 4486 188 187.68982 12.39978 0.68 −5.842 ± 0.054 −6.993 ± 0.177 1.66 ± 0.44 0.98<br />
NGC 4486 189 187.68984 12.41597 1.12 −6.620 ± 0.097 −7.578 ± 0.162 4.38 ± 0.97 0.96<br />
NGC 4486 191 187.68987 12.41281 1.02 −6.050 ± 0.054 −7.515 ± 0.038 1.71 ± 0.22 0.99<br />
NGC 4486 192 187.68994 12.37799 0.77 −6.905 ± 0.035 −8.354 ± 0.026 2.36 ± 0.23 1.00<br />
NGC 4486 193 187.68994 12.37871 0.76 −7.521 ± 0.023 −8.732 ± 0.028 2.53 ± 0.18 1.00<br />
NGC 4486 195 187.68993 12.36917 1.02 −6.048 ± 0.069 −7.655 ± 0.053 2.12 ± 0.32 1.00<br />
NGC 4486 196 187.69004 12.37314 0.90 −8.758 ± 0.013 −9.937 ± 0.017 2.43 ± 0.09 1.00<br />
NGC 4486 197 187.69002 12.39930 0.67 −6.049 ± 0.154 −7.433 ± 0.135 1.23 ± 0.28 0.95<br />
NGC 4486 198 187.69022 12.38822 0.59 −10.468 ± 0.020 −11.782 ± 0.014 3.00 ± 0.17 1.00<br />
NGC 4486 199 187.69017 12.40648 0.82 −7.630 ± 0.026 −8.610 ± 0.052 2.88 ± 0.23 1.00<br />
NGC 4486 200 187.69019 12.40061 0.69 −8.260 ± 0.052 −9.613 ± 0.070 6.88 ± 0.56 1.00<br />
NGC 4486 201 187.69025 12.40534 0.79 −10.034 ± 0.014 −11.475 ± 0.010 2.51 ± 0.11 1.00<br />
NGC 4486 202 187.69024 12.40079 0.69 −7.086 ± 0.031 −8.093 ± 0.030 1.96 ± 0.21 1.00<br />
NGC 4486 203 187.69025 12.40033 0.68 −6.131 ± 0.066 −7.498 ± 0.071 2.39 ± 0.34 1.00<br />
NGC 4486 204 187.69028 12.40694 0.83 −7.334 ± 0.050 −8.430 ± 0.058 3.51 ± 0.24 1.00<br />
Continued on Next Page. . .<br />
346
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4486 205 187.69027 12.39465 0.60 −6.786 ± 0.053 −7.909 ± 0.058 2.48 ± 0.38 1.00<br />
NGC 4486 206 187.69028 12.37838 0.76 −6.671 ± 0.057 −8.211 ± 0.065 2.79 ± 0.38 1.00<br />
NGC 4486 207 187.68999 12.39160 0.59 −7.152 ± 0.032 −8.798 ± 0.032 2.37 ± 0.25 1.00<br />
NGC 4486 208 187.69037 12.38284 0.66 −6.765 ± 0.046 −7.779 ± 0.107 3.35 ± 0.67 0.99<br />
NGC 4486 209 187.68993 12.38703 0.61 −8.498 ± 0.018 −9.483 ± 0.022 2.59 ± 0.14 1.00<br />
NGC 4486 210 187.69045 12.40117 0.69 −7.891 ± 0.026 −8.875 ± 0.029 3.03 ± 0.16 1.00<br />
NGC 4486 211 187.69045 12.38621 0.60 −7.439 ± 0.038 −8.702 ± 0.029 1.98 ± 0.16 1.00<br />
NGC 4486 212 187.69049 12.38304 0.65 −6.017 ± 0.102 −7.420 ± 0.058 2.68 ± 0.40 0.99<br />
NGC 4486 213 187.69049 12.38704 0.59 −5.161 ± 0.123 −6.754 ± 0.342 1.96 ± 0.88 0.99<br />
NGC 4486 214 187.69060 12.38808 0.58 −8.098 ± 0.025 −9.285 ± 0.024 2.23 ± 0.14 1.00<br />
NGC 4486 216 187.69065 12.36268 1.22 −7.204 ± 0.029 −8.202 ± 0.036 2.94 ± 0.17 1.00<br />
NGC 4486 217 187.69069 12.36886 1.02 −6.752 ± 0.053 −7.726 ± 0.069 2.88 ± 0.29 1.00<br />
NGC 4486 218 187.69066 12.39043 0.57 −6.627 ± 0.819 −8.206 ± 0.306 1.37 ± 0.34 0.98<br />
NGC 4486 219 187.69072 12.38592 0.60 −8.267 ± 0.030 −9.531 ± 0.021 2.24 ± 0.13 1.00<br />
NGC 4486 220 187.69071 12.38789 0.58 −7.290 ± 0.026 −8.863 ± 0.025 1.55 ± 0.19 0.99<br />
NGC 4486 221 187.69072 12.38506 0.61 −7.827 ± 0.018 −8.714 ± 0.029 1.65 ± 0.14 1.00<br />
NGC 4486 223 187.69078 12.37696 0.78 −7.717 ± 0.017 −9.153 ± 0.025 1.96 ± 0.14 1.00<br />
NGC 4486 225 187.69078 12.39673 0.60 −5.899 ± 0.079 −6.976 ± 0.198 4.33 ± 0.92 0.88<br />
NGC 4486 226 187.69091 12.41048 0.92 −6.888 ± 0.038 −7.896 ± 0.079 2.77 ± 0.33 1.00<br />
NGC 4486 227 187.69092 12.40582 0.79 −8.240 ± 0.022 −9.142 ± 0.017 2.77 ± 0.12 1.00<br />
NGC 4486 228 187.69095 12.37879 0.73 −7.990 ± 0.021 −8.940 ± 0.022 2.40 ± 0.12 1.00<br />
NGC 4486 230 187.69106 12.39519 0.57 −7.569 ± 0.116 −8.960 ± 0.040 2.01 ± 0.22 1.00<br />
NGC 4486 231 187.69109 12.38390 0.61 −6.192 ± 0.061 −7.079 ± 0.124 2.12 ± 0.53 1.00<br />
NGC 4486 233 187.69110 12.41548 1.08 −5.480 ± 0.146 −7.048 ± 0.061 1.39 ± 0.46 0.96<br />
NGC 4486 234 187.69118 12.40012 0.64 −7.041 ± 0.035 −8.565 ± 0.032 1.70 ± 0.17 1.00<br />
NGC 4486 235 187.69126 12.36241 1.22 −8.591 ± 0.039 −10.171 ± 0.052 4.13 ± 0.47 1.00<br />
NGC 4486 236 187.69138 12.36333 1.18 −8.583 ± 0.023 −9.963 ± 0.017 3.56 ± 0.16 1.00<br />
NGC 4486 237 187.69129 12.39742 0.59 −5.012 ± 0.149 −6.481 ± 0.138 3.16 ± 0.60 0.97<br />
NGC 4486 238 187.69133 12.41375 1.01 −6.215 ± 0.143 −7.611 ± 0.085 3.85 ± 0.71 0.98<br />
NGC 4486 239 187.69136 12.39265 0.54 −8.165 ± 0.025 −9.598 ± 0.024 2.05 ± 0.19 1.00<br />
NGC 4486 240 187.69142 12.37938 0.70 −5.435 ± 0.844 −7.079 ± 0.115 1.52 ± 0.54 0.97<br />
NGC 4486 243 187.69155 12.40473 0.74 −5.892 ± 0.112 −7.135 ± 0.086 3.48 ± 0.50 0.97<br />
NGC 4486 244 187.69111 12.40672 0.81 −6.216 ± 0.060 −7.634 ± 0.060 2.12 ± 0.39 1.00<br />
NGC 4486 245 187.69158 12.40550 0.76 −5.811 ± 0.060 −7.207 ± 0.054 2.09 ± 0.28 1.00<br />
NGC 4486 246 187.69162 12.39466 0.55 −6.836 ± 0.054 −8.039 ± 0.066 2.61 ± 0.30 1.00<br />
NGC 4486 248 187.69170 12.39718 0.58 −6.349 ± 0.087 −7.610 ± 0.268 5.10 ± 2.29 0.92<br />
NGC 4486 249 187.69182 12.40965 0.88 −10.095 ± 0.016 −11.058 ± 0.012 2.45 ± 0.13 1.00<br />
NGC 4486 250 187.69185 12.37298 0.86 −8.524 ± 0.031 −9.278 ± 0.030 5.08 ± 0.21 1.00<br />
NGC 4486 251 187.69188 12.39425 0.53 −9.734 ± 0.016 −10.725 ± 0.020 4.08 ± 0.09 1.00<br />
NGC 4486 252 187.69186 12.38718 0.54 −6.443 ± 0.285 −7.857 ± 0.290 2.31 ± 0.48 1.00<br />
NGC 4486 253 187.69188 12.38911 0.53 −7.878 ± 0.042 −9.404 ± 0.026 2.44 ± 0.27 1.00<br />
NGC 4486 254 187.69188 12.38021 0.67 −7.264 ± 0.031 −8.894 ± 0.029 2.33 ± 0.23 1.00<br />
NGC 4486 255 187.69195 12.38874 0.53 −8.240 ± 0.022 −9.436 ± 0.019 2.34 ± 0.11 1.00<br />
NGC 4486 256 187.69198 12.38470 0.57 −5.463 ± 0.187 −6.426 ± 0.470 5.24 ± 1.86 0.61<br />
NGC 4486 257 187.69207 12.40982 0.88 −5.327 ± 0.379 −6.402 ± 0.270 3.80 ± 1.88 0.92<br />
NGC 4486 258 187.69213 12.37099 0.92 −5.732 ± 0.090 −7.368 ± 0.053 2.92 ± 0.28 0.99<br />
NGC 4486 260 187.69220 12.37774 0.72 −7.206 ± 0.045 −8.747 ± 0.035 2.73 ± 0.21 1.00<br />
NGC 4486 261 187.69229 12.36337 1.17 −5.880 ± 0.096 −7.441 ± 0.045 2.16 ± 0.36 1.00<br />
NGC 4486 262 187.69228 12.39800 0.57 −7.291 ± 0.030 −8.805 ± 0.025 2.09 ± 0.16 1.00<br />
NGC 4486 263 187.69230 12.40779 0.81 −6.571 ± 0.040 −7.766 ± 0.061 2.50 ± 0.30 1.00<br />
NGC 4486 266 187.69237 12.40325 0.68 −5.899 ± 0.370 −6.775 ± 0.088 1.77 ± 0.47 0.98<br />
NGC 4486 267 187.69243 12.37641 0.75 −7.894 ± 0.025 −9.259 ± 0.022 1.60 ± 0.12 1.00<br />
NGC 4486 268 187.69241 12.38173 0.61 −5.877 ± 0.034 −7.096 ± 0.105 3.81 ± 0.41 0.95<br />
NGC 4486 269 187.69243 12.39276 0.50 −7.702 ± 0.023 −8.596 ± 0.032 2.64 ± 0.16 1.00<br />
NGC 4486 270 187.69252 12.38335 0.58 −7.599 ± 0.018 −8.818 ± 0.025 2.60 ± 0.19 1.00<br />
NGC 4486 271 187.69252 12.39737 0.55 −6.190 ± 0.238 −7.600 ± 0.069 2.49 ± 0.58 1.00<br />
NGC 4486 272 187.69253 12.36947 0.96 −5.506 ± 0.071 −6.887 ± 0.033 2.36 ± 0.27 0.99<br />
NGC 4486 273 187.69259 12.37453 0.80 −5.156 ± 0.158 −6.895 ± 0.401 2.22 ± 0.70 0.99<br />
NGC 4486 274 187.69252 12.39791 0.56 −5.097 ± 1.080 −6.915 ± 0.219 4.37 ± 1.42 0.87<br />
NGC 4486 275 187.69269 12.38173 0.61 −8.002 ± 0.076 −8.986 ± 0.129 7.13 ± 0.90 0.95<br />
NGC 4486 276 187.69269 12.37166 0.89 −6.839 ± 0.047 −8.145 ± 0.036 2.22 ± 0.19 1.00<br />
NGC 4486 277 187.69275 12.39708 0.54 −8.552 ± 0.026 −9.952 ± 0.022 2.06 ± 0.23 1.00<br />
Continued on Next Page. . .<br />
347
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4486 278 187.69276 12.40219 0.64 −9.741 ± 0.014 −10.717 ± 0.018 3.36 ± 0.09 1.00<br />
NGC 4486 279 187.69275 12.38140 0.61 −7.320 ± 0.035 −8.679 ± 0.034 2.27 ± 0.26 1.00<br />
NGC 4486 281 187.69273 12.40316 0.67 −6.284 ± 0.088 −7.487 ± 0.440 2.32 ± 0.44 1.00<br />
NGC 4486 282 187.69281 12.40580 0.74 −9.966 ± 0.048 −10.875 ± 0.035 6.92 ± 0.22 1.00<br />
NGC 4486 283 187.69284 12.37914 0.66 −8.396 ± 0.017 −9.477 ± 0.024 3.40 ± 0.10 1.00<br />
NGC 4486 284 187.69286 12.37050 0.92 −8.399 ± 0.022 −9.893 ± 0.021 2.46 ± 0.17 1.00<br />
NGC 4486 286 187.69284 12.41184 0.92 −7.542 ± 0.024 −8.521 ± 0.022 2.50 ± 0.22 1.00<br />
NGC 4486 287 187.69291 12.40710 0.77 −8.252 ± 0.015 −9.218 ± 0.024 2.46 ± 0.12 1.00<br />
NGC 4486 288 187.69290 12.39809 0.55 −7.415 ± 0.042 −8.511 ± 0.041 2.83 ± 0.21 1.00<br />
NGC 4486 291 187.69292 12.39098 0.48 −6.355 ± 0.060 −7.597 ± 0.546 1.60 ± 0.41 0.99<br />
NGC 4486 292 187.69301 12.37849 0.68 −5.118 ± 0.361 −6.200 ± 0.488 3.82 ± 2.35 0.92<br />
NGC 4486 293 187.69302 12.40155 0.62 −5.384 ± 0.152 −7.152 ± 0.206 3.57 ± 1.24 0.97<br />
NGC 4486 294 187.69307 12.40965 0.85 −9.252 ± 0.026 −10.041 ± 0.020 3.80 ± 0.12 1.00<br />
NGC 4486 295 187.69309 12.37566 0.76 −6.517 ± 0.063 −7.322 ± 0.062 2.78 ± 0.33 0.99<br />
NGC 4486 296 187.69312 12.38956 0.48 −6.071 ± 0.132 −7.178 ± 0.093 3.78 ± 0.64 0.96<br />
NGC 4486 297 187.69316 12.39110 0.47 −7.693 ± 0.031 −8.761 ± 0.030 1.81 ± 0.20 1.00<br />
NGC 4486 298 187.69320 12.37168 0.88 −7.804 ± 0.031 −8.612 ± 0.027 2.49 ± 0.20 1.00<br />
NGC 4486 299 187.69315 12.40347 0.67 −6.697 ± 0.198 −7.963 ± 0.056 1.95 ± 0.35 1.00<br />
NGC 4486 300 187.69316 12.41158 0.91 −6.792 ± 0.057 −8.452 ± 0.071 2.78 ± 0.40 1.00<br />
NGC 4486 301 187.69327 12.41768 1.11 −9.480 ± 0.026 −10.938 ± 0.012 2.45 ± 0.13 1.00<br />
NGC 4486 302 187.69324 12.38767 0.49 −8.902 ± 0.034 −9.738 ± 0.043 5.04 ± 0.19 1.00<br />
NGC 4486 303 187.69324 12.40898 0.82 −7.202 ± 0.032 −8.742 ± 0.034 2.48 ± 0.23 1.00<br />
NGC 4486 304 187.69328 12.37405 0.80 −7.339 ± 0.031 −8.780 ± 0.032 2.46 ± 0.21 1.00<br />
NGC 4486 305 187.69321 12.39450 0.49 −5.513 ± 0.511 −7.061 ± 0.288 1.29 ± 0.61 0.95<br />
NGC 4486 306 187.69327 12.39515 0.49 −6.501 ± 0.131 −7.699 ± 0.148 5.64 ± 0.96 0.90<br />
NGC 4486 308 187.69333 12.38484 0.52 −6.938 ± 0.036 −7.787 ± 0.102 2.32 ± 0.35 1.00<br />
NGC 4486 310 187.69336 12.41454 1.00 −7.375 ± 0.031 −8.541 ± 0.032 2.68 ± 0.19 1.00<br />
NGC 4486 311 187.69336 12.40067 0.59 −6.507 ± 0.055 −7.365 ± 0.050 2.19 ± 0.31 1.00<br />
NGC 4486 312 187.69339 12.37150 0.88 −6.720 ± 0.039 −7.548 ± 0.291 1.92 ± 0.29 1.00<br />
NGC 4486 313 187.69342 12.36619 1.05 −6.806 ± 0.055 −8.303 ± 0.038 2.84 ± 0.25 1.00<br />
NGC 4486 314 187.69347 12.38353 0.54 −9.688 ± 0.019 −10.810 ± 0.019 1.83 ± 0.14 1.00<br />
NGC 4486 315 187.69344 12.40475 0.69 −6.838 ± 0.047 −8.279 ± 0.028 1.67 ± 0.26 1.00<br />
NGC 4486 316 187.69349 12.38663 0.49 −7.117 ± 0.032 −8.104 ± 0.077 2.29 ± 0.29 1.00<br />
NGC 4486 317 187.69346 12.39958 0.56 −6.257 ± 0.059 −7.753 ± 0.047 2.51 ± 0.28 1.00<br />
NGC 4486 318 187.69349 12.38467 0.52 −6.456 ± 0.054 −7.874 ± 0.067 1.93 ± 0.35 1.00<br />
NGC 4486 319 187.69356 12.36448 1.11 −7.368 ± 0.029 −8.342 ± 0.025 2.73 ± 0.20 1.00<br />
NGC 4486 320 187.69356 12.40010 0.57 −8.967 ± 0.010 −9.787 ± 0.017 2.84 ± 0.08 1.00<br />
NGC 4486 321 187.69354 12.37786 0.68 −6.960 ± 0.027 −8.253 ± 0.036 2.30 ± 0.22 1.00<br />
NGC 4486 322 187.69361 12.39092 0.46 −9.349 ± 0.031 −10.571 ± 0.013 2.12 ± 0.09 1.00<br />
NGC 4486 323 187.69355 12.39239 0.46 −6.517 ± 0.058 −8.053 ± 0.236 4.93 ± 2.48 0.97<br />
NGC 4486 324 187.69362 12.38818 0.47 −8.872 ± 0.020 −9.857 ± 0.021 2.55 ± 0.12 1.00<br />
NGC 4486 328 187.69367 12.39110 0.45 −6.717 ± 0.050 −8.436 ± 0.069 3.07 ± 0.37 1.00<br />
NGC 4486 329 187.69372 12.39216 0.45 −8.083 ± 0.034 −9.468 ± 0.021 2.46 ± 0.14 1.00<br />
NGC 4486 330 187.69369 12.39387 0.47 −5.683 ± 0.091 −7.092 ± 0.107 2.92 ± 0.59 0.99<br />
NGC 4486 331 187.69372 12.39413 0.47 −8.284 ± 0.027 −9.720 ± 0.020 2.74 ± 0.12 1.00<br />
NGC 4486 332 187.69367 12.41037 0.86 −9.058 ± 0.014 −9.988 ± 0.013 2.62 ± 0.10 1.00<br />
NGC 4486 333 187.69368 12.41439 0.99 −5.136 ± 0.093 −6.350 ± 0.556 2.91 ± 1.29 0.98<br />
NGC 4486 334 187.69373 12.39942 0.55 −5.615 ± 0.115 −6.979 ± 0.121 2.41 ± 0.62 0.99<br />
NGC 4486 335 187.69379 12.39555 0.48 −8.978 ± 0.020 −10.325 ± 0.024 2.26 ± 0.15 1.00<br />
NGC 4486 336 187.69377 12.40194 0.61 −7.278 ± 0.044 −8.286 ± 0.029 2.05 ± 0.20 1.00<br />
NGC 4486 337 187.69379 12.39588 0.48 −7.416 ± 0.030 −8.435 ± 0.039 2.41 ± 0.20 1.00<br />
NGC 4486 341 187.69391 12.38182 0.57 −7.497 ± 0.040 −8.964 ± 0.020 2.10 ± 0.16 1.00<br />
NGC 4486 342 187.69393 12.37516 0.75 −7.654 ± 0.038 −9.295 ± 0.021 2.47 ± 0.17 1.00<br />
NGC 4486 343 187.69391 12.40067 0.57 −6.852 ± 0.052 −8.194 ± 0.268 1.84 ± 0.38 1.00<br />
NGC 4486 344 187.69392 12.40148 0.59 −6.872 ± 0.065 −8.444 ± 0.076 3.39 ± 0.47 1.00<br />
NGC 4486 345 187.69393 12.40316 0.64 −7.821 ± 0.021 −8.901 ± 0.035 2.91 ± 0.17 1.00<br />
NGC 4486 346 187.69393 12.37567 0.74 −5.480 ± 0.350 −6.855 ± 0.178 5.51 ± 3.69 0.62<br />
NGC 4486 348 187.69408 12.37697 0.69 −8.974 ± 0.022 −10.402 ± 0.018 2.68 ± 0.09 1.00<br />
NGC 4486 349 187.69406 12.37074 0.89 −8.652 ± 0.020 −9.546 ± 0.027 3.44 ± 0.12 1.00<br />
NGC 4486 350 187.69407 12.39609 0.48 −9.708 ± 0.015 −10.853 ± 0.010 2.57 ± 0.08 1.00<br />
NGC 4486 351 187.69405 12.36929 0.94 −5.924 ± 0.161 −7.411 ± 0.059 5.09 ± 0.83 0.88<br />
NGC 4486 352 187.69406 12.37537 0.74 −6.110 ± 0.083 −7.518 ± 0.108 4.01 ± 0.49 0.97<br />
Continued on Next Page. . .<br />
348
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4486 354 187.69411 12.39575 0.47 −8.551 ± 0.016 −9.427 ± 0.034 2.56 ± 0.15 1.00<br />
NGC 4486 355 187.69419 12.38943 0.44 −7.187 ± 0.035 −8.598 ± 0.033 1.82 ± 0.24 1.00<br />
NGC 4486 357 187.69420 12.41572 1.03 −7.356 ± 0.047 −8.371 ± 0.076 6.90 ± 0.42 0.84<br />
NGC 4486 358 187.69425 12.38920 0.44 −7.521 ± 0.027 −8.794 ± 0.032 2.11 ± 0.13 1.00<br />
NGC 4486 359 187.69423 12.38643 0.47 −8.048 ± 0.019 −9.672 ± 0.026 1.60 ± 0.16 1.00<br />
NGC 4486 360 187.69429 12.40655 0.73 −7.143 ± 0.040 −8.561 ± 0.034 2.32 ± 0.16 1.00<br />
NGC 4486 362 187.69429 12.40718 0.75 −6.826 ± 0.042 −8.099 ± 0.056 3.55 ± 0.21 0.99<br />
NGC 4486 363 187.69435 12.41321 0.94 −8.408 ± 0.069 −9.588 ± 0.025 2.30 ± 0.21 1.00<br />
NGC 4486 364 187.69441 12.37609 0.71 −7.617 ± 0.030 −8.703 ± 0.029 2.38 ± 0.16 1.00<br />
NGC 4486 365 187.69452 12.38854 0.43 −6.716 ± 0.067 −7.979 ± 0.060 2.36 ± 0.36 1.00<br />
NGC 4486 366 187.69452 12.40041 0.55 −6.454 ± 0.214 −8.290 ± 0.138 7.11 ± 1.58 0.78<br />
NGC 4486 367 187.69461 12.40046 0.55 −8.712 ± 0.021 −10.154 ± 0.014 2.12 ± 0.10 1.00<br />
NGC 4486 368 187.69459 12.39551 0.45 −6.714 ± 0.055 −8.246 ± 0.039 1.96 ± 0.21 1.00<br />
NGC 4486 369 187.69464 12.37124 0.86 −7.375 ± 0.028 −8.309 ± 0.038 2.94 ± 0.20 1.00<br />
NGC 4486 370 187.69464 12.38022 0.59 −7.685 ± 0.046 −8.652 ± 0.045 3.59 ± 0.28 1.00<br />
NGC 4486 371 187.69467 12.37718 0.67 −7.577 ± 0.024 −8.812 ± 0.026 1.77 ± 0.19 1.00<br />
NGC 4486 372 187.69474 12.38287 0.52 −9.759 ± 0.015 −10.568 ± 0.012 4.01 ± 0.06 1.00<br />
NGC 4486 374 187.69475 12.38094 0.57 −9.351 ± 0.011 −10.309 ± 0.014 2.00 ± 0.11 1.00<br />
NGC 4486 376 187.69480 12.37835 0.64 −6.805 ± 0.047 −8.271 ± 0.036 1.86 ± 0.20 1.00<br />
NGC 4486 377 187.69489 12.37448 0.75 −8.905 ± 0.015 −9.859 ± 0.020 3.29 ± 0.11 1.00<br />
NGC 4486 379 187.69489 12.36464 1.09 −8.712 ± 0.073 −9.364 ± 0.027 3.70 ± 0.28 1.00<br />
NGC 4486 380 187.69498 12.38188 0.54 −6.087 ± 0.069 −7.611 ± 0.121 2.88 ± 0.52 1.00<br />
NGC 4486 382 187.69507 12.40380 0.63 −8.295 ± 0.025 −9.325 ± 0.025 2.34 ± 0.18 1.00<br />
NGC 4486 384 187.69509 12.41742 1.08 −7.276 ± 0.057 −8.527 ± 0.076 5.23 ± 0.36 0.98<br />
NGC 4486 385 187.69516 12.39077 0.40 −7.306 ± 0.043 −8.626 ± 0.027 2.08 ± 0.25 1.00<br />
NGC 4486 386 187.69519 12.39602 0.44 −8.390 ± 0.028 −9.247 ± 0.017 2.33 ± 0.15 1.00<br />
NGC 4486 387 187.69524 12.36700 1.00 −6.279 ± 0.056 −7.984 ± 0.054 2.47 ± 0.31 1.00<br />
NGC 4486 388 187.69525 12.40541 0.67 −7.762 ± 0.019 −9.111 ± 0.019 1.75 ± 0.15 1.00<br />
NGC 4486 389 187.69530 12.38579 0.44 −8.096 ± 0.022 −9.007 ± 0.024 2.31 ± 0.16 1.00<br />
NGC 4486 390 187.69529 12.38718 0.42 −6.300 ± 0.047 −7.752 ± 0.057 2.30 ± 0.35 1.00<br />
NGC 4486 391 187.69531 12.37873 0.61 −5.914 ± 0.082 −7.262 ± 0.051 2.36 ± 0.41 1.00<br />
NGC 4486 392 187.69543 12.40279 0.59 −7.494 ± 0.030 −8.994 ± 0.026 2.20 ± 0.14 1.00<br />
NGC 4486 394 187.69544 12.37781 0.64 −7.210 ± 0.035 −8.596 ± 0.031 2.87 ± 0.22 1.00<br />
NGC 4486 395 187.69541 12.39712 0.45 −6.483 ± 0.064 −7.646 ± 0.065 1.91 ± 0.32 1.00<br />
NGC 4486 396 187.69547 12.38719 0.42 −8.029 ± 0.025 −8.994 ± 0.040 3.06 ± 0.25 1.00<br />
NGC 4486 397 187.69547 12.39994 0.51 −7.396 ± 0.035 −8.699 ± 0.054 3.31 ± 0.32 1.00<br />
NGC 4486 398 187.69554 12.37911 0.60 −8.413 ± 0.030 −9.733 ± 0.020 2.88 ± 0.15 1.00<br />
NGC 4486 400 187.69553 12.40508 0.65 −8.836 ± 0.015 −10.303 ± 0.013 2.06 ± 0.07 1.00<br />
NGC 4486 401 187.69552 12.40832 0.76 −6.002 ± 0.107 −7.074 ± 0.119 3.62 ± 0.59 0.96<br />
NGC 4486 402 187.69556 12.37186 0.83 −7.117 ± 0.031 −8.831 ± 0.025 2.22 ± 0.17 1.00<br />
NGC 4486 403 187.69555 12.39630 0.43 −7.314 ± 0.033 −8.337 ± 0.049 2.84 ± 0.15 1.00<br />
NGC 4486 404 187.69556 12.40596 0.68 −7.023 ± 0.043 −8.298 ± 0.045 2.22 ± 0.29 1.00<br />
NGC 4486 405 187.69563 12.37313 0.78 −6.839 ± 0.081 −8.593 ± 0.062 4.67 ± 0.37 1.00<br />
NGC 4486 406 187.69562 12.36999 0.89 −5.882 ± 0.052 −7.207 ± 0.046 1.63 ± 0.33 0.98<br />
NGC 4486 408 187.69567 12.38919 0.39 −8.432 ± 0.022 −9.547 ± 0.032 2.91 ± 0.20 1.00<br />
NGC 4486 409 187.69568 12.36237 1.16 −7.222 ± 0.047 −8.636 ± 0.032 2.53 ± 0.27 1.00<br />
NGC 4486 410 187.69571 12.39734 0.45 −9.184 ± 0.016 −10.374 ± 0.013 2.14 ± 0.14 1.00<br />
NGC 4486 411 187.69568 12.41200 0.88 −6.243 ± 0.039 −7.873 ± 0.059 2.76 ± 0.28 1.00<br />
NGC 4486 412 187.69573 12.36260 1.15 −5.813 ± 0.074 −6.662 ± 0.088 2.65 ± 0.42 0.99<br />
NGC 4486 414 187.69574 12.40229 0.57 −6.805 ± 0.031 −8.354 ± 0.053 2.72 ± 0.29 1.00<br />
NGC 4486 415 187.69582 12.36601 1.02 −9.063 ± 0.012 −10.636 ± 0.025 2.76 ± 0.11 1.00<br />
NGC 4486 416 187.69582 12.40626 0.69 −8.058 ± 0.025 −8.876 ± 0.023 2.55 ± 0.15 1.00<br />
NGC 4486 417 187.69579 12.39888 0.48 −5.512 ± 0.996 −6.545 ± 0.389 1.23 ± 0.45 0.92<br />
NGC 4486 418 187.69586 12.37676 0.66 −7.597 ± 0.032 −8.804 ± 0.033 2.13 ± 0.27 1.00<br />
NGC 4486 419 187.69586 12.40208 0.56 −8.222 ± 0.030 −9.743 ± 0.025 3.24 ± 0.14 1.00<br />
NGC 4486 420 187.69592 12.39619 0.42 −5.288 ± 0.734 −6.914 ± 0.600 1.86 ± 0.82 0.99<br />
NGC 4486 421 187.69600 12.39993 0.50 −7.765 ± 0.014 −8.783 ± 0.019 1.86 ± 0.19 1.00<br />
NGC 4486 422 187.69600 12.37355 0.76 −7.490 ± 0.028 −8.762 ± 0.025 2.39 ± 0.14 1.00<br />
NGC 4486 424 187.69606 12.38721 0.39 −8.498 ± 0.021 −9.932 ± 0.012 2.17 ± 0.11 1.00<br />
NGC 4486 426 187.69608 12.38489 0.44 −7.212 ± 0.040 −8.475 ± 0.030 2.19 ± 0.29 1.00<br />
NGC 4486 427 187.69609 12.38271 0.48 −6.377 ± 0.074 −7.502 ± 0.142 3.42 ± 0.77 0.99<br />
NGC 4486 428 187.69612 12.41154 0.86 −8.573 ± 0.024 −9.723 ± 0.024 3.22 ± 0.13 1.00<br />
Continued on Next Page. . .<br />
349
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4486 429 187.69613 12.36689 0.99 −6.278 ± 0.051 −7.850 ± 0.036 2.12 ± 0.26 1.00<br />
NGC 4486 432 187.69615 12.37900 0.59 −6.172 ± 0.057 −8.069 ± 0.147 5.14 ± 0.78 0.97<br />
NGC 4486 433 187.69619 12.37025 0.87 −6.549 ± 0.035 −7.717 ± 0.043 1.82 ± 0.23 1.00<br />
NGC 4486 434 187.69625 12.37794 0.62 −9.083 ± 0.020 −10.096 ± 0.015 2.31 ± 0.11 1.00<br />
NGC 4486 435 187.69638 12.37784 0.62 −9.619 ± 0.019 −10.884 ± 0.012 3.04 ± 0.09 1.00<br />
NGC 4486 436 187.69621 12.37933 0.57 −8.816 ± 0.015 −10.256 ± 0.011 2.08 ± 0.10 1.00<br />
NGC 4486 438 187.69623 12.38170 0.51 −7.890 ± 0.034 −9.391 ± 0.020 2.26 ± 0.17 1.00<br />
NGC 4486 439 187.69633 12.40077 0.51 −7.845 ± 0.038 −8.842 ± 0.041 3.37 ± 0.21 1.00<br />
NGC 4486 441 187.69639 12.38889 0.36 −7.745 ± 0.025 −8.731 ± 0.052 2.88 ± 0.27 1.00<br />
NGC 4486 442 187.69642 12.38206 0.49 −7.960 ± 0.070 −8.513 ± 0.088 9.08 ± 0.84 0.71<br />
NGC 4486 443 187.69643 12.38443 0.43 −8.015 ± 0.029 −9.453 ± 0.022 1.81 ± 0.16 1.00<br />
NGC 4486 445 187.69647 12.40917 0.77 −6.382 ± 0.053 −7.511 ± 0.090 2.43 ± 0.42 1.00<br />
NGC 4486 446 187.69655 12.40820 0.74 −7.360 ± 0.044 −8.375 ± 0.094 4.81 ± 0.38 0.99<br />
NGC 4486 448 187.69655 12.38007 0.54 −7.145 ± 0.037 −8.419 ± 0.056 3.99 ± 0.26 1.00<br />
NGC 4486 449 187.69657 12.38519 0.41 −8.370 ± 0.027 −9.723 ± 0.041 2.14 ± 0.29 1.00<br />
NGC 4486 450 187.69654 12.37347 0.75 −7.749 ± 0.025 −8.645 ± 0.032 2.26 ± 0.17 1.00<br />
NGC 4486 451 187.69670 12.36310 1.12 −7.508 ± 0.116 −8.311 ± 0.109 7.31 ± 0.81 0.76<br />
NGC 4486 452 187.69670 12.38356 0.45 −7.852 ± 0.023 −9.330 ± 0.022 2.23 ± 0.15 1.00<br />
NGC 4486 453 187.69669 12.39800 0.43 −6.677 ± 0.159 −8.255 ± 0.411 1.95 ± 0.36 1.00<br />
NGC 4486 455 187.69675 12.40886 0.75 −5.918 ± 0.066 −7.527 ± 0.077 2.04 ± 0.35 1.00<br />
NGC 4486 456 187.69678 12.39145 0.34 −7.374 ± 0.033 −8.778 ± 0.070 3.47 ± 0.39 1.00<br />
NGC 4486 457 187.69681 12.37209 0.80 −5.910 ± 0.068 −7.551 ± 0.306 2.25 ± 0.36 1.00<br />
NGC 4486 458 187.69690 12.39228 0.34 −8.005 ± 0.035 −8.835 ± 0.034 2.81 ± 0.22 1.00<br />
NGC 4486 459 187.69692 12.37497 0.70 −8.529 ± 0.021 −9.902 ± 0.020 2.65 ± 0.14 1.00<br />
NGC 4486 460 187.69693 12.38177 0.49 −8.442 ± 0.029 −9.305 ± 0.031 4.00 ± 0.19 1.00<br />
NGC 4486 461 187.69689 12.39646 0.39 −5.389 ± 0.288 −7.208 ± 0.097 1.72 ± 0.50 0.99<br />
NGC 4486 462 187.69695 12.39960 0.46 −6.716 ± 0.050 −8.244 ± 0.064 3.21 ± 0.28 1.00<br />
NGC 4486 463 187.69704 12.41484 0.96 −9.206 ± 0.029 −10.742 ± 0.018 2.42 ± 0.23 1.00<br />
NGC 4486 465 187.69703 12.39007 0.33 −6.293 ± 0.097 −7.576 ± 0.030 2.10 ± 0.36 1.00<br />
NGC 4486 466 187.69716 12.36478 1.05 −7.075 ± 0.029 −8.596 ± 0.041 2.18 ± 0.24 1.00<br />
NGC 4486 468 187.69716 12.37491 0.70 −5.236 ± 0.118 −7.125 ± 0.144 2.10 ± 0.60 1.00<br />
NGC 4486 469 187.69719 12.38781 0.35 −7.538 ± 0.046 −8.988 ± 0.024 1.98 ± 0.17 1.00<br />
NGC 4486 470 187.69721 12.38063 0.51 −7.551 ± 0.027 −8.476 ± 0.037 2.48 ± 0.20 1.00<br />
NGC 4486 471 187.69721 12.40557 0.64 −5.392 ± 0.112 −6.442 ± 0.439 2.07 ± 0.52 0.99<br />
NGC 4486 472 187.69715 12.40041 0.48 −5.588 ± 0.197 −7.244 ± 0.270 3.63 ± 1.49 0.97<br />
NGC 4486 474 187.69731 12.40305 0.55 −9.279 ± 0.023 −10.520 ± 0.007 2.53 ± 0.11 1.00<br />
NGC 4486 475 187.69730 12.38715 0.35 −6.900 ± 0.046 −7.798 ± 0.064 2.60 ± 0.32 1.00<br />
NGC 4486 477 187.69728 12.40846 0.73 −6.353 ± 0.047 −7.785 ± 0.034 1.48 ± 0.23 0.99<br />
NGC 4486 480 187.69741 12.38312 0.44 −7.346 ± 0.030 −8.939 ± 0.036 2.03 ± 0.20 1.00<br />
NGC 4486 482 187.69750 12.39168 0.31 −7.959 ± 0.029 −8.982 ± 0.042 2.32 ± 0.19 1.00<br />
NGC 4486 484 187.69751 12.39068 0.31 −8.641 ± 0.021 −9.463 ± 0.024 2.27 ± 0.15 1.00<br />
NGC 4486 486 187.69765 12.38156 0.48 −6.908 ± 0.085 −8.603 ± 0.124 4.42 ± 0.85 1.00<br />
NGC 4486 487 187.69757 12.38811 0.33 −5.807 ± 0.096 −7.290 ± 0.106 3.41 ± 0.46 0.98<br />
NGC 4486 490 187.69757 12.39343 0.32 −5.983 ± 0.356 −7.402 ± 0.083 2.14 ± 0.38 1.00<br />
NGC 4486 492 187.69762 12.40404 0.58 −8.571 ± 0.022 −9.569 ± 0.017 2.41 ± 0.11 1.00<br />
NGC 4486 493 187.69762 12.39972 0.45 −6.455 ± 0.115 −7.787 ± 0.069 3.02 ± 0.47 1.00<br />
NGC 4486 494 187.69759 12.38147 0.48 −9.300 ± 0.011 −10.250 ± 0.016 3.06 ± 0.08 1.00<br />
NGC 4486 495 187.69762 12.41695 1.03 −6.932 ± 0.033 −8.554 ± 0.024 2.18 ± 0.17 1.00<br />
NGC 4486 496 187.69765 12.39691 0.38 −5.953 ± 0.084 −7.557 ± 0.114 2.37 ± 0.56 1.00<br />
NGC 4486 497 187.69765 12.39783 0.40 −6.948 ± 0.033 −8.025 ± 0.057 3.20 ± 0.24 1.00<br />
NGC 4486 500 187.69771 12.40120 0.49 −8.364 ± 0.024 −9.660 ± 0.029 2.72 ± 0.13 1.00<br />
NGC 4486 503 187.69771 12.40234 0.52 −6.364 ± 0.083 −7.827 ± 0.065 3.01 ± 0.38 1.00<br />
NGC 4486 504 187.69779 12.38846 0.32 −7.796 ± 0.046 −9.472 ± 0.052 3.95 ± 0.29 1.00<br />
NGC 4486 505 187.69789 12.38787 0.32 −11.028 ± 0.017 −12.396 ± 0.019 3.52 ± 0.15 1.00<br />
NGC 4486 506 187.69782 12.39126 0.30 −7.642 ± 0.030 −8.675 ± 0.038 2.80 ± 0.21 1.00<br />
NGC 4486 507 187.69785 12.38661 0.35 −8.126 ± 0.024 −9.572 ± 0.036 1.96 ± 0.17 1.00<br />
NGC 4486 508 187.69785 12.38685 0.34 −7.438 ± 0.053 −8.274 ± 0.094 3.22 ± 0.36 1.00<br />
NGC 4486 510 187.69794 12.39710 0.37 −7.085 ± 0.093 −7.738 ± 0.137 4.51 ± 0.58 0.96<br />
NGC 4486 511 187.69797 12.37222 0.78 −6.081 ± 0.059 −7.863 ± 0.058 2.87 ± 0.34 1.00<br />
NGC 4486 512 187.69802 12.39652 0.36 −7.188 ± 0.041 −8.376 ± 0.034 2.08 ± 0.22 1.00<br />
NGC 4486 514 187.69809 12.38844 0.31 −9.288 ± 0.011 −10.460 ± 0.023 2.73 ± 0.10 1.00<br />
NGC 4486 515 187.69807 12.36737 0.95 −6.659 ± 0.039 −7.883 ± 0.032 2.89 ± 0.29 1.00<br />
Continued on Next Page. . .<br />
350
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4486 516 187.69811 12.37333 0.73 −6.719 ± 0.035 −7.872 ± 0.042 2.33 ± 0.29 1.00<br />
NGC 4486 517 187.69816 12.39390 0.31 −6.571 ± 0.103 −7.909 ± 0.062 2.74 ± 0.46 1.00<br />
NGC 4486 518 187.69820 12.38667 0.33 −7.993 ± 0.037 −8.877 ± 0.033 2.76 ± 0.22 1.00<br />
NGC 4486 519 187.69825 12.36506 1.03 −6.732 ± 0.042 −8.114 ± 0.335 1.87 ± 0.28 1.00<br />
NGC 4486 520 187.69829 12.36824 0.91 −7.602 ± 0.030 −9.238 ± 0.031 2.68 ± 0.17 1.00<br />
NGC 4486 521 187.69826 12.39409 0.31 −7.531 ± 0.059 −8.469 ± 0.078 4.02 ± 0.32 1.00<br />
NGC 4486 522 187.69822 12.41779 1.05 −5.630 ± 0.438 −6.669 ± 0.139 1.50 ± 0.46 0.96<br />
NGC 4486 523 187.69809 12.38216 0.45 −5.970 ± 0.091 −7.443 ± 0.068 1.85 ± 0.38 0.99<br />
NGC 4486 524 187.69831 12.38034 0.50 −6.138 ± 0.062 −7.377 ± 0.537 2.41 ± 0.49 1.00<br />
NGC 4486 525 187.69835 12.38214 0.44 −5.450 ± 0.571 −6.811 ± 0.253 1.46 ± 0.55 0.96<br />
NGC 4486 526 187.69838 12.38339 0.41 −7.765 ± 0.018 −8.885 ± 0.032 2.61 ± 0.20 1.00<br />
NGC 4486 527 187.69846 12.39119 0.28 −8.037 ± 0.024 −9.543 ± 0.028 2.21 ± 0.21 1.00<br />
NGC 4486 529 187.69850 12.40701 0.66 −8.582 ± 0.030 −9.370 ± 0.028 3.11 ± 0.16 1.00<br />
NGC 4486 530 187.69852 12.36320 1.09 −7.723 ± 0.039 −8.888 ± 0.046 4.63 ± 0.27 1.00<br />
NGC 4486 532 187.69852 12.38624 0.33 −7.221 ± 0.272 −8.437 ± 0.044 1.59 ± 0.23 1.00<br />
NGC 4486 533 187.69853 12.39801 0.38 −7.995 ± 0.033 −9.287 ± 0.023 2.65 ± 0.17 1.00<br />
NGC 4486 534 187.69855 12.38228 0.43 −6.395 ± 0.039 −7.968 ± 0.040 2.55 ± 0.40 1.00<br />
NGC 4486 535 187.69858 12.39128 0.27 −7.285 ± 0.045 −8.658 ± 0.048 3.01 ± 0.27 1.00<br />
NGC 4486 536 187.69858 12.40806 0.70 −5.798 ± 0.087 −7.406 ± 0.114 3.18 ± 0.44 0.99<br />
NGC 4486 538 187.69864 12.39491 0.31 −6.752 ± 0.050 −8.249 ± 0.045 2.05 ± 0.31 1.00<br />
NGC 4486 539 187.69873 12.41335 0.88 −6.086 ± 0.066 −7.611 ± 0.039 1.62 ± 0.31 0.99<br />
NGC 4486 542 187.69884 12.40977 0.75 −8.397 ± 0.029 −9.801 ± 0.018 2.59 ± 0.15 1.00<br />
NGC 4486 543 187.69879 12.37723 0.59 −6.080 ± 0.087 −7.461 ± 0.054 2.62 ± 0.33 1.00<br />
NGC 4486 544 187.69888 12.37698 0.60 −7.697 ± 0.026 −9.418 ± 0.023 2.06 ± 0.22 1.00<br />
NGC 4486 545 187.69899 12.41748 1.03 −8.496 ± 0.028 −9.826 ± 0.020 3.85 ± 0.16 1.00<br />
NGC 4486 547 187.69899 12.41255 0.85 −5.623 ± 0.091 −7.432 ± 1.148 0.85 ± 0.42 0.82<br />
NGC 4486 548 187.69899 12.41275 0.86 −6.278 ± 0.033 −7.549 ± 0.069 2.24 ± 0.28 1.00<br />
NGC 4486 549 187.69902 12.38520 0.34 −7.077 ± 0.054 −7.908 ± 0.055 1.57 ± 0.40 0.99<br />
NGC 4486 550 187.69903 12.38571 0.33 −6.681 ± 0.234 −7.971 ± 0.051 2.22 ± 0.34 1.00<br />
NGC 4486 551 187.69905 12.39606 0.32 −7.613 ± 0.041 −8.501 ± 0.102 4.43 ± 0.48 1.00<br />
NGC 4486 552 187.69904 12.40175 0.48 −7.569 ± 0.066 −8.552 ± 0.072 3.91 ± 0.37 1.00<br />
NGC 4486 553 187.69904 12.37829 0.55 −6.409 ± 0.052 −7.985 ± 0.075 2.88 ± 0.56 1.00<br />
NGC 4486 554 187.69911 12.37990 0.50 −8.330 ± 0.019 −9.235 ± 0.032 2.28 ± 0.18 1.00<br />
NGC 4486 555 187.69875 12.40822 0.70 −8.396 ± 0.028 −9.361 ± 0.018 2.65 ± 0.18 1.00<br />
NGC 4486 556 187.69917 12.38750 0.29 −7.236 ± 0.042 −8.417 ± 0.077 3.20 ± 0.30 1.00<br />
NGC 4486 557 187.69928 12.37937 0.51 −9.357 ± 0.019 −10.666 ± 0.020 2.18 ± 0.17 1.00<br />
NGC 4486 558 187.69931 12.37863 0.53 −9.677 ± 0.016 −10.903 ± 0.022 2.26 ± 0.16 1.00<br />
NGC 4486 559 187.69928 12.39789 0.36 −7.687 ± 0.041 −9.242 ± 0.026 2.57 ± 0.15 1.00<br />
NGC 4486 560 187.69931 12.38753 0.28 −6.645 ± 0.067 −7.350 ± 0.119 1.79 ± 0.31 0.99<br />
NGC 4486 562 187.69930 12.41137 0.81 −7.584 ± 0.042 −8.522 ± 0.065 4.33 ± 0.31 1.00<br />
NGC 4486 563 187.69934 12.40038 0.43 −8.043 ± 0.019 −9.580 ± 0.013 1.69 ± 0.17 1.00<br />
NGC 4486 565 187.69933 12.37995 0.49 −6.968 ± 0.582 −8.608 ± 0.028 1.35 ± 0.29 0.98<br />
NGC 4486 566 187.69940 12.39939 0.40 −6.951 ± 0.092 −7.717 ± 0.078 3.18 ± 0.31 0.99<br />
NGC 4486 567 187.69939 12.38229 0.41 −6.007 ± 0.083 −7.083 ± 0.080 2.02 ± 0.46 0.99<br />
NGC 4486 568 187.69940 12.38390 0.37 −7.240 ± 0.051 −8.008 ± 0.047 2.81 ± 0.21 1.00<br />
NGC 4486 569 187.69945 12.39196 0.24 −7.423 ± 0.041 −8.736 ± 0.039 1.86 ± 0.19 1.00<br />
NGC 4486 570 187.69946 12.38034 0.47 −5.988 ± 0.094 −7.290 ± 0.129 1.20 ± 0.40 0.94<br />
NGC 4486 571 187.69949 12.38301 0.39 −6.962 ± 0.043 −8.266 ± 0.036 2.20 ± 0.20 1.00<br />
NGC 4486 573 187.69957 12.40948 0.74 −6.444 ± 0.263 −7.895 ± 0.045 1.67 ± 0.28 0.99<br />
NGC 4486 574 187.69962 12.36665 0.96 −7.686 ± 0.038 −8.549 ± 0.030 3.03 ± 0.22 1.00<br />
NGC 4486 577 187.69969 12.41709 1.01 −9.393 ± 0.024 −10.370 ± 0.013 2.63 ± 0.13 1.00<br />
NGC 4486 580 187.69966 12.36934 0.86 −4.988 ± 0.291 −6.282 ± 0.154 4.14 ± 1.28 0.85<br />
NGC 4486 581 187.69968 12.38749 0.27 −6.509 ± 0.131 −7.852 ± 0.109 3.69 ± 0.64 0.99<br />
NGC 4486 582 187.69980 12.39027 0.23 −7.438 ± 0.055 −8.387 ± 0.050 3.33 ± 0.24 1.00<br />
NGC 4486 583 187.69977 12.41612 0.98 −6.379 ± 0.042 −7.557 ± 0.033 2.11 ± 0.22 1.00<br />
NGC 4486 584 187.69982 12.36965 0.85 −7.603 ± 0.038 −8.483 ± 0.030 2.66 ± 0.23 1.00<br />
NGC 4486 585 187.69980 12.39826 0.35 −7.151 ± 0.041 −8.229 ± 0.048 1.98 ± 0.25 1.00<br />
NGC 4486 586 187.69982 12.38313 0.38 −5.950 ± 0.041 −7.441 ± 0.054 2.39 ± 0.45 1.00<br />
NGC 4486 587 187.69988 12.40343 0.52 −7.964 ± 0.027 −9.044 ± 0.036 2.70 ± 0.20 1.00<br />
NGC 4486 588 187.69992 12.38476 0.33 −8.383 ± 0.027 −9.958 ± 0.020 2.40 ± 0.17 1.00<br />
NGC 4486 589 187.69991 12.37720 0.57 −6.887 ± 0.054 −8.462 ± 0.029 2.81 ± 0.17 1.00<br />
NGC 4486 591 187.69994 12.38876 0.24 −7.693 ± 0.025 −8.970 ± 0.034 2.09 ± 0.23 1.00<br />
Continued on Next Page. . .<br />
351
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4486 592 187.69995 12.40889 0.71 −7.686 ± 0.030 −9.260 ± 0.030 2.48 ± 0.21 1.00<br />
NGC 4486 594 187.69998 12.39902 0.37 −6.614 ± 0.046 −7.856 ± 0.082 1.95 ± 0.38 1.00<br />
NGC 4486 595 187.70003 12.38775 0.25 −9.741 ± 0.016 −10.992 ± 0.013 3.20 ± 0.11 1.00<br />
NGC 4486 596 187.70000 12.40904 0.71 −9.997 ± 0.020 −11.491 ± 0.013 2.18 ± 0.13 1.00<br />
NGC 4486 597 187.70011 12.39476 0.26 −8.253 ± 0.020 −9.731 ± 0.019 2.23 ± 0.14 1.00<br />
NGC 4486 598 187.70014 12.41814 1.05 −7.777 ± 0.026 −9.157 ± 0.016 2.07 ± 0.16 1.00<br />
NGC 4486 599 187.70024 12.36491 1.02 −7.407 ± 0.030 −8.165 ± 0.037 2.38 ± 0.21 1.00<br />
NGC 4486 600 187.70023 12.38635 0.28 −7.036 ± 0.058 −8.541 ± 0.062 2.23 ± 0.35 1.00<br />
NGC 4486 601 187.70026 12.41590 0.96 −8.561 ± 0.016 −9.965 ± 0.011 2.27 ± 0.11 1.00<br />
NGC 4486 602 187.70025 12.40793 0.67 −6.271 ± 0.067 −7.515 ± 0.342 1.58 ± 0.45 0.99<br />
NGC 4486 603 187.70030 12.38411 0.34 −6.366 ± 0.064 −7.691 ± 0.271 5.33 ± 1.90 0.92<br />
NGC 4486 604 187.70039 12.37110 0.79 −9.418 ± 0.023 −10.408 ± 0.013 2.59 ± 0.11 1.00<br />
NGC 4486 605 187.70041 12.38019 0.46 −7.608 ± 0.023 −8.591 ± 0.046 3.02 ± 0.25 1.00<br />
NGC 4486 608 187.70043 12.38765 0.24 −7.419 ± 0.030 −8.478 ± 0.098 3.82 ± 0.42 1.00<br />
NGC 4486 609 187.70043 12.39618 0.28 −6.831 ± 0.057 −7.833 ± 0.109 2.34 ± 0.45 1.00<br />
NGC 4486 610 187.70048 12.40175 0.45 −8.223 ± 0.019 −9.144 ± 0.024 2.42 ± 0.15 1.00<br />
NGC 4486 611 187.70047 12.40217 0.47 −7.094 ± 0.053 −7.748 ± 0.049 2.98 ± 0.28 1.00<br />
NGC 4486 612 187.70051 12.37384 0.69 −8.075 ± 0.030 −9.286 ± 0.033 3.96 ± 0.21 1.00<br />
NGC 4486 613 187.70050 12.37496 0.65 −5.570 ± 0.372 −6.979 ± 0.074 1.62 ± 0.42 0.98<br />
NGC 4486 614 187.70053 12.39397 0.23 −8.289 ± 0.031 −9.843 ± 0.021 2.39 ± 0.12 1.00<br />
NGC 4486 615 187.70063 12.40616 0.60 −7.959 ± 0.020 −8.859 ± 0.029 2.58 ± 0.24 1.00<br />
NGC 4486 616 187.70066 12.39482 0.24 −7.759 ± 0.033 −9.180 ± 0.036 2.08 ± 0.29 1.00<br />
NGC 4486 617 187.70074 12.40223 0.46 −6.490 ± 0.879 −7.757 ± 0.053 2.78 ± 0.39 1.00<br />
NGC 4486 620 187.70085 12.40398 0.52 −7.643 ± 0.030 −8.748 ± 0.027 1.97 ± 0.18 1.00<br />
NGC 4486 621 187.70084 12.36770 0.91 −6.295 ± 0.049 −7.985 ± 0.081 2.81 ± 0.34 1.00<br />
NGC 4486 622 187.70085 12.38785 0.23 −6.693 ± 0.055 −8.198 ± 0.092 3.36 ± 0.46 1.00<br />
NGC 4486 623 187.70081 12.37835 0.52 −9.692 ± 0.013 −10.961 ± 0.010 2.81 ± 0.06 1.00<br />
NGC 4486 624 187.70094 12.41089 0.77 −7.608 ± 0.031 −8.555 ± 0.034 2.58 ± 0.20 1.00<br />
NGC 4486 626 187.70099 12.37947 0.48 −7.823 ± 0.088 −8.906 ± 0.097 4.99 ± 0.55 0.99<br />
NGC 4486 627 187.70095 12.38716 0.24 −6.995 ± 0.034 −8.558 ± 0.044 2.70 ± 0.21 1.00<br />
NGC 4486 628 187.70097 12.40281 0.48 −7.879 ± 0.031 −9.240 ± 0.031 2.17 ± 0.15 1.00<br />
NGC 4486 629 187.70107 12.39047 0.18 −6.873 ± 0.078 −8.305 ± 0.088 2.09 ± 0.43 1.00<br />
NGC 4486 630 187.70111 12.40931 0.71 −5.294 ± 0.249 −6.048 ± 0.684 1.37 ± 1.07 0.95<br />
NGC 4486 631 187.70118 12.39028 0.18 −8.547 ± 0.022 −10.082 ± 0.024 1.85 ± 0.14 1.00<br />
NGC 4486 632 187.70115 12.40428 0.53 −6.697 ± 0.035 −8.082 ± 0.039 1.94 ± 0.25 1.00<br />
NGC 4486 634 187.70120 12.41133 0.79 −7.708 ± 0.071 −8.833 ± 0.109 7.68 ± 0.67 0.88<br />
NGC 4486 636 187.70131 12.40230 0.46 −7.848 ± 0.033 −9.062 ± 0.033 3.12 ± 0.18 1.00<br />
NGC 4486 637 187.70129 12.37933 0.48 −7.901 ± 0.025 −9.155 ± 0.023 2.57 ± 0.16 1.00<br />
NGC 4486 639 187.70131 12.40502 0.55 −7.323 ± 0.044 −8.138 ± 0.051 3.27 ± 0.28 1.00<br />
NGC 4486 641 187.70134 12.37536 0.62 −6.989 ± 0.069 −8.671 ± 0.075 3.72 ± 0.48 1.00<br />
NGC 4486 642 187.70136 12.39664 0.27 −7.944 ± 0.030 −9.322 ± 0.027 2.59 ± 0.19 1.00<br />
NGC 4486 644 187.70145 12.40439 0.53 −9.347 ± 0.020 −10.552 ± 0.009 2.62 ± 0.10 1.00<br />
NGC 4486 645 187.70150 12.41067 0.76 −9.291 ± 0.019 −10.852 ± 0.010 3.07 ± 0.12 1.00<br />
NGC 4486 646 187.70148 12.38715 0.22 −7.256 ± 0.061 −8.441 ± 0.090 2.73 ± 0.33 1.00<br />
NGC 4486 648 187.70145 12.40535 0.56 −8.447 ± 0.019 −9.758 ± 0.012 2.08 ± 0.10 1.00<br />
NGC 4486 649 187.70148 12.37998 0.45 −7.385 ± 0.041 −8.434 ± 0.033 2.51 ± 0.24 1.00<br />
NGC 4486 651 187.70153 12.39057 0.16 −7.613 ± 0.043 −8.706 ± 0.058 3.00 ± 0.28 1.00<br />
NGC 4486 654 187.70167 12.40733 0.63 −7.958 ± 0.026 −8.795 ± 0.026 2.66 ± 0.12 1.00<br />
NGC 4486 655 187.70169 12.39788 0.30 −7.777 ± 0.020 −9.173 ± 0.039 2.83 ± 0.16 1.00<br />
NGC 4486 656 187.70168 12.38073 0.42 −7.451 ± 0.041 −8.912 ± 0.029 1.36 ± 0.27 0.98<br />
NGC 4486 657 187.70175 12.41487 0.91 −7.448 ± 0.026 −8.960 ± 0.021 1.87 ± 0.15 1.00<br />
NGC 4486 658 187.70182 12.38171 0.39 −7.864 ± 0.032 −9.420 ± 0.022 1.46 ± 0.18 0.98<br />
NGC 4486 660 187.70182 12.41195 0.80 −7.582 ± 0.029 −8.559 ± 0.036 2.69 ± 0.15 1.00<br />
NGC 4486 662 187.70189 12.38060 0.43 −9.698 ± 0.025 −10.664 ± 0.015 2.74 ± 0.18 1.00<br />
NGC 4486 663 187.70177 12.40386 0.51 −8.249 ± 0.031 −9.174 ± 0.057 4.07 ± 0.19 1.00<br />
NGC 4486 664 187.70191 12.37862 0.50 −5.490 ± 0.154 −7.179 ± 0.130 2.76 ± 0.73 0.99<br />
NGC 4486 665 187.70194 12.37887 0.49 −8.935 ± 0.018 −10.340 ± 0.019 1.75 ± 0.09 1.00<br />
NGC 4486 666 187.70195 12.39481 0.20 −8.657 ± 0.026 −9.703 ± 0.015 2.00 ± 0.14 1.00<br />
NGC 4486 668 187.70200 12.38371 0.32 −8.217 ± 0.028 −9.451 ± 0.028 2.31 ± 0.22 1.00<br />
NGC 4486 669 187.70168 12.41087 0.77 −7.424 ± 0.030 −9.196 ± 0.041 2.95 ± 0.24 1.00<br />
NGC 4486 670 187.70205 12.40618 0.59 −8.411 ± 0.027 −9.435 ± 0.021 3.02 ± 0.14 1.00<br />
NGC 4486 671 187.70201 12.38256 0.36 −7.255 ± 0.039 −8.599 ± 0.054 2.25 ± 0.25 1.00<br />
Continued on Next Page. . .<br />
352
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4486 672 187.70205 12.38945 0.16 −8.062 ± 0.078 −9.044 ± 0.100 5.17 ± 0.65 0.99<br />
NGC 4486 673 187.70209 12.37621 0.58 −8.026 ± 0.023 −8.992 ± 0.029 2.81 ± 0.15 1.00<br />
NGC 4486 677 187.70220 12.40743 0.63 −9.275 ± 0.037 −10.170 ± 0.025 4.04 ± 0.15 1.00<br />
NGC 4486 678 187.70219 12.37003 0.81 −6.770 ± 0.053 −7.870 ± 0.083 4.00 ± 0.36 0.99<br />
NGC 4486 680 187.70221 12.39339 0.16 −8.629 ± 0.029 −9.951 ± 0.020 1.55 ± 0.19 0.99<br />
NGC 4486 682 187.70236 12.37781 0.52 −6.837 ± 0.059 −8.480 ± 0.057 3.40 ± 0.37 1.00<br />
NGC 4486 684 187.70235 12.39703 0.26 −8.942 ± 0.014 −10.130 ± 0.023 2.71 ± 0.08 1.00<br />
NGC 4486 685 187.70236 12.40474 0.53 −7.951 ± 0.026 −9.172 ± 0.015 1.75 ± 0.19 1.00<br />
NGC 4486 686 187.70240 12.38235 0.36 −8.059 ± 0.028 −9.103 ± 0.033 2.17 ± 0.16 1.00<br />
NGC 4486 687 187.70239 12.40596 0.58 −6.548 ± 0.073 −7.537 ± 0.065 3.28 ± 0.37 0.99<br />
NGC 4486 689 187.70243 12.40274 0.46 −5.653 ± 2.252 −7.186 ± 0.368 1.99 ± 0.78 0.99<br />
NGC 4486 690 187.70247 12.41322 0.85 −7.448 ± 0.028 −8.177 ± 0.027 1.89 ± 0.16 1.00<br />
NGC 4486 691 187.70261 12.41327 0.85 −7.866 ± 0.028 −9.192 ± 0.024 2.24 ± 0.13 1.00<br />
NGC 4486 692 187.70250 12.38700 0.20 −10.373 ± 0.014 −11.484 ± 0.010 2.60 ± 0.10 1.00<br />
NGC 4486 693 187.70250 12.39550 0.21 −7.962 ± 0.051 −9.027 ± 0.022 3.37 ± 0.20 1.00<br />
NGC 4486 694 187.70255 12.39819 0.30 −7.862 ± 0.046 −9.132 ± 0.034 2.41 ± 0.31 1.00<br />
NGC 4486 695 187.70259 12.38296 0.33 −7.566 ± 0.025 −9.084 ± 0.025 2.08 ± 0.16 1.00<br />
NGC 4486 696 187.70261 12.38885 0.15 −7.443 ± 0.037 −9.111 ± 0.030 2.92 ± 0.22 1.00<br />
NGC 4486 697 187.70265 12.37573 0.60 −7.104 ± 0.038 −8.188 ± 0.046 2.79 ± 0.25 1.00<br />
NGC 4486 698 187.70269 12.40286 0.46 −8.021 ± 0.028 −8.826 ± 0.018 3.55 ± 0.14 1.00<br />
NGC 4486 700 187.70269 12.40029 0.37 −9.041 ± 0.021 −10.072 ± 0.013 2.71 ± 0.19 1.00<br />
NGC 4486 701 187.70269 12.36617 0.95 −7.276 ± 0.029 −8.278 ± 0.034 3.32 ± 0.19 1.00<br />
NGC 4486 702 187.70270 12.38089 0.41 −8.062 ± 0.021 −9.609 ± 0.016 1.98 ± 0.14 1.00<br />
NGC 4486 703 187.70270 12.38985 0.13 −7.498 ± 0.046 −8.395 ± 0.072 2.37 ± 0.36 1.00<br />
NGC 4486 704 187.70273 12.39889 0.32 −8.067 ± 0.026 −9.167 ± 0.046 4.18 ± 0.25 1.00<br />
NGC 4486 706 187.70273 12.40483 0.53 −8.606 ± 0.019 −9.563 ± 0.018 2.45 ± 0.09 1.00<br />
NGC 4486 708 187.70285 12.36847 0.87 −7.964 ± 0.031 −8.868 ± 0.029 3.23 ± 0.16 1.00<br />
NGC 4486 709 187.70282 12.39587 0.21 −6.356 ± 0.126 −7.938 ± 1.012 1.52 ± 0.40 0.99<br />
NGC 4486 711 187.70287 12.39553 0.20 −7.407 ± 0.046 −8.569 ± 0.043 2.27 ± 0.19 1.00<br />
NGC 4486 712 187.70290 12.37162 0.75 −6.149 ± 0.110 −7.412 ± 0.061 2.89 ± 0.44 0.99<br />
NGC 4486 713 187.70293 12.38286 0.33 −8.155 ± 0.017 −9.121 ± 0.031 2.58 ± 0.17 1.00<br />
NGC 4486 714 187.70297 12.39841 0.30 −6.843 ± 0.743 −8.425 ± 0.056 1.07 ± 0.52 0.92<br />
NGC 4486 715 187.70308 12.37448 0.64 −9.852 ± 0.020 −10.959 ± 0.011 2.97 ± 0.12 1.00<br />
NGC 4486 717 187.70310 12.38956 0.12 −6.923 ± 0.310 −8.201 ± 0.426 1.83 ± 0.60 1.00<br />
NGC 4486 720 187.70312 12.38717 0.18 −5.765 ± 0.429 −7.219 ± 1.448 0.81 ± 0.55 0.77<br />
NGC 4486 721 187.70316 12.37212 0.73 −7.307 ± 0.038 −8.765 ± 0.029 2.62 ± 0.20 1.00<br />
NGC 4486 723 187.70322 12.38777 0.16 −8.700 ± 0.029 −10.249 ± 0.018 2.34 ± 0.14 1.00<br />
NGC 4486 724 187.70327 12.37048 0.79 −7.478 ± 0.029 −8.565 ± 0.057 3.23 ± 0.41 1.00<br />
NGC 4486 725 187.70328 12.40175 0.42 −9.570 ± 0.014 −10.858 ± 0.013 3.06 ± 0.09 1.00<br />
NGC 4486 726 187.70323 12.41193 0.80 −6.393 ± 0.057 −7.783 ± 0.087 1.62 ± 0.27 0.99<br />
NGC 4486 727 187.70332 12.39456 0.16 −7.611 ± 0.037 −8.870 ± 0.090 3.17 ± 0.33 1.00<br />
NGC 4486 728 187.70330 12.40301 0.46 −6.869 ± 0.048 −7.776 ± 0.037 2.69 ± 0.22 1.00<br />
NGC 4486 729 187.70334 12.38753 0.17 −7.718 ± 0.040 −8.695 ± 0.086 2.93 ± 0.31 1.00<br />
NGC 4486 730 187.70322 12.40553 0.56 −7.565 ± 0.042 −8.257 ± 0.017 2.54 ± 0.15 1.00<br />
NGC 4486 732 187.70342 12.37947 0.45 −6.286 ± 0.077 −7.781 ± 0.229 1.55 ± 0.24 0.99<br />
NGC 4486 733 187.70342 12.37870 0.48 −6.600 ± 0.059 −7.870 ± 0.040 1.83 ± 0.26 1.00<br />
NGC 4486 734 187.70347 12.36650 0.94 −6.217 ± 0.117 −7.432 ± 0.046 2.59 ± 0.41 1.00<br />
NGC 4486 735 187.70345 12.39707 0.24 −6.083 ± 0.083 −7.906 ± 0.121 3.08 ± 0.60 1.00<br />
NGC 4486 736 187.70346 12.40625 0.58 −5.442 ± 0.148 −7.223 ± 0.141 3.04 ± 0.79 0.99<br />
NGC 4486 737 187.70354 12.40600 0.57 −8.483 ± 0.024 −9.804 ± 0.014 2.10 ± 0.17 1.00<br />
NGC 4486 739 187.70366 12.37647 0.56 −7.408 ± 0.031 −8.882 ± 0.025 2.30 ± 0.20 1.00<br />
NGC 4486 740 187.70368 12.40952 0.70 −7.005 ± 0.053 −7.938 ± 0.076 3.42 ± 0.30 0.99<br />
NGC 4486 743 187.70374 12.36451 1.01 −7.665 ± 0.029 −8.565 ± 0.024 2.35 ± 0.18 1.00<br />
NGC 4486 744 187.70369 12.37000 0.81 −6.807 ± 0.030 −8.228 ± 0.052 2.27 ± 0.26 1.00<br />
NGC 4486 745 187.70375 12.40586 0.56 −7.619 ± 0.051 −8.616 ± 0.028 3.69 ± 0.22 1.00<br />
NGC 4486 746 187.70380 12.40313 0.46 −8.590 ± 0.050 −9.726 ± 0.060 2.35 ± 0.42 1.00<br />
NGC 4486 747 187.70380 12.40625 0.58 −7.816 ± 0.031 −9.254 ± 0.033 2.38 ± 0.17 1.00<br />
NGC 4486 748 187.70377 12.39293 0.11 −9.215 ± 0.024 −10.396 ± 0.122 2.55 ± 0.25 1.00<br />
NGC 4486 749 187.70386 12.41666 0.97 −8.637 ± 0.019 −9.795 ± 0.019 2.57 ± 0.15 1.00<br />
NGC 4486 751 187.70384 12.40795 0.64 −6.162 ± 0.065 −7.531 ± 0.273 2.19 ± 0.39 1.00<br />
NGC 4486 752 187.70387 12.41021 0.73 −7.595 ± 0.037 −8.461 ± 0.063 3.35 ± 0.27 1.00<br />
NGC 4486 753 187.70389 12.40002 0.35 −7.799 ± 0.037 −8.883 ± 0.033 3.08 ± 0.22 1.00<br />
Continued on Next Page. . .<br />
353
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4486 754 187.70387 12.41216 0.80 −7.984 ± 0.023 −8.849 ± 0.031 1.99 ± 0.15 1.00<br />
NGC 4486 755 187.70389 12.36550 0.98 −9.934 ± 0.025 −10.980 ± 0.021 10.22 ± 0.23 1.00<br />
NGC 4486 757 187.70401 12.36760 0.90 −6.602 ± 0.068 −7.826 ± 0.063 3.37 ± 0.32 0.99<br />
NGC 4486 758 187.70400 12.40268 0.44 −6.352 ± 0.054 −7.590 ± 0.085 2.66 ± 0.35 1.00<br />
NGC 4486 760 187.70412 12.41021 0.73 −9.285 ± 0.018 −10.464 ± 0.024 4.12 ± 0.12 1.00<br />
NGC 4486 761 187.70409 12.39660 0.22 −7.139 ± 0.042 −8.587 ± 0.024 2.31 ± 0.25 1.00<br />
NGC 4486 762 187.70415 12.37806 0.50 −6.581 ± 0.112 −8.033 ± 0.037 1.79 ± 0.26 1.00<br />
NGC 4486 763 187.70418 12.41176 0.79 −8.315 ± 0.027 −9.234 ± 0.026 2.38 ± 0.16 1.00<br />
NGC 4486 764 187.70418 12.40942 0.70 −7.329 ± 0.033 −8.196 ± 0.038 2.68 ± 0.20 1.00<br />
NGC 4486 765 187.70421 12.40792 0.64 −7.514 ± 0.043 −8.444 ± 0.041 3.65 ± 0.20 1.00<br />
NGC 4486 766 187.70421 12.37711 0.54 −6.112 ± 0.313 −7.722 ± 0.942 1.18 ± 0.40 0.95<br />
NGC 4486 767 187.70426 12.38012 0.42 −9.126 ± 0.022 −10.062 ± 0.015 2.39 ± 0.17 1.00<br />
NGC 4486 768 187.70432 12.37236 0.71 −8.700 ± 0.020 −9.899 ± 0.017 2.46 ± 0.10 1.00<br />
NGC 4486 771 187.70435 12.39621 0.20 −8.047 ± 0.036 −9.052 ± 0.041 3.16 ± 0.21 1.00<br />
NGC 4486 772 187.70449 12.39617 0.20 −8.516 ± 0.036 −9.955 ± 0.016 2.70 ± 0.12 1.00<br />
NGC 4486 774 187.70443 12.39100 0.06 −7.906 ± 0.038 −9.386 ± 0.057 2.19 ± 0.26 1.00<br />
NGC 4486 775 187.70441 12.38520 0.23 −5.749 ± 0.703 −7.315 ± 0.183 1.75 ± 0.80 0.99<br />
NGC 4486 776 187.70444 12.36844 0.86 −6.530 ± 0.137 −7.376 ± 0.084 4.93 ± 0.84 0.89<br />
NGC 4486 778 187.70447 12.40685 0.60 −6.343 ± 0.070 −7.891 ± 0.047 2.55 ± 0.43 1.00<br />
NGC 4486 779 187.70449 12.36288 1.07 −7.181 ± 0.033 −8.417 ± 0.023 2.36 ± 0.21 1.00<br />
NGC 4486 780 187.70452 12.38083 0.39 −6.754 ± 0.047 −8.420 ± 0.053 2.54 ± 0.29 1.00<br />
NGC 4486 781 187.70454 12.38560 0.22 −8.631 ± 0.014 −9.560 ± 0.024 1.92 ± 0.14 1.00<br />
NGC 4486 783 187.70462 12.37152 0.75 −9.029 ± 0.018 −10.543 ± 0.020 4.66 ± 0.17 1.00<br />
NGC 4486 784 187.70459 12.37878 0.47 −6.654 ± 0.078 −7.265 ± 0.260 2.57 ± 0.47 0.99<br />
NGC 4486 785 187.70456 12.37960 0.44 −7.627 ± 0.040 −8.620 ± 0.034 2.36 ± 0.23 1.00<br />
NGC 4486 786 187.70458 12.38625 0.19 −7.320 ± 0.029 −8.452 ± 0.055 1.89 ± 0.21 1.00<br />
NGC 4486 788 187.70465 12.39455 0.14 −6.792 ± 0.084 −7.453 ± 2.355 1.99 ± 0.44 1.00<br />
NGC 4486 789 187.70464 12.39076 0.05 −7.025 ± 0.097 −8.484 ± 0.072 1.69 ± 0.37 1.00<br />
NGC 4486 791 187.70473 12.38724 0.15 −8.492 ± 0.030 −9.513 ± 0.026 2.78 ± 0.19 1.00<br />
NGC 4486 792 187.70481 12.40576 0.56 −9.975 ± 0.020 −11.050 ± 0.014 3.90 ± 0.09 1.00<br />
NGC 4486 794 187.70479 12.36975 0.81 −7.550 ± 0.023 −9.158 ± 0.028 2.61 ± 0.13 1.00<br />
NGC 4486 795 187.70491 12.36972 0.81 −9.119 ± 0.023 −10.522 ± 0.032 4.08 ± 0.21 1.00<br />
NGC 4486 796 187.70476 12.38006 0.42 −7.472 ± 0.027 −8.521 ± 0.029 2.13 ± 0.24 1.00<br />
NGC 4486 797 187.70479 12.41279 0.82 −7.034 ± 0.052 −8.579 ± 0.026 1.80 ± 0.26 1.00<br />
NGC 4486 799 187.70482 12.40860 0.66 −5.506 ± 0.105 −6.760 ± 0.142 2.44 ± 0.71 0.99<br />
NGC 4486 800 187.70482 12.36496 0.99 −5.624 ± 0.115 −6.870 ± 0.164 3.78 ± 0.97 0.94<br />
NGC 4486 801 187.70484 12.40132 0.39 −6.126 ± 0.086 −7.076 ± 0.152 2.92 ± 0.54 0.99<br />
NGC 4486 803 187.70488 12.38575 0.21 −7.316 ± 0.045 −8.705 ± 0.040 1.79 ± 0.29 1.00<br />
NGC 4486 804 187.70497 12.37859 0.48 −9.619 ± 0.023 −11.118 ± 0.021 1.89 ± 0.19 1.00<br />
NGC 4486 805 187.70493 12.38105 0.38 −7.136 ± 0.049 −8.225 ± 0.064 3.30 ± 0.38 1.00<br />
NGC 4486 808 187.70497 12.39932 0.31 −8.156 ± 0.026 −9.140 ± 0.028 2.80 ± 0.20 1.00<br />
NGC 4486 809 187.70508 12.40380 0.48 −7.140 ± 0.053 −8.711 ± 0.032 2.35 ± 0.20 1.00<br />
NGC 4486 810 187.70509 12.39727 0.24 −6.283 ± 0.181 −7.395 ± 0.272 2.82 ± 1.58 0.99<br />
NGC 4486 811 187.70512 12.40240 0.43 −6.180 ± 0.115 −8.053 ± 0.077 2.86 ± 0.54 1.00<br />
NGC 4486 812 187.70519 12.40472 0.52 −9.268 ± 0.024 −10.742 ± 0.022 2.78 ± 0.13 1.00<br />
NGC 4486 817 187.70526 12.37212 0.72 −8.669 ± 0.014 −10.067 ± 0.014 2.55 ± 0.10 1.00<br />
NGC 4486 819 187.70528 12.40229 0.42 −9.701 ± 0.016 −10.734 ± 0.018 2.84 ± 0.14 1.00<br />
NGC 4486 820 187.70532 12.38461 0.25 −7.774 ± 0.052 −9.048 ± 0.048 2.92 ± 0.28 1.00<br />
NGC 4486 821 187.70532 12.40826 0.65 −6.363 ± 0.169 −7.379 ± 0.234 5.67 ± 1.74 0.81<br />
NGC 4486 822 187.70534 12.36386 1.03 −6.706 ± 0.077 −7.969 ± 0.037 2.69 ± 0.32 1.00<br />
NGC 4486 823 187.70531 12.37152 0.74 −5.225 ± 0.130 −6.972 ± 0.363 5.09 ± 1.69 0.75<br />
NGC 4486 824 187.70536 12.41384 0.86 −6.843 ± 0.063 −7.656 ± 0.090 3.89 ± 0.40 0.98<br />
NGC 4486 825 187.70535 12.38632 0.18 −7.112 ± 0.169 −8.577 ± 0.042 2.38 ± 0.34 1.00<br />
NGC 4486 826 187.70531 12.38056 0.40 −9.396 ± 0.023 −10.497 ± 0.015 2.98 ± 0.11 1.00<br />
NGC 4486 827 187.70539 12.40396 0.49 −7.789 ± 0.041 −8.774 ± 0.061 5.05 ± 0.20 0.99<br />
NGC 4486 828 187.70545 12.37590 0.58 −9.501 ± 0.018 −10.891 ± 0.015 2.61 ± 0.14 1.00<br />
NGC 4486 829 187.70546 12.37599 0.57 −7.109 ± 0.027 −8.359 ± 0.048 1.78 ± 0.24 1.00<br />
NGC 4486 830 187.70540 12.37380 0.66 −5.943 ± 0.240 −7.546 ± 0.177 3.80 ± 0.92 0.98<br />
NGC 4486 831 187.70546 12.37692 0.54 −8.003 ± 0.036 −9.342 ± 0.033 3.80 ± 0.17 1.00<br />
NGC 4486 832 187.70545 12.40011 0.34 −8.875 ± 0.022 −10.040 ± 0.018 2.78 ± 0.15 1.00<br />
NGC 4486 834 187.70547 12.40219 0.42 −6.250 ± 0.138 −7.700 ± 0.095 4.11 ± 0.63 0.98<br />
NGC 4486 835 187.70547 12.37082 0.77 −6.184 ± 0.088 −7.090 ± 0.109 3.71 ± 0.49 0.96<br />
Continued on Next Page. . .<br />
354
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4486 837 187.70546 12.40368 0.48 −6.926 ± 0.037 −8.203 ± 0.022 2.31 ± 0.16 1.00<br />
NGC 4486 838 187.70555 12.41734 1.00 −8.569 ± 0.025 −10.045 ± 0.015 2.17 ± 0.16 1.00<br />
NGC 4486 839 187.70558 12.38484 0.24 −8.902 ± 0.032 −10.525 ± 0.027 2.18 ± 0.20 1.00<br />
NGC 4486 841 187.70555 12.37682 0.54 −6.565 ± 0.073 −8.078 ± 0.244 2.13 ± 0.35 1.00<br />
NGC 4486 842 187.70562 12.40793 0.64 −9.069 ± 0.019 −9.884 ± 0.017 3.27 ± 0.10 1.00<br />
NGC 4486 846 187.70539 12.38525 0.22 −7.253 ± 0.050 −8.681 ± 0.061 1.97 ± 0.40 1.00<br />
NGC 4486 847 187.70560 12.40350 0.47 −7.119 ± 0.039 −8.740 ± 0.055 3.38 ± 0.34 1.00<br />
NGC 4486 848 187.70563 12.38446 0.25 −7.964 ± 0.027 −8.819 ± 0.055 2.65 ± 0.23 1.00<br />
NGC 4486 852 187.70572 12.38103 0.38 −7.849 ± 0.019 −9.202 ± 0.027 1.69 ± 0.16 1.00<br />
NGC 4486 853 187.70574 12.40641 0.58 −7.764 ± 0.041 −9.072 ± 0.030 2.72 ± 0.17 1.00<br />
NGC 4486 854 187.70572 12.37522 0.60 −6.024 ± 0.427 −7.410 ± 0.138 2.92 ± 0.80 0.99<br />
NGC 4486 856 187.70575 12.38609 0.19 −6.526 ± 0.068 −7.978 ± 0.065 2.48 ± 0.31 1.00<br />
NGC 4486 857 187.70581 12.40377 0.48 −8.615 ± 0.022 −10.098 ± 0.014 2.19 ± 0.16 1.00<br />
NGC 4486 858 187.70580 12.40350 0.47 −6.489 ± 0.159 −8.015 ± 0.030 1.34 ± 0.28 0.97<br />
NGC 4486 859 187.70580 12.36785 0.88 −5.323 ± 0.104 −6.217 ± 0.147 2.84 ± 0.52 0.98<br />
NGC 4486 860 187.70584 12.38489 0.24 −7.111 ± 0.057 −8.538 ± 0.049 2.17 ± 0.27 1.00<br />
NGC 4486 861 187.70569 12.41606 0.95 −6.022 ± 0.060 −6.772 ± 0.062 2.47 ± 0.36 0.99<br />
NGC 4486 863 187.70591 12.40575 0.56 −7.801 ± 0.038 −8.941 ± 0.045 3.21 ± 0.22 1.00<br />
NGC 4486 864 187.70591 12.41076 0.75 −5.912 ± 0.118 −7.201 ± 0.098 5.45 ± 0.58 0.78<br />
NGC 4486 865 187.70596 12.38998 0.04 −9.258 ± 0.031 −10.620 ± 0.018 1.46 ± 0.18 0.97<br />
NGC 4486 868 187.70607 12.37702 0.54 −8.421 ± 0.021 −9.995 ± 0.022 3.13 ± 0.12 1.00<br />
NGC 4486 869 187.70604 12.39626 0.20 −6.824 ± 0.098 −8.288 ± 0.288 1.32 ± 0.43 0.97<br />
NGC 4486 870 187.70607 12.37771 0.51 −7.553 ± 0.071 −9.158 ± 0.022 1.90 ± 0.22 1.00<br />
NGC 4486 871 187.70611 12.41512 0.91 −7.876 ± 0.033 −8.781 ± 0.019 2.65 ± 0.16 1.00<br />
NGC 4486 872 187.70622 12.41469 0.89 −7.810 ± 0.026 −8.671 ± 0.030 2.60 ± 0.15 1.00<br />
NGC 4486 873 187.70629 12.37761 0.51 −9.385 ± 0.018 −10.718 ± 0.018 2.74 ± 0.13 1.00<br />
NGC 4486 874 187.70626 12.39025 0.04 −7.781 ± 0.063 −9.136 ± 0.056 2.89 ± 0.34 1.00<br />
NGC 4486 875 187.70630 12.37581 0.58 −6.080 ± 0.074 −7.155 ± 0.385 3.60 ± 4.05 0.97<br />
NGC 4486 877 187.70633 12.39216 0.04 −8.070 ± 0.143 −9.530 ± 1.002 1.62 ± 0.36 1.00<br />
NGC 4486 879 187.70642 12.41359 0.85 −9.046 ± 0.019 −9.945 ± 0.015 3.14 ± 0.11 1.00<br />
NGC 4486 881 187.70648 12.36432 1.02 −7.905 ± 0.024 −9.434 ± 0.025 2.41 ± 0.14 1.00<br />
NGC 4486 882 187.70647 12.36834 0.86 −6.918 ± 0.051 −7.867 ± 0.074 3.37 ± 0.31 0.99<br />
NGC 4486 883 187.70648 12.37216 0.72 −7.089 ± 0.038 −7.932 ± 0.044 2.40 ± 0.21 1.00<br />
NGC 4486 885 187.70650 12.38438 0.26 −7.563 ± 0.025 −8.690 ± 0.064 3.34 ± 0.33 1.00<br />
NGC 4486 886 187.70650 12.40689 0.60 −7.973 ± 0.029 −9.318 ± 0.029 2.96 ± 0.14 1.00<br />
NGC 4486 887 187.70656 12.40206 0.42 −8.076 ± 0.027 −9.403 ± 0.021 2.52 ± 0.13 1.00<br />
NGC 4486 889 187.70656 12.36726 0.91 −6.321 ± 0.038 −7.463 ± 0.108 2.81 ± 0.44 0.99<br />
NGC 4486 890 187.70658 12.36266 1.08 −7.186 ± 0.167 −8.607 ± 0.845 1.51 ± 0.50 0.99<br />
NGC 4486 891 187.70666 12.38993 0.05 −8.309 ± 0.068 −9.372 ± 0.270 3.16 ± 0.97 1.00<br />
NGC 4486 893 187.70664 12.37835 0.49 −6.727 ± 0.046 −7.792 ± 0.089 2.24 ± 0.43 1.00<br />
NGC 4486 896 187.70673 12.37609 0.57 −7.154 ± 0.042 −8.048 ± 0.048 2.88 ± 0.27 1.00<br />
NGC 4486 898 187.70674 12.40301 0.45 −6.838 ± 0.046 −8.081 ± 0.050 2.81 ± 0.27 1.00<br />
NGC 4486 899 187.70671 12.38021 0.42 −5.108 ± 0.443 −6.677 ± 0.973 1.70 ± 0.51 0.98<br />
NGC 4486 901 187.70681 12.40789 0.64 −9.491 ± 0.022 −10.493 ± 0.033 6.98 ± 0.15 1.00<br />
NGC 4486 902 187.70691 12.39836 0.28 −10.913 ± 0.017 −12.093 ± 0.010 3.72 ± 0.10 1.00<br />
NGC 4486 903 187.70681 12.39590 0.18 −7.155 ± 0.038 −8.526 ± 0.094 2.53 ± 0.37 1.00<br />
NGC 4486 905 187.70685 12.39982 0.33 −5.758 ± 0.195 −7.173 ± 0.108 2.33 ± 0.50 1.00<br />
NGC 4486 906 187.70690 12.39003 0.05 −7.467 ± 0.163 −8.442 ± 0.161 4.20 ± 0.94 1.00<br />
NGC 4486 907 187.70691 12.39123 0.04 −7.335 ± 0.137 −9.022 ± 0.218 4.41 ± 1.67 1.00<br />
NGC 4486 908 187.70700 12.40012 0.34 −6.172 ± 0.105 −7.799 ± 0.171 2.83 ± 1.18 1.00<br />
NGC 4486 909 187.70685 12.38510 0.23 −7.085 ± 0.061 −8.592 ± 0.129 3.35 ± 0.50 1.00<br />
NGC 4486 910 187.70706 12.39884 0.30 −9.040 ± 0.024 −10.468 ± 0.010 2.25 ± 0.16 1.00<br />
NGC 4486 911 187.70700 12.37949 0.44 −7.793 ± 0.031 −9.081 ± 0.021 2.62 ± 0.16 1.00<br />
NGC 4486 912 187.70705 12.40351 0.47 −6.406 ± 0.077 −7.498 ± 0.057 2.98 ± 0.31 0.99<br />
NGC 4486 914 187.70706 12.40109 0.38 −6.776 ± 0.046 −8.310 ± 0.036 2.44 ± 0.19 1.00<br />
NGC 4486 915 187.70714 12.39187 0.05 −9.904 ± 0.022 −11.330 ± 0.023 1.62 ± 0.20 1.00<br />
NGC 4486 916 187.70718 12.37020 0.80 −8.071 ± 0.023 −9.468 ± 0.025 2.99 ± 0.18 1.00<br />
NGC 4486 917 187.70724 12.37931 0.45 −7.857 ± 0.057 −9.540 ± 0.081 5.66 ± 0.46 1.00<br />
NGC 4486 918 187.70722 12.38141 0.37 −6.698 ± 0.071 −7.942 ± 0.179 4.17 ± 1.23 0.99<br />
NGC 4486 919 187.70728 12.41232 0.81 −7.734 ± 0.030 −8.876 ± 0.030 2.52 ± 0.16 1.00<br />
NGC 4486 920 187.70726 12.37841 0.48 −7.913 ± 0.031 −9.403 ± 0.036 2.23 ± 0.14 1.00<br />
NGC 4486 922 187.70722 12.38118 0.38 −5.178 ± 0.660 −6.722 ± 0.153 2.83 ± 0.74 0.98<br />
Continued on Next Page. . .<br />
355
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4486 924 187.70726 12.37634 0.56 −5.771 ± 0.935 −7.377 ± 0.460 2.54 ± 0.88 1.00<br />
NGC 4486 926 187.70737 12.37225 0.72 −7.361 ± 0.051 −8.886 ± 0.022 2.48 ± 0.23 1.00<br />
NGC 4486 927 187.70743 12.40834 0.66 −7.760 ± 0.031 −8.875 ± 0.024 2.31 ± 0.16 1.00<br />
NGC 4486 930 187.70741 12.40778 0.63 −5.942 ± 0.064 −7.343 ± 0.309 2.39 ± 0.38 1.00<br />
NGC 4486 931 187.70746 12.40656 0.59 −6.408 ± 0.071 −7.734 ± 0.082 2.76 ± 0.37 1.00<br />
NGC 4486 932 187.70749 12.36430 1.02 −6.066 ± 0.092 −7.609 ± 0.319 2.67 ± 0.63 1.00<br />
NGC 4486 935 187.70760 12.37681 0.55 −7.558 ± 0.036 −8.398 ± 0.048 3.14 ± 0.23 1.00<br />
NGC 4486 937 187.70760 12.39552 0.18 −9.547 ± 0.014 −10.643 ± 0.020 3.20 ± 0.10 1.00<br />
NGC 4486 938 187.70760 12.40529 0.54 −7.866 ± 0.024 −9.320 ± 0.021 2.67 ± 0.16 1.00<br />
NGC 4486 943 187.70775 12.40260 0.44 −7.853 ± 0.844 −9.412 ± 0.039 2.17 ± 0.40 1.00<br />
NGC 4486 945 187.70778 12.37261 0.71 −6.082 ± 0.083 −6.986 ± 0.416 1.34 ± 0.40 0.95<br />
NGC 4486 947 187.70784 12.41373 0.86 −5.808 ± 0.659 −7.485 ± 0.082 2.09 ± 0.60 1.00<br />
NGC 4486 949 187.70784 12.41179 0.79 −5.553 ± 0.273 −7.057 ± 0.101 1.97 ± 0.50 0.99<br />
NGC 4486 950 187.70791 12.38112 0.39 −6.323 ± 0.263 −7.551 ± 0.109 2.51 ± 0.47 1.00<br />
NGC 4486 951 187.70794 12.39640 0.21 −7.888 ± 0.042 −9.415 ± 0.026 2.34 ± 0.20 1.00<br />
NGC 4486 953 187.70801 12.40881 0.68 −5.728 ± 0.204 −6.930 ± 0.199 3.84 ± 1.09 0.94<br />
NGC 4486 954 187.70804 12.41687 0.98 −4.956 ± 0.238 −6.366 ± 0.172 4.07 ± 1.18 0.87<br />
NGC 4486 955 187.70809 12.38183 0.36 −7.691 ± 0.038 −9.247 ± 0.034 3.42 ± 0.23 1.00<br />
NGC 4486 957 187.70815 12.40167 0.41 −8.423 ± 0.026 −9.785 ± 0.022 2.41 ± 0.12 1.00<br />
NGC 4486 958 187.70813 12.37934 0.45 −8.026 ± 0.030 −9.345 ± 0.031 1.64 ± 0.20 1.00<br />
NGC 4486 959 187.70820 12.41088 0.75 −8.383 ± 0.042 −9.910 ± 0.015 2.04 ± 0.19 1.00<br />
NGC 4486 961 187.70825 12.37558 0.60 −6.711 ± 0.048 −8.442 ± 0.066 3.28 ± 0.28 1.00<br />
NGC 4486 962 187.70823 12.36472 1.01 −5.104 ± 0.142 −6.240 ± 0.444 4.75 ± 4.12 0.75<br />
NGC 4486 963 187.70826 12.38098 0.39 −7.057 ± 0.067 −7.891 ± 0.115 4.74 ± 0.53 0.97<br />
NGC 4486 964 187.70830 12.39591 0.20 −7.415 ± 0.051 −8.760 ± 0.078 2.79 ± 0.37 1.00<br />
NGC 4486 966 187.70827 12.38457 0.26 −6.219 ± 0.094 −7.872 ± 0.284 1.93 ± 0.52 1.00<br />
NGC 4486 968 187.70820 12.39616 0.21 −6.934 ± 1.146 −7.725 ± 0.366 1.88 ± 0.66 1.00<br />
NGC 4486 971 187.70841 12.39618 0.21 −6.393 ± 0.107 −7.374 ± 1.142 2.11 ± 0.50 1.00<br />
NGC 4486 972 187.70842 12.37006 0.80 −5.959 ± 0.094 −7.352 ± 0.032 2.45 ± 0.36 1.00<br />
NGC 4486 973 187.70845 12.39564 0.20 −7.047 ± 0.063 −8.288 ± 0.122 2.15 ± 0.24 1.00<br />
NGC 4486 974 187.70849 12.38250 0.34 −9.165 ± 0.026 −10.070 ± 0.018 2.51 ± 0.19 1.00<br />
NGC 4486 975 187.70851 12.40137 0.40 −7.279 ± 0.036 −8.326 ± 0.039 1.54 ± 0.22 0.99<br />
NGC 4486 976 187.70856 12.36335 1.06 −7.453 ± 0.040 −8.710 ± 0.031 3.40 ± 0.23 1.00<br />
NGC 4486 977 187.70853 12.38227 0.35 −7.748 ± 0.034 −8.593 ± 0.047 2.03 ± 0.21 1.00<br />
NGC 4486 979 187.70856 12.36625 0.95 −7.017 ± 0.033 −8.554 ± 0.029 2.32 ± 0.23 1.00<br />
NGC 4486 980 187.70857 12.40805 0.65 −8.400 ± 0.016 −9.391 ± 0.025 2.97 ± 0.14 1.00<br />
NGC 4486 981 187.70853 12.39045 0.10 −8.789 ± 0.023 −9.953 ± 0.031 2.46 ± 0.15 1.00<br />
NGC 4486 982 187.70835 12.37459 0.63 −5.511 ± 0.100 −7.089 ± 0.063 5.51 ± 0.38 0.72<br />
NGC 4486 985 187.70868 12.38030 0.42 −7.895 ± 0.021 −9.402 ± 0.025 1.65 ± 0.15 1.00<br />
NGC 4486 987 187.70870 12.37158 0.75 −7.548 ± 0.027 −8.556 ± 0.034 2.59 ± 0.18 1.00<br />
NGC 4486 989 187.70872 12.38477 0.26 −9.168 ± 0.019 −10.265 ± 0.017 3.14 ± 0.14 1.00<br />
NGC 4486 991 187.70885 12.38250 0.34 −7.997 ± 0.035 −9.552 ± 0.024 2.07 ± 0.19 1.00<br />
NGC 4486 994 187.70890 12.37647 0.57 −8.999 ± 0.019 −9.957 ± 0.016 3.25 ± 0.15 1.00<br />
NGC 4486 996 187.70886 12.38154 0.38 −5.999 ± 0.184 −7.436 ± 0.215 2.81 ± 1.04 0.99<br />
NGC 4486 997 187.70886 12.38415 0.29 −7.436 ± 0.037 −8.976 ± 0.036 2.47 ± 0.22 1.00<br />
NGC 4486 998 187.70888 12.40133 0.40 −6.738 ± 0.047 −8.271 ± 0.028 2.05 ± 0.27 1.00<br />
NGC 4486 999 187.70892 12.40658 0.60 −7.490 ± 0.028 −8.323 ± 0.028 2.17 ± 0.23 1.00<br />
NGC 4486 1000 187.70897 12.40274 0.45 −7.325 ± 0.117 −8.554 ± 0.142 7.88 ± 0.93 0.80<br />
NGC 4486 1001 187.70894 12.39310 0.13 −7.857 ± 0.044 −9.050 ± 0.047 2.33 ± 0.27 1.00<br />
NGC 4486 1002 187.70894 12.39558 0.20 −7.491 ± 0.034 −8.487 ± 0.032 2.70 ± 0.20 1.00<br />
NGC 4486 1003 187.70899 12.39736 0.26 −8.882 ± 0.022 −10.505 ± 0.011 2.23 ± 0.12 1.00<br />
NGC 4486 1004 187.70907 12.38108 0.40 −10.446 ± 0.022 −11.791 ± 0.013 2.77 ± 0.13 1.00<br />
NGC 4486 1005 187.70904 12.38133 0.39 −8.969 ± 0.017 −10.132 ± 0.018 1.78 ± 0.11 1.00<br />
NGC 4486 1006 187.70907 12.36870 0.86 −7.337 ± 0.099 −8.209 ± 0.199 6.40 ± 1.52 0.87<br />
NGC 4486 1007 187.70905 12.39683 0.25 −8.982 ± 0.016 −9.951 ± 0.013 2.56 ± 0.12 1.00<br />
NGC 4486 1009 187.70905 12.41112 0.77 −6.583 ± 0.038 −8.196 ± 0.205 1.20 ± 0.25 0.95<br />
NGC 4486 1010 187.70905 12.39330 0.14 −6.646 ± 0.395 −8.503 ± 0.121 2.61 ± 0.62 1.00<br />
NGC 4486 1012 187.70910 12.40168 0.42 −6.623 ± 0.096 −7.226 ± 0.111 3.02 ± 0.44 0.99<br />
NGC 4486 1013 187.70909 12.39977 0.35 −6.032 ± 0.114 −6.975 ± 0.666 2.41 ± 0.68 0.99<br />
NGC 4486 1014 187.70911 12.37913 0.47 −5.002 ± 0.222 −6.860 ± 0.462 3.17 ± 1.04 0.97<br />
NGC 4486 1015 187.70916 12.38233 0.35 −6.173 ± 0.120 −7.444 ± 0.066 2.04 ± 0.57 1.00<br />
NGC 4486 1016 187.70917 12.41414 0.88 −7.859 ± 0.026 −9.013 ± 0.027 2.49 ± 0.17 1.00<br />
Continued on Next Page. . .<br />
356
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4486 1018 187.70924 12.38387 0.30 −5.969 ± 0.301 −7.302 ± 0.276 2.11 ± 0.45 1.00<br />
NGC 4486 1019 187.70932 12.39941 0.34 −6.923 ± 0.058 −8.366 ± 0.049 2.35 ± 0.28 1.00<br />
NGC 4486 1020 187.70936 12.41498 0.91 −8.992 ± 0.017 −9.940 ± 0.010 2.71 ± 0.09 1.00<br />
NGC 4486 1021 187.70933 12.36913 0.84 −5.865 ± 0.091 −7.052 ± 0.379 2.65 ± 1.42 0.99<br />
NGC 4486 1022 187.70905 12.40247 0.45 −7.663 ± 0.044 −8.513 ± 0.058 3.60 ± 0.29 1.00<br />
NGC 4486 1023 187.70940 12.37924 0.47 −9.215 ± 0.038 −10.213 ± 0.020 2.23 ± 0.15 1.00<br />
NGC 4486 1024 187.70939 12.37821 0.51 −6.919 ± 0.051 −7.891 ± 0.087 3.12 ± 0.41 1.00<br />
NGC 4486 1025 187.70940 12.37377 0.67 −7.369 ± 0.024 −8.542 ± 0.041 2.57 ± 0.14 1.00<br />
NGC 4486 1026 187.70942 12.37722 0.54 −7.402 ± 0.027 −8.509 ± 0.039 2.72 ± 0.26 1.00<br />
NGC 4486 1027 187.70941 12.39476 0.19 −8.101 ± 0.024 −9.305 ± 0.028 2.14 ± 0.18 1.00<br />
NGC 4486 1028 187.70946 12.40545 0.56 −7.648 ± 0.024 −8.730 ± 0.030 2.83 ± 0.19 1.00<br />
NGC 4486 1029 187.70949 12.38307 0.33 −6.042 ± 0.119 −7.095 ± 1.036 1.54 ± 0.89 0.98<br />
NGC 4486 1030 187.70954 12.39530 0.21 −8.632 ± 0.019 −9.668 ± 0.026 3.27 ± 0.10 1.00<br />
NGC 4486 1031 187.70952 12.41035 0.74 −6.333 ± 0.057 −7.807 ± 0.054 1.58 ± 0.37 0.99<br />
NGC 4486 1032 187.70954 12.41464 0.90 −7.293 ± 0.031 −8.776 ± 0.029 2.29 ± 0.18 1.00<br />
NGC 4486 1033 187.70956 12.41109 0.77 −6.286 ± 0.044 −7.876 ± 0.044 2.02 ± 0.33 1.00<br />
NGC 4486 1034 187.70961 12.39741 0.27 −6.416 ± 0.104 −7.270 ± 0.174 3.63 ± 0.74 0.97<br />
NGC 4486 1035 187.70963 12.39652 0.25 −6.948 ± 0.067 −7.653 ± 0.076 3.16 ± 0.33 0.99<br />
NGC 4486 1036 187.70970 12.38164 0.39 −10.173 ± 0.026 −11.224 ± 0.013 2.43 ± 0.17 1.00<br />
NGC 4486 1037 187.70970 12.38305 0.34 −7.460 ± 0.029 −8.867 ± 0.024 2.49 ± 0.16 1.00<br />
NGC 4486 1038 187.70967 12.40564 0.57 −6.317 ± 0.089 −6.978 ± 0.206 3.96 ± 0.81 0.93<br />
NGC 4486 1039 187.70975 12.38218 0.37 −7.893 ± 0.089 −9.268 ± 0.157 2.44 ± 0.51 1.00<br />
NGC 4486 1040 187.70972 12.40743 0.63 −7.669 ± 0.051 −8.830 ± 0.040 4.17 ± 0.19 1.00<br />
NGC 4486 1041 187.70970 12.36954 0.83 −7.025 ± 0.035 −8.551 ± 0.049 2.07 ± 0.27 1.00<br />
NGC 4486 1042 187.70982 12.37899 0.48 −5.981 ± 0.485 −7.554 ± 0.496 0.88 ± 0.38 0.85<br />
NGC 4486 1043 187.70981 12.38041 0.43 −6.569 ± 0.069 −8.142 ± 0.049 1.88 ± 0.26 1.00<br />
NGC 4486 1044 187.70987 12.36670 0.94 −7.069 ± 0.028 −8.728 ± 0.029 2.85 ± 0.21 1.00<br />
NGC 4486 1046 187.70989 12.41011 0.74 −6.724 ± 0.049 −7.705 ± 0.061 4.20 ± 0.22 0.98<br />
NGC 4486 1047 187.70992 12.40055 0.39 −9.417 ± 0.020 −10.719 ± 0.019 2.67 ± 0.17 1.00<br />
NGC 4486 1048 187.70992 12.40170 0.43 −7.589 ± 0.029 −8.763 ± 0.076 3.83 ± 0.35 1.00<br />
NGC 4486 1049 187.70991 12.40457 0.53 −5.443 ± 0.167 −7.068 ± 0.221 4.08 ± 1.23 0.93<br />
NGC 4486 1050 187.70974 12.37015 0.81 −7.492 ± 0.030 −8.444 ± 0.035 2.85 ± 0.17 1.00<br />
NGC 4486 1051 187.70993 12.36804 0.89 −6.744 ± 2.243 −7.261 ± 0.088 0.95 ± 0.56 0.86<br />
NGC 4486 1053 187.71002 12.40276 0.47 −7.803 ± 0.025 −9.134 ± 0.022 2.31 ± 0.23 1.00<br />
NGC 4486 1055 187.71007 12.36322 1.07 −6.914 ± 0.038 −8.013 ± 0.072 3.48 ± 0.41 0.99<br />
NGC 4486 1057 187.71015 12.37125 0.77 −7.670 ± 0.070 −8.459 ± 0.052 5.51 ± 0.36 0.96<br />
NGC 4486 1058 187.71011 12.39620 0.25 −6.715 ± 0.062 −8.221 ± 0.069 2.39 ± 0.28 1.00<br />
NGC 4486 1059 187.71013 12.40446 0.53 −7.846 ± 0.028 −9.353 ± 0.022 1.87 ± 0.20 1.00<br />
NGC 4486 1061 187.71029 12.41375 0.87 −6.850 ± 0.037 −8.314 ± 0.037 2.08 ± 0.24 1.00<br />
NGC 4486 1062 187.71027 12.38295 0.35 −5.793 ± 0.075 −7.105 ± 0.414 1.36 ± 0.44 0.96<br />
NGC 4486 1064 187.71024 12.40219 0.45 −6.063 ± 0.158 −7.418 ± 0.084 3.69 ± 0.60 0.98<br />
NGC 4486 1066 187.71030 12.40163 0.43 −6.052 ± 0.066 −7.504 ± 0.627 2.71 ± 0.56 1.00<br />
NGC 4486 1067 187.71036 12.37641 0.58 −5.801 ± 0.960 −7.153 ± 0.090 0.94 ± 0.51 0.85<br />
NGC 4486 1071 187.71051 12.38853 0.20 −6.913 ± 0.048 −8.418 ± 0.074 2.40 ± 0.34 1.00<br />
NGC 4486 1072 187.71055 12.39230 0.18 −9.163 ± 0.019 −10.517 ± 0.012 1.93 ± 0.12 1.00<br />
NGC 4486 1073 187.71055 12.39982 0.37 −7.612 ± 0.050 −9.066 ± 0.035 2.99 ± 0.30 1.00<br />
NGC 4486 1074 187.71055 12.40021 0.38 −6.620 ± 0.069 −8.505 ± 0.075 3.11 ± 0.43 1.00<br />
NGC 4486 1077 187.71062 12.38331 0.34 −6.352 ± 0.091 −7.997 ± 0.143 4.49 ± 0.96 0.98<br />
NGC 4486 1079 187.71070 12.36603 0.97 −6.458 ± 0.108 −8.002 ± 0.036 1.96 ± 0.39 1.00<br />
NGC 4486 1080 187.71073 12.39190 0.18 −7.944 ± 0.037 −8.749 ± 0.029 2.53 ± 0.18 1.00<br />
NGC 4486 1081 187.71076 12.40933 0.71 −8.177 ± 0.027 −9.608 ± 0.019 2.43 ± 0.16 1.00<br />
NGC 4486 1082 187.71076 12.40949 0.72 −8.364 ± 0.051 −9.300 ± 0.035 2.19 ± 0.26 1.00<br />
NGC 4486 1083 187.71070 12.38749 0.22 −5.975 ± 0.374 −7.134 ± 0.164 3.06 ± 0.77 0.99<br />
NGC 4486 1084 187.71075 12.36968 0.83 −7.796 ± 0.028 −9.262 ± 0.022 2.17 ± 0.14 1.00<br />
NGC 4486 1086 187.71076 12.38154 0.41 −7.289 ± 0.113 −8.797 ± 0.032 2.35 ± 0.26 1.00<br />
NGC 4486 1088 187.71085 12.37994 0.46 −7.167 ± 0.062 −7.757 ± 0.047 2.41 ± 0.29 1.00<br />
NGC 4486 1089 187.71090 12.40461 0.54 −7.702 ± 0.059 −8.376 ± 0.046 4.44 ± 0.21 1.00<br />
NGC 4486 1090 187.71097 12.40181 0.45 −8.663 ± 0.031 −10.076 ± 0.034 4.80 ± 0.22 1.00<br />
NGC 4486 1091 187.71091 12.37904 0.49 −6.207 ± 0.688 −7.649 ± 0.096 2.27 ± 0.51 1.00<br />
NGC 4486 1093 187.71095 12.40015 0.39 −7.120 ± 0.084 −8.399 ± 0.242 4.96 ± 1.92 0.99<br />
NGC 4486 1095 187.71105 12.37914 0.49 −6.982 ± 0.040 −8.660 ± 0.046 2.00 ± 0.21 1.00<br />
NGC 4486 1098 187.71103 12.39452 0.23 −7.768 ± 0.036 −9.181 ± 0.032 2.48 ± 0.16 1.00<br />
Continued on Next Page. . .<br />
357
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4486 1099 187.71107 12.40129 0.43 −6.077 ± 0.092 −7.347 ± 0.139 2.98 ± 0.69 0.99<br />
NGC 4486 1101 187.71115 12.40683 0.63 −8.296 ± 0.025 −9.678 ± 0.014 2.55 ± 0.15 1.00<br />
NGC 4486 1102 187.71115 12.39465 0.24 −7.585 ± 0.051 −8.406 ± 0.057 2.66 ± 0.31 1.00<br />
NGC 4486 1103 187.71117 12.40217 0.46 −7.220 ± 0.028 −8.588 ± 0.037 2.55 ± 0.25 1.00<br />
NGC 4486 1104 187.71121 12.38997 0.20 −8.937 ± 0.017 −9.988 ± 0.017 2.53 ± 0.14 1.00<br />
NGC 4486 1105 187.71120 12.38293 0.37 −7.189 ± 0.026 −8.739 ± 0.272 2.27 ± 0.32 1.00<br />
NGC 4486 1107 187.71136 12.39406 0.23 −8.121 ± 0.023 −9.553 ± 0.022 2.13 ± 0.18 1.00<br />
NGC 4486 1109 187.71142 12.40794 0.67 −6.234 ± 0.252 −8.000 ± 0.072 3.14 ± 0.41 1.00<br />
NGC 4486 1111 187.71146 12.36336 1.07 −7.275 ± 0.054 −8.858 ± 0.044 3.35 ± 0.27 1.00<br />
NGC 4486 1114 187.71164 12.36385 1.06 −7.520 ± 0.029 −8.249 ± 0.033 2.80 ± 0.22 1.00<br />
NGC 4486 1116 187.71161 12.41359 0.88 −7.381 ± 0.029 −8.386 ± 0.045 3.23 ± 0.17 1.00<br />
NGC 4486 1117 187.71175 12.39950 0.38 −8.459 ± 0.028 −9.355 ± 0.028 2.53 ± 0.17 1.00<br />
NGC 4486 1118 187.71174 12.36968 0.84 −6.726 ± 0.044 −8.197 ± 0.042 1.47 ± 0.24 0.99<br />
NGC 4486 1119 187.71173 12.40371 0.52 −6.916 ± 0.035 −8.256 ± 0.032 2.35 ± 0.18 1.00<br />
NGC 4486 1120 187.71181 12.40731 0.65 −8.674 ± 0.020 −10.178 ± 0.010 2.27 ± 0.14 1.00<br />
NGC 4486 1121 187.71181 12.40436 0.55 −7.454 ± 0.031 −8.957 ± 0.022 2.02 ± 0.22 1.00<br />
NGC 4486 1122 187.71187 12.37645 0.60 −6.681 ± 0.308 −8.268 ± 0.039 1.72 ± 0.28 1.00<br />
NGC 4486 1123 187.71192 12.36855 0.88 −7.301 ± 0.032 −8.350 ± 0.033 2.33 ± 0.19 1.00<br />
NGC 4486 1124 187.71193 12.41018 0.76 −6.218 ± 0.294 −7.769 ± 0.039 1.67 ± 0.26 0.99<br />
NGC 4486 1125 187.71200 12.40301 0.50 −7.779 ± 0.017 −9.069 ± 0.079 2.75 ± 0.39 1.00<br />
NGC 4486 1126 187.71205 12.41101 0.79 −7.741 ± 0.030 −8.665 ± 0.044 3.37 ± 0.17 1.00<br />
NGC 4486 1127 187.71210 12.41062 0.77 −6.918 ± 0.035 −8.266 ± 0.024 2.28 ± 0.22 1.00<br />
NGC 4486 1128 187.71213 12.36325 1.08 −7.045 ± 0.044 −8.344 ± 0.048 4.20 ± 0.20 1.00<br />
NGC 4486 1129 187.71211 12.37340 0.71 −6.006 ± 0.197 −7.626 ± 0.057 1.96 ± 0.37 1.00<br />
NGC 4486 1130 187.71225 12.36839 0.89 −10.014 ± 0.012 −10.991 ± 0.015 4.06 ± 0.05 1.00<br />
NGC 4486 1131 187.71215 12.37831 0.54 −6.010 ± 0.152 −7.635 ± 0.143 4.64 ± 1.01 0.95<br />
NGC 4486 1132 187.71218 12.36989 0.84 −6.492 ± 0.034 −7.778 ± 0.035 2.26 ± 0.22 1.00<br />
NGC 4486 1133 187.71224 12.38425 0.35 −8.477 ± 0.028 −9.486 ± 0.027 2.35 ± 0.19 1.00<br />
NGC 4486 1135 187.71230 12.36609 0.98 −7.241 ± 0.025 −8.764 ± 0.090 2.05 ± 0.22 1.00<br />
NGC 4486 1136 187.71239 12.37374 0.70 −7.720 ± 0.069 −9.135 ± 0.074 4.78 ± 0.39 1.00<br />
NGC 4486 1137 187.71237 12.41407 0.90 −6.446 ± 0.059 −7.791 ± 0.041 1.99 ± 0.29 1.00<br />
NGC 4486 1138 187.71240 12.37110 0.80 −7.122 ± 0.052 −8.561 ± 0.034 2.78 ± 0.28 1.00<br />
NGC 4486 1139 187.71249 12.38108 0.45 −10.315 ± 0.030 −11.764 ± 0.020 2.82 ± 0.14 1.00<br />
NGC 4486 1140 187.71244 12.36906 0.87 −7.428 ± 0.030 −8.711 ± 0.042 2.42 ± 0.25 1.00<br />
NGC 4486 1142 187.71262 12.37823 0.55 −8.884 ± 0.019 −10.434 ± 0.016 2.23 ± 0.14 1.00<br />
NGC 4486 1143 187.71254 12.38788 0.27 −6.521 ± 0.978 −8.003 ± 0.448 1.50 ± 0.42 0.99<br />
NGC 4486 1144 187.71261 12.36943 0.86 −7.879 ± 0.025 −9.191 ± 0.025 2.41 ± 0.17 1.00<br />
NGC 4486 1145 187.71258 12.39208 0.25 −7.774 ± 0.036 −9.254 ± 0.039 2.29 ± 0.25 1.00<br />
NGC 4486 1146 187.71258 12.41807 1.05 −5.610 ± 0.075 −7.052 ± 0.130 4.58 ± 0.57 0.87<br />
NGC 4486 1147 187.71262 12.38056 0.47 −7.637 ± 0.034 −8.684 ± 0.039 2.42 ± 0.24 1.00<br />
NGC 4486 1149 187.71275 12.36716 0.94 −6.631 ± 0.038 −7.748 ± 0.080 2.92 ± 0.42 1.00<br />
NGC 4486 1150 187.71273 12.37784 0.56 −5.416 ± 0.339 −6.939 ± 0.132 3.39 ± 0.94 0.97<br />
NGC 4486 1151 187.71277 12.40177 0.48 −6.188 ± 0.045 −7.403 ± 0.088 2.33 ± 0.52 1.00<br />
NGC 4486 1152 187.71288 12.39013 0.26 −8.584 ± 0.024 −9.888 ± 0.025 2.58 ± 0.14 1.00<br />
NGC 4486 1153 187.71287 12.36810 0.91 −7.615 ± 0.033 −8.636 ± 0.036 2.73 ± 0.22 1.00<br />
NGC 4486 1154 187.71280 12.38872 0.27 −6.282 ± 0.106 −7.732 ± 0.269 2.05 ± 0.55 1.00<br />
NGC 4486 1156 187.71288 12.36469 1.04 −6.390 ± 0.125 −7.777 ± 0.246 5.95 ± 1.68 0.88<br />
NGC 4486 1157 187.71300 12.38135 0.45 −8.792 ± 0.021 −10.029 ± 0.021 1.93 ± 0.17 1.00<br />
NGC 4486 1162 187.71300 12.39276 0.27 −6.182 ± 0.063 −7.875 ± 1.459 2.43 ± 0.43 1.00<br />
NGC 4486 1164 187.71314 12.37851 0.55 −7.611 ± 0.037 −8.940 ± 0.023 2.40 ± 0.15 1.00<br />
NGC 4486 1165 187.71300 12.40206 0.49 −8.579 ± 0.032 −9.905 ± 0.012 2.71 ± 0.20 1.00<br />
NGC 4486 1168 187.71315 12.36657 0.97 −7.370 ± 0.048 −8.789 ± 0.018 2.00 ± 0.19 1.00<br />
NGC 4486 1169 187.71314 12.37276 0.75 −7.524 ± 0.026 −8.355 ± 0.043 2.33 ± 0.21 1.00<br />
NGC 4486 1170 187.71318 12.37250 0.76 −8.009 ± 0.028 −9.529 ± 0.023 2.66 ± 0.14 1.00<br />
NGC 4486 1171 187.71320 12.37323 0.73 −8.926 ± 0.018 −10.174 ± 0.019 2.23 ± 0.15 1.00<br />
NGC 4486 1172 187.71323 12.38126 0.46 −6.001 ± 0.101 −6.649 ± 0.208 2.24 ± 1.11 0.99<br />
NGC 4486 1173 187.71324 12.40735 0.67 −6.515 ± 0.051 −7.878 ± 0.398 2.93 ± 0.41 1.00<br />
NGC 4486 1175 187.71331 12.37271 0.75 −5.921 ± 0.084 −6.977 ± 0.198 2.88 ± 0.39 0.99<br />
NGC 4486 1177 187.71342 12.36398 1.07 −8.142 ± 0.022 −9.690 ± 0.016 2.22 ± 0.14 1.00<br />
NGC 4486 1178 187.71344 12.39878 0.40 −7.280 ± 0.071 −7.874 ± 0.079 3.55 ± 0.51 0.99<br />
NGC 4486 1179 187.71343 12.39202 0.28 −8.558 ± 0.024 −9.805 ± 0.020 2.13 ± 0.13 1.00<br />
NGC 4486 1182 187.71357 12.38172 0.46 −7.263 ± 0.022 −8.822 ± 0.027 2.07 ± 0.17 1.00<br />
Continued on Next Page. . .<br />
358
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4486 1183 187.71358 12.39227 0.29 −7.053 ± 0.031 −8.531 ± 0.051 2.67 ± 0.22 1.00<br />
NGC 4486 1184 187.71360 12.38003 0.51 −6.827 ± 0.025 −8.225 ± 0.029 1.98 ± 0.25 1.00<br />
NGC 4486 1185 187.71359 12.40380 0.56 −6.287 ± 0.042 −7.632 ± 0.070 2.43 ± 0.34 1.00<br />
NGC 4486 1186 187.71362 12.41321 0.89 −6.995 ± 0.044 −8.010 ± 0.052 2.81 ± 0.28 1.00<br />
NGC 4486 1187 187.71372 12.36286 1.11 −10.059 ± 0.024 −10.843 ± 0.045 3.62 ± 0.14 1.00<br />
NGC 4486 1189 187.71365 12.38886 0.30 −7.922 ± 0.033 −9.437 ± 0.036 3.07 ± 0.18 1.00<br />
NGC 4486 1190 187.71364 12.39092 0.29 −6.995 ± 0.051 −8.350 ± 0.049 2.36 ± 0.31 1.00<br />
NGC 4486 1191 187.71365 12.37485 0.68 −5.986 ± 0.463 −6.972 ± 0.249 1.97 ± 0.58 0.99<br />
NGC 4486 1192 187.71367 12.37752 0.59 −5.778 ± 0.103 −7.069 ± 0.180 3.79 ± 0.96 0.95<br />
NGC 4486 1194 187.71368 12.40461 0.59 −5.217 ± 0.086 −6.812 ± 0.406 4.45 ± 2.57 0.84<br />
NGC 4486 1195 187.71374 12.40909 0.74 −7.452 ± 0.030 −8.546 ± 0.034 3.36 ± 0.16 1.00<br />
NGC 4486 1197 187.71376 12.40872 0.73 −6.607 ± 0.059 −8.054 ± 0.041 2.50 ± 0.27 1.00<br />
NGC 4486 1198 187.71381 12.40658 0.66 −5.385 ± 0.511 −7.049 ± 0.148 2.88 ± 1.13 0.99<br />
NGC 4486 1199 187.71393 12.38089 0.49 −8.555 ± 0.019 −9.518 ± 0.021 2.45 ± 0.17 1.00<br />
NGC 4486 1200 187.71393 12.36535 1.02 −7.188 ± 0.036 −8.508 ± 0.043 2.84 ± 0.25 1.00<br />
NGC 4486 1202 187.71394 12.40713 0.68 −7.137 ± 0.032 −8.638 ± 0.038 2.36 ± 0.20 1.00<br />
NGC 4486 1203 187.71396 12.36455 1.05 −7.085 ± 0.033 −8.776 ± 0.041 2.16 ± 0.28 1.00<br />
NGC 4486 1206 187.71404 12.36797 0.93 −5.947 ± 0.067 −6.956 ± 0.137 3.94 ± 0.55 0.93<br />
NGC 4486 1208 187.71409 12.41034 0.79 −7.223 ± 0.056 −8.715 ± 0.034 2.85 ± 0.26 1.00<br />
NGC 4486 1209 187.71409 12.41688 1.02 −7.581 ± 0.022 −9.070 ± 0.021 2.02 ± 0.13 1.00<br />
NGC 4486 1210 187.71400 12.40011 0.45 −6.870 ± 0.030 −7.685 ± 0.061 2.58 ± 0.23 1.00<br />
NGC 4486 1211 187.71412 12.38263 0.44 −7.014 ± 0.120 −8.448 ± 0.344 1.37 ± 0.27 0.98<br />
NGC 4486 1212 187.71415 12.40315 0.55 −9.052 ± 0.016 −9.969 ± 0.017 3.15 ± 0.13 1.00<br />
NGC 4486 1214 187.71421 12.38174 0.47 −7.242 ± 0.040 −8.228 ± 0.062 2.69 ± 0.21 1.00<br />
NGC 4486 1215 187.71422 12.39017 0.31 −7.628 ± 0.699 −9.078 ± 0.209 1.65 ± 0.55 1.00<br />
NGC 4486 1216 187.71420 12.38368 0.42 −5.666 ± 0.110 −7.067 ± 0.527 2.06 ± 0.66 0.99<br />
NGC 4486 1217 187.71425 12.40399 0.58 −7.086 ± 0.064 −8.131 ± 0.066 3.28 ± 0.27 1.00<br />
NGC 4486 1218 187.71430 12.38041 0.51 −8.468 ± 0.016 −9.354 ± 0.025 2.37 ± 0.14 1.00<br />
NGC 4486 1219 187.71432 12.40528 0.62 −9.102 ± 0.021 −10.230 ± 0.015 1.63 ± 0.13 1.00<br />
NGC 4486 1220 187.71434 12.41353 0.91 −8.709 ± 0.020 −9.853 ± 0.021 2.31 ± 0.13 1.00<br />
NGC 4486 1221 187.71434 12.36424 1.07 −7.947 ± 0.026 −9.573 ± 0.015 2.15 ± 0.12 1.00<br />
NGC 4486 1222 187.71437 12.40947 0.76 −7.938 ± 0.030 −8.778 ± 0.031 2.63 ± 0.16 1.00<br />
NGC 4486 1224 187.71436 12.38196 0.47 −6.789 ± 0.043 −7.686 ± 0.083 2.95 ± 0.28 1.00<br />
NGC 4486 1227 187.71448 12.41479 0.95 −6.158 ± 0.057 −7.244 ± 0.168 3.93 ± 1.02 0.96<br />
NGC 4486 1229 187.71451 12.39079 0.32 −7.385 ± 0.207 −8.299 ± 0.054 6.35 ± 2.24 0.89<br />
NGC 4486 1230 187.71434 12.38267 0.45 −7.810 ± 1.205 −9.353 ± 0.040 2.63 ± 0.42 1.00<br />
NGC 4486 1231 187.71454 12.41675 1.02 −6.471 ± 0.064 −7.799 ± 0.038 2.53 ± 0.25 1.00<br />
NGC 4486 1232 187.71455 12.37157 0.81 −5.828 ± 0.349 −7.283 ± 0.615 1.93 ± 0.46 0.99<br />
NGC 4486 1234 187.71500 12.39726 0.41 −6.435 ± 0.207 −7.921 ± 0.191 4.56 ± 1.38 0.98<br />
NGC 4486 1236 187.71457 12.39054 0.32 −5.746 ± 1.168 −7.253 ± 0.060 1.66 ± 0.31 0.99<br />
NGC 4486 1237 187.71474 12.40240 0.54 −7.730 ± 0.019 −9.226 ± 0.019 2.48 ± 0.17 1.00<br />
NGC 4486 1238 187.71471 12.40481 0.61 −5.746 ± 1.145 −6.889 ± 0.080 3.07 ± 0.38 0.98<br />
NGC 4486 1239 187.71477 12.40761 0.71 −8.296 ± 0.027 −9.306 ± 0.031 2.84 ± 0.19 1.00<br />
NGC 4486 1240 187.71479 12.36535 1.03 −6.843 ± 0.036 −8.109 ± 0.054 2.87 ± 0.27 1.00<br />
NGC 4486 1241 187.71482 12.39807 0.42 −8.631 ± 0.025 −9.715 ± 0.016 2.75 ± 0.18 1.00<br />
NGC 4486 1244 187.71486 12.40532 0.63 −8.957 ± 0.024 −9.925 ± 0.015 2.75 ± 0.12 1.00<br />
NGC 4486 1245 187.71484 12.36961 0.88 −6.475 ± 0.040 −7.640 ± 0.078 2.96 ± 0.27 1.00<br />
NGC 4486 1246 187.71487 12.41763 1.06 −6.844 ± 0.060 −8.122 ± 0.098 5.51 ± 0.58 0.95<br />
NGC 4486 1247 187.71489 12.40079 0.49 −7.125 ± 0.035 −8.604 ± 0.033 2.55 ± 0.18 1.00<br />
NGC 4486 1249 187.71489 12.39464 0.36 −6.897 ± 0.041 −7.524 ± 0.058 3.13 ± 0.39 0.99<br />
NGC 4486 1250 187.71497 12.40991 0.79 −7.138 ± 0.036 −8.412 ± 0.044 2.84 ± 0.24 1.00<br />
NGC 4486 1252 187.71498 12.40020 0.48 −7.437 ± 0.026 −9.014 ± 0.023 2.17 ± 0.19 1.00<br />
NGC 4486 1253 187.71503 12.38348 0.44 −8.932 ± 0.015 −9.811 ± 0.016 2.09 ± 0.11 1.00<br />
NGC 4486 1254 187.71504 12.39130 0.34 −9.074 ± 0.018 −10.153 ± 0.018 3.07 ± 0.11 1.00<br />
NGC 4486 1255 187.71505 12.40239 0.54 −8.874 ± 0.020 −9.878 ± 0.019 3.12 ± 0.12 1.00<br />
NGC 4486 1256 187.71503 12.39327 0.35 −7.077 ± 0.047 −8.459 ± 0.038 1.82 ± 0.23 1.00<br />
NGC 4486 1257 187.71506 12.39695 0.40 −7.888 ± 0.042 −8.657 ± 0.045 2.92 ± 0.22 1.00<br />
NGC 4486 1258 187.71512 12.40658 0.68 −9.358 ± 0.018 −10.159 ± 0.016 2.57 ± 0.10 1.00<br />
NGC 4486 1260 187.71515 12.41458 0.95 −8.475 ± 0.041 −10.154 ± 0.049 5.24 ± 0.32 1.00<br />
NGC 4486 1261 187.71512 12.41482 0.96 −6.931 ± 0.036 −8.503 ± 0.026 1.59 ± 0.22 1.00<br />
NGC 4486 1262 187.71520 12.39627 0.40 −9.177 ± 0.015 −10.605 ± 0.013 2.50 ± 0.11 1.00<br />
NGC 4486 1263 187.71524 12.37333 0.76 −7.337 ± 0.033 −8.869 ± 0.023 1.86 ± 0.24 1.00<br />
Continued on Next Page. . .<br />
359
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4486 1264 187.71523 12.36441 1.07 −7.318 ± 0.033 −8.308 ± 0.055 3.25 ± 0.26 1.00<br />
NGC 4486 1265 187.71519 12.41326 0.91 −5.141 ± 0.132 −6.783 ± 0.137 4.97 ± 0.58 0.73<br />
NGC 4486 1266 187.71522 12.37015 0.87 −6.486 ± 0.043 −7.493 ± 0.085 2.80 ± 0.44 0.99<br />
NGC 4486 1267 187.71526 12.37031 0.86 −6.853 ± 0.049 −8.399 ± 0.035 2.18 ± 0.35 1.00<br />
NGC 4486 1268 187.71527 12.39727 0.42 −6.616 ± 0.068 −8.271 ± 0.141 2.62 ± 0.59 1.00<br />
NGC 4486 1269 187.71532 12.40035 0.49 −8.789 ± 0.020 −9.820 ± 0.014 2.57 ± 0.14 1.00<br />
NGC 4486 1270 187.71531 12.37586 0.68 −6.209 ± 0.058 −7.535 ± 0.114 2.43 ± 0.40 1.00<br />
NGC 4486 1273 187.71548 12.38337 0.46 −8.376 ± 0.012 −9.734 ± 0.016 1.61 ± 0.17 1.00<br />
NGC 4486 1274 187.71550 12.36903 0.91 −6.741 ± 0.048 −8.261 ± 0.031 1.53 ± 0.23 0.99<br />
NGC 4486 1276 187.71552 12.38680 0.39 −7.438 ± 0.031 −8.790 ± 0.038 1.96 ± 0.19 1.00<br />
NGC 4486 1277 187.71561 12.40023 0.50 −8.944 ± 0.018 −10.394 ± 0.019 2.62 ± 0.15 1.00<br />
NGC 4486 1278 187.71559 12.40131 0.53 −8.188 ± 0.021 −9.330 ± 0.022 3.00 ± 0.14 1.00<br />
NGC 4486 1279 187.71569 12.37617 0.67 −8.449 ± 0.070 −9.398 ± 0.073 7.49 ± 0.47 0.98<br />
NGC 4486 1281 187.71576 12.39380 0.38 −7.278 ± 0.046 −8.359 ± 0.073 3.52 ± 0.34 1.00<br />
NGC 4486 1282 187.71577 12.41269 0.90 −7.726 ± 0.024 −9.064 ± 0.030 3.12 ± 0.21 1.00<br />
NGC 4486 1283 187.71557 12.39252 0.36 −6.784 ± 0.123 −8.373 ± 0.082 2.79 ± 0.43 1.00<br />
NGC 4486 1284 187.71587 12.37923 0.58 −6.501 ± 0.066 −7.660 ± 0.112 3.60 ± 0.39 0.99<br />
NGC 4486 1285 187.71590 12.40010 0.50 −8.043 ± 0.058 −9.516 ± 0.057 5.89 ± 0.38 1.00<br />
NGC 4486 1287 187.71602 12.40714 0.71 −8.943 ± 0.019 −10.538 ± 0.011 2.34 ± 0.11 1.00<br />
NGC 4486 1288 187.71593 12.41237 0.89 −5.113 ± 0.245 −6.415 ± 0.144 1.94 ± 0.55 0.98<br />
NGC 4486 1289 187.71615 12.40865 0.77 −11.108 ± 0.023 −12.160 ± 0.015 5.46 ± 0.12 1.00<br />
NGC 4486 1290 187.71602 12.39399 0.39 −7.255 ± 0.059 −8.383 ± 0.136 5.78 ± 0.91 0.94<br />
NGC 4486 1291 187.71601 12.40843 0.76 −7.236 ± 0.045 −8.413 ± 0.040 3.21 ± 0.21 1.00<br />
NGC 4486 1292 187.71600 12.40546 0.66 −5.764 ± 0.091 −7.336 ± 0.109 2.47 ± 0.47 1.00<br />
NGC 4486 1295 187.71614 12.38107 0.54 −9.503 ± 0.015 −11.028 ± 0.017 2.56 ± 0.09 1.00<br />
NGC 4486 1296 187.71608 12.38612 0.42 −6.667 ± 0.216 −8.248 ± 0.058 1.81 ± 0.30 1.00<br />
NGC 4486 1297 187.71616 12.37982 0.57 −9.312 ± 0.021 −10.468 ± 0.015 2.43 ± 0.21 1.00<br />
NGC 4486 1298 187.71611 12.39264 0.38 −6.952 ± 0.079 −8.286 ± 0.101 3.88 ± 0.43 1.00<br />
NGC 4486 1300 187.71617 12.36663 1.00 −7.962 ± 0.031 −9.408 ± 0.020 1.69 ± 0.12 1.00<br />
NGC 4486 1301 187.71616 12.38251 0.50 −7.458 ± 0.042 −8.317 ± 0.052 3.31 ± 0.29 1.00<br />
NGC 4486 1302 187.71617 12.38041 0.56 −7.955 ± 0.024 −9.350 ± 0.026 1.86 ± 0.13 1.00<br />
NGC 4486 1303 187.71616 12.41861 1.11 −6.698 ± 0.063 −7.738 ± 0.099 3.94 ± 0.51 0.99<br />
NGC 4486 1304 187.71608 12.36848 0.94 −5.967 ± 0.075 −7.085 ± 0.151 3.68 ± 0.64 0.96<br />
NGC 4486 1305 187.71628 12.39031 0.38 −7.278 ± 0.046 −8.196 ± 0.054 2.40 ± 0.31 1.00<br />
NGC 4486 1306 187.71625 12.39193 0.38 −5.682 ± 0.183 −6.541 ± 0.722 1.34 ± 0.46 0.94<br />
NGC 4486 1307 187.71634 12.36346 1.12 −8.221 ± 0.030 −9.669 ± 0.022 1.96 ± 0.20 1.00<br />
NGC 4486 1308 187.71633 12.40969 0.80 −5.362 ± 0.107 −6.003 ± 0.149 2.79 ± 0.49 0.98<br />
NGC 4486 1309 187.71639 12.38708 0.42 −7.303 ± 0.138 −8.554 ± 0.089 1.42 ± 0.25 0.98<br />
NGC 4486 1310 187.71639 12.38875 0.40 −6.926 ± 0.048 −8.267 ± 0.145 4.55 ± 0.78 0.99<br />
NGC 4486 1311 187.71640 12.41506 0.99 −6.427 ± 0.055 −7.240 ± 0.075 4.89 ± 0.29 0.87<br />
NGC 4486 1312 187.71642 12.36732 0.98 −7.659 ± 0.028 −8.631 ± 0.025 2.39 ± 0.16 1.00<br />
NGC 4486 1313 187.71644 12.39951 0.50 −8.315 ± 0.027 −9.783 ± 0.017 2.70 ± 0.17 1.00<br />
NGC 4486 1314 187.71644 12.39999 0.51 −7.088 ± 0.038 −8.540 ± 0.052 3.09 ± 0.24 1.00<br />
NGC 4486 1315 187.71646 12.39979 0.51 −5.783 ± 1.139 −7.228 ± 0.072 2.39 ± 0.59 1.00<br />
NGC 4486 1316 187.71648 12.39279 0.40 −6.253 ± 0.076 −7.778 ± 0.067 2.62 ± 0.34 1.00<br />
NGC 4486 1317 187.71653 12.41362 0.94 −6.445 ± 0.050 −7.717 ± 0.042 1.71 ± 0.27 0.99<br />
NGC 4486 1318 187.71663 12.40203 0.57 −6.220 ± 0.073 −7.279 ± 0.100 2.49 ± 0.42 1.00<br />
NGC 4486 1319 187.71669 12.41409 0.96 −9.835 ± 0.019 −10.982 ± 0.040 6.03 ± 0.17 1.00<br />
NGC 4486 1320 187.71673 12.38954 0.40 −7.253 ± 0.031 −8.779 ± 0.037 2.14 ± 0.19 1.00<br />
NGC 4486 1321 187.71675 12.40843 0.77 −7.840 ± 0.028 −8.852 ± 0.027 2.62 ± 0.16 1.00<br />
NGC 4486 1322 187.71673 12.41615 1.03 −6.428 ± 0.119 −7.499 ± 0.115 4.60 ± 0.57 0.94<br />
NGC 4486 1323 187.71674 12.38210 0.53 −6.051 ± 0.055 −7.444 ± 0.046 2.23 ± 0.29 1.00<br />
NGC 4486 1324 187.71683 12.41136 0.87 −6.748 ± 0.060 −7.689 ± 0.133 5.91 ± 0.81 0.86<br />
NGC 4486 1325 187.71683 12.39333 0.41 −6.407 ± 0.309 −7.661 ± 0.091 5.53 ± 1.97 0.90<br />
NGC 4486 1326 187.71691 12.40276 0.60 −8.285 ± 0.022 −9.695 ± 0.022 2.51 ± 0.18 1.00<br />
NGC 4486 1327 187.71681 12.38400 0.49 −5.247 ± 1.531 −6.628 ± 0.937 0.82 ± 1.20 0.80<br />
NGC 4486 1328 187.71686 12.38429 0.48 −7.524 ± 0.026 −8.609 ± 0.048 2.64 ± 0.19 1.00<br />
NGC 4486 1329 187.71686 12.39096 0.41 −7.843 ± 0.094 −8.919 ± 0.106 4.68 ± 0.52 1.00<br />
NGC 4486 1330 187.71693 12.36446 1.09 −6.876 ± 0.096 −7.881 ± 0.203 3.15 ± 0.43 1.00<br />
NGC 4486 1331 187.71698 12.36972 0.91 −8.603 ± 0.030 −9.562 ± 0.024 3.89 ± 0.14 1.00<br />
NGC 4486 1332 187.71700 12.36326 1.13 −8.164 ± 0.030 −9.423 ± 0.023 3.00 ± 0.21 1.00<br />
NGC 4486 1333 187.71698 12.37563 0.72 −5.185 ± 0.833 −6.702 ± 0.477 1.07 ± 0.75 0.88<br />
Continued on Next Page. . .<br />
360
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4486 1334 187.71705 12.36453 1.09 −5.759 ± 0.118 −7.058 ± 0.160 3.44 ± 0.87 0.97<br />
NGC 4486 1335 187.71712 12.40321 0.62 −10.469 ± 0.020 −11.978 ± 0.010 2.83 ± 0.11 1.00<br />
NGC 4486 1336 187.71712 12.39915 0.51 −9.033 ± 0.015 −10.353 ± 0.016 2.46 ± 0.10 1.00<br />
NGC 4486 1337 187.71715 12.41599 1.03 −8.258 ± 0.033 −9.644 ± 0.018 2.10 ± 0.13 1.00<br />
NGC 4486 1339 187.71717 12.40116 0.56 −8.679 ± 0.022 −9.640 ± 0.017 2.07 ± 0.17 1.00<br />
NGC 4486 1340 187.71725 12.39691 0.47 −8.113 ± 0.029 −9.334 ± 0.019 2.66 ± 0.12 1.00<br />
NGC 4486 1341 187.71738 12.38633 0.46 −8.055 ± 0.029 −9.260 ± 0.034 1.59 ± 0.19 1.00<br />
NGC 4486 1342 187.71739 12.41260 0.92 −5.342 ± 0.076 −6.928 ± 0.264 1.86 ± 0.51 0.99<br />
NGC 4486 1343 187.71743 12.39509 0.45 −7.064 ± 0.046 −8.544 ± 0.117 4.39 ± 0.69 1.00<br />
NGC 4486 1344 187.71746 12.36969 0.92 −6.439 ± 0.063 −7.820 ± 0.049 2.31 ± 0.35 1.00<br />
NGC 4486 1345 187.71752 12.38536 0.48 −5.932 ± 0.127 −7.405 ± 0.124 4.68 ± 0.61 0.92<br />
NGC 4486 1346 187.71758 12.37908 0.63 −7.026 ± 0.047 −8.208 ± 0.051 2.44 ± 0.29 1.00<br />
NGC 4486 1347 187.71760 12.38237 0.55 −6.743 ± 0.130 −8.221 ± 0.312 1.68 ± 0.37 1.00<br />
NGC 4486 1348 187.71767 12.37758 0.67 −5.676 ± 0.079 −7.111 ± 0.163 2.20 ± 0.31 1.00<br />
NGC 4486 1350 187.71775 12.38029 0.60 −7.181 ± 0.036 −8.598 ± 0.039 1.86 ± 0.21 1.00<br />
NGC 4486 1351 187.71776 12.40084 0.57 −7.470 ± 0.043 −8.847 ± 0.027 2.03 ± 0.19 1.00<br />
NGC 4486 1352 187.71781 12.41446 0.99 −8.878 ± 0.022 −10.299 ± 0.016 2.09 ± 0.11 1.00<br />
NGC 4486 1353 187.71788 12.37986 0.62 −7.404 ± 0.029 −8.747 ± 0.033 2.77 ± 0.19 1.00<br />
NGC 4486 1354 187.71790 12.40814 0.78 −7.365 ± 0.026 −8.787 ± 0.035 2.35 ± 0.13 1.00<br />
NGC 4486 1355 187.71796 12.37805 0.67 −8.792 ± 0.019 −9.850 ± 0.014 2.50 ± 0.12 1.00<br />
NGC 4486 1356 187.71801 12.37753 0.68 −7.663 ± 0.034 −9.181 ± 0.025 3.57 ± 0.15 1.00<br />
NGC 4486 1357 187.71797 12.39471 0.47 −6.596 ± 0.042 −7.683 ± 0.050 2.16 ± 0.28 1.00<br />
NGC 4486 1358 187.71805 12.41744 1.09 −8.113 ± 0.023 −9.475 ± 0.017 3.12 ± 0.13 1.00<br />
NGC 4486 1359 187.71806 12.40351 0.65 −8.023 ± 0.016 −8.835 ± 0.028 2.71 ± 0.15 1.00<br />
NGC 4486 1360 187.71819 12.37450 0.78 −6.116 ± 0.072 −7.117 ± 0.251 2.71 ± 0.41 0.99<br />
NGC 4486 1361 187.71822 12.40938 0.83 −6.580 ± 0.039 −7.752 ± 0.055 2.82 ± 0.30 1.00<br />
NGC 4486 1363 187.71826 12.38516 0.51 −7.230 ± 0.043 −8.197 ± 0.039 2.61 ± 0.25 1.00<br />
NGC 4486 1364 187.71825 12.40537 0.71 −4.856 ± 0.163 −6.678 ± 0.347 2.83 ± 0.59 0.98<br />
NGC 4486 1365 187.71830 12.36811 0.99 −5.170 ± 0.266 −6.404 ± 0.218 4.45 ± 1.82 0.79<br />
NGC 4486 1366 187.71831 12.37831 0.67 −6.377 ± 0.335 −8.047 ± 0.032 1.52 ± 0.35 0.99<br />
NGC 4486 1367 187.71832 12.38536 0.51 −6.586 ± 0.067 −7.648 ± 0.397 2.02 ± 0.31 1.00<br />
NGC 4486 1368 187.71843 12.39392 0.48 −6.665 ± 0.069 −8.200 ± 0.042 1.75 ± 0.34 1.00<br />
NGC 4486 1369 187.71860 12.37167 0.87 −8.738 ± 0.046 −9.781 ± 0.047 3.53 ± 0.43 1.00<br />
NGC 4486 1370 187.71857 12.40253 0.64 −6.169 ± 0.076 −7.488 ± 0.081 2.63 ± 0.38 1.00<br />
NGC 4486 1371 187.71858 12.39414 0.48 −5.076 ± 0.514 −6.869 ± 0.715 2.61 ± 0.88 0.99<br />
NGC 4486 1372 187.71866 12.40617 0.74 −7.870 ± 0.031 −9.192 ± 0.028 2.83 ± 0.16 1.00<br />
NGC 4486 1373 187.71865 12.37886 0.66 −7.986 ± 0.022 −9.095 ± 0.032 2.78 ± 0.21 1.00<br />
NGC 4486 1375 187.71866 12.39309 0.48 −7.259 ± 0.052 −8.369 ± 0.052 3.16 ± 0.22 1.00<br />
NGC 4486 1376 187.71877 12.37207 0.87 −9.461 ± 0.026 −10.388 ± 0.020 3.82 ± 0.12 1.00<br />
NGC 4486 1377 187.71872 12.38509 0.53 −7.254 ± 0.033 −8.296 ± 0.030 2.25 ± 0.22 1.00<br />
NGC 4486 1378 187.71876 12.38888 0.48 −7.046 ± 0.078 −8.330 ± 0.056 2.99 ± 0.47 1.00<br />
NGC 4486 1379 187.71883 12.39466 0.50 −5.538 ± 0.255 −6.273 ± 0.392 3.27 ± 1.67 0.96<br />
NGC 4486 1380 187.71890 12.38412 0.55 −8.385 ± 0.017 −9.973 ± 0.022 3.08 ± 0.14 1.00<br />
NGC 4486 1381 187.71886 12.41024 0.87 −6.934 ± 0.026 −8.315 ± 0.029 2.26 ± 0.21 1.00<br />
NGC 4486 1382 187.71906 12.39873 0.57 −10.156 ± 0.077 −11.039 ± 0.100 6.96 ± 0.64 1.00<br />
NGC 4486 1383 187.71901 12.38494 0.54 −7.785 ± 0.022 −9.249 ± 0.017 1.84 ± 0.12 1.00<br />
NGC 4486 1384 187.71901 12.40015 0.59 −6.590 ± 0.051 −8.011 ± 0.041 1.89 ± 0.33 1.00<br />
NGC 4486 1385 187.71910 12.40286 0.66 −7.308 ± 0.038 −8.196 ± 0.065 4.34 ± 0.24 0.99<br />
NGC 4486 1386 187.71913 12.36801 1.00 −6.758 ± 0.043 −8.313 ± 0.039 2.16 ± 0.22 1.00<br />
NGC 4486 1388 187.71912 12.41508 1.03 −5.373 ± 0.088 −6.932 ± 0.131 2.46 ± 0.51 0.99<br />
NGC 4486 1389 187.71921 12.39515 0.52 −6.968 ± 0.031 −8.642 ± 0.028 2.07 ± 0.17 1.00<br />
NGC 4486 1390 187.71929 12.39217 0.50 −6.990 ± 0.040 −8.198 ± 0.048 2.63 ± 0.24 1.00<br />
NGC 4486 1392 187.71937 12.40066 0.62 −6.983 ± 0.055 −8.455 ± 0.049 2.92 ± 0.24 1.00<br />
NGC 4486 1394 187.71945 12.40347 0.69 −5.721 ± 0.341 −6.862 ± 0.137 4.36 ± 2.37 0.86<br />
NGC 4486 1395 187.71949 12.40136 0.64 −6.159 ± 0.089 −7.021 ± 0.188 3.11 ± 1.26 0.98<br />
NGC 4486 1397 187.71897 12.39322 0.49 −6.570 ± 0.098 −7.487 ± 0.248 4.57 ± 1.59 0.94<br />
NGC 4486 1398 187.71962 12.38113 0.63 −8.341 ± 0.028 −10.000 ± 0.025 2.85 ± 0.22 1.00<br />
NGC 4486 1399 187.71956 12.38672 0.53 −5.148 ± 0.536 −6.566 ± 0.188 3.38 ± 0.85 0.96<br />
NGC 4486 1401 187.71961 12.40137 0.64 −5.677 ± 0.069 −6.732 ± 0.097 2.59 ± 0.39 0.99<br />
NGC 4486 1402 187.71963 12.40255 0.67 −4.997 ± 0.531 −6.214 ± 0.125 1.79 ± 0.97 0.98<br />
NGC 4486 1403 187.71965 12.39658 0.55 −7.828 ± 0.031 −9.188 ± 0.024 2.33 ± 0.16 1.00<br />
NGC 4486 1404 187.71968 12.41854 1.16 −6.327 ± 0.066 −7.230 ± 0.066 2.57 ± 0.30 0.99<br />
Continued on Next Page. . .<br />
361
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4486 1405 187.71982 12.40643 0.78 −10.946 ± 0.022 −12.157 ± 0.023 6.27 ± 0.14 1.00<br />
NGC 4486 1407 187.71971 12.41668 1.10 −6.838 ± 0.040 −8.118 ± 0.035 1.73 ± 0.19 1.00<br />
NGC 4486 1408 187.71979 12.38811 0.53 −5.318 ± 0.539 −6.943 ± 0.182 0.81 ± 0.50 0.76<br />
NGC 4486 1409 187.71981 12.38906 0.52 −5.772 ± 0.064 −7.003 ± 0.386 2.86 ± 0.49 0.99<br />
NGC 4486 1412 187.71973 12.41747 1.12 −8.512 ± 0.036 −9.460 ± 0.026 1.88 ± 0.31 1.00<br />
NGC 4486 1414 187.71997 12.41011 0.89 −7.538 ± 0.030 −9.047 ± 0.022 1.70 ± 0.16 1.00<br />
NGC 4486 1415 187.71999 12.40187 0.66 −5.610 ± 0.143 −7.105 ± 0.167 2.59 ± 0.83 0.99<br />
NGC 4486 1416 187.72002 12.36701 1.05 −5.889 ± 0.081 −7.740 ± 0.155 4.02 ± 0.92 0.98<br />
NGC 4486 1417 187.72009 12.39010 0.53 −7.332 ± 0.044 −8.810 ± 0.022 1.98 ± 0.18 1.00<br />
NGC 4486 1418 187.72017 12.41257 0.97 −9.714 ± 0.027 −10.622 ± 0.027 3.20 ± 0.15 1.00<br />
NGC 4486 1419 187.72013 12.36423 1.15 −7.791 ± 0.024 −9.048 ± 0.022 2.19 ± 0.12 1.00<br />
NGC 4486 1420 187.72012 12.40781 0.82 −5.728 ± 0.157 −6.502 ± 0.665 2.33 ± 0.67 0.99<br />
NGC 4486 1421 187.72012 12.37485 0.81 −6.230 ± 0.053 −7.362 ± 0.088 2.43 ± 0.37 1.00<br />
NGC 4486 1422 187.72012 12.39881 0.60 −5.614 ± 0.115 −6.495 ± 0.368 2.44 ± 0.59 0.99<br />
NGC 4486 1423 187.72017 12.37059 0.94 −7.488 ± 0.025 −8.638 ± 0.033 2.29 ± 0.21 1.00<br />
NGC 4486 1424 187.72013 12.38255 0.62 −5.667 ± 0.086 −7.390 ± 0.124 2.44 ± 0.51 1.00<br />
NGC 4486 1426 187.72020 12.38987 0.53 −6.532 ± 0.069 −7.553 ± 0.088 2.66 ± 0.50 1.00<br />
NGC 4486 1427 187.72018 12.39516 0.55 −6.754 ± 0.089 −7.289 ± 0.035 2.07 ± 0.25 1.00<br />
NGC 4486 1428 187.72038 12.37422 0.84 −10.161 ± 0.029 −11.133 ± 0.021 4.91 ± 0.14 0.98<br />
NGC 4486 1429 187.72023 12.37484 0.81 −6.763 ± 0.033 −7.549 ± 0.057 3.48 ± 0.22 0.99<br />
NGC 4486 1430 187.72034 12.40067 0.65 −7.364 ± 0.029 −8.371 ± 0.041 2.60 ± 0.16 1.00<br />
NGC 4486 1431 187.72035 12.40533 0.76 −7.304 ± 0.031 −8.640 ± 0.032 2.54 ± 0.17 1.00<br />
NGC 4486 1432 187.72042 12.37666 0.77 −7.549 ± 0.041 −8.655 ± 0.052 3.35 ± 0.34 1.00<br />
NGC 4486 1433 187.72052 12.36561 1.11 −6.878 ± 0.049 −8.260 ± 0.041 2.65 ± 0.23 1.00<br />
NGC 4486 1434 187.72052 12.38598 0.57 −7.328 ± 0.040 −8.327 ± 0.108 4.45 ± 0.51 0.99<br />
NGC 4486 1435 187.72052 12.39401 0.55 −7.063 ± 0.027 −8.279 ± 0.031 1.88 ± 0.18 1.00<br />
NGC 4486 1436 187.72053 12.38228 0.64 −6.693 ± 0.088 −8.178 ± 0.025 1.28 ± 0.24 0.97<br />
NGC 4486 1437 187.72056 12.39697 0.59 −5.672 ± 0.078 −6.679 ± 0.121 2.80 ± 0.40 0.98<br />
NGC 4486 1438 187.72060 12.40102 0.66 −6.526 ± 0.090 −7.912 ± 0.036 1.84 ± 0.38 1.00<br />
NGC 4486 1440 187.72069 12.40433 0.74 −9.123 ± 0.013 −10.033 ± 0.013 2.80 ± 0.12 1.00<br />
NGC 4486 1441 187.72077 12.40660 0.80 −7.577 ± 0.022 −9.236 ± 0.017 2.07 ± 0.11 1.00<br />
NGC 4486 1443 187.72077 12.39093 0.55 −6.713 ± 0.189 −7.956 ± 0.113 6.58 ± 1.20 0.78<br />
NGC 4486 1444 187.72078 12.39288 0.55 −7.775 ± 0.028 −9.293 ± 0.026 2.46 ± 0.15 1.00<br />
NGC 4486 1447 187.72087 12.40546 0.78 −7.479 ± 0.021 −8.998 ± 0.020 2.23 ± 0.11 1.00<br />
NGC 4486 1448 187.72095 12.41495 1.06 −7.134 ± 0.036 −8.182 ± 0.035 2.05 ± 0.22 1.00<br />
NGC 4486 1449 187.72097 12.38221 0.65 −5.399 ± 0.266 −7.215 ± 0.461 5.31 ± 11.59 0.80<br />
NGC 4486 1450 187.72103 12.38608 0.59 −8.033 ± 0.021 −9.506 ± 0.025 2.44 ± 0.18 1.00<br />
NGC 4486 1451 187.72107 12.41453 1.05 −8.592 ± 0.023 −9.406 ± 0.029 2.95 ± 0.16 1.00<br />
NGC 4486 1452 187.72075 12.39683 0.59 −9.229 ± 0.020 −10.536 ± 0.012 2.59 ± 0.12 1.00<br />
NGC 4486 1453 187.72109 12.41652 1.12 −6.757 ± 0.062 −7.887 ± 0.083 3.54 ± 0.48 0.99<br />
NGC 4486 1454 187.72115 12.40714 0.83 −6.251 ± 0.099 −7.538 ± 0.087 3.32 ± 0.37 0.99<br />
NGC 4486 1455 187.72115 12.39355 0.57 −7.217 ± 0.026 −8.631 ± 0.288 1.25 ± 0.21 0.96<br />
NGC 4486 1456 187.72126 12.39379 0.58 −9.143 ± 0.017 −10.405 ± 0.010 2.79 ± 0.07 1.00<br />
NGC 4486 1457 187.72138 12.39380 0.58 −8.056 ± 0.024 −9.270 ± 0.019 2.09 ± 0.16 1.00<br />
NGC 4486 1458 187.72119 12.38949 0.57 −6.778 ± 0.034 −8.251 ± 0.044 2.67 ± 0.22 1.00<br />
NGC 4486 1459 187.72122 12.37964 0.71 −6.485 ± 0.059 −7.617 ± 0.071 3.46 ± 0.33 0.99<br />
NGC 4486 1460 187.72125 12.37277 0.90 −7.030 ± 0.031 −8.561 ± 0.033 2.03 ± 0.19 1.00<br />
NGC 4486 1461 187.72127 12.39903 0.64 −6.944 ± 0.079 −8.145 ± 0.047 3.11 ± 0.41 1.00<br />
NGC 4486 1462 187.72127 12.41592 1.10 −7.548 ± 0.024 −9.058 ± 0.049 3.39 ± 0.29 1.00<br />
NGC 4486 1463 187.72132 12.40734 0.84 −8.767 ± 0.023 −9.833 ± 0.022 2.25 ± 0.19 1.00<br />
NGC 4486 1464 187.72135 12.40144 0.69 −6.507 ± 0.092 −7.142 ± 0.370 5.95 ± 3.66 0.65<br />
NGC 4486 1466 187.72157 12.40288 0.73 −6.057 ± 0.082 −7.537 ± 0.105 2.30 ± 0.60 1.00<br />
NGC 4486 1467 187.72159 12.40837 0.87 −7.581 ± 0.023 −8.804 ± 0.027 2.55 ± 0.12 1.00<br />
NGC 4486 1469 187.72166 12.37145 0.95 −6.571 ± 0.035 −8.027 ± 0.026 1.72 ± 0.28 0.99<br />
NGC 4486 1470 187.72168 12.39370 0.59 −7.021 ± 0.049 −8.365 ± 0.050 2.12 ± 0.24 1.00<br />
NGC 4486 1472 187.72170 12.41549 1.09 −6.910 ± 0.030 −8.283 ± 0.029 1.84 ± 0.22 1.00<br />
NGC 4486 1473 187.72170 12.39155 0.58 −6.767 ± 0.047 −8.113 ± 0.029 2.30 ± 0.29 1.00<br />
NGC 4486 1474 187.72174 12.40668 0.83 −7.586 ± 0.033 −8.671 ± 0.029 2.65 ± 0.22 1.00<br />
NGC 4486 1475 187.72175 12.37846 0.76 −7.800 ± 0.026 −8.923 ± 0.030 2.73 ± 0.16 1.00<br />
NGC 4486 1476 187.72179 12.39513 0.61 −8.099 ± 0.026 −9.021 ± 0.030 2.55 ± 0.22 1.00<br />
NGC 4486 1477 187.72177 12.40852 0.88 −6.746 ± 0.050 −7.587 ± 0.063 3.92 ± 0.34 0.98<br />
NGC 4486 1478 187.72183 12.36983 1.00 −6.516 ± 0.105 −7.299 ± 0.056 3.85 ± 0.42 0.97<br />
Continued on Next Page. . .<br />
362
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4486 1479 187.72189 12.38182 0.69 −6.549 ± 0.059 −7.936 ± 0.058 2.97 ± 0.33 1.00<br />
NGC 4486 1481 187.72186 12.40247 0.73 −6.595 ± 0.039 −8.191 ± 0.040 1.95 ± 0.27 1.00<br />
NGC 4486 1482 187.72194 12.39505 0.61 −6.356 ± 0.091 −7.917 ± 0.086 3.72 ± 0.45 0.99<br />
NGC 4486 1483 187.72202 12.40157 0.72 −9.036 ± 0.014 −10.170 ± 0.017 2.58 ± 0.07 1.00<br />
NGC 4486 1484 187.72196 12.40850 0.89 −6.336 ± 0.076 −7.909 ± 0.050 1.95 ± 0.33 1.00<br />
NGC 4486 1485 187.72217 12.39161 0.60 −7.004 ± 0.039 −8.334 ± 0.016 2.21 ± 0.27 1.00<br />
NGC 4486 1486 187.72220 12.37812 0.78 −7.000 ± 0.044 −8.309 ± 0.031 2.26 ± 0.27 1.00<br />
NGC 4486 1487 187.72193 12.40881 0.90 −6.982 ± 0.046 −8.732 ± 0.023 1.96 ± 0.21 1.00<br />
NGC 4486 1488 187.72218 12.38101 0.71 −5.686 ± 0.079 −7.000 ± 0.359 5.98 ± 3.84 0.59<br />
NGC 4486 1489 187.72217 12.38251 0.68 −5.992 ± 0.059 −7.093 ± 0.067 2.53 ± 0.35 0.99<br />
NGC 4486 1490 187.72223 12.38265 0.68 −7.991 ± 0.049 −8.828 ± 0.258 2.05 ± 0.33 1.00<br />
NGC 4486 1491 187.72221 12.41105 0.97 −5.202 ± 0.575 −7.012 ± 0.070 1.86 ± 0.66 0.99<br />
NGC 4486 1493 187.72223 12.37839 0.77 −4.810 ± 0.488 −6.055 ± 0.182 2.09 ± 0.68 0.99<br />
NGC 4486 1494 187.72231 12.40008 0.70 −7.141 ± 0.041 −8.754 ± 0.038 3.56 ± 0.17 1.00<br />
NGC 4486 1495 187.72231 12.38757 0.62 −7.055 ± 0.088 −8.379 ± 0.100 4.40 ± 0.60 1.00<br />
NGC 4486 1496 187.72235 12.40565 0.82 −9.190 ± 0.018 −10.505 ± 0.015 2.40 ± 0.10 1.00<br />
NGC 4486 1497 187.72235 12.38046 0.73 −5.970 ± 1.388 −7.514 ± 0.109 1.78 ± 0.34 0.99<br />
NGC 4486 1498 187.72238 12.36886 1.04 −5.283 ± 0.085 −6.833 ± 0.098 1.86 ± 0.55 0.99<br />
NGC 4486 1499 187.72252 12.40261 0.75 −8.769 ± 0.018 −9.826 ± 0.017 2.44 ± 0.09 1.00<br />
NGC 4486 1500 187.72255 12.36575 1.14 −5.936 ± 0.097 −7.494 ± 0.125 6.15 ± 0.90 0.75<br />
NGC 4486 1501 187.72254 12.39228 0.62 −7.075 ± 0.089 −7.685 ± 0.126 4.43 ± 0.49 0.96<br />
NGC 4486 1502 187.72254 12.40119 0.72 −5.835 ± 0.556 −7.213 ± 0.051 1.08 ± 0.42 0.91<br />
NGC 4486 1504 187.72272 12.40652 0.85 −5.188 ± 0.188 −6.237 ± 0.193 4.95 ± 0.94 0.71<br />
NGC 4486 1507 187.72282 12.37580 0.85 −8.665 ± 0.021 −10.035 ± 0.022 3.16 ± 0.14 1.00<br />
NGC 4486 1508 187.72285 12.39377 0.64 −7.156 ± 0.029 −8.446 ± 0.052 2.77 ± 0.31 1.00<br />
NGC 4486 1509 187.72287 12.38866 0.63 −6.409 ± 0.046 −7.801 ± 0.068 2.25 ± 0.35 1.00<br />
NGC 4486 1510 187.72292 12.39730 0.67 −7.423 ± 0.063 −8.727 ± 0.099 8.11 ± 0.81 0.85<br />
NGC 4486 1512 187.72305 12.38114 0.74 −8.133 ± 0.022 −9.003 ± 0.021 2.51 ± 0.12 1.00<br />
NGC 4486 1513 187.72303 12.37080 1.00 −6.330 ± 0.055 −7.856 ± 0.081 2.74 ± 0.37 1.00<br />
NGC 4486 1514 187.72312 12.36381 1.22 −8.709 ± 0.021 −10.189 ± 0.030 2.23 ± 0.13 1.00<br />
NGC 4486 1516 187.72310 12.39204 0.64 −7.538 ± 0.028 −8.480 ± 0.045 2.94 ± 0.21 1.00<br />
NGC 4486 1517 187.72316 12.39841 0.70 −7.953 ± 0.028 −9.330 ± 0.036 2.65 ± 0.26 1.00<br />
NGC 4486 1518 187.72315 12.40283 0.78 −8.953 ± 0.019 −10.053 ± 0.018 3.22 ± 0.19 1.00<br />
NGC 4486 1521 187.72318 12.38054 0.75 −7.626 ± 0.042 −8.535 ± 0.050 4.22 ± 0.32 1.00<br />
NGC 4486 1522 187.72319 12.36832 1.08 −7.417 ± 0.031 −8.649 ± 0.028 2.57 ± 0.16 1.00<br />
NGC 4486 1523 187.72330 12.38929 0.65 −8.714 ± 0.024 −10.241 ± 0.020 2.49 ± 0.16 1.00<br />
NGC 4486 1524 187.72329 12.39982 0.72 −8.207 ± 0.037 −9.040 ± 0.032 4.61 ± 0.14 1.00<br />
NGC 4486 1525 187.72310 12.41775 1.19 −4.803 ± 0.173 −6.508 ± 0.203 3.66 ± 1.09 0.93<br />
NGC 4486 1526 187.72330 12.41628 1.15 −8.706 ± 0.025 −9.720 ± 0.017 2.29 ± 0.12 1.00<br />
NGC 4486 1527 187.72339 12.39014 0.65 −6.777 ± 0.058 −7.706 ± 0.074 3.43 ± 0.33 0.99<br />
NGC 4486 1528 187.72346 12.40376 0.81 −9.051 ± 0.018 −10.153 ± 0.022 2.33 ± 0.14 1.00<br />
NGC 4486 1530 187.72341 12.39221 0.65 −5.136 ± 0.200 −6.176 ± 1.130 1.39 ± 1.05 0.95<br />
NGC 4486 1531 187.72350 12.40796 0.91 −7.579 ± 0.029 −9.211 ± 0.013 1.73 ± 0.16 1.00<br />
NGC 4486 1532 187.72351 12.40302 0.79 −7.921 ± 0.016 −8.993 ± 0.023 2.02 ± 0.20 1.00<br />
NGC 4486 1533 187.72356 12.39748 0.70 −8.972 ± 0.016 −10.097 ± 0.013 2.07 ± 0.09 1.00<br />
NGC 4486 1534 187.72352 12.41369 1.08 −5.609 ± 0.112 −6.900 ± 0.140 3.80 ± 0.67 0.94<br />
NGC 4486 1535 187.72354 12.41833 1.22 −7.154 ± 0.037 −7.933 ± 0.049 2.84 ± 0.26 1.00<br />
NGC 4486 1536 187.72360 12.38901 0.66 −7.770 ± 0.018 −9.137 ± 0.020 1.94 ± 0.14 1.00<br />
NGC 4486 1537 187.72363 12.37214 0.97 −6.002 ± 0.093 −7.569 ± 0.083 3.37 ± 0.50 0.99<br />
NGC 4486 1538 187.72368 12.39507 0.67 −8.064 ± 0.025 −9.329 ± 0.029 2.98 ± 0.18 1.00<br />
NGC 4486 1539 187.72367 12.39284 0.66 −7.620 ± 0.036 −8.408 ± 0.055 2.95 ± 0.21 1.00<br />
NGC 4486 1540 187.72376 12.41318 1.07 −8.565 ± 0.018 −9.453 ± 0.030 3.86 ± 0.10 1.00<br />
NGC 4486 1541 187.72377 12.41281 1.06 −7.819 ± 0.020 −8.732 ± 0.042 2.94 ± 0.22 1.00<br />
NGC 4486 1542 187.72380 12.40471 0.84 −8.152 ± 0.027 −9.777 ± 0.019 2.13 ± 0.12 1.00<br />
NGC 4486 1543 187.72386 12.38576 0.70 −6.921 ± 0.608 −8.405 ± 0.049 1.91 ± 0.59 1.00<br />
NGC 4486 1544 187.72394 12.37575 0.89 −8.708 ± 0.025 −9.842 ± 0.020 2.64 ± 0.14 1.00<br />
NGC 4486 1545 187.72415 12.37580 0.89 −9.617 ± 0.038 −10.585 ± 0.022 5.64 ± 0.24 1.00<br />
NGC 4486 1546 187.72392 12.39180 0.67 −6.465 ± 0.063 −8.227 ± 0.080 2.38 ± 0.38 1.00<br />
NGC 4486 1547 187.72391 12.41803 1.22 −7.390 ± 0.035 −8.283 ± 0.043 2.75 ± 0.17 1.00<br />
NGC 4486 1548 187.72398 12.39705 0.71 −6.883 ± 0.046 −7.796 ± 0.114 1.88 ± 0.30 1.00<br />
NGC 4486 1549 187.72397 12.40466 0.84 −8.693 ± 0.027 −9.626 ± 0.015 2.40 ± 0.15 1.00<br />
NGC 4486 1550 187.72394 12.38949 0.67 −5.843 ± 0.107 −7.101 ± 0.073 1.84 ± 0.40 0.99<br />
Continued on Next Page. . .<br />
363
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4486 1551 187.72399 12.38628 0.69 −6.824 ± 0.061 −7.652 ± 0.080 3.99 ± 0.37 0.98<br />
NGC 4486 1552 187.72396 12.38938 0.67 −6.232 ± 0.375 −7.731 ± 0.104 2.40 ± 0.46 1.00<br />
NGC 4486 1553 187.72405 12.40594 0.88 −6.684 ± 0.052 −8.196 ± 0.037 2.56 ± 0.28 1.00<br />
NGC 4486 1554 187.72413 12.41211 1.04 −7.745 ± 0.018 −9.140 ± 0.015 2.16 ± 0.18 1.00<br />
NGC 4486 1555 187.72417 12.38930 0.68 −7.518 ± 0.133 −8.104 ± 0.114 6.51 ± 0.87 0.84<br />
NGC 4486 1556 187.72417 12.36786 1.11 −6.846 ± 0.055 −7.937 ± 0.067 4.14 ± 0.34 0.99<br />
NGC 4486 1560 187.72440 12.38405 0.74 −5.869 ± 0.125 −6.958 ± 0.223 2.15 ± 0.64 0.99<br />
NGC 4486 1561 187.72444 12.37140 1.02 −6.781 ± 0.052 −8.020 ± 0.083 2.53 ± 0.44 1.00<br />
NGC 4486 1562 187.72449 12.41759 1.22 −8.370 ± 0.024 −9.391 ± 0.047 3.45 ± 0.25 1.00<br />
NGC 4486 1563 187.72452 12.37877 0.83 −7.340 ± 0.031 −8.651 ± 0.045 2.22 ± 0.31 1.00<br />
NGC 4486 1567 187.72469 12.39656 0.73 −7.591 ± 0.029 −8.984 ± 0.098 2.25 ± 0.26 1.00<br />
NGC 4486 1568 187.72467 12.40097 0.79 −6.638 ± 0.064 −7.878 ± 0.247 4.34 ± 3.67 0.98<br />
NGC 4486 1569 187.72474 12.38997 0.70 −7.016 ± 0.051 −8.287 ± 0.048 2.20 ± 0.20 1.00<br />
NGC 4486 1570 187.72482 12.39838 0.75 −7.155 ± 0.029 −8.437 ± 0.075 3.70 ± 0.35 1.00<br />
NGC 4486 1571 187.72484 12.40079 0.79 −7.451 ± 0.059 −8.678 ± 0.079 5.08 ± 0.34 0.99<br />
NGC 4486 1572 187.72481 12.41284 1.08 −7.335 ± 0.033 −8.225 ± 0.032 2.25 ± 0.24 1.00<br />
NGC 4486 1576 187.72497 12.38830 0.71 −7.575 ± 0.026 −8.687 ± 0.026 2.65 ± 0.16 1.00<br />
NGC 4486 1577 187.72500 12.37644 0.90 −8.046 ± 0.020 −8.854 ± 0.023 3.00 ± 0.18 1.00<br />
NGC 4486 1578 187.72499 12.39813 0.75 −7.989 ± 0.022 −9.305 ± 0.022 2.41 ± 0.16 1.00<br />
NGC 4486 1579 187.72504 12.38280 0.78 −5.785 ± 0.100 −7.156 ± 0.182 4.35 ± 0.94 0.91<br />
NGC 4486 1581 187.72519 12.37240 1.01 −8.379 ± 0.023 −9.838 ± 0.044 2.20 ± 0.23 1.00<br />
NGC 4486 1583 187.72518 12.37784 0.87 −5.036 ± 0.591 −6.163 ± 1.405 1.51 ± 0.83 0.96<br />
NGC 4486 1584 187.72520 12.40816 0.96 −5.960 ± 0.234 −6.793 ± 0.285 5.48 ± 2.88 0.61<br />
NGC 4486 1585 187.72531 12.37282 1.00 −8.349 ± 0.020 −9.503 ± 0.015 2.46 ± 0.15 1.00<br />
NGC 4486 1586 187.72523 12.38999 0.72 −6.746 ± 0.068 −7.604 ± 0.083 3.21 ± 0.35 0.99<br />
NGC 4486 1587 187.72536 12.40196 0.83 −7.916 ± 0.024 −9.426 ± 0.016 2.70 ± 0.11 1.00<br />
NGC 4486 1588 187.72540 12.39965 0.79 −8.292 ± 0.024 −9.739 ± 0.014 1.19 ± 0.15 0.94<br />
NGC 4486 1589 187.72548 12.38201 0.80 −10.250 ± 0.020 −11.609 ± 0.018 5.28 ± 0.10 0.98<br />
NGC 4486 1590 187.72548 12.38710 0.74 −7.650 ± 0.025 −9.101 ± 0.018 1.98 ± 0.19 1.00<br />
NGC 4486 1591 187.72556 12.37741 0.89 −7.146 ± 0.051 −8.348 ± 0.179 7.29 ± 1.56 0.78<br />
NGC 4486 1592 187.72559 12.39776 0.77 −8.562 ± 0.020 −9.464 ± 0.018 2.61 ± 0.15 1.00<br />
NGC 4486 1593 187.72563 12.39242 0.73 −7.196 ± 0.034 −8.583 ± 0.025 2.41 ± 0.16 1.00<br />
NGC 4486 1594 187.72566 12.38799 0.74 −6.491 ± 0.473 −7.556 ± 0.040 1.21 ± 0.44 0.95<br />
NGC 4486 1596 187.72577 12.37864 0.87 −9.645 ± 0.023 −10.572 ± 0.017 4.34 ± 0.09 1.00<br />
NGC 4486 1597 187.72543 12.39013 0.72 −5.861 ± 0.059 −7.359 ± 0.265 2.76 ± 0.47 0.99<br />
NGC 4486 1598 187.72575 12.36413 1.26 −7.446 ± 0.032 −9.188 ± 0.023 1.80 ± 0.20 1.00<br />
NGC 4486 1599 187.72572 12.39640 0.76 −4.937 ± 0.934 −6.730 ± 0.839 1.14 ± 0.50 0.90<br />
NGC 4486 1600 187.72583 12.39399 0.75 −8.863 ± 0.031 −10.136 ± 0.021 2.68 ± 0.16 1.00<br />
NGC 4486 1601 187.72592 12.39396 0.75 −8.739 ± 0.024 −9.899 ± 0.016 1.71 ± 0.13 1.00<br />
NGC 4486 1602 187.72578 12.41359 1.13 −7.476 ± 0.032 −8.180 ± 0.023 2.11 ± 0.18 1.00<br />
NGC 4486 1604 187.72582 12.41653 1.21 −5.941 ± 0.076 −7.401 ± 0.030 1.76 ± 0.28 0.99<br />
NGC 4486 1605 187.72591 12.37831 0.89 −8.032 ± 0.033 −9.112 ± 0.046 4.08 ± 0.26 1.00<br />
NGC 4486 1606 187.72588 12.39963 0.81 −6.800 ± 0.036 −7.815 ± 0.060 2.41 ± 0.29 1.00<br />
NGC 4486 1607 187.72590 12.41156 1.07 −6.886 ± 0.040 −8.070 ± 0.034 2.28 ± 0.20 1.00<br />
NGC 4486 1608 187.72589 12.39344 0.75 −6.717 ± 0.052 −7.944 ± 0.036 2.14 ± 0.22 1.00<br />
NGC 4486 1609 187.72592 12.38523 0.77 −7.039 ± 0.033 −8.595 ± 0.045 3.17 ± 0.26 1.00<br />
NGC 4486 1610 187.72603 12.41141 1.07 −9.575 ± 0.017 −10.510 ± 0.019 3.09 ± 0.11 1.00<br />
NGC 4486 1611 187.72594 12.39295 0.74 −5.748 ± 0.497 −7.258 ± 0.053 1.45 ± 0.31 0.97<br />
NGC 4486 1612 187.72608 12.40753 0.97 −9.553 ± 0.018 −10.434 ± 0.018 3.25 ± 0.10 1.00<br />
NGC 4486 1613 187.72600 12.37006 1.09 −5.480 ± 0.069 −6.034 ± 0.303 1.93 ± 0.35 0.98<br />
NGC 4486 1614 187.72609 12.38591 0.77 −8.982 ± 0.011 −9.892 ± 0.014 2.34 ± 0.06 1.00<br />
NGC 4486 1615 187.72618 12.37108 1.07 −8.436 ± 0.031 −9.551 ± 0.021 2.64 ± 0.18 1.00<br />
NGC 4486 1616 187.72623 12.38812 0.76 −7.751 ± 0.033 −8.701 ± 0.041 2.64 ± 0.21 1.00<br />
NGC 4486 1617 187.72632 12.41510 1.18 −6.272 ± 0.088 −7.510 ± 0.078 4.43 ± 0.36 0.95<br />
NGC 4486 1619 187.72643 12.37884 0.89 −6.772 ± 0.055 −8.131 ± 0.047 2.89 ± 0.31 1.00<br />
NGC 4486 1620 187.72647 12.41353 1.14 −5.889 ± 0.145 −7.558 ± 0.205 6.04 ± 1.44 0.80<br />
NGC 4486 1621 187.72652 12.40829 1.00 −6.396 ± 0.088 −7.806 ± 0.067 3.13 ± 0.40 1.00<br />
NGC 4486 1622 187.72656 12.38593 0.79 −5.435 ± 0.414 −6.850 ± 0.093 2.16 ± 0.57 0.99<br />
NGC 4486 1624 187.72666 12.39137 0.77 −6.166 ± 0.058 −7.574 ± 0.056 2.22 ± 0.33 1.00<br />
NGC 4486 1625 187.72681 12.37890 0.90 −7.131 ± 0.038 −8.289 ± 0.030 2.02 ± 0.16 1.00<br />
NGC 4486 1628 187.72691 12.37555 0.98 −7.432 ± 0.033 −8.525 ± 0.425 2.79 ± 0.43 1.00<br />
NGC 4486 1630 187.72699 12.38206 0.85 −8.275 ± 0.038 −9.223 ± 0.082 7.76 ± 0.51 0.94<br />
Continued on Next Page. . .<br />
364
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4486 1632 187.72699 12.39078 0.78 −8.512 ± 0.017 −9.856 ± 0.012 2.45 ± 0.13 1.00<br />
NGC 4486 1633 187.72710 12.41764 1.28 −9.739 ± 0.034 −10.697 ± 0.017 5.18 ± 0.18 1.00<br />
NGC 4486 1635 187.72713 12.37447 1.01 −7.743 ± 0.031 −8.801 ± 0.027 2.45 ± 0.17 1.00<br />
NGC 4486 1636 187.72714 12.40015 0.86 −8.006 ± 0.017 −8.911 ± 0.032 2.10 ± 0.11 1.00<br />
NGC 4486 1637 187.72721 12.39540 0.81 −7.690 ± 0.043 −9.087 ± 0.023 1.30 ± 0.19 0.97<br />
NGC 4486 1638 187.72719 12.40168 0.88 −6.822 ± 0.036 −7.619 ± 0.074 2.35 ± 0.37 1.00<br />
NGC 4486 1639 187.72727 12.36986 1.13 −7.491 ± 0.033 −8.314 ± 0.068 3.17 ± 0.40 1.00<br />
NGC 4486 1640 187.72738 12.41398 1.18 −6.433 ± 0.093 −7.828 ± 0.131 6.23 ± 0.90 0.83<br />
NGC 4486 1641 187.72740 12.36503 1.27 −6.523 ± 0.046 −8.010 ± 0.043 2.51 ± 0.23 1.00<br />
NGC 4486 1643 187.72753 12.36419 1.30 −8.719 ± 0.053 −9.583 ± 0.091 6.96 ± 0.48 1.00<br />
NGC 4486 1644 187.72753 12.41418 1.19 −5.871 ± 0.145 −6.817 ± 0.157 2.76 ± 0.95 0.99<br />
NGC 4486 1645 187.72757 12.38912 0.81 −6.015 ± 0.074 −6.861 ± 0.916 2.52 ± 0.41 0.99<br />
NGC 4486 1646 187.72758 12.37891 0.93 −6.813 ± 0.038 −7.895 ± 0.047 2.60 ± 0.22 1.00<br />
NGC 4486 1647 187.72768 12.37348 1.05 −8.808 ± 0.020 −10.313 ± 0.023 2.16 ± 0.11 1.00<br />
NGC 4486 1648 187.72751 12.39357 0.81 −5.589 ± 0.064 −6.657 ± 0.101 1.79 ± 0.40 0.98<br />
NGC 4486 1649 187.72760 12.37059 1.12 −5.479 ± 0.152 −6.769 ± 0.213 5.63 ± 1.37 0.57<br />
NGC 4486 1650 187.72769 12.40323 0.93 −6.281 ± 0.087 −7.198 ± 0.235 4.21 ± 1.71 0.93<br />
NGC 4486 1651 187.72768 12.41646 1.25 −4.885 ± 0.305 −6.362 ± 0.176 2.22 ± 0.75 0.99<br />
NGC 4486 1652 187.72770 12.40655 1.00 −7.054 ± 0.039 −8.566 ± 0.032 2.01 ± 0.18 1.00<br />
NGC 4486 1653 187.72786 12.38645 0.83 −8.548 ± 0.020 −9.498 ± 0.024 3.52 ± 0.16 1.00<br />
NGC 4486 1654 187.72789 12.40936 1.07 −9.529 ± 0.013 −10.503 ± 0.010 2.12 ± 0.11 1.00<br />
NGC 4486 1655 187.72786 12.39782 0.85 −8.967 ± 0.018 −9.930 ± 0.022 2.72 ± 0.16 1.00<br />
NGC 4486 1656 187.72794 12.41491 1.22 −7.729 ± 0.024 −8.719 ± 0.024 2.26 ± 0.19 1.00<br />
NGC 4486 1659 187.72797 12.39105 0.82 −9.188 ± 0.012 −10.046 ± 0.014 3.81 ± 0.09 1.00<br />
NGC 4486 1660 187.72783 12.38472 0.85 −7.787 ± 0.023 −8.805 ± 0.032 2.27 ± 0.19 1.00<br />
NGC 4486 1661 187.72809 12.40402 0.96 −6.152 ± 0.043 −7.080 ± 0.065 2.33 ± 0.27 1.00<br />
NGC 4486 1663 187.72818 12.40262 0.93 −5.337 ± 0.192 −6.242 ± 0.521 2.13 ± 1.77 0.99<br />
NGC 4486 1664 187.72820 12.39533 0.84 −5.787 ± 0.111 −7.239 ± 0.095 2.40 ± 0.57 1.00<br />
NGC 4486 1665 187.72832 12.40349 0.95 −10.296 ± 0.035 −11.301 ± 0.029 6.19 ± 0.16 1.00<br />
NGC 4486 1666 187.72826 12.39407 0.84 −6.786 ± 0.172 −8.157 ± 0.037 2.23 ± 0.26 1.00<br />
NGC 4486 1667 187.72833 12.40709 1.03 −7.775 ± 0.025 −8.976 ± 0.031 2.55 ± 0.14 1.00<br />
NGC 4486 1668 187.72830 12.37483 1.03 −7.346 ± 0.033 −8.235 ± 0.067 2.90 ± 0.25 1.00<br />
NGC 4486 1670 187.72836 12.41166 1.14 −7.060 ± 0.038 −8.376 ± 0.043 2.92 ± 0.28 1.00<br />
NGC 4486 1671 187.72844 12.38230 0.90 −8.193 ± 0.032 −9.437 ± 0.025 2.84 ± 0.15 1.00<br />
NGC 4486 1672 187.72839 12.38928 0.84 −6.770 ± 0.049 −7.462 ± 0.098 2.76 ± 0.47 0.99<br />
NGC 4486 1673 187.72850 12.36888 1.19 −9.234 ± 0.013 −10.249 ± 0.015 2.48 ± 0.12 1.00<br />
NGC 4486 1674 187.72844 12.40776 1.05 −7.549 ± 0.027 −8.438 ± 0.036 3.03 ± 0.17 1.00<br />
NGC 4486 1675 187.72843 12.41783 1.31 −7.255 ± 0.038 −8.455 ± 0.045 3.11 ± 0.26 1.00<br />
NGC 4486 1676 187.72845 12.39165 0.83 −6.242 ± 0.100 −7.680 ± 0.051 1.52 ± 0.28 0.99<br />
NGC 4486 1677 187.72853 12.37334 1.08 −7.604 ± 0.023 −9.025 ± 0.022 1.39 ± 0.15 0.98<br />
NGC 4486 1678 187.72849 12.38813 0.84 −5.687 ± 0.699 −7.381 ± 0.040 2.82 ± 0.50 0.99<br />
NGC 4486 1680 187.72856 12.39484 0.85 −7.882 ± 0.020 −9.101 ± 0.028 2.46 ± 0.14 1.00<br />
NGC 4486 1681 187.72860 12.39235 0.84 −8.564 ± 0.019 −9.934 ± 0.016 1.80 ± 0.20 1.00<br />
NGC 4486 1682 187.72859 12.41899 1.35 −7.535 ± 0.026 −8.842 ± 0.029 2.72 ± 0.15 1.00<br />
NGC 4486 1683 187.72859 12.39466 0.85 −7.488 ± 0.020 −8.713 ± 0.017 1.92 ± 0.09 1.00<br />
NGC 4486 1684 187.72857 12.39767 0.87 −5.442 ± 0.469 −7.155 ± 0.174 2.65 ± 0.94 0.99<br />
NGC 4486 1685 187.72864 12.38345 0.89 −8.511 ± 0.030 −9.376 ± 0.014 2.59 ± 0.20 1.00<br />
NGC 4486 1686 187.72863 12.41971 1.37 −7.598 ± 0.058 −9.233 ± 0.044 5.32 ± 0.28 0.99<br />
NGC 4486 1687 187.72864 12.41201 1.16 −5.612 ± 0.457 −7.385 ± 0.071 1.42 ± 0.45 0.97<br />
NGC 4486 1688 187.72864 12.40624 1.02 −9.180 ± 0.031 −10.007 ± 0.014 3.27 ± 0.16 1.00<br />
NGC 4486 1689 187.72870 12.36800 1.22 −6.277 ± 0.058 −7.358 ± 0.081 3.18 ± 0.37 0.99<br />
NGC 4486 1690 187.72896 12.40925 1.10 −8.437 ± 0.023 −9.880 ± 0.015 1.72 ± 0.11 1.00<br />
NGC 4486 1692 187.72905 12.37805 0.99 −8.289 ± 0.023 −9.308 ± 0.028 2.65 ± 0.16 1.00<br />
NGC 4486 1693 187.72908 12.39991 0.92 −7.941 ± 0.020 −9.524 ± 0.024 2.53 ± 0.14 1.00<br />
NGC 4486 1697 187.72936 12.40100 0.95 −8.994 ± 0.019 −10.253 ± 0.009 2.05 ± 0.08 1.00<br />
NGC 4486 1698 187.72937 12.37150 1.14 −6.908 ± 0.025 −8.193 ± 0.036 2.14 ± 0.14 1.00<br />
NGC 4486 1699 187.72934 12.41647 1.30 −5.401 ± 0.183 −6.733 ± 0.116 5.06 ± 0.87 0.70<br />
NGC 4486 1700 187.72951 12.38849 0.88 −10.216 ± 0.032 −11.188 ± 0.025 4.26 ± 0.16 0.99<br />
NGC 4486 1701 187.72960 12.38838 0.88 −8.031 ± 0.025 −9.097 ± 0.024 2.73 ± 0.23 1.00<br />
NGC 4486 1702 187.72948 12.38903 0.88 −8.721 ± 0.026 −9.518 ± 0.024 8.87 ± 0.17 0.87<br />
NGC 4486 1703 187.72944 12.36686 1.27 −6.589 ± 0.064 −7.709 ± 0.057 3.19 ± 0.32 0.99<br />
NGC 4486 1704 187.72954 12.38061 0.96 −7.368 ± 0.038 −8.675 ± 0.038 2.71 ± 0.23 1.00<br />
Continued on Next Page. . .<br />
365
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4486 1705 187.72957 12.40079 0.95 −7.829 ± 0.021 −8.911 ± 0.037 2.99 ± 0.18 1.00<br />
NGC 4486 1706 187.72954 12.39904 0.93 −6.987 ± 0.055 −8.609 ± 0.026 3.28 ± 0.22 1.00<br />
NGC 4486 1708 187.72960 12.39335 0.88 −9.018 ± 0.031 −10.268 ± 0.044 4.11 ± 0.30 1.00<br />
NGC 4486 1709 187.72960 12.39969 0.94 −5.426 ± 0.148 −7.065 ± 0.073 2.63 ± 0.45 0.99<br />
NGC 4486 1710 187.72965 12.40811 1.09 −7.168 ± 0.037 −8.525 ± 0.034 2.83 ± 0.20 1.00<br />
NGC 4486 1712 187.72974 12.41832 1.36 −6.954 ± 0.034 −7.996 ± 0.026 2.51 ± 0.24 1.00<br />
NGC 4486 1713 187.72974 12.38890 0.89 −7.639 ± 0.047 −8.550 ± 0.048 4.65 ± 0.21 1.00<br />
NGC 4486 1716 187.72979 12.37638 1.05 −6.711 ± 0.031 −8.272 ± 0.025 2.27 ± 0.27 1.00<br />
NGC 4486 1718 187.72984 12.37659 1.04 −8.527 ± 0.019 −9.478 ± 0.022 3.40 ± 0.13 1.00<br />
NGC 4486 1719 187.73007 12.37673 1.05 −10.452 ± 0.015 −11.843 ± 0.017 4.33 ± 0.13 0.99<br />
NGC 4486 1720 187.72992 12.40577 1.05 −8.176 ± 0.038 −9.245 ± 0.029 4.95 ± 0.14 1.00<br />
NGC 4486 1722 187.72998 12.39308 0.89 −8.353 ± 0.016 −9.484 ± 0.021 2.22 ± 0.11 1.00<br />
NGC 4486 1723 187.73004 12.39376 0.90 −8.202 ± 0.025 −9.292 ± 0.021 2.25 ± 0.12 1.00<br />
NGC 4486 1724 187.73000 12.39862 0.94 −7.197 ± 0.035 −8.003 ± 0.038 3.41 ± 0.20 0.99<br />
NGC 4486 1725 187.73004 12.40149 0.98 −6.285 ± 0.241 −7.755 ± 0.051 1.62 ± 0.28 0.99<br />
NGC 4486 1726 187.73011 12.39202 0.90 −7.951 ± 0.043 −8.831 ± 0.057 5.09 ± 0.26 0.99<br />
NGC 4486 1728 187.73012 12.37534 1.08 −6.776 ± 0.028 −8.073 ± 0.039 2.02 ± 0.17 1.00<br />
NGC 4486 1729 187.73018 12.40185 0.99 −5.483 ± 0.101 −6.113 ± 0.123 2.51 ± 0.54 0.99<br />
NGC 4486 1730 187.73024 12.38312 0.95 −6.662 ± 0.080 −7.839 ± 0.046 3.52 ± 0.34 0.99<br />
NGC 4486 1731 187.73026 12.38466 0.93 −7.398 ± 0.030 −8.538 ± 0.049 2.55 ± 0.22 1.00<br />
NGC 4486 1732 187.73028 12.41901 1.39 −7.075 ± 0.062 −8.570 ± 0.025 2.85 ± 0.21 1.00<br />
NGC 4486 1733 187.73030 12.36813 1.26 −6.722 ± 0.028 −8.119 ± 0.045 1.84 ± 0.29 1.00<br />
NGC 4486 1734 187.73035 12.39332 0.91 −6.583 ± 0.052 −7.377 ± 0.079 5.76 ± 0.34 0.79<br />
NGC 4486 1735 187.73041 12.38659 0.92 −7.348 ± 0.020 −8.902 ± 0.039 2.37 ± 0.29 1.00<br />
NGC 4486 1736 187.73042 12.38773 0.92 −7.610 ± 0.020 −9.216 ± 0.147 1.86 ± 0.23 1.00<br />
NGC 4486 1738 187.73045 12.41239 1.22 −7.650 ± 0.020 −9.160 ± 0.023 2.39 ± 0.13 1.00<br />
NGC 4486 1739 187.73050 12.40941 1.14 −6.823 ± 0.032 −8.191 ± 0.039 2.57 ± 0.25 1.00<br />
NGC 4486 1742 187.73059 12.39080 0.91 −6.393 ± 0.049 −8.038 ± 0.051 2.54 ± 0.26 1.00<br />
NGC 4486 1743 187.73067 12.38249 0.97 −8.736 ± 0.019 −9.719 ± 0.025 3.54 ± 0.09 1.00<br />
NGC 4486 1744 187.73075 12.40466 1.05 −9.266 ± 0.020 −10.590 ± 0.015 2.36 ± 0.13 1.00<br />
NGC 4486 1745 187.73081 12.37342 1.14 −6.442 ± 0.065 −8.038 ± 0.052 2.58 ± 0.31 1.00<br />
NGC 4486 1746 187.73088 12.38092 1.00 −9.546 ± 0.014 −10.447 ± 0.016 3.60 ± 0.11 1.00<br />
NGC 4486 1747 187.73082 12.39719 0.95 −6.127 ± 0.093 −7.427 ± 0.067 2.42 ± 0.42 1.00<br />
NGC 4486 1748 187.73093 12.36895 1.25 −8.197 ± 0.033 −9.026 ± 0.047 5.14 ± 0.33 0.99<br />
NGC 4486 1749 187.73096 12.36533 1.35 −7.727 ± 0.033 −9.079 ± 0.029 2.74 ± 0.18 1.00<br />
NGC 4486 1750 187.73101 12.38731 0.94 −8.976 ± 0.022 −10.077 ± 0.010 2.03 ± 0.07 1.00<br />
NGC 4486 1751 187.73101 12.38183 0.99 −7.049 ± 0.022 −8.477 ± 0.235 2.04 ± 0.21 1.00<br />
NGC 4486 1752 187.73098 12.39933 0.98 −5.931 ± 0.119 −7.071 ± 0.152 3.49 ± 0.76 0.97<br />
NGC 4486 1754 187.73113 12.40848 1.14 −8.401 ± 0.021 −9.934 ± 0.011 2.99 ± 0.12 1.00<br />
NGC 4486 1755 187.73118 12.40872 1.15 −8.154 ± 0.022 −8.992 ± 0.034 3.86 ± 0.22 1.00<br />
NGC 4486 1756 187.73128 12.37175 1.19 −6.050 ± 0.113 −7.282 ± 0.135 3.84 ± 0.71 0.96<br />
NGC 4486 1757 187.73131 12.36868 1.27 −7.681 ± 0.021 −9.246 ± 0.021 1.97 ± 0.11 1.00<br />
NGC 4486 1758 187.73132 12.38142 1.01 −6.446 ± 0.053 −7.850 ± 0.046 1.80 ± 0.30 1.00<br />
NGC 4486 1759 187.73134 12.39833 0.98 −6.336 ± 0.071 −7.757 ± 0.086 4.98 ± 0.59 0.94<br />
NGC 4486 1761 187.73146 12.38004 1.04 −7.970 ± 0.026 −9.420 ± 0.020 2.31 ± 0.13 1.00<br />
NGC 4486 1762 187.73149 12.37609 1.11 −7.885 ± 0.032 −8.995 ± 0.033 3.52 ± 0.18 1.00<br />
NGC 4486 1763 187.73151 12.36791 1.29 −7.330 ± 0.051 −8.105 ± 0.043 2.48 ± 0.25 1.00<br />
NGC 4486 1765 187.73155 12.40867 1.16 −6.607 ± 0.121 −8.297 ± 0.065 8.89 ± 0.83 0.62<br />
NGC 4486 1766 187.73165 12.41885 1.42 −8.787 ± 0.020 −10.003 ± 0.020 2.13 ± 0.18 1.00<br />
NGC 4486 1767 187.73163 12.37456 1.14 −7.392 ± 0.021 −8.304 ± 0.030 2.53 ± 0.18 1.00<br />
NGC 4486 1768 187.73163 12.38498 0.98 −5.552 ± 0.150 −6.603 ± 0.299 5.53 ± 2.29 0.55<br />
NGC 4486 1769 187.73163 12.38571 0.97 −6.894 ± 0.044 −7.553 ± 0.032 2.29 ± 0.24 1.00<br />
NGC 4486 1771 187.73165 12.40691 1.13 −7.085 ± 0.084 −8.040 ± 0.083 4.54 ± 0.36 0.98<br />
NGC 4486 1772 187.73165 12.40397 1.07 −6.461 ± 0.050 −8.148 ± 0.068 2.62 ± 0.29 1.00<br />
NGC 4486 1773 187.73176 12.40507 1.09 −6.909 ± 0.041 −8.580 ± 0.023 2.08 ± 0.18 1.00<br />
NGC 4486 1774 187.73191 12.39424 0.97 −9.016 ± 0.022 −10.004 ± 0.022 3.67 ± 0.16 1.00<br />
NGC 4486 1775 187.73195 12.40372 1.08 −7.405 ± 0.029 −8.497 ± 0.046 3.05 ± 0.19 1.00<br />
NGC 4486 1776 187.73200 12.39042 0.97 −8.224 ± 0.029 −9.072 ± 0.023 2.55 ± 0.19 1.00<br />
NGC 4486 1777 187.73197 12.40172 1.05 −5.509 ± 0.280 −6.426 ± 0.141 5.65 ± 2.10 0.52<br />
NGC 4486 1778 187.73206 12.40643 1.13 −8.118 ± 0.034 −9.099 ± 0.023 2.41 ± 0.20 1.00<br />
NGC 4486 1779 187.73204 12.36593 1.36 −5.260 ± 0.136 −6.142 ± 0.132 2.67 ± 0.59 0.98<br />
NGC 4486 1780 187.73205 12.39512 0.98 −5.334 ± 0.050 −7.023 ± 0.131 2.61 ± 0.56 0.99<br />
Continued on Next Page. . .<br />
366
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4486 1781 187.73222 12.36420 1.41 −7.553 ± 0.018 −8.466 ± 0.039 3.38 ± 0.17 1.00<br />
NGC 4486 1782 187.73230 12.38941 0.98 −9.316 ± 0.016 −10.313 ± 0.016 3.32 ± 0.11 1.00<br />
NGC 4486 1784 187.73230 12.38743 0.99 −5.173 ± 0.085 −6.677 ± 0.113 2.69 ± 0.50 0.99<br />
NGC 4486 1785 187.73233 12.36644 1.35 −7.020 ± 0.039 −7.905 ± 0.062 2.70 ± 0.32 1.00<br />
NGC 4486 1786 187.73239 12.36832 1.31 −7.328 ± 0.113 −8.385 ± 0.113 7.30 ± 0.98 0.79<br />
NGC 4486 1787 187.73238 12.40448 1.10 −6.731 ± 0.118 −7.476 ± 0.079 6.91 ± 0.69 0.52<br />
NGC 4486 1788 187.73241 12.39143 0.98 −8.523 ± 0.018 −9.830 ± 0.014 2.57 ± 0.13 1.00<br />
NGC 4486 1791 187.73250 12.40255 1.08 −6.824 ± 0.092 −8.063 ± 0.125 6.43 ± 0.85 0.84<br />
NGC 4486 1793 187.73254 12.41237 1.27 −5.283 ± 0.179 −6.875 ± 0.260 3.10 ± 1.55 0.98<br />
NGC 4486 1794 187.73258 12.40848 1.19 −7.234 ± 0.025 −8.795 ± 0.023 1.87 ± 0.18 1.00<br />
NGC 4486 1796 187.73273 12.38144 1.06 −7.600 ± 0.042 −8.432 ± 0.036 2.89 ± 0.20 1.00<br />
NGC 4486 1797 187.73271 12.39399 1.00 −6.626 ± 0.049 −8.269 ± 0.070 3.11 ± 0.42 1.00<br />
NGC 4486 1798 187.73277 12.41460 1.34 −8.423 ± 0.023 −9.380 ± 0.017 2.69 ± 0.16 1.00<br />
NGC 4486 1799 187.73276 12.41066 1.24 −6.386 ± 0.050 −7.691 ± 0.055 2.95 ± 0.27 1.00<br />
NGC 4486 1800 187.73280 12.38353 1.04 −7.693 ± 0.022 −8.966 ± 0.025 2.03 ± 0.24 1.00<br />
NGC 4486 1801 187.73285 12.36867 1.31 −8.321 ± 0.020 −9.386 ± 0.027 3.40 ± 0.14 1.00<br />
NGC 4486 1802 187.73285 12.38960 1.00 −7.380 ± 0.032 −8.712 ± 0.028 2.37 ± 0.17 1.00<br />
NGC 4486 1803 187.73288 12.36402 1.43 −6.629 ± 0.043 −8.028 ± 0.029 2.33 ± 0.26 1.00<br />
NGC 4486 1805 187.73293 12.39567 1.02 −5.779 ± 0.087 −7.180 ± 0.069 2.23 ± 0.42 1.00<br />
NGC 4486 1806 187.73302 12.38940 1.01 −7.765 ± 0.019 −9.230 ± 0.023 2.41 ± 0.17 1.00<br />
NGC 4486 1807 187.73300 12.39551 1.02 −5.819 ± 0.101 −7.643 ± 0.041 1.83 ± 0.36 1.00<br />
NGC 4486 1808 187.73302 12.40484 1.13 −7.721 ± 0.013 −9.185 ± 0.019 2.14 ± 0.11 1.00<br />
NGC 4486 1809 187.73304 12.39124 1.00 −7.162 ± 0.029 −8.486 ± 0.026 2.12 ± 0.15 1.00<br />
NGC 4486 1810 187.73315 12.39360 1.01 −7.605 ± 0.027 −8.692 ± 0.073 3.70 ± 0.34 1.00<br />
NGC 4486 1811 187.73319 12.36766 1.35 −8.296 ± 0.035 −9.552 ± 0.025 4.04 ± 0.18 1.00<br />
NGC 4486 1812 187.73315 12.37555 1.17 −6.252 ± 0.087 −7.908 ± 0.079 3.40 ± 0.56 0.99<br />
NGC 4486 1813 187.73321 12.40875 1.21 −9.874 ± 0.012 −11.154 ± 0.010 2.29 ± 0.08 1.00<br />
NGC 4486 1814 187.73320 12.40913 1.22 −6.658 ± 0.065 −8.088 ± 0.036 2.53 ± 0.25 1.00<br />
NGC 4486 1815 187.73320 12.36486 1.42 −7.682 ± 0.029 −8.800 ± 0.038 2.27 ± 0.19 1.00<br />
NGC 4486 1816 187.73323 12.39953 1.06 −8.048 ± 0.021 −9.515 ± 0.027 3.13 ± 0.18 1.00<br />
NGC 4486 1817 187.73325 12.39542 1.03 −8.138 ± 0.025 −9.551 ± 0.015 2.10 ± 0.12 1.00<br />
NGC 4486 1818 187.73326 12.39794 1.05 −7.376 ± 0.038 −8.109 ± 0.071 3.98 ± 0.24 0.99<br />
NGC 4486 1819 187.73332 12.37393 1.21 −7.760 ± 0.031 −8.727 ± 0.035 3.57 ± 0.19 1.00<br />
NGC 4486 1821 187.73330 12.40130 1.09 −7.252 ± 0.079 −8.472 ± 0.126 5.86 ± 0.76 0.94<br />
NGC 4486 1822 187.73343 12.39763 1.05 −10.251 ± 0.014 −11.462 ± 0.017 3.28 ± 0.14 1.00<br />
NGC 4486 1823 187.73338 12.41075 1.26 −7.234 ± 0.025 −8.628 ± 0.027 2.28 ± 0.13 1.00<br />
NGC 4486 1824 187.73337 12.40195 1.10 −5.564 ± 0.070 −7.157 ± 0.075 1.77 ± 0.49 0.99<br />
NGC 4486 1825 187.73340 12.37592 1.17 −7.689 ± 0.024 −8.515 ± 0.030 2.35 ± 0.15 1.00<br />
NGC 4486 1826 187.73352 12.41129 1.28 −8.284 ± 0.015 −9.660 ± 0.023 2.86 ± 0.12 1.00<br />
NGC 4486 1827 187.73351 12.40592 1.17 −7.273 ± 0.031 −8.700 ± 0.030 2.10 ± 0.16 1.00<br />
NGC 4486 1829 187.73360 12.40548 1.16 −7.956 ± 0.018 −9.430 ± 0.018 2.57 ± 0.13 1.00<br />
NGC 4486 1830 187.73358 12.36873 1.33 −6.343 ± 0.060 −7.765 ± 0.039 1.69 ± 0.29 0.99<br />
NGC 4486 1831 187.73365 12.37556 1.19 −6.535 ± 0.042 −7.940 ± 0.033 2.35 ± 0.22 1.00<br />
NGC 4486 1832 187.73369 12.39239 1.03 −9.333 ± 0.015 −10.364 ± 0.020 2.40 ± 0.19 1.00<br />
NGC 4486 1833 187.73373 12.39861 1.07 −7.508 ± 0.034 −8.730 ± 0.034 3.17 ± 0.21 1.00<br />
NGC 4486 1834 187.73375 12.37829 1.14 −7.495 ± 0.033 −8.261 ± 0.030 2.71 ± 0.19 1.00<br />
NGC 4486 1835 187.73380 12.37378 1.22 −7.062 ± 0.028 −8.490 ± 0.023 2.08 ± 0.20 1.00<br />
NGC 4486 1836 187.73383 12.37011 1.31 −6.130 ± 0.436 −7.480 ± 0.598 1.75 ± 0.47 0.99<br />
NGC 4486 1838 187.73386 12.38582 1.05 −6.740 ± 0.032 −8.249 ± 0.043 2.41 ± 0.25 1.00<br />
NGC 4486 1839 187.73398 12.36896 1.34 −7.659 ± 0.038 −8.563 ± 0.038 3.43 ± 0.20 1.00<br />
NGC 4486 1840 187.73401 12.37077 1.30 −7.550 ± 0.029 −8.843 ± 0.046 3.48 ± 0.23 1.00<br />
NGC 4486 1841 187.73399 12.41737 1.44 −6.494 ± 0.056 −7.987 ± 0.034 2.49 ± 0.26 1.00<br />
NGC 4486 1843 187.73416 12.39190 1.05 −10.530 ± 0.075 −11.676 ± 0.086 7.15 ± 0.57 1.00<br />
NGC 4486 1844 187.73404 12.41014 1.27 −6.067 ± 0.415 −7.547 ± 0.052 2.16 ± 0.49 1.00<br />
NGC 4486 1846 187.73419 12.37093 1.30 −7.441 ± 0.028 −8.400 ± 0.050 3.16 ± 0.19 1.00<br />
NGC 4486 1847 187.73422 12.40542 1.18 −6.728 ± 0.044 −8.227 ± 0.040 2.51 ± 0.22 1.00<br />
NGC 4486 1848 187.73424 12.41267 1.33 −5.293 ± 0.277 −6.226 ± 0.095 2.74 ± 0.63 0.98<br />
NGC 4486 1849 187.73433 12.39562 1.07 −7.352 ± 0.061 −8.636 ± 0.057 3.50 ± 0.35 1.00<br />
NGC 4486 1850 187.73408 12.38057 1.12 −7.031 ± 0.039 −8.250 ± 0.041 3.05 ± 0.18 1.00<br />
NGC 4486 1851 187.73438 12.37803 1.17 −7.692 ± 0.045 −9.066 ± 0.049 4.94 ± 0.31 1.00<br />
NGC 4486 1852 187.73447 12.38951 1.06 −8.379 ± 0.025 −9.245 ± 0.033 4.15 ± 0.15 1.00<br />
NGC 4486 1854 187.73452 12.38568 1.08 −7.231 ± 0.027 −8.449 ± 0.044 2.44 ± 0.23 1.00<br />
Continued on Next Page. . .<br />
367
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4486 1855 187.73450 12.38748 1.07 −6.548 ± 0.049 −8.062 ± 0.053 3.02 ± 0.32 1.00<br />
NGC 4486 1856 187.73454 12.38431 1.09 −7.441 ± 0.024 −8.532 ± 0.039 3.13 ± 0.18 1.00<br />
NGC 4486 1857 187.73406 12.36648 1.40 −7.040 ± 0.030 −8.616 ± 0.039 2.15 ± 0.18 1.00<br />
NGC 4486 1859 187.73476 12.40977 1.28 −9.406 ± 0.012 −10.459 ± 0.012 3.56 ± 0.09 1.00<br />
NGC 4486 1860 187.73474 12.40709 1.23 −8.743 ± 0.045 −9.922 ± 0.036 3.54 ± 0.29 1.00<br />
NGC 4486 1862 187.73482 12.40953 1.28 −8.506 ± 0.014 −9.595 ± 0.015 3.76 ± 0.12 1.00<br />
NGC 4486 1865 187.73494 12.37252 1.29 −5.719 ± 0.132 −6.627 ± 0.131 3.04 ± 0.86 0.98<br />
NGC 4486 1866 187.73403 12.40875 1.24 −5.767 ± 0.081 −6.962 ± 0.044 1.74 ± 0.23 0.99<br />
NGC 4486 1870 187.73508 12.39125 1.08 −6.202 ± 0.092 −7.799 ± 0.054 2.10 ± 0.28 1.00<br />
NGC 4486 1871 187.73507 12.36825 1.39 −5.517 ± 0.065 −6.610 ± 0.353 2.31 ± 0.44 0.99<br />
NGC 4486 1872 187.73513 12.40839 1.26 −8.138 ± 0.031 −9.672 ± 0.017 1.77 ± 0.14 1.00<br />
NGC 4486 1874 187.73520 12.36682 1.42 −7.183 ± 0.025 −8.637 ± 0.032 2.08 ± 0.20 1.00<br />
NGC 4486 1875 187.73520 12.38901 1.09 −8.021 ± 0.030 −8.670 ± 0.036 5.36 ± 0.23 0.98<br />
NGC 4486 1876 187.73523 12.38406 1.12 −5.633 ± 0.635 −7.305 ± 0.069 1.73 ± 0.41 0.99<br />
NGC 4486 1877 187.73526 12.37968 1.17 −6.297 ± 0.039 −7.384 ± 0.050 1.76 ± 0.29 0.99<br />
NGC 4486 1878 187.73531 12.37815 1.19 −5.116 ± 0.114 −6.698 ± 0.066 1.91 ± 0.56 0.99<br />
NGC 4486 1880 187.73552 12.41308 1.38 −9.401 ± 0.015 −10.568 ± 0.016 2.49 ± 0.10 1.00<br />
NGC 4486 1882 187.73556 12.40395 1.20 −6.942 ± 0.053 −8.183 ± 0.410 2.50 ± 0.68 1.00<br />
NGC 4486 1883 187.73564 12.38558 1.12 −8.921 ± 0.012 −10.225 ± 0.016 2.28 ± 0.11 1.00<br />
NGC 4486 1884 187.73566 12.39022 1.10 −8.369 ± 0.025 −9.268 ± 0.027 3.02 ± 0.14 1.00<br />
NGC 4486 1885 187.73563 12.38235 1.15 −7.028 ± 0.026 −8.001 ± 0.048 2.07 ± 0.30 1.00<br />
NGC 4486 1886 187.73572 12.41954 1.54 −5.374 ± 0.153 −6.831 ± 0.444 2.63 ± 0.78 0.99<br />
NGC 4486 1888 187.73584 12.37938 1.19 −6.981 ± 0.041 −8.605 ± 0.025 2.25 ± 0.20 1.00<br />
NGC 4486 1889 187.73592 12.38053 1.18 −9.218 ± 0.018 −10.699 ± 0.020 3.86 ± 0.17 1.00<br />
NGC 4486 1890 187.73587 12.39039 1.11 −6.856 ± 0.046 −8.365 ± 0.032 2.20 ± 0.23 1.00<br />
NGC 4486 1891 187.73591 12.39525 1.12 −7.194 ± 0.062 −8.497 ± 0.042 5.01 ± 0.40 0.99<br />
NGC 4486 1892 187.73592 12.38859 1.12 −7.533 ± 0.028 −8.765 ± 0.029 3.07 ± 0.18 1.00<br />
NGC 4486 1893 187.73600 12.37400 1.29 −6.003 ± 0.061 −7.176 ± 0.059 1.89 ± 0.39 0.99<br />
NGC 4486 1894 187.73621 12.38852 1.13 −6.231 ± 0.058 −7.193 ± 0.100 3.50 ± 0.52 0.97<br />
NGC 4486 1895 187.73632 12.36706 1.45 −6.843 ± 0.043 −8.170 ± 0.044 3.41 ± 0.25 1.00<br />
NGC 4486 1897 187.73653 12.39180 1.13 −8.529 ± 0.024 −9.453 ± 0.024 3.02 ± 0.19 1.00<br />
NGC 4486 1898 187.73650 12.38868 1.14 −6.776 ± 0.044 −7.527 ± 0.062 2.72 ± 0.27 1.00<br />
NGC 4486 1900 187.73661 12.39466 1.14 −8.259 ± 0.023 −9.122 ± 0.032 3.97 ± 0.15 1.00<br />
NGC 4486 1901 187.73661 12.40189 1.21 −7.908 ± 0.018 −8.972 ± 0.017 2.58 ± 0.12 1.00<br />
NGC 4486 1902 187.73678 12.37908 1.23 −8.589 ± 0.028 −9.989 ± 0.021 2.55 ± 0.12 1.00<br />
NGC 4486 1903 187.73680 12.38864 1.15 −8.202 ± 0.019 −9.297 ± 0.026 2.78 ± 0.16 1.00<br />
NGC 4486 1904 187.73677 12.39154 1.14 −6.519 ± 0.055 −7.421 ± 0.066 3.35 ± 0.31 0.99<br />
NGC 4486 1905 187.73678 12.41509 1.46 −5.862 ± 0.086 −6.783 ± 0.059 1.57 ± 0.38 0.97<br />
NGC 4486 1906 187.73684 12.38325 1.18 −7.299 ± 0.035 −8.649 ± 0.025 2.78 ± 0.18 1.00<br />
NGC 4486 1907 187.73691 12.36967 1.41 −6.459 ± 0.037 −7.762 ± 0.034 1.46 ± 0.17 0.98<br />
NGC 4486 1908 187.73703 12.38439 1.18 −7.264 ± 0.054 −8.416 ± 0.032 3.66 ± 0.19 1.00<br />
NGC 4486 1909 187.73708 12.36813 1.45 −6.975 ± 0.036 −8.331 ± 0.031 2.45 ± 0.22 1.00<br />
NGC 4486 1910 187.73715 12.41444 1.46 −5.452 ± 0.165 −6.387 ± 0.393 2.75 ± 0.68 0.98<br />
NGC 4486 1911 187.73718 12.38198 1.21 −6.968 ± 0.033 −8.066 ± 0.044 2.56 ± 0.18 1.00<br />
NGC 4486 1912 187.73723 12.37752 1.27 −5.112 ± 0.132 −6.209 ± 0.090 2.31 ± 0.50 0.99<br />
NGC 4486 1913 187.73732 12.39215 1.16 −9.465 ± 0.015 −10.469 ± 0.015 2.73 ± 0.10 1.00<br />
NGC 4486 1914 187.73732 12.39614 1.18 −7.010 ± 0.027 −7.980 ± 1.790 2.03 ± 0.31 1.00<br />
NGC 4486 1915 187.73746 12.38809 1.17 −8.482 ± 0.021 −9.332 ± 0.025 2.57 ± 0.20 1.00<br />
NGC 4486 1916 187.73749 12.36671 1.49 −8.209 ± 0.021 −9.407 ± 0.023 2.56 ± 0.23 1.00<br />
NGC 4486 1917 187.73743 12.40110 1.23 −5.933 ± 0.067 −7.455 ± 0.960 1.97 ± 0.42 1.00<br />
NGC 4486 1918 187.73746 12.38145 1.22 −5.903 ± 0.082 −6.804 ± 0.121 2.35 ± 0.61 0.99<br />
NGC 4486 1919 187.73752 12.40334 1.26 −7.658 ± 0.039 −8.611 ± 0.035 3.33 ± 0.22 1.00<br />
NGC 4486 1921 187.73761 12.40708 1.32 −8.112 ± 0.018 −8.925 ± 0.020 3.23 ± 0.09 1.00<br />
NGC 4486 1922 187.73760 12.37044 1.41 −5.505 ± 0.784 −6.792 ± 0.539 1.09 ± 0.65 0.89<br />
NGC 4486 1923 187.73769 12.36591 1.52 −9.848 ± 0.012 −10.907 ± 0.014 3.48 ± 0.07 1.00<br />
NGC 4486 1924 187.73763 12.38677 1.19 −6.768 ± 0.034 −8.113 ± 0.038 1.94 ± 0.22 1.00<br />
NGC 4486 1926 187.73773 12.38564 1.20 −6.637 ± 0.033 −7.811 ± 0.040 2.48 ± 0.16 1.00<br />
NGC 4486 1928 187.73776 12.41139 1.41 −7.668 ± 0.026 −8.526 ± 0.032 2.70 ± 0.20 1.00<br />
NGC 4486 1931 187.73796 12.41298 1.45 −7.845 ± 0.034 −9.265 ± 0.025 2.36 ± 0.14 1.00<br />
NGC 4486 1933 187.73789 12.39090 1.18 −8.762 ± 0.026 −9.856 ± 0.017 2.85 ± 0.17 1.00<br />
NGC 4486 1934 187.73796 12.40053 1.24 −9.233 ± 0.012 −10.198 ± 0.020 3.03 ± 0.13 1.00<br />
NGC 4486 1935 187.73799 12.41861 1.58 −9.334 ± 0.025 −10.215 ± 0.021 5.12 ± 0.13 1.00<br />
Continued on Next Page. . .<br />
368
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4486 1936 187.73801 12.42004 1.62 −9.501 ± 0.024 −10.628 ± 0.012 3.18 ± 0.12 1.00<br />
NGC 4486 1937 187.73793 12.41279 1.44 −5.702 ± 0.074 −6.469 ± 0.124 2.71 ± 0.38 0.98<br />
NGC 4486 1938 187.73792 12.39349 1.19 −6.024 ± 0.086 −7.346 ± 0.088 3.62 ± 0.52 0.98<br />
NGC 4486 1939 187.73827 12.38881 1.20 −9.729 ± 0.018 −10.801 ± 0.013 3.63 ± 0.08 1.00<br />
NGC 4486 1940 187.73807 12.40726 1.34 −8.053 ± 0.020 −9.048 ± 0.033 3.04 ± 0.19 1.00<br />
NGC 4486 1941 187.73837 12.41097 1.42 −7.336 ± 0.024 −8.517 ± 0.026 2.35 ± 0.15 1.00<br />
NGC 4486 1943 187.73848 12.37110 1.43 −5.662 ± 0.074 −6.926 ± 0.188 5.00 ± 0.96 0.76<br />
NGC 4486 1945 187.73859 12.37961 1.29 −7.872 ± 0.015 −9.279 ± 0.019 2.19 ± 0.14 1.00<br />
NGC 4486 1948 187.73876 12.36988 1.46 −7.236 ± 0.067 −7.900 ± 0.097 5.06 ± 0.50 0.96<br />
NGC 4486 1949 187.73883 12.38049 1.28 −7.944 ± 0.027 −9.055 ± 0.028 2.89 ± 0.17 1.00<br />
NGC 4486 1950 187.73889 12.38117 1.28 −8.626 ± 0.022 −9.424 ± 0.021 3.24 ± 0.15 1.00<br />
NGC 4486 1951 187.73888 12.41304 1.48 −7.506 ± 0.030 −8.700 ± 0.031 2.62 ± 0.22 1.00<br />
NGC 4486 1954 187.73897 12.41912 1.62 −7.055 ± 0.427 −8.473 ± 0.383 2.23 ± 0.56 1.00<br />
NGC 4486 1955 187.73903 12.40807 1.39 −6.188 ± 0.085 −7.793 ± 0.057 3.03 ± 0.45 1.00<br />
NGC 4486 1959 187.73935 12.41059 1.44 −8.278 ± 0.020 −9.155 ± 0.035 3.29 ± 0.15 1.00<br />
NGC 4486 1960 187.73937 12.36363 1.62 −9.268 ± 0.017 −10.170 ± 0.024 2.98 ± 0.17 1.00<br />
NGC 4486 1961 187.73938 12.39933 1.28 −8.118 ± 0.018 −9.557 ± 0.017 2.51 ± 0.10 1.00<br />
NGC 4486 1962 187.73937 12.41138 1.46 −5.615 ± 0.068 −6.787 ± 0.071 2.57 ± 0.36 0.99<br />
NGC 4486 1963 187.73813 12.38181 1.24 −7.937 ± 0.028 −9.231 ± 0.020 2.68 ± 0.15 1.00<br />
NGC 4486 1964 187.73950 12.38662 1.26 −8.527 ± 0.009 −9.869 ± 0.014 2.49 ± 0.09 1.00<br />
NGC 4486 1967 187.73966 12.41413 1.52 −7.530 ± 0.031 −8.927 ± 0.021 2.66 ± 0.19 1.00<br />
NGC 4486 1968 187.73979 12.38900 1.26 −6.129 ± 0.046 −7.635 ± 0.055 2.19 ± 0.29 1.00<br />
NGC 4486 1969 187.73981 12.40566 1.37 −5.423 ± 0.420 −6.929 ± 0.059 2.05 ± 0.34 0.99<br />
NGC 4486 1970 187.73996 12.38074 1.32 −8.940 ± 0.036 −9.773 ± 0.016 2.83 ± 0.15 1.00<br />
NGC 4486 1972 187.74007 12.38188 1.31 −6.511 ± 0.045 −7.541 ± 0.103 4.50 ± 0.58 0.95<br />
NGC 4486 1974 187.74036 12.39128 1.28 −9.209 ± 0.010 −10.167 ± 0.016 3.01 ± 0.09 1.00<br />
NGC 4486 1975 187.74036 12.39629 1.29 −8.181 ± 0.022 −9.602 ± 0.020 2.36 ± 0.13 1.00<br />
NGC 4486 1976 187.74045 12.40608 1.40 −6.732 ± 0.059 −7.974 ± 0.051 3.15 ± 0.22 1.00<br />
NGC 4486 1977 187.74052 12.38545 1.30 −9.067 ± 0.020 −9.956 ± 0.016 3.42 ± 0.15 1.00<br />
NGC 4486 1979 187.74060 12.37369 1.45 −9.174 ± 0.014 −10.163 ± 0.020 2.81 ± 0.09 1.00<br />
NGC 4486 1981 187.74056 12.36385 1.65 −5.913 ± 0.128 −7.133 ± 0.126 5.64 ± 0.72 0.71<br />
NGC 4486 1982 187.74063 12.38663 1.30 −7.252 ± 0.040 −8.048 ± 0.047 3.51 ± 0.24 0.99<br />
NGC 4486 1983 187.74066 12.39003 1.29 −6.898 ± 0.046 −7.829 ± 0.058 4.16 ± 0.26 0.98<br />
NGC 4486 1984 187.74071 12.39224 1.29 −8.206 ± 0.023 −9.580 ± 0.019 3.06 ± 0.12 1.00<br />
NGC 4486 1985 187.74075 12.40296 1.37 −8.013 ± 0.046 −8.965 ± 0.067 5.16 ± 0.28 0.99<br />
NGC 4486 1986 187.74088 12.41522 1.59 −9.058 ± 0.280 −10.432 ± 0.032 2.28 ± 0.34 1.00<br />
NGC 4486 1987 187.74093 12.38786 1.30 −9.533 ± 0.020 −10.802 ± 0.021 3.62 ± 0.13 1.00<br />
NGC 4486 1988 187.74095 12.36578 1.62 −8.522 ± 0.045 −9.752 ± 0.038 4.48 ± 0.26 1.00<br />
NGC 4486 1990 187.74107 12.37790 1.40 −8.512 ± 0.020 −9.584 ± 0.019 2.84 ± 0.13 1.00<br />
NGC 4486 1991 187.74115 12.40751 1.45 −9.101 ± 0.022 −10.640 ± 0.016 4.97 ± 0.15 1.00<br />
NGC 4486 1992 187.74124 12.38213 1.35 −8.174 ± 0.028 −9.021 ± 0.038 3.29 ± 0.19 1.00<br />
NGC 4486 1993 187.74135 12.41719 1.64 −7.728 ± 0.057 −9.027 ± 0.105 3.11 ± 0.35 1.00<br />
NGC 4486 1995 187.74132 12.41939 1.69 −5.118 ± 0.162 −6.247 ± 0.295 4.95 ± 1.72 0.70<br />
NGC 4486 1996 187.74149 12.40747 1.46 −9.693 ± 0.016 −10.915 ± 0.013 3.07 ± 0.09 1.00<br />
NGC 4486 1997 187.74154 12.41713 1.65 −8.024 ± 0.027 −9.175 ± 0.031 3.48 ± 0.17 1.00<br />
NGC 4526 1 188.53656 7.69903 1.94 −6.872 ± 0.111 −8.270 ± 0.057 4.67 ± 0.53 0.92<br />
NGC 4526 2 188.54054 7.71130 2.46 −6.777 ± 0.069 −7.739 ± 0.204 4.49 ± 1.21 0.79<br />
NGC 4526 10 188.53103 7.68715 1.79 −4.867 ± 0.465 −6.641 ± 0.177 3.08 ± 4.83 0.76<br />
NGC 4526 12 188.53250 7.69182 1.72 −6.605 ± 0.685 −7.321 ± 0.681 1.77 ± 0.68 0.86<br />
NGC 4526 14 188.53311 7.69415 1.71 −9.344 ± 0.026 −10.272 ± 0.033 4.49 ± 0.16 1.00<br />
NGC 4526 22 188.53184 7.69171 1.68 −7.586 ± 0.033 −9.119 ± 0.026 2.62 ± 0.14 1.00<br />
NGC 4526 24 188.53134 7.69111 1.66 −5.666 ± 0.189 −7.403 ± 0.175 4.38 ± 1.20 0.70<br />
NGC 4526 25 188.53283 7.69590 1.66 −8.447 ± 0.018 −9.292 ± 0.027 2.56 ± 0.14 1.00<br />
NGC 4526 31 188.53610 7.70586 1.97 −8.200 ± 0.036 −9.473 ± 0.025 4.56 ± 0.18 1.00<br />
NGC 4526 32 188.53461 7.70160 1.79 −6.575 ± 0.071 −7.404 ± 0.089 3.57 ± 0.42 0.86<br />
NGC 4526 33 188.52916 7.68661 1.70 −7.143 ± 0.092 −8.243 ± 0.030 5.72 ± 0.36 0.63<br />
NGC 4526 36 188.52941 7.68807 1.64 −6.236 ± 0.060 −7.601 ± 0.086 2.95 ± 0.37 0.95<br />
NGC 4526 37 188.53346 7.69981 1.69 −8.169 ± 0.026 −9.545 ± 0.027 3.98 ± 0.18 1.00<br />
NGC 4526 38 188.52792 7.68404 1.76 −7.015 ± 0.036 −8.009 ± 0.060 3.29 ± 0.27 0.96<br />
NGC 4526 50 188.53276 7.70021 1.64 −6.789 ± 0.046 −8.037 ± 0.066 3.90 ± 0.32 0.95<br />
NGC 4526 54 188.52884 7.68980 1.53 −5.669 ± 0.136 −7.343 ± 0.231 4.34 ± 2.54 0.68<br />
Continued on Next Page. . .<br />
369
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4526 58 188.53117 7.69709 1.52 −6.861 ± 0.045 −8.328 ± 0.090 3.37 ± 0.36 1.00<br />
NGC 4526 62 188.53046 7.69737 1.46 −7.371 ± 0.040 −8.710 ± 0.042 3.61 ± 0.24 1.00<br />
NGC 4526 69 188.52714 7.68916 1.44 −7.493 ± 0.036 −8.426 ± 0.056 2.81 ± 0.28 1.00<br />
NGC 4526 76 188.52484 7.68340 1.63 −6.816 ± 0.098 −8.031 ± 0.050 5.56 ± 0.55 0.67<br />
NGC 4526 81 188.52564 7.68782 1.41 −6.068 ± 0.062 −7.788 ± 0.108 4.09 ± 0.48 0.89<br />
NGC 4526 83 188.52693 7.69164 1.32 −7.693 ± 0.035 −9.076 ± 0.020 2.00 ± 0.15 1.00<br />
NGC 4526 88 188.52550 7.68833 1.38 −8.237 ± 0.019 −9.594 ± 0.019 2.31 ± 0.13 1.00<br />
NGC 4526 91 188.52548 7.68917 1.33 −7.360 ± 0.049 −8.537 ± 0.075 4.75 ± 0.34 0.95<br />
NGC 4526 92 188.52690 7.69347 1.26 −7.791 ± 0.039 −8.697 ± 0.061 3.60 ± 0.23 1.00<br />
NGC 4526 94 188.52711 7.69419 1.25 −7.245 ± 0.041 −8.228 ± 0.039 1.81 ± 0.20 1.00<br />
NGC 4526 98 188.52411 7.68652 1.40 −7.481 ± 0.028 −8.597 ± 0.049 2.70 ± 0.16 1.00<br />
NGC 4526 100 188.52779 7.69695 1.25 −6.636 ± 0.037 −7.925 ± 0.058 3.23 ± 0.31 0.96<br />
NGC 4526 107 188.52617 7.69326 1.21 −7.012 ± 0.050 −8.268 ± 0.044 2.74 ± 0.23 1.00<br />
NGC 4526 119 188.52548 7.69268 1.18 −5.755 ± 0.783 −7.385 ± 0.155 1.89 ± 0.69 0.91<br />
NGC 4526 121 188.52511 7.69195 1.18 −8.504 ± 0.020 −9.868 ± 0.015 2.18 ± 0.09 1.00<br />
NGC 4526 131 188.52679 7.69819 1.16 −7.740 ± 0.024 −8.611 ± 0.034 2.52 ± 0.17 1.00<br />
NGC 4526 132 188.52315 7.68804 1.26 −7.129 ± 0.034 −8.315 ± 0.018 1.94 ± 0.16 1.00<br />
NGC 4526 137 188.52501 7.69382 1.11 −6.346 ± 0.062 −7.840 ± 0.094 2.79 ± 0.59 0.97<br />
NGC 4526 138 188.52430 7.69194 1.13 −8.179 ± 0.018 −9.078 ± 0.030 2.97 ± 0.11 1.00<br />
NGC 4526 139 188.52165 7.68478 1.39 −9.165 ± 0.012 −9.967 ± 0.013 3.10 ± 0.08 1.00<br />
NGC 4526 141 188.52621 7.69785 1.11 −5.908 ± 0.200 −7.484 ± 0.099 4.82 ± 0.85 0.60<br />
NGC 4526 145 188.52330 7.69036 1.14 −8.001 ± 0.022 −9.203 ± 0.025 2.46 ± 0.15 1.00<br />
NGC 4526 147 188.52484 7.69503 1.06 −6.073 ± 0.124 −6.617 ± 0.191 2.37 ± 0.56 0.83<br />
NGC 4526 155 188.52380 7.69374 1.02 −6.422 ± 0.114 −8.035 ± 0.068 4.89 ± 0.44 0.82<br />
NGC 4526 156 188.52738 7.70426 1.27 −8.516 ± 0.026 −9.395 ± 0.026 3.90 ± 0.17 1.00<br />
NGC 4526 160 188.52429 7.69636 0.98 −5.697 ± 0.238 −7.007 ± 0.131 4.26 ± 1.23 0.52<br />
NGC 4526 163 188.52574 7.70099 1.08 −9.183 ± 0.020 −10.174 ± 0.014 2.88 ± 0.08 1.00<br />
NGC 4526 169 188.52272 7.69320 0.97 −8.762 ± 0.019 −10.017 ± 0.021 2.89 ± 0.13 1.00<br />
NGC 4526 174 188.52515 7.70054 1.03 −6.091 ± 0.089 −7.780 ± 0.096 5.70 ± 0.65 0.55<br />
NGC 4526 178 188.52129 7.69054 1.01 −8.414 ± 0.023 −9.296 ± 0.031 2.40 ± 0.31 1.00<br />
NGC 4526 179 188.52556 7.70274 1.09 −7.391 ± 0.024 −8.801 ± 0.038 2.35 ± 0.14 1.00<br />
NGC 4526 181 188.52560 7.70319 1.10 −7.464 ± 0.017 −8.875 ± 0.021 2.23 ± 0.14 1.00<br />
NGC 4526 184 188.52300 7.69625 0.88 −9.667 ± 0.030 −10.580 ± 0.030 3.91 ± 0.16 1.00<br />
NGC 4526 188 188.52150 7.69256 0.91 −8.005 ± 0.023 −9.204 ± 0.024 2.75 ± 0.15 1.00<br />
NGC 4526 190 188.51532 7.67506 1.98 −6.621 ± 0.047 −7.320 ± 0.074 3.66 ± 0.28 0.82<br />
NGC 4526 197 188.52327 7.69837 0.87 −4.819 ± 0.536 −6.256 ± 0.399 3.05 ± 0.84 0.68<br />
NGC 4526 198 188.52386 7.70034 0.92 −7.048 ± 0.046 −8.347 ± 0.035 1.79 ± 0.25 1.00<br />
NGC 4526 203 188.52780 7.71256 1.64 −5.591 ± 0.087 −6.363 ± 0.080 2.29 ± 0.33 0.76<br />
NGC 4526 204 188.51883 7.68726 1.11 −8.769 ± 0.020 −9.601 ± 0.015 2.14 ± 0.11 1.00<br />
NGC 4526 206 188.51884 7.68752 1.09 −4.954 ± 0.521 −6.681 ± 0.138 3.60 ± 0.80 0.63<br />
NGC 4526 210 188.51780 7.68518 1.23 −6.005 ± 0.057 −7.382 ± 0.131 2.74 ± 0.66 0.94<br />
NGC 4526 212 188.52340 7.70160 0.90 −8.208 ± 0.029 −9.640 ± 0.025 2.04 ± 0.19 1.00<br />
NGC 4526 216 188.52010 7.69351 0.78 −5.873 ± 0.294 −7.573 ± 0.212 4.12 ± 1.18 0.83<br />
NGC 4526 218 188.51851 7.69034 0.88 −7.205 ± 0.034 −8.457 ± 0.042 2.89 ± 0.23 1.00<br />
NGC 4526 225 188.51845 7.69256 0.73 −7.368 ± 0.035 −8.729 ± 0.042 2.21 ± 0.45 1.00<br />
NGC 4526 231 188.51849 7.69414 0.64 −8.502 ± 0.044 −9.335 ± 0.048 6.37 ± 0.22 0.93<br />
NGC 4526 234 188.52802 7.72231 2.25 −9.673 ± 0.018 −10.516 ± 0.016 3.42 ± 0.10 1.00<br />
NGC 4526 237 188.51601 7.68834 0.94 −8.143 ± 0.026 −9.379 ± 0.027 2.90 ± 0.17 1.00<br />
NGC 4526 238 188.51909 7.69712 0.56 −7.643 ± 0.036 −9.216 ± 0.019 1.50 ± 0.23 0.80<br />
NGC 4526 239 188.51874 7.69608 0.57 −6.905 ± 0.047 −7.805 ± 0.074 3.56 ± 0.25 0.93<br />
NGC 4526 242 188.52077 7.70245 0.72 −7.833 ± 0.029 −8.942 ± 0.039 3.27 ± 0.20 1.00<br />
NGC 4526 245 188.52446 7.71408 1.54 −7.387 ± 0.026 −8.383 ± 0.024 1.94 ± 0.14 1.00<br />
NGC 4526 249 188.50967 7.67309 2.14 −8.917 ± 0.027 −9.849 ± 0.014 3.10 ± 0.09 1.00<br />
NGC 4526 251 188.51782 7.69630 0.50 −7.833 ± 0.038 −9.384 ± 0.030 2.36 ± 0.16 1.00<br />
NGC 4526 253 188.51976 7.70219 0.63 −8.800 ± 0.046 −10.365 ± 0.042 9.25 ± 0.48 0.56<br />
NGC 4526 254 188.51889 7.69975 0.52 −8.299 ± 0.028 −9.301 ± 0.024 2.10 ± 0.11 1.00<br />
NGC 4526 256 188.52237 7.70178 0.82 −7.724 ± 0.047 −8.506 ± 0.054 3.94 ± 0.26 1.00<br />
NGC 4526 257 188.51915 7.70090 0.55 −8.705 ± 0.020 −9.981 ± 0.015 2.01 ± 0.09 1.00<br />
NGC 4526 258 188.51919 7.70127 0.56 −7.804 ± 0.026 −8.526 ± 0.029 2.06 ± 0.17 1.00<br />
NGC 4526 260 188.51886 7.70084 0.53 −5.619 ± 0.463 −7.504 ± 0.190 1.45 ± 0.45 0.71<br />
NGC 4526 264 188.51428 7.68914 0.84 −7.193 ± 0.306 −8.812 ± 0.041 3.12 ± 0.38 1.00<br />
NGC 4526 270 188.51020 7.68000 1.58 −7.274 ± 0.051 −8.118 ± 0.053 4.11 ± 0.21 1.00<br />
Continued on Next Page. . .<br />
370
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4526 272 188.51699 7.69944 0.37 −8.775 ± 0.050 −9.698 ± 0.068 4.52 ± 0.28 1.00<br />
NGC 4526 279 188.51264 7.68804 0.92 −6.608 ± 0.042 −7.923 ± 0.069 2.79 ± 0.46 0.97<br />
NGC 4526 280 188.51276 7.68861 0.87 −7.690 ± 0.032 −9.065 ± 0.025 3.68 ± 0.17 1.00<br />
NGC 4526 283 188.51269 7.68936 0.81 −7.740 ± 0.026 −9.083 ± 0.027 1.93 ± 0.20 1.00<br />
NGC 4526 284 188.51160 7.68657 1.04 −8.413 ± 0.026 −9.325 ± 0.014 2.51 ± 0.16 1.00<br />
NGC 4526 285 188.51523 7.69688 0.30 −7.393 ± 0.049 −8.966 ± 0.080 3.86 ± 0.32 1.00<br />
NGC 4526 291 188.51816 7.70589 0.70 −5.930 ± 0.136 −6.432 ± 0.507 2.38 ± 1.97 0.78<br />
NGC 4526 292 188.51793 7.70545 0.66 −7.721 ± 0.040 −8.483 ± 0.036 1.93 ± 0.22 1.00<br />
NGC 4526 293 188.51741 7.70403 0.55 −7.706 ± 0.041 −8.749 ± 0.029 1.58 ± 0.19 1.00<br />
NGC 4526 295 188.51250 7.69154 0.63 −7.410 ± 0.043 −8.920 ± 0.027 2.78 ± 0.18 1.00<br />
NGC 4526 296 188.50795 7.67884 1.70 −7.657 ± 0.027 −8.887 ± 0.030 2.90 ± 0.27 1.00<br />
NGC 4526 299 188.52009 7.71416 1.35 −5.488 ± 0.113 −6.140 ± 0.190 2.35 ± 0.47 0.71<br />
NGC 4526 300 188.51564 7.70163 0.32 −6.537 ± 1.089 −7.427 ± 0.387 1.62 ± 0.74 0.81<br />
NGC 4526 303 188.51358 7.69628 0.26 −7.250 ± 0.096 −8.355 ± 0.496 1.48 ± 0.37 0.82<br />
NGC 4526 305 188.51797 7.70899 0.90 −7.216 ± 0.055 −8.454 ± 0.043 3.53 ± 0.23 1.00<br />
NGC 4526 307 188.50949 7.68562 1.14 −6.720 ± 0.042 −7.592 ± 0.030 2.54 ± 0.26 0.96<br />
NGC 4526 308 188.51640 7.70544 0.59 −5.149 ± 0.487 −6.568 ± 0.197 2.65 ± 1.60 0.80<br />
NGC 4526 309 188.52048 7.69709 0.67 −6.820 ± 0.105 −7.908 ± 0.101 4.99 ± 0.74 0.75<br />
NGC 4526 314 188.51312 7.69726 0.18 −7.032 ± 0.073 −8.301 ± 0.371 2.83 ± 0.44 1.00<br />
NGC 4526 316 188.51329 7.69782 0.14 −7.810 ± 0.038 −8.527 ± 0.054 2.27 ± 0.23 1.00<br />
NGC 4526 326 188.51449 7.70326 0.36 −7.910 ± 0.021 −9.362 ± 0.022 2.12 ± 0.20 1.00<br />
NGC 4526 328 188.50937 7.68920 0.86 −7.776 ± 0.023 −8.784 ± 0.036 3.47 ± 0.16 1.00<br />
NGC 4526 330 188.52162 7.72457 2.18 −6.078 ± 0.094 −7.015 ± 0.044 1.88 ± 0.43 0.85<br />
NGC 4526 333 188.51568 7.70835 0.78 −6.702 ± 0.045 −8.043 ± 0.038 1.62 ± 0.23 0.88<br />
NGC 4526 334 188.50923 7.69024 0.78 −5.527 ± 0.693 −6.340 ± 0.143 2.56 ± 0.52 0.75<br />
NGC 4526 336 188.51641 7.71135 1.02 −7.711 ± 0.031 −8.729 ± 0.058 3.87 ± 0.22 1.00<br />
NGC 4526 340 188.51313 7.70250 0.26 −9.018 ± 0.025 −10.224 ± 0.034 2.36 ± 0.16 1.00<br />
NGC 4526 342 188.51663 7.71327 1.18 −9.051 ± 0.033 −9.986 ± 0.029 5.46 ± 0.13 1.00<br />
NGC 4526 343 188.51115 7.69743 0.19 −7.197 ± 0.043 −8.333 ± 0.154 2.02 ± 0.35 1.00<br />
NGC 4526 346 188.51268 7.70221 0.23 −9.111 ± 0.022 −10.568 ± 0.020 1.94 ± 0.14 1.00<br />
NGC 4526 352 188.51489 7.70959 0.86 −6.952 ± 0.041 −8.055 ± 0.040 2.90 ± 0.18 0.97<br />
NGC 4526 354 188.51905 7.69326 0.73 −7.884 ± 0.028 −8.694 ± 0.043 2.32 ± 0.29 1.00<br />
NGC 4526 357 188.50238 7.67467 2.16 −6.733 ± 0.054 −7.538 ± 0.063 2.38 ± 0.31 0.96<br />
NGC 4526 361 188.50597 7.68539 1.25 −7.417 ± 0.031 −8.701 ± 0.032 2.98 ± 0.17 1.00<br />
NGC 4526 363 188.50363 7.67894 1.80 −7.155 ± 0.049 −8.242 ± 0.049 3.29 ± 0.24 1.00<br />
NGC 4526 366 188.50924 7.69499 0.44 −7.504 ± 0.039 −8.950 ± 0.043 2.50 ± 0.29 1.00<br />
NGC 4526 368 188.50797 7.69167 0.72 −6.237 ± 0.066 −7.197 ± 0.030 2.65 ± 0.38 0.92<br />
NGC 4526 373 188.51210 7.70417 0.39 −7.409 ± 0.045 −8.855 ± 0.040 1.54 ± 0.32 0.85<br />
NGC 4526 376 188.51236 7.70601 0.54 −7.603 ± 0.031 −8.664 ± 0.031 1.61 ± 0.20 1.00<br />
NGC 4526 378 188.50337 7.68100 1.66 −6.721 ± 0.051 −7.920 ± 0.042 3.30 ± 0.25 0.95<br />
NGC 4526 379 188.50570 7.68781 1.08 −9.432 ± 0.025 −10.268 ± 0.013 3.67 ± 0.09 1.00<br />
NGC 4526 381 188.51183 7.70562 0.51 −7.934 ± 0.037 −8.712 ± 0.037 2.61 ± 0.20 1.00<br />
NGC 4526 384 188.50889 7.69810 0.30 −6.318 ± 0.376 −7.735 ± 0.071 2.52 ± 0.70 0.97<br />
NGC 4526 385 188.50821 7.69622 0.42 −7.587 ± 0.031 −8.763 ± 0.050 3.10 ± 0.23 1.00<br />
NGC 4526 386 188.51209 7.70746 0.66 −8.311 ± 0.016 −9.156 ± 0.027 2.85 ± 0.15 1.00<br />
NGC 4526 387 188.51146 7.70567 0.52 −7.860 ± 0.033 −9.349 ± 0.025 1.79 ± 0.16 1.00<br />
NGC 4526 390 188.50879 7.69874 0.30 −6.967 ± 0.045 −8.135 ± 0.050 2.64 ± 0.33 1.00<br />
NGC 4526 392 188.50862 7.69857 0.31 −7.487 ± 0.039 −8.827 ± 0.022 1.86 ± 0.17 1.00<br />
NGC 4526 396 188.51069 7.70546 0.52 −8.715 ± 0.023 −9.631 ± 0.013 2.36 ± 0.14 1.00<br />
NGC 4526 399 188.51154 7.70828 0.73 −4.860 ± 0.189 −6.431 ± 0.114 3.23 ± 0.55 0.68<br />
NGC 4526 402 188.51329 7.71414 1.20 −8.593 ± 0.023 −9.747 ± 0.014 2.48 ± 0.12 1.00<br />
NGC 4526 403 188.50744 7.69761 0.43 −6.652 ± 0.067 −8.021 ± 0.046 1.26 ± 0.39 0.58<br />
NGC 4526 407 188.50816 7.70011 0.35 −6.921 ± 0.065 −7.719 ± 0.047 1.83 ± 0.26 0.94<br />
NGC 4526 410 188.51456 7.71882 1.59 −5.996 ± 0.447 −7.015 ± 0.656 2.02 ± 0.51 0.90<br />
NGC 4526 414 188.50812 7.70152 0.39 −6.940 ± 0.048 −7.990 ± 0.052 2.30 ± 0.24 0.98<br />
NGC 4526 417 188.50938 7.70840 0.78 −8.235 ± 0.030 −9.691 ± 0.015 1.35 ± 0.10 0.63<br />
NGC 4526 418 188.50842 7.70556 0.60 −7.347 ± 0.083 −8.656 ± 0.072 4.73 ± 0.36 0.96<br />
NGC 4526 422 188.50633 7.70030 0.50 −7.312 ± 0.050 −8.354 ± 0.060 2.19 ± 0.30 1.00<br />
NGC 4526 427 188.50851 7.70718 0.71 −6.929 ± 0.038 −8.236 ± 0.032 2.42 ± 0.25 1.00<br />
NGC 4526 428 188.50893 7.70858 0.80 −6.263 ± 0.057 −6.942 ± 0.109 3.39 ± 0.35 0.76<br />
NGC 4526 436 188.51233 7.72042 1.71 −7.365 ± 0.033 −8.213 ± 0.031 2.85 ± 0.22 1.00<br />
NGC 4526 439 188.50621 7.70338 0.60 −7.066 ± 0.052 −8.548 ± 0.055 2.28 ± 0.32 1.00<br />
Continued on Next Page. . .<br />
371
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4526 440 188.50994 7.71432 1.23 −9.043 ± 0.013 −9.921 ± 0.012 2.90 ± 0.10 1.00<br />
NGC 4526 443 188.50670 7.70612 0.72 −8.238 ± 0.035 −9.668 ± 0.020 3.03 ± 0.19 1.00<br />
NGC 4526 444 188.50586 7.70366 0.63 −7.299 ± 0.055 −8.040 ± 0.051 3.52 ± 0.21 0.95<br />
NGC 4526 445 188.49682 7.67801 2.14 −5.997 ± 0.082 −7.131 ± 0.059 2.28 ± 0.31 0.93<br />
NGC 4526 447 188.50673 7.70730 0.79 −6.767 ± 0.069 −8.395 ± 0.113 4.59 ± 0.60 0.95<br />
NGC 4526 452 188.50536 7.70509 0.74 −7.889 ± 0.031 −8.838 ± 0.035 1.46 ± 0.22 0.80<br />
NGC 4526 455 188.50723 7.71097 1.03 −8.666 ± 0.018 −9.602 ± 0.016 2.59 ± 0.08 1.00<br />
NGC 4526 457 188.50468 7.70373 0.72 −7.226 ± 0.163 −7.895 ± 0.180 5.33 ± 1.16 0.69<br />
NGC 4526 458 188.50248 7.69802 0.81 −5.962 ± 0.134 −7.174 ± 0.217 3.24 ± 1.31 0.85<br />
NGC 4526 459 188.50758 7.71315 1.19 −8.224 ± 0.022 −9.732 ± 0.016 2.66 ± 0.11 1.00<br />
NGC 4526 461 188.50313 7.70051 0.75 −6.953 ± 0.327 −8.418 ± 0.261 1.77 ± 0.30 1.00<br />
NGC 4526 463 188.50523 7.70684 0.84 −6.873 ± 0.028 −8.241 ± 0.328 2.08 ± 0.31 1.00<br />
NGC 4526 465 188.49816 7.68707 1.52 −8.606 ± 0.034 −9.950 ± 0.033 4.51 ± 0.21 1.00<br />
NGC 4526 466 188.50539 7.70782 0.89 −8.360 ± 0.025 −9.844 ± 0.022 2.76 ± 0.19 1.00<br />
NGC 4526 469 188.50735 7.71379 1.24 −8.222 ± 0.021 −9.020 ± 0.029 3.82 ± 0.13 1.00<br />
NGC 4526 471 188.50249 7.70008 0.80 −9.292 ± 0.023 −10.681 ± 0.017 2.71 ± 0.12 1.00<br />
NGC 4526 484 188.49948 7.69555 1.09 −8.406 ± 0.017 −9.297 ± 0.020 2.16 ± 0.15 1.00<br />
NGC 4526 485 188.50110 7.70030 0.92 −5.159 ± 0.509 −6.645 ± 0.131 3.35 ± 0.99 0.69<br />
NGC 4526 490 188.50182 7.70318 0.91 −5.309 ± 1.211 −6.686 ± 0.115 2.34 ± 0.50 0.85<br />
NGC 4526 491 188.50687 7.71819 1.59 −8.598 ± 0.023 −9.810 ± 0.022 3.74 ± 0.15 1.00<br />
NGC 4526 497 188.49980 7.69843 1.02 −6.149 ± 0.052 −7.154 ± 0.257 2.52 ± 0.37 0.93<br />
NGC 4526 498 188.50175 7.70433 0.95 −7.734 ± 0.047 −9.284 ± 0.026 3.40 ± 0.22 1.00<br />
NGC 4526 508 188.50070 7.70313 0.99 −8.248 ± 0.024 −9.198 ± 0.025 2.66 ± 0.14 1.00<br />
NGC 4526 512 188.50172 7.70623 1.03 −6.984 ± 0.034 −8.368 ± 0.044 1.92 ± 0.21 1.00<br />
NGC 4526 513 188.50282 7.70949 1.13 −7.745 ± 0.020 −9.236 ± 0.035 4.13 ± 0.14 1.00<br />
NGC 4526 517 188.49974 7.70124 1.03 −8.056 ± 0.025 −9.346 ± 0.025 2.35 ± 0.18 1.00<br />
NGC 4526 519 188.49821 7.69771 1.15 −7.429 ± 0.056 −8.295 ± 0.040 3.16 ± 0.38 1.00<br />
NGC 4526 527 188.49681 7.69539 1.30 −8.781 ± 0.032 −9.954 ± 0.020 2.75 ± 0.15 1.00<br />
NGC 4526 534 188.49968 7.70522 1.13 −7.663 ± 0.045 −9.046 ± 0.030 1.53 ± 0.23 0.83<br />
NGC 4526 535 188.50862 7.73092 2.58 −7.017 ± 0.042 −8.054 ± 0.054 4.69 ± 0.19 0.86<br />
NGC 4526 539 188.49792 7.70194 1.19 −8.746 ± 0.023 −9.679 ± 0.021 3.72 ± 0.18 1.00<br />
NGC 4526 545 188.49956 7.70767 1.24 −7.381 ± 0.194 −8.878 ± 0.064 7.55 ± 1.48 0.50<br />
NGC 4526 553 188.49631 7.70078 1.30 −7.786 ± 0.013 −9.040 ± 0.036 1.20 ± 0.17 0.54<br />
NGC 4526 557 188.49839 7.70755 1.31 −5.625 ± 0.153 −6.651 ± 0.095 3.21 ± 0.68 0.73<br />
NGC 4526 558 188.49685 7.70320 1.29 −7.448 ± 0.036 −8.192 ± 0.035 1.76 ± 0.19 1.00<br />
NGC 4526 565 188.49666 7.70375 1.32 −7.984 ± 0.041 −9.122 ± 0.030 3.18 ± 0.16 1.00<br />
NGC 4526 566 188.48941 7.68365 2.25 −8.108 ± 0.021 −9.105 ± 0.020 2.83 ± 0.12 1.00<br />
NGC 4526 569 188.49915 7.71200 1.48 −8.218 ± 0.024 −9.650 ± 0.022 2.28 ± 0.14 1.00<br />
NGC 4526 572 188.49600 7.70350 1.36 −7.693 ± 0.033 −8.665 ± 0.044 2.66 ± 0.20 1.00<br />
NGC 4526 579 188.49698 7.70721 1.40 −7.172 ± 0.027 −8.082 ± 0.056 2.42 ± 0.28 0.98<br />
NGC 4526 580 188.49126 7.69048 1.85 −6.449 ± 0.049 −8.014 ± 0.102 4.63 ± 0.49 0.86<br />
NGC 4526 584 188.49806 7.71142 1.52 −5.968 ± 0.484 −7.427 ± 3.506 1.40 ± 0.40 0.65<br />
NGC 4526 585 188.50122 7.72068 1.95 −8.143 ± 0.026 −9.466 ± 0.021 3.70 ± 0.14 1.00<br />
NGC 4526 588 188.50140 7.72137 2.00 −6.620 ± 0.036 −7.615 ± 0.085 2.37 ± 0.54 0.97<br />
NGC 4526 589 188.49610 7.70676 1.45 −7.103 ± 0.045 −8.691 ± 0.057 3.35 ± 0.27 1.00<br />
NGC 4526 590 188.49705 7.70967 1.49 −8.898 ± 0.015 −10.263 ± 0.021 3.00 ± 0.16 1.00<br />
NGC 4526 591 188.49342 7.69970 1.53 −9.031 ± 0.019 −9.837 ± 0.017 2.73 ± 0.11 1.00<br />
NGC 4526 596 188.49121 7.69447 1.75 −7.926 ± 0.023 −9.193 ± 0.015 2.21 ± 0.12 1.00<br />
NGC 4526 600 188.49073 7.69402 1.80 −7.455 ± 0.050 −9.235 ± 0.059 7.92 ± 0.46 0.67<br />
NGC 4526 605 188.49635 7.71235 1.67 −10.604 ± 0.025 −11.668 ± 0.031 5.20 ± 0.20 0.86<br />
NGC 4526 607 188.49534 7.70952 1.60 −8.653 ± 0.019 −9.562 ± 0.020 2.74 ± 0.13 1.00<br />
NGC 4526 614 188.49387 7.70856 1.67 −8.765 ± 0.017 −10.117 ± 0.023 2.28 ± 0.14 1.00<br />
NGC 4526 615 188.49628 7.71537 1.84 −5.347 ± 0.087 −6.694 ± 0.132 3.14 ± 0.56 0.75<br />
NGC 4526 618 188.49413 7.71008 1.71 −6.654 ± 0.949 −7.751 ± 0.544 5.34 ± 5.97 0.62<br />
NGC 4526 620 188.49462 7.71219 1.77 −7.576 ± 0.076 −8.405 ± 0.142 5.52 ± 1.05 0.75<br />
NGC 4526 626 188.49907 7.72674 2.47 −8.187 ± 0.023 −9.120 ± 0.033 2.27 ± 0.20 1.00<br />
NGC 4526 634 188.49237 7.70845 1.77 −5.140 ± 0.313 −6.161 ± 0.131 3.39 ± 0.53 0.57<br />
NGC 4526 637 188.49035 7.70339 1.81 −8.265 ± 0.040 −9.072 ± 0.050 4.34 ± 0.20 1.00<br />
NGC 4526 639 188.48897 7.69873 1.89 −7.531 ± 0.027 −8.868 ± 0.022 2.58 ± 0.13 1.00<br />
NGC 4526 651 188.49574 7.72211 2.28 −7.218 ± 0.049 −8.105 ± 0.048 4.69 ± 0.22 0.88<br />
NGC 4526 656 188.48851 7.70275 1.94 −5.804 ± 0.106 −7.415 ± 0.151 4.62 ± 0.75 0.63<br />
NGC 4526 657 188.49196 7.71289 1.98 −8.206 ± 0.020 −9.507 ± 0.021 2.68 ± 0.16 1.00<br />
Continued on Next Page. . .<br />
372
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4526 661 188.49002 7.70795 1.93 −7.059 ± 0.036 −8.409 ± 0.040 3.06 ± 0.22 1.00<br />
NGC 4526 666 188.49028 7.71015 1.99 −7.309 ± 0.032 −8.704 ± 0.025 2.23 ± 0.19 1.00<br />
NGC 4526 668 188.49144 7.71410 2.07 −6.575 ± 0.063 −8.330 ± 0.092 5.95 ± 0.47 0.57<br />
NGC 4526 674 188.49168 7.71640 2.17 −7.772 ± 0.110 −9.383 ± 0.056 7.36 ± 0.67 0.87<br />
NGC 4526 678 188.49171 7.71729 2.21 −6.963 ± 0.079 −8.523 ± 0.076 4.68 ± 0.50 0.96<br />
NGC 4526 682 188.48656 7.70330 2.11 −9.275 ± 0.024 −10.157 ± 0.016 2.76 ± 0.14 1.00<br />
NGC 4526 684 188.48764 7.70635 2.07 −5.450 ± 0.716 −6.540 ± 0.216 3.37 ± 1.15 0.66<br />
NGC 4526 692 188.48261 7.69354 2.44 −6.273 ± 0.077 −7.613 ± 0.124 4.48 ± 0.54 0.75<br />
NGC 4526 696 188.49202 7.72132 2.42 −9.792 ± 0.015 −10.926 ± 0.021 2.87 ± 0.12 1.00<br />
NGC 4526 697 188.49475 7.72952 2.83 −7.654 ± 0.030 −8.714 ± 0.031 3.24 ± 0.14 1.00<br />
NGC 4526 701 188.47970 7.68486 2.88 −6.026 ± 0.091 −6.623 ± 0.141 2.83 ± 0.72 0.80<br />
NGC 4526 702 188.49069 7.71898 2.37 −8.558 ± 0.076 −9.432 ± 0.057 5.48 ± 0.41 0.97<br />
NGC 4526 706 188.49057 7.71943 2.40 −9.126 ± 0.015 −10.034 ± 0.016 3.38 ± 0.15 1.00<br />
NGC 4526 712 188.47952 7.68896 2.78 −6.923 ± 0.039 −7.929 ± 0.035 2.59 ± 0.20 0.98<br />
NGC 4526 715 188.48927 7.71728 2.36 −7.197 ± 0.088 −7.843 ± 0.079 5.01 ± 0.48 0.72<br />
NGC 4526 720 188.48958 7.71969 2.47 −8.842 ± 0.041 −10.185 ± 0.027 4.04 ± 0.20 1.00<br />
NGC 4526 723 188.49086 7.72491 2.70 −8.155 ± 0.026 −9.507 ± 0.032 3.14 ± 0.16 1.00<br />
NGC 4526 724 188.49215 7.72950 2.94 −9.608 ± 0.019 −10.847 ± 0.019 2.89 ± 0.14 1.00<br />
NGC 4526 730 188.48224 7.70195 2.44 −7.035 ± 0.027 −7.906 ± 0.051 2.86 ± 0.26 0.97<br />
NGC 4526 734 188.48413 7.70803 2.38 −9.206 ± 0.027 −10.098 ± 0.015 1.66 ± 0.17 1.00<br />
NGC 4526 735 188.48791 7.71888 2.53 −7.541 ± 0.028 −8.874 ± 0.029 2.51 ± 0.13 1.00<br />
NGC 4526 738 188.49165 7.72997 3.00 −6.819 ± 0.030 −7.592 ± 0.046 1.79 ± 0.21 0.91<br />
NGC 4526 746 188.48075 7.70092 2.55 −5.076 ± 0.300 −6.715 ± 0.170 3.86 ± 1.23 0.55<br />
NGC 4526 748 188.48523 7.71449 2.51 −5.074 ± 0.440 −6.676 ± 0.080 3.63 ± 0.81 0.62<br />
NGC 4526 750 188.47577 7.68802 3.09 −7.048 ± 0.036 −8.006 ± 0.030 3.30 ± 0.15 0.96<br />
NGC 4526 757 188.48651 7.71991 2.67 −8.340 ± 0.025 −9.362 ± 0.025 4.50 ± 0.19 1.00<br />
NGC 4526 770 188.47570 7.69268 3.00 −9.140 ± 0.016 −10.050 ± 0.018 4.16 ± 0.09 1.00<br />
NGC 4526 773 188.48132 7.70888 2.62 −7.488 ± 0.019 −8.362 ± 0.028 2.39 ± 0.13 1.00<br />
NGC 4526 776 188.47351 7.68662 3.30 −6.758 ± 0.043 −7.816 ± 0.048 2.76 ± 0.25 0.97<br />
NGC 4526 777 188.47865 7.70196 2.72 −7.253 ± 0.032 −8.152 ± 0.051 3.54 ± 0.19 1.00<br />
NGC 4526 783 188.48254 7.71496 2.72 −6.211 ± 0.064 −7.009 ± 0.086 2.88 ± 0.37 0.87<br />
NGC 4526 786 188.48844 7.73247 3.31 −6.578 ± 0.060 −7.457 ± 0.073 3.46 ± 0.34 0.89<br />
NGC 4526 789 188.48779 7.73162 3.28 −6.296 ± 0.091 −7.243 ± 0.264 2.57 ± 0.51 0.93<br />
NGC 4526 795 188.48026 7.71226 2.79 −6.493 ± 0.052 −7.977 ± 0.053 3.45 ± 0.25 0.95<br />
NGC 4526 797 188.47341 7.69330 3.18 −8.348 ± 0.015 −9.372 ± 0.018 2.72 ± 0.10 1.00<br />
NGC 4552 8 188.93604 12.54685 2.68 −6.740 ± 0.044 −8.179 ± 0.306 2.01 ± 0.28 1.00<br />
NGC 4552 9 188.94660 12.57430 4.29 −6.405 ± 0.053 −7.995 ± 0.028 3.26 ± 0.19 0.98<br />
NGC 4552 10 188.93411 12.54248 2.77 −7.662 ± 0.025 −9.016 ± 0.023 1.87 ± 0.13 1.00<br />
NGC 4552 11 188.94055 12.55897 2.98 −7.267 ± 0.026 −8.239 ± 0.028 3.01 ± 0.14 1.00<br />
NGC 4552 12 188.94186 12.56281 3.22 −7.331 ± 0.044 −8.349 ± 0.026 3.68 ± 0.16 1.00<br />
NGC 4552 16 188.93282 12.54057 2.81 −8.049 ± 0.016 −9.505 ± 0.015 2.04 ± 0.11 1.00<br />
NGC 4552 18 188.93466 12.54556 2.61 −6.926 ± 0.075 −8.472 ± 0.081 5.40 ± 0.40 0.86<br />
NGC 4552 20 188.93250 12.54059 2.78 −6.388 ± 0.033 −7.677 ± 0.041 2.46 ± 0.25 0.99<br />
NGC 4552 21 188.92757 12.52829 3.72 −6.742 ± 0.032 −7.605 ± 0.038 2.71 ± 0.27 0.98<br />
NGC 4552 28 188.93556 12.54959 2.50 −9.740 ± 0.023 −10.997 ± 0.015 3.18 ± 0.13 1.00<br />
NGC 4552 30 188.94263 12.56754 3.49 −8.092 ± 0.022 −8.967 ± 0.022 2.49 ± 0.17 1.00<br />
NGC 4552 33 188.93916 12.55985 2.83 −8.948 ± 0.020 −10.238 ± 0.020 2.33 ± 0.11 1.00<br />
NGC 4552 34 188.92934 12.53477 3.10 −6.621 ± 0.050 −8.093 ± 0.034 1.71 ± 0.34 1.00<br />
NGC 4552 38 188.93533 12.55065 2.44 −7.473 ± 0.033 −8.319 ± 0.028 2.57 ± 0.17 1.00<br />
NGC 4552 40 188.93572 12.55260 2.42 −6.476 ± 0.085 −7.611 ± 0.060 2.98 ± 0.38 0.98<br />
NGC 4552 46 188.93962 12.56377 2.99 −8.111 ± 0.020 −8.909 ± 0.020 3.44 ± 0.09 1.00<br />
NGC 4552 47 188.92561 12.52792 3.68 −7.119 ± 0.034 −8.347 ± 0.029 2.56 ± 0.19 1.00<br />
NGC 4552 48 188.94304 12.57292 3.84 −10.364 ± 0.035 −11.898 ± 0.009 3.79 ± 0.13 1.00<br />
NGC 4552 50 188.93407 12.54985 2.32 −7.368 ± 0.040 −8.193 ± 0.026 2.39 ± 0.18 1.00<br />
NGC 4552 53 188.93465 12.55144 2.33 −6.081 ± 0.105 −7.426 ± 0.093 4.10 ± 0.47 0.86<br />
NGC 4552 54 188.93550 12.55467 2.36 −8.118 ± 0.025 −8.929 ± 0.026 5.23 ± 0.10 0.95<br />
NGC 4552 56 188.93325 12.54953 2.25 −8.539 ± 0.020 −9.461 ± 0.016 2.49 ± 0.11 1.00<br />
NGC 4552 59 188.93153 12.54541 2.31 −5.802 ± 1.459 −7.259 ± 0.943 1.01 ± 0.28 0.78<br />
NGC 4552 60 188.93775 12.56158 2.70 −8.342 ± 0.017 −9.341 ± 0.020 2.12 ± 0.11 1.00<br />
NGC 4552 62 188.94292 12.57536 4.00 −7.528 ± 0.045 −8.980 ± 0.013 2.14 ± 0.19 1.00<br />
NGC 4552 63 188.94216 12.57360 3.80 −7.346 ± 0.045 −8.341 ± 0.020 2.04 ± 0.17 1.00<br />
Continued on Next Page. . .<br />
373
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4552 67 188.93827 12.56452 2.87 −10.015 ± 0.026 −11.056 ± 0.016 3.91 ± 0.11 1.00<br />
NGC 4552 69 188.93098 12.54614 2.20 −7.551 ± 0.032 −8.929 ± 0.026 1.65 ± 0.12 1.00<br />
NGC 4552 71 188.93251 12.55009 2.14 −8.247 ± 0.020 −9.226 ± 0.029 3.15 ± 0.13 1.00<br />
NGC 4552 73 188.93254 12.55042 2.13 −7.762 ± 0.039 −8.594 ± 0.032 4.17 ± 0.15 1.00<br />
NGC 4552 77 188.93611 12.55978 2.46 −5.171 ± 0.080 −6.646 ± 0.099 2.85 ± 0.44 0.90<br />
NGC 4552 84 188.92906 12.54319 2.26 −6.757 ± 0.044 −7.794 ± 0.035 1.88 ± 0.21 0.99<br />
NGC 4552 85 188.92857 12.54189 2.34 −5.136 ± 0.110 −6.031 ± 0.105 3.64 ± 0.55 0.56<br />
NGC 4552 86 188.92938 12.54410 2.21 −6.961 ± 0.034 −8.196 ± 0.040 2.35 ± 0.20 1.00<br />
NGC 4552 87 188.92285 12.52747 3.64 −5.537 ± 0.800 −7.365 ± 1.055 1.74 ± 0.94 0.98<br />
NGC 4552 91 188.92825 12.54192 2.31 −7.253 ± 0.028 −8.767 ± 0.556 1.46 ± 0.25 0.97<br />
NGC 4552 94 188.92418 12.53168 3.19 −6.608 ± 0.038 −8.114 ± 0.019 1.69 ± 0.15 1.00<br />
NGC 4552 95 188.93929 12.57036 3.29 −6.396 ± 0.088 −7.525 ± 0.165 4.10 ± 0.87 0.88<br />
NGC 4552 96 188.93645 12.56333 2.61 −8.952 ± 0.021 −9.885 ± 0.021 2.77 ± 0.19 1.00<br />
NGC 4552 98 188.93981 12.57210 3.46 −7.400 ± 0.029 −8.258 ± 0.028 3.38 ± 0.19 1.00<br />
NGC 4552 104 188.92407 12.53315 3.01 −8.497 ± 0.021 −9.921 ± 0.019 2.56 ± 0.11 1.00<br />
NGC 4552 105 188.92612 12.53846 2.52 −5.762 ± 0.073 −6.730 ± 0.558 1.22 ± 0.34 0.79<br />
NGC 4552 106 188.92817 12.54409 2.11 −5.048 ± 0.298 −5.894 ± 0.183 2.52 ± 0.53 0.85<br />
NGC 4552 112 188.92453 12.53592 2.71 −6.024 ± 0.091 −7.234 ± 0.193 4.92 ± 1.28 0.60<br />
NGC 4552 115 188.92837 12.54638 1.93 −6.833 ± 0.027 −8.340 ± 0.025 1.57 ± 0.12 1.00<br />
NGC 4552 119 188.93102 12.55417 1.84 −8.436 ± 0.024 −9.275 ± 0.019 2.10 ± 0.23 1.00<br />
NGC 4552 120 188.92704 12.54397 2.03 −5.072 ± 0.402 −5.974 ± 0.121 1.86 ± 0.44 0.88<br />
NGC 4552 121 188.93181 12.55655 1.91 −7.938 ± 0.032 −9.208 ± 0.018 2.08 ± 0.16 1.00<br />
NGC 4552 122 188.93856 12.57405 3.48 −6.002 ± 0.089 −7.161 ± 0.068 2.96 ± 0.40 0.95<br />
NGC 4552 124 188.93315 12.56120 2.16 −7.930 ± 0.019 −8.732 ± 0.025 3.04 ± 0.15 1.00<br />
NGC 4552 125 188.93553 12.56753 2.73 −6.949 ± 0.029 −8.095 ± 0.257 2.18 ± 0.29 1.00<br />
NGC 4552 126 188.92691 12.54563 1.87 −6.904 ± 0.044 −7.808 ± 0.213 2.79 ± 0.41 0.99<br />
NGC 4552 127 188.93517 12.56689 2.65 −4.987 ± 0.506 −6.245 ± 0.156 1.43 ± 0.46 0.83<br />
NGC 4552 132 188.92331 12.53766 2.46 −5.297 ± 0.141 −6.615 ± 0.231 2.79 ± 1.10 0.90<br />
NGC 4552 134 188.93233 12.56126 2.06 −5.567 ± 0.445 −6.922 ± 0.051 1.87 ± 0.37 0.97<br />
NGC 4552 136 188.92628 12.54616 1.77 −8.084 ± 0.019 −9.311 ± 0.019 1.75 ± 0.12 1.00<br />
NGC 4552 138 188.93318 12.56419 2.29 −8.235 ± 0.022 −9.282 ± 0.016 2.81 ± 0.09 1.00<br />
NGC 4552 139 188.93070 12.55787 1.79 −8.071 ± 0.023 −9.056 ± 0.023 2.13 ± 0.15 1.00<br />
NGC 4552 143 188.92731 12.55058 1.54 −9.962 ± 0.011 −11.212 ± 0.017 3.12 ± 0.10 1.00<br />
NGC 4552 146 188.92358 12.54146 2.05 −8.709 ± 0.020 −9.548 ± 0.016 3.02 ± 0.09 1.00<br />
NGC 4552 148 188.92152 12.53628 2.55 −7.313 ± 0.025 −8.218 ± 0.027 2.32 ± 0.16 1.00<br />
NGC 4552 150 188.93318 12.56604 2.39 −6.568 ± 0.038 −7.623 ± 0.047 1.94 ± 0.30 0.99<br />
NGC 4552 151 188.92810 12.55354 1.51 −6.603 ± 0.080 −7.922 ± 0.137 2.33 ± 0.36 0.99<br />
NGC 4552 152 188.92630 12.54891 1.55 −5.024 ± 0.316 −5.966 ± 0.733 2.66 ± 0.76 0.84<br />
NGC 4552 153 188.93464 12.57120 2.90 −8.048 ± 0.056 −9.269 ± 0.033 5.30 ± 0.32 0.98<br />
NGC 4552 156 188.93434 12.57082 2.84 −7.260 ± 0.032 −8.129 ± 0.032 2.67 ± 0.17 1.00<br />
NGC 4552 158 188.92625 12.55050 1.44 −6.778 ± 0.038 −8.195 ± 0.051 2.49 ± 0.24 1.00<br />
NGC 4552 160 188.92512 12.54766 1.54 −5.154 ± 0.144 −6.714 ± 0.246 3.39 ± 0.85 0.80<br />
NGC 4552 162 188.93161 12.56458 2.14 −7.671 ± 0.026 −8.460 ± 0.023 2.70 ± 0.21 1.00<br />
NGC 4552 163 188.92291 12.54269 1.88 −8.167 ± 0.024 −9.703 ± 0.016 3.21 ± 0.14 1.00<br />
NGC 4552 164 188.92169 12.53975 2.15 −5.836 ± 0.106 −6.895 ± 0.062 2.44 ± 0.40 0.96<br />
NGC 4552 165 188.93018 12.56190 1.85 −6.290 ± 0.052 −7.859 ± 0.094 1.96 ± 0.30 0.99<br />
NGC 4552 166 188.92485 12.54833 1.46 −4.936 ± 0.251 −6.017 ± 0.134 2.39 ± 0.60 0.87<br />
NGC 4552 167 188.91803 12.53104 3.12 −6.040 ± 0.068 −7.547 ± 0.117 4.36 ± 0.53 0.85<br />
NGC 4552 169 188.93345 12.57081 2.76 −7.174 ± 0.030 −8.686 ± 0.032 2.38 ± 0.20 1.00<br />
NGC 4552 170 188.92510 12.54971 1.37 −8.081 ± 0.022 −8.949 ± 0.019 3.73 ± 0.12 1.00<br />
NGC 4552 172 188.92537 12.55074 1.33 −6.002 ± 0.171 −7.175 ± 0.057 4.36 ± 0.89 0.72<br />
NGC 4552 173 188.91862 12.53364 2.81 −7.588 ± 0.023 −8.601 ± 0.018 2.26 ± 0.14 1.00<br />
NGC 4552 174 188.92081 12.53918 2.19 −7.315 ± 0.031 −8.802 ± 0.025 2.59 ± 0.12 1.00<br />
NGC 4552 177 188.92022 12.53843 2.26 −7.808 ± 0.073 −8.492 ± 0.165 7.17 ± 1.20 0.57<br />
NGC 4552 178 188.92026 12.53855 2.25 −6.855 ± 0.043 −7.808 ± 0.038 2.32 ± 0.25 0.99<br />
NGC 4552 179 188.92613 12.55348 1.28 −8.682 ± 0.013 −9.617 ± 0.020 3.48 ± 0.09 1.00<br />
NGC 4552 181 188.91999 12.53795 2.31 −6.984 ± 0.034 −8.432 ± 0.038 2.46 ± 0.19 1.00<br />
NGC 4552 187 188.92700 12.55805 1.35 −10.102 ± 0.019 −11.486 ± 0.017 2.17 ± 0.13 1.00<br />
NGC 4552 189 188.92561 12.55462 1.19 −7.291 ± 0.029 −8.212 ± 0.407 1.53 ± 0.27 1.00<br />
NGC 4552 190 188.93057 12.56742 2.23 −5.692 ± 0.045 −7.175 ± 0.429 2.57 ± 0.35 0.97<br />
NGC 4552 191 188.92638 12.55682 1.26 −6.194 ± 0.050 −7.550 ± 0.058 1.87 ± 0.28 0.99<br />
NGC 4552 192 188.92228 12.54641 1.44 −8.237 ± 0.017 −9.558 ± 0.024 2.37 ± 0.19 1.00<br />
Continued on Next Page. . .<br />
374
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4552 195 188.92088 12.54283 1.76 −6.338 ± 0.067 −7.571 ± 0.025 2.97 ± 0.17 0.98<br />
NGC 4552 196 188.92531 12.55417 1.16 −6.204 ± 0.062 −7.264 ± 0.541 2.08 ± 0.41 0.99<br />
NGC 4552 199 188.93241 12.57299 2.85 −6.483 ± 0.064 −7.848 ± 0.021 1.81 ± 0.24 0.99<br />
NGC 4552 200 188.92558 12.55575 1.17 −8.484 ± 0.022 −9.928 ± 0.017 2.10 ± 0.16 1.00<br />
NGC 4552 205 188.92143 12.54627 1.40 −7.941 ± 0.032 −9.380 ± 0.017 1.74 ± 0.15 1.00<br />
NGC 4552 206 188.92229 12.54849 1.23 −8.809 ± 0.018 −9.929 ± 0.014 2.44 ± 0.12 1.00<br />
NGC 4552 207 188.92166 12.54774 1.26 −8.764 ± 0.019 −9.913 ± 0.013 2.28 ± 0.11 1.00<br />
NGC 4552 209 188.92210 12.54949 1.13 −9.472 ± 0.072 −10.578 ± 0.075 5.22 ± 0.36 1.00<br />
NGC 4552 215 188.92961 12.56916 2.28 −5.993 ± 0.084 −7.305 ± 0.318 2.84 ± 0.36 0.97<br />
NGC 4552 216 188.92298 12.55232 0.99 −7.426 ± 0.031 −8.582 ± 0.028 2.46 ± 0.25 1.00<br />
NGC 4552 218 188.93319 12.57908 3.48 −6.766 ± 0.049 −7.763 ± 0.026 2.50 ± 0.32 0.99<br />
NGC 4552 225 188.91745 12.53931 2.10 −7.340 ± 0.034 −8.191 ± 0.040 1.97 ± 0.17 1.00<br />
NGC 4552 226 188.92830 12.56710 1.99 −7.253 ± 0.076 −8.433 ± 0.059 4.96 ± 0.41 0.94<br />
NGC 4552 227 188.93028 12.57224 2.61 −5.279 ± 0.159 −6.421 ± 0.268 3.98 ± 1.07 0.50<br />
NGC 4552 228 188.92254 12.55231 0.94 −6.669 ± 0.075 −7.778 ± 0.050 2.21 ± 0.27 0.99<br />
NGC 4552 229 188.92138 12.54979 1.04 −5.670 ± 1.149 −6.790 ± 0.096 2.37 ± 0.46 0.96<br />
NGC 4552 230 188.92183 12.55105 0.97 −9.851 ± 0.019 −11.223 ± 0.020 1.71 ± 0.15 1.00<br />
NGC 4552 231 188.91998 12.54734 1.21 −9.017 ± 0.025 −9.969 ± 0.019 2.83 ± 0.15 1.00<br />
NGC 4552 234 188.92399 12.55770 0.99 −5.415 ± 0.796 −6.834 ± 0.392 1.30 ± 0.55 0.85<br />
NGC 4552 235 188.92276 12.55469 0.85 −7.030 ± 0.070 −8.306 ± 0.042 2.98 ± 0.28 1.00<br />
NGC 4552 237 188.91896 12.54542 1.39 −6.255 ± 0.047 −8.071 ± 0.053 2.47 ± 0.38 1.00<br />
NGC 4552 239 188.92520 12.56189 1.31 −8.495 ± 0.022 −9.522 ± 0.016 2.28 ± 0.10 1.00<br />
NGC 4552 240 188.92377 12.55834 0.98 −8.315 ± 0.024 −9.535 ± 0.018 2.24 ± 0.16 1.00<br />
NGC 4552 241 188.92737 12.56745 1.94 −6.784 ± 0.042 −8.104 ± 0.028 1.50 ± 0.18 0.97<br />
NGC 4552 244 188.91769 12.54306 1.65 −7.950 ± 0.023 −8.701 ± 0.031 2.32 ± 0.14 1.00<br />
NGC 4552 245 188.93143 12.57596 3.05 −5.387 ± 0.164 −6.778 ± 0.062 2.29 ± 0.68 0.96<br />
NGC 4552 247 188.91951 12.54837 1.07 −9.498 ± 0.020 −10.652 ± 0.013 2.46 ± 0.10 1.00<br />
NGC 4552 248 188.91501 12.53703 2.37 −6.758 ± 0.052 −7.821 ± 0.041 2.51 ± 0.24 0.99<br />
NGC 4552 249 188.92213 12.55527 0.76 −5.818 ± 0.112 −6.786 ± 0.460 1.96 ± 0.51 0.96<br />
NGC 4552 252 188.92100 12.55282 0.75 −7.727 ± 0.041 −9.027 ± 0.018 2.01 ± 0.19 1.00<br />
NGC 4552 253 188.91817 12.54573 1.33 −7.018 ± 0.040 −7.805 ± 0.041 2.76 ± 0.25 0.99<br />
NGC 4552 255 188.92091 12.55352 0.70 −8.260 ± 0.027 −9.130 ± 0.029 2.65 ± 0.21 1.00<br />
NGC 4552 258 188.91511 12.53871 2.17 −6.182 ± 0.050 −7.111 ± 0.144 1.62 ± 0.34 0.95<br />
NGC 4552 262 188.92331 12.56036 1.02 −7.873 ± 0.123 −8.606 ± 0.127 6.67 ± 0.96 0.70<br />
NGC 4552 266 188.92317 12.56058 1.02 −7.270 ± 0.031 −8.387 ± 0.030 2.58 ± 0.25 1.00<br />
NGC 4552 267 188.91614 12.54334 1.60 −7.403 ± 0.036 −8.417 ± 0.019 2.13 ± 0.25 1.00<br />
NGC 4552 268 188.92021 12.55372 0.61 −6.175 ± 0.424 −7.956 ± 0.066 1.51 ± 0.38 0.97<br />
NGC 4552 269 188.91674 12.54515 1.38 −7.926 ± 0.031 −8.872 ± 0.015 1.79 ± 0.25 1.00<br />
NGC 4552 272 188.91293 12.53585 2.54 −7.242 ± 0.033 −8.703 ± 0.021 2.08 ± 0.19 1.00<br />
NGC 4552 273 188.91741 12.54748 1.10 −7.315 ± 0.031 −8.510 ± 0.037 2.31 ± 0.22 1.00<br />
NGC 4552 274 188.92304 12.56194 1.10 −5.959 ± 0.079 −6.607 ± 0.095 1.96 ± 0.39 0.94<br />
NGC 4552 275 188.91960 12.55312 0.60 −7.188 ± 0.032 −8.710 ± 0.115 2.11 ± 0.31 1.00<br />
NGC 4552 277 188.92247 12.56069 0.95 −7.598 ± 0.025 −8.588 ± 0.030 2.07 ± 0.25 1.00<br />
NGC 4552 279 188.91678 12.54687 1.17 −8.347 ± 0.025 −9.456 ± 0.026 2.71 ± 0.18 1.00<br />
NGC 4552 282 188.91826 12.54259 1.71 −7.242 ± 0.033 −8.741 ± 0.028 2.13 ± 0.17 1.00<br />
NGC 4552 283 188.92253 12.56234 1.09 −7.908 ± 0.037 −9.263 ± 0.038 1.97 ± 0.34 1.00<br />
NGC 4552 284 188.91869 12.55256 0.57 −7.649 ± 0.035 −9.052 ± 0.018 1.59 ± 0.14 1.00<br />
NGC 4552 285 188.92483 12.56867 1.86 −7.983 ± 0.022 −8.787 ± 0.031 2.66 ± 0.21 1.00<br />
NGC 4552 288 188.91760 12.55054 0.74 −6.631 ± 0.059 −8.043 ± 0.085 3.39 ± 0.28 1.00<br />
NGC 4552 293 188.91924 12.55528 0.42 −7.584 ± 0.038 −8.612 ± 0.073 1.57 ± 0.26 1.00<br />
NGC 4552 294 188.92022 12.55808 0.56 −6.578 ± 0.053 −8.428 ± 0.045 1.40 ± 0.25 0.96<br />
NGC 4552 299 188.91966 12.55711 0.46 −6.680 ± 1.064 −8.255 ± 0.041 1.19 ± 0.27 0.90<br />
NGC 4552 300 188.91965 12.55732 0.47 −8.063 ± 0.037 −8.858 ± 0.048 2.56 ± 0.21 1.00<br />
NGC 4552 301 188.91429 12.54355 1.58 −6.713 ± 0.041 −8.163 ± 0.423 1.67 ± 0.28 1.00<br />
NGC 4552 303 188.92297 12.56583 1.44 −5.620 ± 0.423 −7.026 ± 0.061 2.51 ± 0.42 0.97<br />
NGC 4552 304 188.91618 12.54874 0.93 −7.629 ± 0.027 −9.038 ± 0.024 2.34 ± 0.14 1.00<br />
NGC 4552 305 188.91086 12.53532 2.65 −6.392 ± 0.114 −7.409 ± 0.085 3.98 ± 0.55 0.87<br />
NGC 4552 306 188.91515 12.54674 1.18 −8.676 ± 0.021 −9.847 ± 0.016 2.05 ± 0.19 1.00<br />
NGC 4552 307 188.91651 12.55064 0.70 −6.528 ± 0.109 −7.084 ± 0.204 4.27 ± 1.06 0.69<br />
NGC 4552 308 188.92158 12.56376 1.14 −9.892 ± 0.013 −10.825 ± 0.017 3.81 ± 0.10 1.00<br />
NGC 4552 309 188.91519 12.54729 1.11 −5.525 ± 0.301 −6.748 ± 0.453 1.46 ± 0.63 0.89<br />
NGC 4552 310 188.90854 12.53042 3.30 −4.690 ± 0.728 −6.485 ± 0.376 1.58 ± 0.70 0.89<br />
Continued on Next Page. . .<br />
375
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4552 311 188.90833 12.53004 3.35 −8.058 ± 0.039 −9.109 ± 0.021 2.55 ± 0.17 1.00<br />
NGC 4552 312 188.91176 12.53885 2.20 −8.134 ± 0.027 −9.178 ± 0.025 2.93 ± 0.14 1.00<br />
NGC 4552 313 188.91954 12.55842 0.51 −7.222 ± 0.033 −8.167 ± 0.045 1.61 ± 0.27 1.00<br />
NGC 4552 317 188.92834 12.58176 3.46 −5.645 ± 0.118 −6.507 ± 0.143 3.29 ± 0.77 0.78<br />
NGC 4552 319 188.91515 12.54853 0.96 −7.161 ± 0.041 −8.698 ± 0.031 1.88 ± 0.24 1.00<br />
NGC 4552 320 188.92357 12.57018 1.93 −9.485 ± 0.022 −10.557 ± 0.016 3.18 ± 0.08 1.00<br />
NGC 4552 321 188.90817 12.53109 3.24 −9.388 ± 0.022 −10.512 ± 0.014 2.88 ± 0.12 1.00<br />
NGC 4552 324 188.91111 12.53872 2.24 −7.663 ± 0.024 −9.015 ± 0.034 2.21 ± 0.19 1.00<br />
NGC 4552 327 188.90871 12.53303 2.99 −7.280 ± 0.053 −8.308 ± 0.028 2.73 ± 0.22 1.00<br />
NGC 4552 328 188.91846 12.55793 0.37 −7.856 ± 0.028 −8.968 ± 0.277 1.72 ± 0.22 1.00<br />
NGC 4552 329 188.92431 12.57199 2.17 −6.613 ± 0.041 −7.842 ± 0.322 2.17 ± 0.27 1.00<br />
NGC 4552 330 188.91783 12.55649 0.24 −7.460 ± 0.050 −8.906 ± 0.742 1.81 ± 0.36 1.00<br />
NGC 4552 333 188.91872 12.55903 0.48 −7.294 ± 0.032 −8.742 ± 0.042 2.60 ± 0.17 1.00<br />
NGC 4552 335 188.91789 12.55720 0.26 −8.995 ± 0.024 −9.885 ± 0.021 1.77 ± 0.13 1.00<br />
NGC 4552 336 188.91876 12.55938 0.51 −8.338 ± 0.027 −9.390 ± 0.022 1.90 ± 0.25 1.00<br />
NGC 4552 338 188.91536 12.55115 0.64 −6.455 ± 0.298 −7.806 ± 1.013 1.82 ± 0.51 0.99<br />
NGC 4552 339 188.91345 12.54634 1.26 −5.798 ± 0.564 −7.661 ± 0.124 2.95 ± 0.71 0.98<br />
NGC 4552 340 188.92096 12.56556 1.29 −6.094 ± 0.050 −7.095 ± 0.501 2.24 ± 0.37 0.98<br />
NGC 4552 342 188.91060 12.53955 2.16 −8.363 ± 0.026 −9.239 ± 0.021 2.88 ± 0.13 1.00<br />
NGC 4552 343 188.92274 12.57051 1.93 −7.737 ± 0.027 −8.581 ± 0.038 2.99 ± 0.17 1.00<br />
NGC 4552 345 188.91100 12.54119 1.95 −6.357 ± 0.069 −7.697 ± 0.042 1.80 ± 0.36 0.99<br />
NGC 4552 346 188.91585 12.55391 0.30 −7.171 ± 0.058 −7.904 ± 1.469 1.57 ± 0.33 0.98<br />
NGC 4552 347 188.91481 12.55128 0.63 −6.561 ± 0.066 −7.728 ± 0.068 2.09 ± 0.38 0.99<br />
NGC 4552 348 188.91803 12.55953 0.47 −5.547 ± 0.450 −7.096 ± 0.456 1.77 ± 0.61 0.97<br />
NGC 4552 349 188.91305 12.54696 1.20 −7.095 ± 0.039 −7.779 ± 0.059 2.93 ± 0.31 0.98<br />
NGC 4552 350 188.92458 12.57648 2.68 −7.646 ± 0.029 −8.655 ± 0.023 2.72 ± 0.22 1.00<br />
NGC 4552 352 188.91205 12.54486 1.48 −6.938 ± 0.461 −7.583 ± 1.368 1.34 ± 0.41 0.94<br />
NGC 4552 353 188.91139 12.54371 1.64 −8.032 ± 0.026 −9.232 ± 0.024 2.32 ± 0.22 1.00<br />
NGC 4552 354 188.91016 12.54061 2.05 −8.064 ± 0.023 −9.539 ± 0.015 2.19 ± 0.12 1.00<br />
NGC 4552 356 188.91757 12.56002 0.50 −8.720 ± 0.019 −9.701 ± 0.019 1.97 ± 0.16 1.00<br />
NGC 4552 357 188.91635 12.55683 0.08 −8.906 ± 0.304 −10.095 ± 0.035 2.19 ± 0.30 1.00<br />
NGC 4552 359 188.92024 12.56702 1.41 −7.988 ± 0.036 −9.372 ± 0.026 1.72 ± 0.24 1.00<br />
NGC 4552 360 188.91409 12.55149 0.63 −6.663 ± 0.808 −7.578 ± 0.041 1.75 ± 0.33 0.98<br />
NGC 4552 361 188.91501 12.55424 0.28 −8.451 ± 0.033 −9.761 ± 0.027 1.89 ± 0.16 1.00<br />
NGC 4552 362 188.91754 12.56102 0.61 −7.604 ± 0.029 −8.798 ± 0.045 2.58 ± 0.21 1.00<br />
NGC 4552 363 188.91946 12.56598 1.26 −6.620 ± 0.050 −7.642 ± 0.063 1.69 ± 0.31 0.98<br />
NGC 4552 365 188.90948 12.54095 2.04 −7.857 ± 0.037 −8.812 ± 0.024 2.73 ± 0.15 1.00<br />
NGC 4552 366 188.91785 12.56237 0.78 −5.749 ± 0.694 −6.806 ± 0.518 0.97 ± 0.60 0.66<br />
NGC 4552 368 188.91203 12.54780 1.15 −5.885 ± 0.140 −7.231 ± 0.078 3.15 ± 0.43 0.93<br />
NGC 4552 371 188.91393 12.55328 0.44 −7.843 ± 0.042 −9.122 ± 0.047 2.06 ± 0.23 1.00<br />
NGC 4552 372 188.91472 12.55539 0.18 −7.938 ± 0.039 −9.507 ± 0.024 1.24 ± 0.17 0.90<br />
NGC 4552 374 188.91266 12.55050 0.81 −7.578 ± 0.020 −9.002 ± 0.022 2.20 ± 0.17 1.00<br />
NGC 4552 375 188.92212 12.57465 2.37 −5.841 ± 0.093 −6.845 ± 0.611 2.07 ± 0.41 0.97<br />
NGC 4552 376 188.91718 12.56253 0.78 −10.454 ± 0.022 −11.659 ± 0.013 3.65 ± 0.09 1.00<br />
NGC 4552 377 188.91303 12.55210 0.62 −9.299 ± 0.024 −10.147 ± 0.015 3.00 ± 0.11 1.00<br />
NGC 4552 378 188.91349 12.55331 0.47 −6.814 ± 0.066 −8.165 ± 0.043 1.99 ± 0.25 1.00<br />
NGC 4552 379 188.91519 12.55797 0.22 −8.068 ± 0.039 −9.450 ± 0.031 1.94 ± 0.21 1.00<br />
NGC 4552 380 188.91915 12.56848 1.54 −6.317 ± 0.075 −7.482 ± 0.043 2.27 ± 0.29 0.99<br />
NGC 4552 381 188.91362 12.55437 0.36 −6.696 ± 0.878 −7.962 ± 0.242 1.58 ± 0.44 0.98<br />
NGC 4552 382 188.91539 12.55921 0.36 −8.480 ± 0.039 −9.680 ± 0.038 2.96 ± 0.20 1.00<br />
NGC 4552 383 188.90475 12.53195 3.28 −5.580 ± 0.117 −6.641 ± 0.343 2.00 ± 0.52 0.95<br />
NGC 4552 384 188.91330 12.55394 0.43 −8.459 ± 0.031 −9.290 ± 0.028 3.13 ± 0.12 1.00<br />
NGC 4552 385 188.91183 12.55014 0.90 −7.511 ± 0.061 −8.622 ± 0.029 2.93 ± 0.23 1.00<br />
NGC 4552 386 188.90863 12.54197 1.97 −5.756 ± 0.211 −7.445 ± 0.122 3.97 ± 1.62 0.88<br />
NGC 4552 387 188.91968 12.57020 1.76 −6.005 ± 0.181 −7.403 ± 0.060 1.61 ± 0.45 0.97<br />
NGC 4552 388 188.91208 12.55095 0.80 −7.531 ± 0.028 −9.005 ± 0.043 2.49 ± 0.15 1.00<br />
NGC 4552 392 188.91817 12.56697 1.33 −5.357 ± 0.267 −6.608 ± 0.109 1.71 ± 0.49 0.93<br />
NGC 4552 394 188.92445 12.58315 3.45 −5.109 ± 0.104 −6.383 ± 0.165 3.35 ± 1.04 0.74<br />
NGC 4552 395 188.90687 12.53845 2.45 −8.637 ± 0.038 −9.722 ± 0.015 2.05 ± 0.18 1.00<br />
NGC 4552 397 188.91618 12.56227 0.73 −7.884 ± 0.022 −9.210 ± 0.034 1.91 ± 0.19 1.00<br />
NGC 4552 398 188.91538 12.56030 0.49 −6.004 ± 0.782 −7.205 ± 0.676 1.49 ± 0.51 0.94<br />
NGC 4552 400 188.92142 12.57592 2.49 −6.737 ± 0.022 −7.925 ± 0.038 1.95 ± 0.21 0.99<br />
Continued on Next Page. . .<br />
376
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4552 401 188.91484 12.55943 0.40 −7.724 ± 0.033 −8.716 ± 0.042 2.37 ± 0.31 1.00<br />
NGC 4552 402 188.90598 12.53685 2.67 −8.247 ± 0.035 −9.578 ± 0.019 2.13 ± 0.17 1.00<br />
NGC 4552 403 188.92010 12.57277 2.08 −5.257 ± 0.427 −7.040 ± 0.203 1.92 ± 2.30 0.97<br />
NGC 4552 405 188.91818 12.56823 1.49 −7.422 ± 0.020 −8.908 ± 0.023 1.72 ± 0.15 1.00<br />
NGC 4552 407 188.91226 12.55352 0.55 −6.791 ± 0.107 −7.980 ± 0.145 2.73 ± 0.42 0.99<br />
NGC 4552 408 188.91291 12.55520 0.38 −6.311 ± 0.090 −7.546 ± 0.435 2.00 ± 0.50 0.99<br />
NGC 4552 410 188.90469 12.53448 3.00 −7.710 ± 0.041 −9.121 ± 0.021 2.28 ± 0.18 1.00<br />
NGC 4552 412 188.90374 12.53227 3.29 −7.338 ± 0.065 −8.166 ± 0.074 5.33 ± 0.42 0.85<br />
NGC 4552 413 188.91511 12.56131 0.62 −6.854 ± 0.048 −8.285 ± 0.460 1.80 ± 0.36 1.00<br />
NGC 4552 414 188.91167 12.55260 0.68 −5.575 ± 0.395 −6.761 ± 0.198 3.03 ± 1.20 0.88<br />
NGC 4552 416 188.91945 12.57268 2.05 −8.764 ± 0.019 −9.792 ± 0.014 1.85 ± 0.11 1.00<br />
NGC 4552 417 188.91430 12.55950 0.43 −7.859 ± 0.031 −9.212 ± 0.024 2.09 ± 0.19 1.00<br />
NGC 4552 418 188.91040 12.54965 1.05 −8.095 ± 0.025 −9.308 ± 0.016 2.24 ± 0.13 1.00<br />
NGC 4552 420 188.91244 12.55548 0.42 −9.875 ± 0.018 −10.913 ± 0.023 2.43 ± 0.20 1.00<br />
NGC 4552 422 188.92352 12.58352 3.46 −4.701 ± 0.335 −6.463 ± 0.458 0.94 ± 1.66 0.57<br />
NGC 4552 423 188.92317 12.58281 3.37 −7.208 ± 0.054 −7.913 ± 0.038 2.50 ± 0.29 0.99<br />
NGC 4552 424 188.90991 12.54911 1.14 −7.057 ± 0.032 −8.130 ± 0.033 2.48 ± 0.27 1.00<br />
NGC 4552 425 188.91116 12.55230 0.75 −9.976 ± 0.015 −11.002 ± 0.013 3.02 ± 0.12 1.00<br />
NGC 4552 426 188.91078 12.55120 0.88 −8.597 ± 0.028 −9.918 ± 0.016 2.67 ± 0.12 1.00<br />
NGC 4552 427 188.91305 12.55727 0.36 −6.654 ± 0.426 −8.104 ± 0.310 1.93 ± 0.41 1.00<br />
NGC 4552 428 188.92086 12.57730 2.64 −6.928 ± 0.044 −8.271 ± 0.034 2.89 ± 0.22 1.00<br />
NGC 4552 429 188.90943 12.54810 1.27 −6.437 ± 0.141 −7.387 ± 0.589 1.57 ± 0.35 0.96<br />
NGC 4552 430 188.91639 12.56620 1.21 −5.591 ± 0.313 −7.134 ± 0.326 2.47 ± 0.50 0.97<br />
NGC 4552 432 188.91213 12.55542 0.46 −7.747 ± 0.041 −8.714 ± 0.153 2.72 ± 0.74 1.00<br />
NGC 4552 433 188.91095 12.55248 0.76 −7.150 ± 0.043 −8.053 ± 0.062 2.66 ± 0.42 1.00<br />
NGC 4552 434 188.91012 12.54987 1.05 −7.566 ± 0.035 −9.143 ± 0.033 2.15 ± 0.21 1.00<br />
NGC 4552 436 188.91014 12.55062 0.98 −7.222 ± 0.028 −8.339 ± 0.039 3.15 ± 0.22 1.00<br />
NGC 4552 437 188.91289 12.55781 0.40 −7.547 ± 0.045 −9.086 ± 0.035 2.79 ± 0.19 1.00<br />
NGC 4552 438 188.91066 12.55229 0.80 −10.404 ± 0.024 −11.588 ± 0.016 3.12 ± 0.14 1.00<br />
NGC 4552 440 188.91319 12.55897 0.45 −8.271 ± 0.025 −9.815 ± 0.018 1.69 ± 0.12 1.00<br />
NGC 4552 442 188.91323 12.55951 0.50 −7.267 ± 0.031 −8.889 ± 0.407 1.59 ± 0.25 1.00<br />
NGC 4552 446 188.90877 12.54846 1.29 −9.229 ± 0.023 −10.460 ± 0.015 3.18 ± 0.10 1.00<br />
NGC 4552 447 188.91524 12.56550 1.13 −7.378 ± 0.036 −8.379 ± 0.041 2.68 ± 0.20 1.00<br />
NGC 4552 448 188.91126 12.55546 0.56 −7.117 ± 0.038 −8.374 ± 0.028 2.07 ± 0.20 1.00<br />
NGC 4552 449 188.91589 12.56730 1.35 −7.289 ± 0.040 −8.662 ± 0.026 1.04 ± 0.16 0.83<br />
NGC 4552 450 188.92180 12.58246 3.28 −5.465 ± 0.087 −6.530 ± 0.109 2.99 ± 0.43 0.86<br />
NGC 4552 451 188.91562 12.56687 1.29 −8.219 ± 0.024 −9.539 ± 0.028 2.80 ± 0.16 1.00<br />
NGC 4552 452 188.91325 12.56070 0.62 −6.085 ± 0.515 −7.429 ± 0.664 1.01 ± 0.50 0.80<br />
NGC 4552 453 188.90960 12.55159 0.95 −8.977 ± 0.033 −9.914 ± 0.018 4.12 ± 0.11 1.00<br />
NGC 4552 456 188.91440 12.56431 0.99 −7.070 ± 0.041 −8.542 ± 0.031 2.30 ± 0.22 1.00<br />
NGC 4552 457 188.91503 12.56610 1.20 −8.500 ± 0.019 −9.448 ± 0.017 2.24 ± 0.12 1.00<br />
NGC 4552 460 188.91352 12.56246 0.80 −8.854 ± 0.029 −10.278 ± 0.017 1.67 ± 0.15 1.00<br />
NGC 4552 461 188.90578 12.54290 2.05 −8.507 ± 0.015 −9.520 ± 0.020 3.14 ± 0.12 1.00<br />
NGC 4552 462 188.90312 12.53586 2.94 −7.969 ± 0.031 −8.845 ± 0.017 2.34 ± 0.18 1.00<br />
NGC 4552 463 188.90965 12.55309 0.85 −6.492 ± 0.074 −8.132 ± 0.154 5.81 ± 1.06 0.70<br />
NGC 4552 467 188.90959 12.55414 0.80 −8.825 ± 0.025 −9.604 ± 0.018 2.78 ± 0.11 1.00<br />
NGC 4552 469 188.90774 12.54950 1.29 −9.578 ± 0.017 −10.739 ± 0.012 2.52 ± 0.11 1.00<br />
NGC 4552 470 188.91154 12.55931 0.63 −7.523 ± 0.034 −9.076 ± 0.253 1.90 ± 0.23 1.00<br />
NGC 4552 471 188.91326 12.56374 0.96 −6.493 ± 0.076 −8.071 ± 0.043 1.07 ± 0.33 0.85<br />
NGC 4552 474 188.91165 12.56028 0.70 −7.985 ± 0.025 −8.996 ± 0.022 1.96 ± 0.14 1.00<br />
NGC 4552 476 188.90425 12.54148 2.29 −5.628 ± 0.057 −6.649 ± 0.093 2.07 ± 0.40 0.95<br />
NGC 4552 478 188.90793 12.55191 1.10 −7.490 ± 0.048 −9.146 ± 0.040 2.75 ± 0.25 1.00<br />
NGC 4552 479 188.91367 12.56747 1.39 −9.531 ± 0.027 −10.466 ± 0.019 2.48 ± 0.13 1.00<br />
NGC 4552 482 188.91832 12.58017 2.94 −6.133 ± 0.089 −7.239 ± 0.185 4.64 ± 1.16 0.68<br />
NGC 4552 484 188.90143 12.53726 2.91 −8.497 ± 0.091 −9.593 ± 0.045 5.53 ± 0.41 1.00<br />
NGC 4552 485 188.91007 12.55931 0.78 −5.290 ± 1.383 −6.962 ± 0.098 2.12 ± 0.53 0.98<br />
NGC 4552 486 188.90840 12.55540 0.90 −8.212 ± 0.026 −9.754 ± 0.017 2.01 ± 0.13 1.00<br />
NGC 4552 487 188.91087 12.56181 0.90 −7.330 ± 0.030 −8.797 ± 0.021 2.07 ± 0.23 1.00<br />
NGC 4552 488 188.90807 12.55505 0.95 −5.394 ± 0.073 −6.918 ± 1.007 1.54 ± 0.70 0.92<br />
NGC 4552 489 188.90678 12.55207 1.21 −7.099 ± 0.047 −8.450 ± 0.029 2.26 ± 0.20 1.00<br />
NGC 4552 492 188.90791 12.55568 0.96 −8.349 ± 0.030 −9.623 ± 0.018 1.78 ± 0.17 1.00<br />
NGC 4552 493 188.90583 12.55066 1.39 −6.629 ± 0.083 −7.733 ± 0.037 2.90 ± 0.44 0.98<br />
Continued on Next Page. . .<br />
377
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4552 495 188.90451 12.54735 1.75 −6.881 ± 0.031 −8.228 ± 0.031 2.71 ± 0.24 1.00<br />
NGC 4552 497 188.90851 12.55787 0.90 −6.070 ± 0.140 −7.046 ± 0.139 3.36 ± 0.81 0.87<br />
NGC 4552 500 188.90469 12.54826 1.67 −6.915 ± 0.030 −8.532 ± 0.023 3.09 ± 0.14 1.00<br />
NGC 4552 501 188.90295 12.54416 2.15 −8.013 ± 0.025 −9.345 ± 0.031 3.53 ± 0.16 1.00<br />
NGC 4552 504 188.90971 12.56304 1.10 −8.113 ± 0.022 −9.723 ± 0.025 3.18 ± 0.16 1.00<br />
NGC 4552 505 188.90679 12.55572 1.09 −6.023 ± 0.184 −7.114 ± 0.081 3.38 ± 0.97 0.88<br />
NGC 4552 506 188.90320 12.54667 1.93 −6.791 ± 0.040 −7.974 ± 0.029 2.06 ± 0.22 1.00<br />
NGC 4552 507 188.91101 12.56686 1.42 −8.838 ± 0.022 −9.927 ± 0.017 2.25 ± 0.12 1.00<br />
NGC 4552 508 188.90463 12.55047 1.53 −6.229 ± 0.055 −7.441 ± 0.234 2.34 ± 0.37 0.99<br />
NGC 4552 509 188.91279 12.57179 1.93 −10.135 ± 0.014 −11.076 ± 0.011 3.89 ± 0.06 1.00<br />
NGC 4552 511 188.90580 12.55402 1.24 −5.750 ± 0.387 −6.356 ± 0.149 2.36 ± 0.77 0.91<br />
NGC 4552 512 188.90996 12.56472 1.25 −6.307 ± 0.064 −7.669 ± 0.037 1.88 ± 0.24 0.99<br />
NGC 4552 513 188.90153 12.54340 2.34 −8.038 ± 0.022 −8.960 ± 0.025 2.36 ± 0.16 1.00<br />
NGC 4552 514 188.89847 12.53572 3.28 −6.696 ± 0.420 −7.469 ± 0.047 2.12 ± 0.41 0.99<br />
NGC 4552 517 188.90144 12.54454 2.26 −6.473 ± 0.046 −7.390 ± 0.064 3.95 ± 0.27 0.87<br />
NGC 4552 518 188.90466 12.55314 1.40 −9.986 ± 0.039 −11.068 ± 0.067 3.35 ± 0.19 1.00<br />
NGC 4552 521 188.91354 12.57608 2.44 −6.371 ± 0.049 −7.548 ± 0.029 2.26 ± 0.31 0.99<br />
NGC 4552 524 188.91150 12.57185 1.97 −8.871 ± 0.032 −10.413 ± 0.021 2.37 ± 0.15 1.00<br />
NGC 4552 525 188.90831 12.56358 1.27 −6.120 ± 0.045 −7.674 ± 0.344 2.02 ± 0.42 0.99<br />
NGC 4552 526 188.90730 12.56111 1.18 −6.739 ± 0.034 −8.090 ± 0.059 2.57 ± 0.25 1.00<br />
NGC 4552 528 188.90735 12.56134 1.19 −7.171 ± 0.028 −8.175 ± 0.044 2.23 ± 0.16 1.00<br />
NGC 4552 529 188.90808 12.56338 1.27 −8.993 ± 0.017 −10.197 ± 0.027 2.63 ± 0.19 1.00<br />
NGC 4552 530 188.90318 12.55089 1.66 −7.980 ± 0.032 −9.389 ± 0.021 3.25 ± 0.15 1.00<br />
NGC 4552 531 188.90898 12.56572 1.42 −8.658 ± 0.024 −9.640 ± 0.044 2.38 ± 0.32 1.00<br />
NGC 4552 534 188.89732 12.53676 3.27 −8.016 ± 0.035 −8.906 ± 0.024 2.02 ± 0.16 1.00<br />
NGC 4552 535 188.91031 12.57041 1.85 −6.715 ± 0.034 −8.133 ± 0.040 2.65 ± 0.20 1.00<br />
NGC 4552 537 188.90906 12.56757 1.60 −7.114 ± 0.085 −8.320 ± 0.151 5.04 ± 0.84 0.92<br />
NGC 4552 538 188.91037 12.57137 1.96 −8.314 ± 0.020 −9.279 ± 0.025 3.30 ± 0.12 1.00<br />
NGC 4552 540 188.90924 12.56890 1.73 −7.293 ± 0.034 −8.600 ± 0.029 2.26 ± 0.18 1.00<br />
NGC 4552 541 188.89652 12.53650 3.36 −7.359 ± 0.039 −8.500 ± 0.420 1.28 ± 0.29 0.94<br />
NGC 4552 544 188.90170 12.55048 1.84 −8.707 ± 0.046 −9.680 ± 0.014 2.80 ± 0.19 1.00<br />
NGC 4552 545 188.90361 12.55548 1.47 −5.939 ± 0.670 −7.349 ± 0.098 1.51 ± 0.41 0.95<br />
NGC 4552 546 188.90857 12.56842 1.72 −6.393 ± 0.056 −7.638 ± 0.035 1.95 ± 0.22 0.99<br />
NGC 4552 547 188.90033 12.54758 2.15 −7.159 ± 0.031 −8.717 ± 0.031 2.98 ± 0.15 1.00<br />
NGC 4552 551 188.89685 12.53965 3.06 −6.041 ± 0.075 −7.321 ± 0.040 2.27 ± 0.29 0.99<br />
NGC 4552 552 188.91203 12.57853 2.76 −6.745 ± 0.037 −7.577 ± 0.033 1.96 ± 0.22 0.99<br />
NGC 4552 553 188.91014 12.57394 2.27 −6.689 ± 0.326 −8.096 ± 0.025 1.91 ± 0.29 1.00<br />
NGC 4552 555 188.90169 12.55316 1.74 −7.160 ± 0.034 −8.650 ± 0.021 1.91 ± 0.18 1.00<br />
NGC 4552 557 188.90797 12.56948 1.87 −5.578 ± 0.106 −6.950 ± 0.571 1.34 ± 0.42 0.87<br />
NGC 4552 558 188.90651 12.56601 1.63 −7.032 ± 0.036 −8.417 ± 0.032 2.16 ± 0.21 1.00<br />
NGC 4552 559 188.90357 12.55898 1.51 −9.113 ± 0.024 −10.166 ± 0.011 1.90 ± 0.14 1.00<br />
NGC 4552 560 188.90822 12.57106 2.03 −6.329 ± 0.072 −7.109 ± 0.180 3.85 ± 1.07 0.80<br />
NGC 4552 561 188.90421 12.56078 1.50 −6.535 ± 0.034 −7.759 ± 0.054 1.82 ± 0.24 0.99<br />
NGC 4552 562 188.90582 12.56516 1.62 −6.946 ± 0.040 −8.382 ± 0.026 1.80 ± 0.20 1.00<br />
NGC 4552 563 188.89807 12.54583 2.49 −7.064 ± 0.048 −8.278 ± 0.043 3.42 ± 0.25 1.00<br />
NGC 4552 565 188.90512 12.56471 1.65 −7.372 ± 0.031 −8.730 ± 0.024 2.82 ± 0.21 1.00<br />
NGC 4552 566 188.90474 12.56373 1.61 −6.677 ± 0.048 −7.588 ± 0.044 2.45 ± 0.30 0.99<br />
NGC 4552 568 188.90755 12.57127 2.09 −6.882 ± 0.042 −8.480 ± 0.033 1.93 ± 0.18 1.00<br />
NGC 4552 569 188.90144 12.55572 1.73 −7.183 ± 0.057 −8.018 ± 0.041 3.46 ± 0.27 0.97<br />
NGC 4552 571 188.90277 12.55990 1.63 −6.628 ± 0.056 −8.148 ± 0.084 4.39 ± 0.38 0.96<br />
NGC 4552 576 188.91249 12.58664 3.74 −6.731 ± 0.047 −7.589 ± 0.039 2.11 ± 0.22 0.99<br />
NGC 4552 577 188.90741 12.57375 2.37 −7.609 ± 0.034 −8.795 ± 0.022 2.88 ± 0.17 1.00<br />
NGC 4552 578 188.89673 12.54660 2.59 −6.200 ± 0.045 −7.652 ± 0.038 1.73 ± 0.23 0.98<br />
NGC 4552 579 188.91268 12.58737 3.83 −6.243 ± 0.046 −7.458 ± 0.046 4.33 ± 0.20 0.83<br />
NGC 4552 582 188.90474 12.56830 1.98 −9.697 ± 0.032 −10.755 ± 0.016 2.90 ± 0.15 1.00<br />
NGC 4552 583 188.90260 12.56268 1.77 −5.523 ± 0.096 −6.583 ± 0.096 3.28 ± 0.39 0.80<br />
NGC 4552 585 188.89399 12.54126 3.21 −5.569 ± 0.127 −7.046 ± 0.067 4.07 ± 0.49 0.73<br />
NGC 4552 589 188.90974 12.58286 3.34 −10.121 ± 0.022 −11.351 ± 0.019 4.02 ± 0.09 1.00<br />
NGC 4552 590 188.90778 12.57766 2.79 −6.366 ± 0.043 −7.690 ± 0.048 2.61 ± 0.26 0.99<br />
NGC 4552 592 188.90156 12.56231 1.86 −6.929 ± 0.032 −8.389 ± 0.026 2.24 ± 0.27 1.00<br />
NGC 4552 593 188.90468 12.57049 2.19 −7.492 ± 0.027 −8.485 ± 0.019 2.07 ± 0.17 1.00<br />
NGC 4552 594 188.89963 12.55774 1.95 −7.548 ± 0.020 −8.595 ± 0.031 2.63 ± 0.17 1.00<br />
Continued on Next Page. . .<br />
378
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4552 596 188.89918 12.55686 2.00 −9.005 ± 0.028 −10.355 ± 0.020 2.48 ± 0.17 1.00<br />
NGC 4552 597 188.90584 12.57379 2.46 −6.759 ± 0.068 −7.837 ± 0.094 4.43 ± 0.40 0.91<br />
NGC 4552 598 188.90728 12.57741 2.78 −4.771 ± 0.376 −6.618 ± 0.095 1.97 ± 0.63 0.95<br />
NGC 4552 600 188.90131 12.56289 1.92 −5.631 ± 0.099 −6.646 ± 0.080 2.46 ± 0.44 0.94<br />
NGC 4552 601 188.90438 12.57140 2.31 −5.764 ± 0.092 −7.133 ± 0.069 2.73 ± 0.45 0.96<br />
NGC 4552 602 188.90107 12.56314 1.96 −9.082 ± 0.021 −10.569 ± 0.017 2.30 ± 0.11 1.00<br />
NGC 4552 604 188.89456 12.54679 2.81 −6.870 ± 0.040 −7.754 ± 0.030 2.41 ± 0.18 0.99<br />
NGC 4552 605 188.90684 12.57902 2.99 −8.596 ± 0.014 −9.524 ± 0.023 2.34 ± 0.16 1.00<br />
NGC 4552 606 188.90077 12.56351 2.01 −5.594 ± 1.012 −6.859 ± 1.112 1.25 ± 0.42 0.83<br />
NGC 4552 608 188.90546 12.57590 2.71 −7.375 ± 0.104 −8.157 ± 0.082 6.37 ± 0.72 0.60<br />
NGC 4552 610 188.90009 12.56286 2.05 −6.970 ± 0.464 −8.215 ± 0.043 2.12 ± 0.42 1.00<br />
NGC 4552 611 188.89447 12.54884 2.72 −7.135 ± 0.037 −8.138 ± 0.048 5.05 ± 0.22 0.90<br />
NGC 4552 612 188.89946 12.56176 2.08 −7.857 ± 0.022 −8.979 ± 0.019 2.36 ± 0.12 1.00<br />
NGC 4552 613 188.89398 12.54781 2.82 −7.939 ± 0.030 −9.413 ± 0.020 2.11 ± 0.16 1.00<br />
NGC 4552 614 188.89451 12.54925 2.70 −6.050 ± 0.301 −6.941 ± 0.279 2.09 ± 0.41 0.98<br />
NGC 4552 617 188.90764 12.58370 3.50 −8.468 ± 0.027 −9.360 ± 0.025 2.34 ± 0.20 1.00<br />
NGC 4552 619 188.89721 12.55759 2.24 −5.760 ± 0.655 −7.285 ± 0.043 1.71 ± 0.36 0.97<br />
NGC 4552 621 188.89946 12.56445 2.20 −7.429 ± 0.099 −9.100 ± 0.023 2.33 ± 0.33 1.00<br />
NGC 4552 622 188.89996 12.56567 2.22 −6.467 ± 0.047 −7.858 ± 0.042 1.97 ± 0.29 0.99<br />
NGC 4552 626 188.89923 12.56469 2.24 −7.766 ± 0.884 −9.189 ± 0.272 1.37 ± 0.31 0.94<br />
NGC 4552 627 188.88807 12.53668 4.11 −7.122 ± 0.054 −7.850 ± 0.037 3.61 ± 0.26 0.96<br />
NGC 4552 629 188.89583 12.55706 2.40 −8.744 ± 0.015 −10.007 ± 0.016 2.19 ± 0.11 1.00<br />
NGC 4552 631 188.89119 12.54579 3.23 −6.949 ± 0.032 −8.221 ± 0.032 2.59 ± 0.21 1.00<br />
NGC 4552 632 188.89142 12.54678 3.16 −7.912 ± 0.020 −9.494 ± 0.017 2.12 ± 0.10 1.00<br />
NGC 4552 633 188.89462 12.55540 2.55 −7.965 ± 0.034 −9.268 ± 0.018 1.59 ± 0.15 1.00<br />
NGC 4552 635 188.89665 12.56159 2.39 −11.010 ± 0.009 −11.977 ± 0.010 9.96 ± 0.07 1.00<br />
NGC 4552 636 188.89973 12.56927 2.50 −5.618 ± 0.074 −7.123 ± 0.078 3.58 ± 0.38 0.85<br />
NGC 4552 639 188.90379 12.58075 3.33 −6.556 ± 0.092 −7.941 ± 0.126 5.25 ± 0.70 0.83<br />
NGC 4552 646 188.89483 12.55935 2.55 −6.747 ± 1.109 −7.899 ± 0.050 2.48 ± 0.65 0.99<br />
NGC 4552 650 188.89865 12.56964 2.63 −7.278 ± 0.033 −8.326 ± 0.027 2.29 ± 0.23 1.00<br />
NGC 4552 651 188.88823 12.54301 3.69 −7.028 ± 0.045 −8.286 ± 0.023 2.13 ± 0.18 1.00<br />
NGC 4552 652 188.90225 12.57905 3.23 −8.065 ± 0.022 −9.036 ± 0.020 2.38 ± 0.16 1.00<br />
NGC 4552 653 188.89719 12.56635 2.55 −9.717 ± 0.027 −10.748 ± 0.022 3.56 ± 0.18 1.00<br />
NGC 4552 654 188.90208 12.57898 3.23 −6.665 ± 0.034 −7.762 ± 0.149 4.98 ± 0.80 0.82<br />
NGC 4552 656 188.89592 12.56366 2.55 −8.478 ± 0.020 −9.496 ± 0.019 5.35 ± 0.07 0.99<br />
NGC 4552 657 188.88800 12.54346 3.69 −5.735 ± 0.972 −6.862 ± 0.428 1.26 ± 0.50 0.83<br />
NGC 4552 658 188.90315 12.58230 3.53 −4.743 ± 0.623 −5.936 ± 0.073 1.02 ± 0.35 0.59<br />
NGC 4552 659 188.89642 12.56542 2.58 −5.379 ± 0.088 −6.509 ± 0.057 2.53 ± 0.41 0.92<br />
NGC 4552 660 188.90314 12.58282 3.59 −7.065 ± 0.031 −8.505 ± 0.023 2.19 ± 0.21 1.00<br />
NGC 4552 663 188.89914 12.57305 2.87 −9.197 ± 0.014 −10.289 ± 0.012 2.48 ± 0.10 1.00<br />
NGC 4552 665 188.89337 12.55877 2.71 −5.724 ± 0.552 −7.161 ± 0.065 2.27 ± 0.38 0.98<br />
NGC 4552 666 188.89392 12.56095 2.69 −7.117 ± 0.029 −8.525 ± 0.025 1.82 ± 0.16 1.00<br />
NGC 4552 667 188.89348 12.56017 2.72 −7.556 ± 0.053 −8.696 ± 0.094 7.48 ± 0.70 0.62<br />
NGC 4552 670 188.90465 12.59020 4.37 −5.317 ± 0.110 −6.690 ± 0.559 1.74 ± 0.49 0.94<br />
NGC 4552 673 188.89788 12.57454 3.10 −5.434 ± 0.071 −6.007 ± 0.121 3.62 ± 0.42 0.56<br />
NGC 4552 674 188.89480 12.56685 2.83 −8.793 ± 0.012 −9.754 ± 0.016 2.19 ± 0.11 1.00<br />
NGC 4552 675 188.89377 12.56410 2.81 −5.241 ± 0.113 −6.519 ± 0.195 2.76 ± 0.77 0.89<br />
NGC 4552 676 188.90315 12.58846 4.23 −4.978 ± 1.689 −6.624 ± 0.296 0.87 ± 0.41 0.56<br />
NGC 4552 681 188.90276 12.58921 4.33 −7.272 ± 0.039 −8.160 ± 0.028 2.42 ± 0.20 1.00<br />
NGC 4552 684 188.88982 12.55704 3.12 −7.351 ± 0.023 −8.539 ± 0.026 1.86 ± 0.15 1.00<br />
NGC 4552 686 188.90055 12.58486 3.95 −7.043 ± 0.062 −8.368 ± 0.026 2.20 ± 0.22 1.00<br />
NGC 4552 690 188.88844 12.55524 3.29 −8.516 ± 0.027 −10.004 ± 0.018 2.69 ± 0.14 1.00<br />
NGC 4552 691 188.88565 12.54835 3.75 −9.249 ± 0.017 −10.293 ± 0.015 2.33 ± 0.08 1.00<br />
NGC 4552 695 188.89726 12.58062 3.72 −6.063 ± 0.098 −6.848 ± 1.612 1.08 ± 0.38 0.74<br />
NGC 4552 697 188.88798 12.55727 3.34 −8.068 ± 0.015 −9.365 ± 0.022 2.37 ± 0.15 1.00<br />
NGC 4552 701 188.88300 12.54570 4.15 −8.678 ± 0.019 −9.600 ± 0.019 2.77 ± 0.09 1.00<br />
NGC 4552 705 188.88894 12.56193 3.30 −4.965 ± 0.163 −6.326 ± 0.183 3.38 ± 0.86 0.72<br />
NGC 4552 707 188.89296 12.57249 3.39 −5.917 ± 0.057 −7.277 ± 0.100 2.29 ± 0.55 0.98<br />
NGC 4552 708 188.88732 12.55799 3.43 −4.907 ± 0.087 −6.141 ± 0.644 2.08 ± 0.45 0.90<br />
NGC 4552 711 188.89897 12.58861 4.45 −5.565 ± 0.310 −6.778 ± 0.367 1.50 ± 0.47 0.90<br />
NGC 4552 714 188.88365 12.55215 3.90 −6.995 ± 0.039 −8.389 ± 0.027 2.59 ± 0.17 1.00<br />
NGC 4552 716 188.88031 12.54421 4.51 −7.731 ± 0.019 −8.649 ± 0.031 3.55 ± 0.11 1.00<br />
Continued on Next Page. . .<br />
379
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4552 718 188.89143 12.57343 3.60 −6.350 ± 0.110 −8.004 ± 0.150 4.75 ± 1.12 0.91<br />
NGC 4552 719 188.89544 12.58379 4.16 −6.372 ± 0.059 −7.782 ± 0.147 5.10 ± 0.96 0.81<br />
NGC 4552 723 188.88994 12.57079 3.58 −6.578 ± 0.090 −7.955 ± 0.067 4.21 ± 0.29 0.95<br />
NGC 4552 724 188.87931 12.54383 4.64 −6.837 ± 0.053 −7.761 ± 0.038 2.91 ± 0.26 0.98<br />
NGC 4552 726 188.89351 12.58083 4.03 −7.277 ± 0.026 −8.669 ± 0.023 1.65 ± 0.13 1.00<br />
NGC 4552 727 188.89156 12.57660 3.83 −6.010 ± 0.144 −7.328 ± 0.405 4.81 ± 0.96 0.68<br />
NGC 4552 732 188.88939 12.57270 3.76 −8.038 ± 0.019 −9.120 ± 0.024 2.88 ± 0.15 1.00<br />
NGC 4552 733 188.88945 12.57320 3.78 −7.645 ± 0.016 −8.548 ± 0.019 2.34 ± 0.18 1.00<br />
NGC 4552 738 188.89003 12.57606 3.93 −5.884 ± 0.107 −6.879 ± 0.047 2.88 ± 0.35 0.92<br />
NGC 4552 739 188.88414 12.56108 3.85 −7.535 ± 0.053 −8.576 ± 0.135 1.98 ± 0.30 1.00<br />
NGC 4552 740 188.88289 12.55802 3.96 −5.979 ± 0.085 −7.626 ± 0.094 3.05 ± 0.49 0.98<br />
NGC 4552 742 188.89293 12.58391 4.36 −5.851 ± 0.094 −6.787 ± 0.103 3.20 ± 0.48 0.85<br />
NGC 4552 743 188.89156 12.58039 4.15 −9.966 ± 0.033 −11.574 ± 0.054 10.09 ± 0.55 1.00<br />
NGC 4552 744 188.87849 12.54727 4.61 −5.987 ± 0.147 −7.227 ± 0.105 4.48 ± 0.81 0.71<br />
NGC 4552 747 188.88939 12.57496 3.91 −6.150 ± 0.108 −6.844 ± 0.058 3.39 ± 0.44 0.82<br />
NGC 4552 751 188.87970 12.55218 4.36 −8.107 ± 0.033 −9.671 ± 0.019 3.00 ± 0.15 1.00<br />
NGC 4552 752 188.88074 12.55512 4.21 −5.136 ± 0.468 −6.011 ± 0.073 2.42 ± 0.49 0.87<br />
NGC 4552 753 188.87619 12.54389 4.99 −10.649 ± 0.019 −11.728 ± 0.014 3.84 ± 0.09 1.00<br />
NGC 4552 759 188.87670 12.54735 4.82 −6.875 ± 0.041 −8.124 ± 0.025 2.71 ± 0.17 1.00<br />
NGC 4552 760 188.87996 12.55567 4.30 −4.807 ± 0.214 −6.519 ± 1.114 1.58 ± 0.61 0.90<br />
NGC 4552 762 188.88106 12.56052 4.20 −8.526 ± 0.040 −9.648 ± 0.028 2.87 ± 0.22 1.00<br />
NGC 4552 763 188.88328 12.56631 4.09 −6.360 ± 0.071 −7.754 ± 0.042 2.70 ± 0.37 0.99<br />
NGC 4552 765 188.88899 12.58107 4.43 −7.023 ± 0.029 −8.375 ± 0.026 2.19 ± 0.16 1.00<br />
NGC 4552 767 188.89071 12.58573 4.70 −7.515 ± 0.030 −8.373 ± 0.034 3.18 ± 0.30 1.00<br />
NGC 4552 772 188.88942 12.58337 4.59 −7.304 ± 0.034 −8.260 ± 0.028 3.09 ± 0.14 1.00<br />
NGC 4621 4 190.53869 11.66471 3.00 −7.603 ± 0.027 −8.751 ± 0.021 2.73 ± 0.14 1.00<br />
NGC 4621 17 190.52677 11.63018 2.13 −7.040 ± 0.233 −7.932 ± 0.051 2.65 ± 0.42 1.00<br />
NGC 4621 18 190.52519 11.62518 2.38 −7.957 ± 0.015 −8.901 ± 0.039 4.50 ± 0.14 0.98<br />
NGC 4621 21 190.52475 11.62526 2.35 −7.419 ± 0.031 −8.651 ± 0.030 2.17 ± 0.13 1.00<br />
NGC 4621 31 190.52880 11.64375 1.72 −8.341 ± 0.022 −9.435 ± 0.018 2.37 ± 0.14 1.00<br />
NGC 4621 32 190.53464 11.66308 2.62 −7.969 ± 0.025 −8.888 ± 0.023 2.59 ± 0.12 1.00<br />
NGC 4621 35 190.52247 11.62385 2.35 −5.939 ± 0.092 −6.828 ± 0.161 3.36 ± 0.52 0.78<br />
NGC 4621 37 190.52312 11.62623 2.20 −6.377 ± 0.104 −7.668 ± 0.135 5.24 ± 0.83 0.65<br />
NGC 4621 43 190.52331 11.62822 2.06 −5.716 ± 0.066 −6.325 ± 0.193 2.01 ± 0.95 0.90<br />
NGC 4621 53 190.52171 11.62760 2.03 −8.151 ± 0.019 −9.468 ± 0.044 3.83 ± 0.16 1.00<br />
NGC 4621 55 190.51964 11.62110 2.47 −7.056 ± 0.041 −8.252 ± 0.036 2.85 ± 0.16 1.00<br />
NGC 4621 62 190.52060 11.62697 2.03 −5.149 ± 0.076 −5.734 ± 1.153 2.34 ± 0.70 0.80<br />
NGC 4621 65 190.51878 11.62144 2.41 −7.199 ± 0.060 −8.026 ± 0.063 4.86 ± 0.26 0.84<br />
NGC 4621 69 190.52898 11.65603 1.89 −6.175 ± 0.071 −6.936 ± 0.520 2.22 ± 0.34 0.96<br />
NGC 4621 73 190.52153 11.63312 1.62 −7.912 ± 0.037 −9.219 ± 0.046 4.18 ± 0.21 1.00<br />
NGC 4621 74 190.51780 11.62091 2.43 −7.858 ± 0.026 −9.282 ± 0.037 2.47 ± 0.18 1.00<br />
NGC 4621 75 190.52857 11.65670 1.88 −7.781 ± 0.021 −8.730 ± 0.023 2.88 ± 0.12 1.00<br />
NGC 4621 76 190.52115 11.63235 1.66 −6.849 ± 0.043 −7.718 ± 0.074 2.90 ± 0.31 0.97<br />
NGC 4621 80 190.51800 11.62314 2.25 −6.647 ± 0.044 −7.701 ± 0.064 2.44 ± 0.36 0.99<br />
NGC 4621 88 190.52990 11.66530 2.42 −5.820 ± 0.079 −6.831 ± 0.097 2.18 ± 0.40 0.96<br />
NGC 4621 91 190.51727 11.62020 2.48 −7.941 ± 0.041 −9.375 ± 0.017 1.73 ± 0.21 1.00<br />
NGC 4621 92 190.51645 11.62251 2.26 −8.183 ± 0.021 −9.646 ± 0.015 2.08 ± 0.12 1.00<br />
NGC 4621 93 190.52144 11.63892 1.27 −7.054 ± 0.042 −8.388 ± 0.034 2.28 ± 0.26 1.00<br />
NGC 4621 94 190.52859 11.66346 2.22 −8.524 ± 0.043 −9.426 ± 0.057 5.31 ± 0.26 1.00<br />
NGC 4621 96 190.51568 11.62114 2.36 −7.969 ± 0.027 −9.519 ± 0.021 2.25 ± 0.09 1.00<br />
NGC 4621 103 190.52334 11.64796 1.22 −7.835 ± 0.022 −9.041 ± 0.020 2.09 ± 0.11 1.00<br />
NGC 4621 106 190.52556 11.65580 1.61 −7.915 ± 0.022 −9.200 ± 0.018 2.32 ± 0.12 1.00<br />
NGC 4621 108 190.51975 11.63727 1.25 −7.230 ± 0.025 −8.577 ± 0.033 2.05 ± 0.17 1.00<br />
NGC 4621 109 190.52278 11.64749 1.17 −8.738 ± 0.019 −10.166 ± 0.020 2.94 ± 0.12 1.00<br />
NGC 4621 110 190.52181 11.64457 1.10 −7.470 ± 0.040 −8.630 ± 0.032 3.02 ± 0.15 1.00<br />
NGC 4621 111 190.51578 11.62479 2.05 −6.417 ± 0.088 −8.275 ± 0.157 4.53 ± 0.85 0.94<br />
NGC 4621 112 190.52279 11.64867 1.18 −10.315 ± 0.009 −11.644 ± 0.010 3.47 ± 0.06 1.00<br />
NGC 4621 113 190.51768 11.63201 1.51 −7.413 ± 0.035 −8.744 ± 0.021 2.56 ± 0.14 1.00<br />
NGC 4621 114 190.51660 11.62852 1.76 −7.195 ± 0.027 −8.141 ± 0.048 3.07 ± 0.18 1.00<br />
NGC 4621 115 190.51868 11.63559 1.30 −6.748 ± 0.066 −7.957 ± 0.057 2.10 ± 0.22 1.00<br />
NGC 4621 116 190.52116 11.64415 1.06 −7.582 ± 0.024 −8.805 ± 0.023 2.03 ± 0.13 1.00<br />
Continued on Next Page. . .<br />
380
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4621 118 190.52415 11.65405 1.43 −7.270 ± 0.023 −8.386 ± 0.031 2.12 ± 0.18 1.00<br />
NGC 4621 120 190.52269 11.64955 1.18 −5.101 ± 0.440 −6.274 ± 0.100 1.63 ± 0.46 0.85<br />
NGC 4621 121 190.51474 11.62430 2.07 −6.816 ± 0.032 −8.268 ± 0.038 2.12 ± 0.19 1.00<br />
NGC 4621 125 190.52383 11.65566 1.48 −6.950 ± 0.027 −8.112 ± 0.052 2.63 ± 0.12 1.00<br />
NGC 4621 126 190.51799 11.63664 1.19 −7.778 ± 0.026 −9.167 ± 0.023 2.42 ± 0.19 1.00<br />
NGC 4621 127 190.51500 11.62709 1.84 −7.026 ± 0.028 −8.294 ± 0.023 1.61 ± 0.18 1.00<br />
NGC 4621 129 190.51446 11.62642 1.88 −6.079 ± 0.049 −7.144 ± 0.066 2.03 ± 0.25 0.98<br />
NGC 4621 132 190.51451 11.62731 1.81 −7.698 ± 0.024 −8.900 ± 0.024 1.98 ± 0.14 1.00<br />
NGC 4621 133 190.52281 11.65446 1.35 −6.582 ± 0.032 −7.506 ± 0.487 1.99 ± 0.30 0.99<br />
NGC 4621 135 190.51383 11.62552 1.95 −6.516 ± 0.044 −7.981 ± 0.048 1.98 ± 0.19 1.00<br />
NGC 4621 136 190.51825 11.64014 0.98 −7.961 ± 0.052 −9.574 ± 0.052 5.23 ± 0.23 1.00<br />
NGC 4621 138 190.51448 11.62831 1.72 −7.534 ± 0.021 −8.309 ± 0.037 2.25 ± 0.15 1.00<br />
NGC 4621 140 190.52008 11.64696 0.93 −7.533 ± 0.031 −8.613 ± 0.050 2.38 ± 0.22 1.00<br />
NGC 4621 141 190.51407 11.62718 1.81 −7.307 ± 0.035 −8.704 ± 0.049 1.95 ± 0.20 1.00<br />
NGC 4621 142 190.52070 11.64922 1.01 −7.295 ± 0.042 −8.678 ± 0.045 1.45 ± 0.31 1.00<br />
NGC 4621 144 190.51147 11.61945 2.46 −8.955 ± 0.566 −9.514 ± 0.033 1.60 ± 0.28 1.00<br />
NGC 4621 145 190.52122 11.65150 1.11 −8.801 ± 0.042 −9.745 ± 0.062 5.85 ± 0.27 1.00<br />
NGC 4621 146 190.52035 11.64877 0.97 −8.426 ± 0.023 −9.481 ± 0.019 2.48 ± 0.15 1.00<br />
NGC 4621 150 190.51626 11.63555 1.18 −8.730 ± 0.017 −9.894 ± 0.034 3.10 ± 0.13 1.00<br />
NGC 4621 155 190.51313 11.62785 1.73 −6.708 ± 0.040 −7.857 ± 0.024 2.30 ± 0.16 0.99<br />
NGC 4621 161 190.51299 11.62918 1.61 −7.194 ± 0.047 −8.284 ± 0.082 3.63 ± 0.33 1.00<br />
NGC 4621 164 190.52368 11.66446 1.99 −6.794 ± 0.063 −7.886 ± 0.069 3.70 ± 0.41 1.00<br />
NGC 4621 173 190.51662 11.64370 0.69 −8.733 ± 0.019 −9.860 ± 0.016 2.32 ± 0.09 1.00<br />
NGC 4621 175 190.50937 11.62009 2.39 −7.764 ± 0.025 −9.062 ± 0.027 2.08 ± 0.18 1.00<br />
NGC 4621 177 190.52132 11.65984 1.55 −5.694 ± 0.074 −6.830 ± 0.100 3.24 ± 0.40 0.80<br />
NGC 4621 178 190.52110 11.65940 1.50 −5.069 ± 0.270 −5.791 ± 0.493 2.62 ± 1.92 0.77<br />
NGC 4621 179 190.52177 11.66231 1.74 −7.302 ± 0.025 −8.650 ± 0.015 1.72 ± 0.14 1.00<br />
NGC 4621 185 190.51562 11.64297 0.65 −7.017 ± 0.039 −8.297 ± 0.073 3.27 ± 0.26 1.00<br />
NGC 4621 187 190.51291 11.63435 1.16 −6.907 ± 0.052 −7.962 ± 0.048 2.88 ± 0.23 1.00<br />
NGC 4621 189 190.51346 11.63641 1.00 −6.798 ± 0.043 −7.578 ± 0.075 3.46 ± 0.22 0.94<br />
NGC 4621 192 190.51980 11.65811 1.34 −8.186 ± 0.016 −9.507 ± 0.018 2.00 ± 0.10 1.00<br />
NGC 4621 193 190.51602 11.64559 0.59 −5.929 ± 0.908 −6.692 ± 0.627 1.70 ± 0.45 0.93<br />
NGC 4621 194 190.51404 11.63944 0.78 −8.814 ± 0.014 −9.836 ± 0.019 2.53 ± 0.11 1.00<br />
NGC 4621 197 190.51155 11.63144 1.39 −6.486 ± 0.048 −8.131 ± 0.093 5.40 ± 0.45 0.67<br />
NGC 4621 198 190.51338 11.63771 0.89 −7.104 ± 0.031 −8.585 ± 0.023 2.25 ± 0.14 1.00<br />
NGC 4621 199 190.51594 11.64611 0.58 −7.906 ± 0.026 −8.850 ± 0.025 1.45 ± 0.18 1.00<br />
NGC 4621 200 190.51374 11.63917 0.79 −8.218 ± 0.022 −9.420 ± 0.015 2.13 ± 0.10 1.00<br />
NGC 4621 202 190.51889 11.65694 1.21 −6.778 ± 0.048 −8.604 ± 0.067 4.99 ± 0.31 0.90<br />
NGC 4621 203 190.51440 11.64197 0.62 −7.943 ± 0.037 −9.376 ± 0.031 3.06 ± 0.17 1.00<br />
NGC 4621 204 190.51105 11.63140 1.39 −8.004 ± 0.038 −8.967 ± 0.053 3.92 ± 0.18 1.00<br />
NGC 4621 206 190.51422 11.64189 0.62 −5.806 ± 0.068 −7.101 ± 0.049 2.82 ± 0.29 0.94<br />
NGC 4621 207 190.52243 11.66904 2.27 −6.742 ± 0.036 −7.946 ± 0.041 2.78 ± 0.12 1.00<br />
NGC 4621 209 190.51211 11.63579 1.02 −9.036 ± 0.018 −10.423 ± 0.015 2.98 ± 0.12 1.00<br />
NGC 4621 210 190.51455 11.64388 0.53 −7.217 ± 0.026 −8.510 ± 0.040 1.48 ± 0.17 1.00<br />
NGC 4621 213 190.50742 11.62139 2.28 −8.343 ± 0.029 −9.664 ± 0.016 2.27 ± 0.14 1.00<br />
NGC 4621 214 190.51921 11.66111 1.52 −6.154 ± 0.036 −7.282 ± 0.037 1.93 ± 0.23 0.98<br />
NGC 4621 215 190.51584 11.65006 0.63 −8.040 ± 0.015 −9.005 ± 0.027 1.66 ± 0.13 1.00<br />
NGC 4621 217 190.51604 11.65151 0.71 −7.898 ± 0.030 −8.905 ± 0.025 2.25 ± 0.16 1.00<br />
NGC 4621 218 190.51645 11.65289 0.81 −6.236 ± 0.045 −7.752 ± 0.057 1.76 ± 0.29 0.99<br />
NGC 4621 219 190.51432 11.64593 0.44 −7.303 ± 0.092 −8.799 ± 0.133 5.83 ± 0.82 0.85<br />
NGC 4621 223 190.51062 11.63464 1.10 −6.749 ± 0.031 −7.698 ± 0.030 2.00 ± 0.25 0.99<br />
NGC 4621 225 190.51293 11.64292 0.47 −7.046 ± 0.074 −8.295 ± 0.066 2.94 ± 0.34 1.00<br />
NGC 4621 226 190.51212 11.64040 0.63 −9.220 ± 0.021 −10.184 ± 0.018 2.75 ± 0.14 1.00<br />
NGC 4621 228 190.51068 11.63617 0.97 −6.002 ± 0.082 −7.492 ± 0.081 2.64 ± 0.35 0.98<br />
NGC 4621 229 190.51743 11.65906 1.28 −7.763 ± 0.034 −8.551 ± 0.042 3.79 ± 0.13 1.00<br />
NGC 4621 233 190.51630 11.65625 1.02 −8.414 ± 0.016 −9.379 ± 0.021 2.61 ± 0.15 1.00<br />
NGC 4621 234 190.51737 11.66019 1.37 −8.399 ± 0.028 −9.809 ± 0.028 2.02 ± 0.18 1.00<br />
NGC 4621 235 190.51332 11.64720 0.34 −7.721 ± 0.027 −8.825 ± 0.040 2.25 ± 0.16 1.00<br />
NGC 4621 236 190.51678 11.65874 1.23 −7.117 ± 0.043 −8.309 ± 0.035 2.37 ± 0.20 1.00<br />
NGC 4621 238 190.51080 11.63940 0.68 −7.828 ± 0.037 −9.017 ± 0.031 2.24 ± 0.18 1.00<br />
NGC 4621 239 190.51297 11.64677 0.31 −8.805 ± 0.024 −9.894 ± 0.023 2.48 ± 0.13 1.00<br />
NGC 4621 240 190.51814 11.66370 1.67 −6.510 ± 0.027 −7.658 ± 0.033 1.93 ± 0.19 0.99<br />
Continued on Next Page. . .<br />
381
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4621 241 190.50902 11.63497 1.07 −10.179 ± 0.023 −11.178 ± 0.020 4.22 ± 0.10 0.82<br />
NGC 4621 243 190.51034 11.63840 0.77 −6.270 ± 0.084 −7.535 ± 0.142 3.36 ± 0.54 0.94<br />
NGC 4621 244 190.51865 11.66621 1.89 −4.712 ± 0.365 −5.829 ± 0.073 1.58 ± 0.50 0.78<br />
NGC 4621 246 190.51677 11.66044 1.36 −7.179 ± 0.025 −8.341 ± 0.028 2.40 ± 0.23 1.00<br />
NGC 4621 247 190.51633 11.65949 1.27 −8.543 ± 0.020 −9.548 ± 0.015 1.99 ± 0.10 1.00<br />
NGC 4621 248 190.51395 11.65172 0.58 −5.594 ± 0.666 −6.880 ± 0.723 1.01 ± 0.50 0.60<br />
NGC 4621 254 190.51190 11.64679 0.22 −6.942 ± 0.062 −8.207 ± 0.098 1.79 ± 0.36 1.00<br />
NGC 4621 255 190.51068 11.64305 0.37 −8.807 ± 0.021 −10.035 ± 0.024 2.23 ± 0.17 1.00<br />
NGC 4621 257 190.51111 11.64497 0.23 −6.529 ± 0.074 −7.826 ± 0.133 3.46 ± 0.51 0.96<br />
NGC 4621 258 190.50799 11.63486 1.08 −8.335 ± 0.027 −9.669 ± 0.024 2.33 ± 0.10 1.00<br />
NGC 4621 259 190.50996 11.64180 0.46 −10.304 ± 0.016 −11.444 ± 0.011 2.35 ± 0.10 1.00<br />
NGC 4621 260 190.50774 11.63489 1.08 −7.247 ± 0.026 −8.583 ± 0.034 2.65 ± 0.15 1.00<br />
NGC 4621 262 190.51038 11.64415 0.27 −6.053 ± 0.277 −7.816 ± 0.376 5.18 ± 2.32 0.70<br />
NGC 4621 265 190.51351 11.65509 0.81 −5.961 ± 0.170 −7.480 ± 0.077 1.24 ± 0.29 0.87<br />
NGC 4621 266 190.51456 11.65871 1.14 −7.811 ± 0.024 −9.318 ± 0.019 1.66 ± 0.15 1.00<br />
NGC 4621 267 190.51146 11.64850 0.23 −6.284 ± 0.104 −7.603 ± 0.131 1.72 ± 0.55 0.98<br />
NGC 4621 269 190.50538 11.62912 1.63 −8.167 ± 0.028 −9.515 ± 0.020 2.32 ± 0.17 1.00<br />
NGC 4621 270 190.51105 11.64805 0.17 −8.349 ± 0.030 −9.873 ± 0.023 2.03 ± 0.13 1.00<br />
NGC 4621 271 190.50841 11.63952 0.67 −7.705 ± 0.029 −8.940 ± 0.037 2.66 ± 0.18 1.00<br />
NGC 4621 272 190.51332 11.65633 0.90 −7.969 ± 0.018 −9.385 ± 0.024 2.07 ± 0.17 1.00<br />
NGC 4621 273 190.50832 11.63999 0.63 −6.317 ± 0.582 −7.650 ± 0.093 1.13 ± 0.34 0.81<br />
NGC 4621 275 190.51196 11.65245 0.54 −6.557 ± 0.233 −8.025 ± 0.158 1.42 ± 0.31 1.00<br />
NGC 4621 281 190.51146 11.65132 0.43 −7.320 ± 0.042 −8.251 ± 0.032 1.96 ± 0.23 1.00<br />
NGC 4621 284 190.50872 11.64281 0.38 −8.311 ± 0.120 −9.160 ± 0.072 6.24 ± 0.68 0.96<br />
NGC 4621 286 190.51268 11.65623 0.87 −7.545 ± 0.048 −8.540 ± 0.072 4.06 ± 0.31 0.99<br />
NGC 4621 287 190.51298 11.65724 0.97 −7.469 ± 0.025 −8.491 ± 0.021 1.67 ± 0.18 1.00<br />
NGC 4621 292 190.51190 11.65472 0.72 −6.345 ± 0.124 −8.017 ± 0.061 4.70 ± 0.55 0.88<br />
NGC 4621 293 190.50275 11.62471 2.06 −7.948 ± 0.023 −9.209 ± 0.009 1.28 ± 0.19 0.89<br />
NGC 4621 294 190.50243 11.62375 2.15 −7.405 ± 0.062 −8.394 ± 0.112 4.33 ± 0.69 0.97<br />
NGC 4621 295 190.50934 11.64647 0.04 −7.419 ± 0.054 −8.139 ± 0.398 1.55 ± 0.38 1.00<br />
NGC 4621 296 190.50867 11.64499 0.19 −9.560 ± 0.025 −10.703 ± 0.011 2.50 ± 0.13 1.00<br />
NGC 4621 297 190.50568 11.63584 1.04 −5.816 ± 0.063 −6.718 ± 0.214 2.26 ± 0.77 0.94<br />
NGC 4621 299 190.50586 11.63667 0.97 −6.966 ± 0.043 −8.364 ± 0.033 2.88 ± 0.17 1.00<br />
NGC 4621 300 190.51206 11.65733 0.95 −5.781 ± 0.111 −6.636 ± 1.645 2.01 ± 0.45 0.95<br />
NGC 4621 304 190.50914 11.64931 0.21 −8.432 ± 0.024 −9.559 ± 0.025 2.35 ± 0.09 1.00<br />
NGC 4621 308 190.50097 11.62335 2.23 −10.157 ± 0.027 −11.415 ± 0.015 2.69 ± 0.08 1.00<br />
NGC 4621 309 190.50661 11.64182 0.52 −5.675 ± 0.672 −7.361 ± 0.419 1.41 ± 0.37 0.92<br />
NGC 4621 310 190.50829 11.64786 0.12 −8.789 ± 0.033 −9.628 ± 0.025 2.05 ± 0.17 1.00<br />
NGC 4621 312 190.50796 11.64683 0.13 −6.771 ± 0.100 −8.017 ± 0.077 2.41 ± 0.36 1.00<br />
NGC 4621 313 190.50635 11.64182 0.53 −9.744 ± 0.022 −10.766 ± 0.013 2.55 ± 0.10 1.00<br />
NGC 4621 315 190.51425 11.66791 1.91 −9.338 ± 0.016 −10.323 ± 0.015 3.19 ± 0.08 1.00<br />
NGC 4621 317 190.50916 11.65137 0.39 −9.552 ± 0.017 −10.572 ± 0.018 2.00 ± 0.09 1.00<br />
NGC 4621 318 190.50962 11.65271 0.51 −7.476 ± 0.031 −8.927 ± 0.025 2.05 ± 0.20 1.00<br />
NGC 4621 319 190.50026 11.62214 2.35 −8.371 ± 0.030 −9.792 ± 0.029 2.61 ± 0.14 1.00<br />
NGC 4621 322 190.50644 11.64284 0.45 −7.859 ± 0.028 −9.107 ± 0.031 2.02 ± 0.16 1.00<br />
NGC 4621 323 190.50687 11.64417 0.33 −8.154 ± 0.020 −9.071 ± 0.040 2.07 ± 0.17 1.00<br />
NGC 4621 324 190.51175 11.66031 1.20 −7.232 ± 0.030 −8.272 ± 0.022 1.18 ± 0.19 0.86<br />
NGC 4621 325 190.50253 11.62988 1.63 −7.644 ± 0.034 −8.947 ± 0.023 2.70 ± 0.18 1.00<br />
NGC 4621 327 190.50859 11.65037 0.31 −7.794 ± 0.034 −9.142 ± 0.030 2.01 ± 0.15 1.00<br />
NGC 4621 331 190.50834 11.65012 0.29 −6.286 ± 1.186 −7.469 ± 0.964 1.29 ± 0.42 0.89<br />
NGC 4621 332 190.50786 11.64914 0.23 −7.285 ± 0.072 −8.649 ± 0.031 1.74 ± 0.21 1.00<br />
NGC 4621 333 190.51044 11.65785 0.97 −6.533 ± 0.050 −7.424 ± 0.325 2.52 ± 0.48 0.98<br />
NGC 4621 335 190.50867 11.65213 0.46 −7.063 ± 0.042 −8.431 ± 0.042 1.35 ± 0.26 0.93<br />
NGC 4621 340 190.50516 11.64224 0.56 −7.527 ± 0.034 −9.049 ± 0.026 2.24 ± 0.17 1.00<br />
NGC 4621 341 190.50628 11.64642 0.28 −7.482 ± 0.025 −9.196 ± 0.034 1.69 ± 0.20 1.00<br />
NGC 4621 344 190.50916 11.65644 0.84 −6.683 ± 0.048 −7.978 ± 0.045 1.89 ± 0.25 1.00<br />
NGC 4621 345 190.50590 11.64589 0.32 −10.026 ± 0.016 −11.115 ± 0.018 2.61 ± 0.10 1.00<br />
NGC 4621 347 190.51445 11.67442 2.48 −7.912 ± 0.022 −9.144 ± 0.018 2.58 ± 0.12 1.00<br />
NGC 4621 348 190.50647 11.64814 0.28 −8.428 ± 0.026 −9.861 ± 0.014 1.70 ± 0.20 1.00<br />
NGC 4621 349 190.50719 11.65048 0.37 −6.863 ± 0.093 −8.279 ± 0.107 2.64 ± 0.47 1.00<br />
NGC 4621 350 190.50781 11.65274 0.53 −6.890 ± 0.030 −8.399 ± 0.083 1.81 ± 0.32 1.00<br />
NGC 4621 351 190.50904 11.65797 0.98 −8.978 ± 0.028 −10.043 ± 0.018 2.21 ± 0.13 1.00<br />
Continued on Next Page. . .<br />
382
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4621 352 190.50621 11.64846 0.31 −8.474 ± 0.796 −9.541 ± 0.024 1.72 ± 0.35 1.00<br />
NGC 4621 354 190.50546 11.64713 0.34 −8.405 ± 0.025 −9.613 ± 0.018 2.16 ± 0.18 1.00<br />
NGC 4621 357 190.50827 11.65675 0.88 −7.618 ± 0.036 −8.953 ± 0.021 1.46 ± 0.17 1.00<br />
NGC 4621 358 190.50523 11.64657 0.36 −5.876 ± 0.499 −7.296 ± 0.055 1.68 ± 0.39 0.97<br />
NGC 4621 360 190.50098 11.63305 1.44 −6.690 ± 0.123 −7.453 ± 0.093 4.92 ± 0.64 0.66<br />
NGC 4621 361 190.50743 11.65418 0.66 −6.987 ± 0.033 −8.383 ± 0.050 2.06 ± 0.19 1.00<br />
NGC 4621 363 190.50653 11.65141 0.47 −4.991 ± 0.265 −6.869 ± 0.340 4.19 ± 0.94 0.53<br />
NGC 4621 364 190.50808 11.65673 0.88 −9.146 ± 0.014 −10.446 ± 0.012 2.27 ± 0.12 1.00<br />
NGC 4621 367 190.50520 11.64772 0.37 −7.794 ± 0.041 −9.309 ± 0.019 4.29 ± 0.17 1.00<br />
NGC 4621 368 190.50283 11.63987 0.85 −5.247 ± 0.148 −6.441 ± 0.204 2.08 ± 0.97 0.92<br />
NGC 4621 369 190.50011 11.63062 1.66 −7.892 ± 0.024 −8.913 ± 0.019 2.02 ± 0.21 1.00<br />
NGC 4621 370 190.50595 11.65031 0.42 −7.283 ± 0.039 −8.720 ± 0.034 1.85 ± 0.18 1.00<br />
NGC 4621 372 190.50695 11.65389 0.65 −7.477 ± 0.035 −8.761 ± 0.023 1.35 ± 0.12 0.92<br />
NGC 4621 373 190.50524 11.64900 0.40 −6.629 ± 0.044 −7.425 ± 0.069 2.05 ± 0.24 0.99<br />
NGC 4621 374 190.50624 11.65287 0.59 −8.001 ± 0.050 −9.029 ± 0.020 1.89 ± 0.27 1.00<br />
NGC 4621 375 190.50607 11.65239 0.56 −9.160 ± 0.019 −10.198 ± 0.030 2.31 ± 0.22 1.00<br />
NGC 4621 376 190.50568 11.65115 0.49 −8.033 ± 0.036 −9.355 ± 0.027 2.02 ± 0.26 1.00<br />
NGC 4621 384 190.51021 11.66870 1.93 −6.728 ± 0.031 −8.180 ± 0.027 1.90 ± 0.15 1.00<br />
NGC 4621 385 190.49774 11.62786 1.98 −6.793 ± 0.043 −7.555 ± 0.067 2.75 ± 0.31 0.98<br />
NGC 4621 388 190.50692 11.65982 1.16 −7.513 ± 0.026 −8.892 ± 0.022 1.46 ± 0.15 1.00<br />
NGC 4621 389 190.50098 11.64066 0.92 −7.217 ± 0.033 −8.676 ± 0.029 2.00 ± 0.18 1.00<br />
NGC 4621 390 190.50371 11.64959 0.55 −7.068 ± 0.099 −8.439 ± 0.042 4.93 ± 0.27 0.88<br />
NGC 4621 391 190.50369 11.65068 0.60 −7.902 ± 0.031 −9.001 ± 0.030 2.40 ± 0.22 1.00<br />
NGC 4621 392 190.50482 11.65437 0.77 −6.738 ± 0.055 −7.978 ± 0.043 2.67 ± 0.23 1.00<br />
NGC 4621 395 190.51058 11.67454 2.45 −6.788 ± 0.046 −7.769 ± 0.039 2.85 ± 0.25 0.98<br />
NGC 4621 397 190.50816 11.66687 1.77 −7.638 ± 0.025 −8.459 ± 0.029 2.74 ± 0.14 1.00<br />
NGC 4621 398 190.49847 11.63513 1.42 −7.367 ± 0.089 −8.177 ± 0.093 5.26 ± 0.54 0.72<br />
NGC 4621 399 190.50599 11.66000 1.20 −7.229 ± 0.037 −8.884 ± 0.024 1.61 ± 0.21 1.00<br />
NGC 4621 400 190.50397 11.65331 0.74 −6.167 ± 0.117 −7.725 ± 0.170 1.65 ± 0.29 0.98<br />
NGC 4621 403 190.50627 11.66202 1.37 −7.071 ± 0.047 −8.289 ± 0.054 2.83 ± 0.21 1.00<br />
NGC 4621 406 190.50142 11.64672 0.69 −6.508 ± 0.050 −8.079 ± 0.077 2.52 ± 0.35 1.00<br />
NGC 4621 407 190.49808 11.63575 1.40 −6.360 ± 0.055 −7.901 ± 0.100 3.88 ± 0.39 0.95<br />
NGC 4621 409 190.49527 11.62731 2.14 −8.665 ± 0.021 −9.986 ± 0.013 1.79 ± 0.07 1.00<br />
NGC 4621 410 190.50569 11.66196 1.37 −7.323 ± 0.021 −8.466 ± 0.049 2.31 ± 0.19 1.00<br />
NGC 4621 411 190.50326 11.65473 0.87 −8.744 ± 0.017 −9.634 ± 0.016 2.05 ± 0.12 1.00<br />
NGC 4621 413 190.50116 11.64926 0.75 −8.416 ± 0.014 −9.826 ± 0.024 2.70 ± 0.10 1.00<br />
NGC 4621 415 190.50612 11.66578 1.70 −7.657 ± 0.017 −8.530 ± 0.020 2.31 ± 0.11 1.00<br />
NGC 4621 416 190.50382 11.65856 1.14 −5.510 ± 0.097 −7.046 ± 0.125 2.99 ± 0.51 0.90<br />
NGC 4621 417 190.49984 11.64595 0.84 −9.114 ± 0.018 −10.129 ± 0.017 3.21 ± 0.11 1.00<br />
NGC 4621 418 190.49788 11.63978 1.19 −9.324 ± 0.016 −10.334 ± 0.013 2.72 ± 0.09 1.00<br />
NGC 4621 419 190.49687 11.63647 1.44 −8.251 ± 0.024 −9.739 ± 0.019 2.46 ± 0.11 1.00<br />
NGC 4621 420 190.50563 11.66560 1.69 −7.706 ± 0.033 −9.172 ± 0.033 2.48 ± 0.21 1.00<br />
NGC 4621 421 190.49580 11.63286 1.73 −8.385 ± 0.024 −9.714 ± 0.017 2.74 ± 0.10 1.00<br />
NGC 4621 422 190.50349 11.65871 1.16 −6.191 ± 0.785 −7.512 ± 0.057 1.75 ± 0.41 0.98<br />
NGC 4621 427 190.50189 11.64971 0.70 −6.048 ± 0.065 −7.480 ± 0.076 2.99 ± 0.26 0.96<br />
NGC 4621 430 190.50300 11.65920 1.22 −6.912 ± 0.033 −8.488 ± 0.034 1.68 ± 0.24 1.00<br />
NGC 4621 431 190.49328 11.62820 2.18 −8.672 ± 0.026 −9.731 ± 0.012 1.81 ± 0.14 1.00<br />
NGC 4621 434 190.50137 11.65500 1.00 −5.888 ± 0.063 −7.030 ± 0.070 2.37 ± 0.31 0.96<br />
NGC 4621 443 190.50740 11.67655 2.64 −4.860 ± 0.285 −6.193 ± 1.361 1.48 ± 0.43 0.79<br />
NGC 4621 444 190.50082 11.65525 1.05 −7.601 ± 0.033 −8.413 ± 0.037 2.45 ± 0.19 1.00<br />
NGC 4621 445 190.50270 11.66159 1.42 −6.902 ± 0.077 −7.911 ± 0.053 1.67 ± 0.34 1.00<br />
NGC 4621 447 190.49891 11.64995 0.95 −6.066 ± 0.039 −6.643 ± 0.594 1.73 ± 0.26 0.93<br />
NGC 4621 452 190.50008 11.65445 1.05 −6.547 ± 0.052 −7.203 ± 0.065 3.06 ± 0.27 0.92<br />
NGC 4621 453 190.49806 11.64817 0.99 −9.321 ± 0.029 −10.213 ± 0.031 4.81 ± 0.13 1.00<br />
NGC 4621 454 190.50454 11.66949 2.05 −5.687 ± 0.099 −7.427 ± 0.162 4.19 ± 1.05 0.79<br />
NGC 4621 455 190.49948 11.65402 1.07 −7.545 ± 0.489 −8.749 ± 0.026 1.46 ± 0.29 1.00<br />
NGC 4621 459 190.49747 11.64908 1.06 −8.355 ± 0.023 −9.214 ± 0.022 2.44 ± 0.17 1.00<br />
NGC 4621 461 190.49951 11.65615 1.19 −6.701 ± 0.096 −7.830 ± 0.078 3.88 ± 0.49 0.94<br />
NGC 4621 462 190.50531 11.67531 2.55 −6.206 ± 0.043 −7.382 ± 0.069 1.63 ± 0.27 0.97<br />
NGC 4621 463 190.49501 11.64229 1.32 −7.437 ± 0.034 −8.288 ± 0.029 2.88 ± 0.15 1.00<br />
NGC 4621 464 190.50418 11.67277 2.34 −8.172 ± 0.021 −9.717 ± 0.026 3.08 ± 0.14 1.00<br />
NGC 4621 467 190.50447 11.67477 2.51 −9.123 ± 0.026 −10.453 ± 0.012 1.92 ± 0.11 1.00<br />
Continued on Next Page. . .<br />
383
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4621 470 190.49815 11.65434 1.18 −4.986 ± 0.176 −6.731 ± 0.503 1.44 ± 0.67 0.85<br />
NGC 4621 471 190.49497 11.64423 1.28 −7.608 ± 0.029 −8.893 ± 0.030 2.74 ± 0.13 1.00<br />
NGC 4621 473 190.49946 11.65930 1.40 −6.129 ± 0.052 −7.108 ± 0.067 2.44 ± 0.24 0.96<br />
NGC 4621 476 190.49464 11.64403 1.31 −8.685 ± 0.023 −10.059 ± 0.015 1.54 ± 0.13 1.00<br />
NGC 4621 480 190.49008 11.62965 2.28 −7.698 ± 0.028 −8.525 ± 0.035 2.09 ± 0.15 1.00<br />
NGC 4621 483 190.50107 11.66620 1.86 −7.517 ± 0.020 −9.031 ± 0.020 2.62 ± 0.11 1.00<br />
NGC 4621 484 190.50400 11.67588 2.61 −6.794 ± 0.054 −7.689 ± 0.066 4.33 ± 0.26 0.85<br />
NGC 4621 485 190.50287 11.67235 2.33 −7.999 ± 0.021 −8.907 ± 0.014 2.57 ± 0.09 1.00<br />
NGC 4621 487 190.49304 11.64067 1.53 −7.207 ± 0.039 −8.767 ± 0.031 2.71 ± 0.17 1.00<br />
NGC 4621 489 190.49938 11.66262 1.64 −6.812 ± 0.039 −7.637 ± 0.042 2.77 ± 0.16 0.98<br />
NGC 4621 495 190.49856 11.66315 1.72 −8.870 ± 0.048 −9.844 ± 0.028 2.18 ± 0.23 1.00<br />
NGC 4621 497 190.49431 11.64930 1.33 −7.059 ± 0.031 −8.269 ± 0.024 2.05 ± 0.21 1.00<br />
NGC 4621 498 190.49042 11.63685 1.88 −7.520 ± 0.032 −8.790 ± 0.024 2.59 ± 0.18 1.00<br />
NGC 4621 502 190.49459 11.65141 1.35 −6.160 ± 0.032 −7.550 ± 0.056 1.74 ± 0.25 0.98<br />
NGC 4621 503 190.49943 11.66777 2.04 −7.168 ± 0.052 −8.091 ± 0.121 2.93 ± 0.42 1.00<br />
NGC 4621 506 190.49122 11.64135 1.66 −7.354 ± 0.031 −8.741 ± 0.023 1.78 ± 0.15 1.00<br />
NGC 4621 509 190.48878 11.63385 2.14 −8.045 ± 0.026 −9.263 ± 0.020 2.95 ± 0.14 1.00<br />
NGC 4621 510 190.49238 11.64556 1.49 −7.035 ± 0.023 −8.127 ± 0.037 2.23 ± 0.15 1.00<br />
NGC 4621 515 190.49216 11.64590 1.50 −8.452 ± 0.032 −9.465 ± 0.019 2.74 ± 0.17 1.00<br />
NGC 4621 516 190.49941 11.66969 2.20 −6.806 ± 0.046 −7.663 ± 0.045 2.69 ± 0.23 0.98<br />
NGC 4621 517 190.48582 11.62623 2.76 −7.744 ± 0.030 −8.590 ± 0.022 2.52 ± 0.14 1.00<br />
NGC 4621 518 190.49719 11.66346 1.81 −5.191 ± 0.206 −6.130 ± 0.241 3.47 ± 1.36 0.52<br />
NGC 4621 520 190.49418 11.65391 1.46 −7.172 ± 0.050 −8.401 ± 0.072 4.77 ± 0.41 0.90<br />
NGC 4621 521 190.49654 11.66207 1.75 −8.441 ± 0.025 −9.485 ± 0.018 2.31 ± 0.17 1.00<br />
NGC 4621 522 190.48572 11.62644 2.76 −6.925 ± 0.049 −8.166 ± 0.034 3.65 ± 0.22 1.00<br />
NGC 4621 529 190.48828 11.63717 2.04 −6.804 ± 0.054 −7.785 ± 0.056 3.58 ± 0.26 0.96<br />
NGC 4621 531 190.49006 11.64447 1.70 −8.210 ± 0.025 −9.655 ± 0.035 3.99 ± 0.19 1.00<br />
NGC 4621 532 190.49907 11.67410 2.58 −7.629 ± 0.077 −8.616 ± 0.107 5.79 ± 0.54 0.79<br />
NGC 4621 534 190.49763 11.67099 2.37 −8.343 ± 0.027 −9.259 ± 0.019 2.30 ± 0.19 1.00<br />
NGC 4621 535 190.49677 11.66997 2.32 −5.086 ± 0.246 −6.353 ± 0.118 2.79 ± 1.26 0.82<br />
NGC 4621 538 190.49356 11.66107 1.86 −7.537 ± 0.030 −8.484 ± 0.027 2.62 ± 0.14 1.00<br />
NGC 4621 540 190.48963 11.64864 1.73 −7.623 ± 0.026 −8.558 ± 0.048 4.92 ± 0.15 0.90<br />
NGC 4621 546 190.48936 11.64919 1.76 −6.447 ± 0.069 −7.542 ± 0.062 3.24 ± 0.27 0.95<br />
NGC 4621 551 190.49408 11.66581 2.14 −8.501 ± 0.017 −9.867 ± 0.021 1.79 ± 0.14 1.00<br />
NGC 4621 553 190.48756 11.64444 1.92 −5.632 ± 0.173 −6.588 ± 0.136 1.68 ± 0.60 0.91<br />
NGC 4621 556 190.49072 11.65582 1.81 −8.597 ± 0.024 −9.920 ± 0.016 2.24 ± 0.14 1.00<br />
NGC 4621 557 190.49751 11.67849 2.99 −7.215 ± 1.539 −7.770 ± 0.712 1.04 ± 0.32 0.74<br />
NGC 4621 559 190.48611 11.64242 2.07 −7.085 ± 0.030 −8.409 ± 0.029 1.95 ± 0.23 1.00<br />
NGC 4621 560 190.48230 11.63014 2.80 −7.552 ± 0.032 −8.376 ± 0.028 3.10 ± 0.17 1.00<br />
NGC 4621 566 190.48309 11.63434 2.55 −5.939 ± 0.102 −6.663 ± 0.054 3.70 ± 0.29 0.59<br />
NGC 4621 571 190.48890 11.65402 1.89 −7.620 ± 0.019 −8.710 ± 0.023 1.59 ± 0.13 1.00<br />
NGC 4621 572 190.48219 11.63312 2.67 −7.499 ± 0.121 −8.428 ± 0.052 2.20 ± 0.38 1.00<br />
NGC 4621 582 190.48942 11.66167 2.18 −5.347 ± 0.143 −6.388 ± 0.058 2.41 ± 0.58 0.88<br />
NGC 4621 584 190.48568 11.65038 2.09 −5.473 ± 0.490 −6.325 ± 0.193 2.90 ± 0.95 0.79<br />
NGC 4621 585 190.49153 11.67102 2.65 −8.324 ± 0.035 −9.554 ± 0.018 1.92 ± 0.15 1.00<br />
NGC 4621 586 190.48297 11.64300 2.33 −9.059 ± 0.015 −10.352 ± 0.019 2.64 ± 0.13 1.00<br />
NGC 4621 590 190.48433 11.64780 2.18 −6.968 ± 0.038 −7.793 ± 0.038 2.40 ± 0.21 0.99<br />
NGC 4621 596 190.48793 11.66204 2.30 −6.820 ± 0.040 −7.753 ± 0.052 2.40 ± 0.25 0.99<br />
NGC 4621 600 190.48608 11.65732 2.23 −5.653 ± 0.071 −6.406 ± 0.132 2.60 ± 0.50 0.86<br />
NGC 4621 601 190.48480 11.65366 2.22 −7.759 ± 0.014 −8.635 ± 0.023 1.56 ± 0.08 1.00<br />
NGC 4621 614 190.48912 11.67200 2.84 −8.189 ± 0.024 −9.486 ± 0.026 3.15 ± 0.15 1.00<br />
NGC 4621 617 190.47961 11.64076 2.65 −6.719 ± 0.051 −7.464 ± 0.043 2.80 ± 0.25 0.97<br />
NGC 4621 618 190.47845 11.63705 2.84 −6.624 ± 0.026 −7.956 ± 0.052 2.03 ± 0.17 1.00<br />
NGC 4621 624 190.47823 11.63868 2.81 −7.283 ± 0.024 −8.693 ± 0.028 2.87 ± 0.15 1.00<br />
NGC 4621 630 190.48245 11.65541 2.46 −7.540 ± 0.026 −8.492 ± 0.015 2.00 ± 0.16 1.00<br />
NGC 4621 642 190.48451 11.66539 2.72 −8.175 ± 0.030 −9.115 ± 0.025 2.34 ± 0.20 1.00<br />
NGC 4621 645 190.47962 11.64981 2.61 −6.331 ± 0.069 −7.226 ± 0.098 2.97 ± 0.31 0.94<br />
NGC 4621 646 190.48323 11.66180 2.63 −6.086 ± 0.279 −7.175 ± 0.041 1.42 ± 0.28 0.90<br />
NGC 4621 647 190.48381 11.66390 2.69 −6.218 ± 0.040 −7.591 ± 0.048 2.44 ± 0.19 0.98<br />
NGC 4621 664 190.48130 11.65966 2.70 −4.792 ± 1.037 −6.193 ± 0.608 2.35 ± 37.93 0.86<br />
NGC 4621 672 190.47691 11.64869 2.83 −7.043 ± 0.034 −8.087 ± 0.033 2.39 ± 0.19 1.00<br />
NGC 4621 677 190.48602 11.68026 3.59 −9.280 ± 0.022 −10.514 ± 0.015 2.34 ± 0.17 1.00<br />
Continued on Next Page. . .<br />
384
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4621 678 190.48604 11.68061 3.62 −8.207 ± 0.020 −9.346 ± 0.019 2.57 ± 0.10 1.00<br />
NGC 4621 684 190.48203 11.67035 3.16 −6.871 ± 0.045 −7.769 ± 0.043 2.55 ± 0.22 0.99<br />
NGC 4621 688 190.48336 11.67687 3.49 −8.433 ± 0.015 −9.641 ± 0.018 2.26 ± 0.09 1.00<br />
NGC 4621 696 190.47130 11.64237 3.34 −8.687 ± 0.019 −9.787 ± 0.018 2.93 ± 0.13 1.00<br />
NGC 4649 1 190.94345 11.55608 1.39 −6.240 ± 0.056 −7.383 ± 0.040 2.11 ± 0.24 0.99<br />
NGC 4649 3 190.94472 11.55884 1.47 −6.508 ± 0.145 −7.749 ± 0.064 5.69 ± 0.71 0.81<br />
NGC 4649 4 190.94083 11.55271 1.24 −6.592 ± 0.050 −7.886 ± 1.226 1.74 ± 0.31 0.99<br />
NGC 4649 6 190.94673 11.56364 1.64 −8.291 ± 0.037 −9.621 ± 0.020 2.70 ± 0.15 1.00<br />
NGC 4649 7 190.94118 11.55378 1.26 −7.483 ± 0.021 −8.986 ± 0.028 2.38 ± 0.18 1.00<br />
NGC 4649 8 190.94142 11.55444 1.27 −7.537 ± 0.015 −8.843 ± 0.018 1.80 ± 0.18 1.00<br />
NGC 4649 9 190.93561 11.54411 1.07 −6.200 ± 0.103 −7.119 ± 0.106 4.01 ± 0.39 0.86<br />
NGC 4649 10 190.93537 11.54386 1.07 −5.160 ± 0.442 −6.245 ± 0.662 3.70 ± 1.74 0.87<br />
NGC 4649 11 190.94784 11.56651 1.75 −8.361 ± 0.024 −9.466 ± 0.022 2.23 ± 0.18 1.00<br />
NGC 4649 12 190.93063 11.53553 1.15 −6.691 ± 0.045 −7.940 ± 0.037 2.18 ± 0.21 1.00<br />
NGC 4649 13 190.94620 11.56372 1.62 −7.948 ± 0.033 −8.810 ± 0.034 3.84 ± 0.17 1.00<br />
NGC 4649 14 190.93746 11.54804 1.10 −5.347 ± 0.104 −6.339 ± 0.185 2.36 ± 0.39 0.98<br />
NGC 4649 17 190.93041 11.53582 1.13 −7.257 ± 0.022 −8.669 ± 0.025 1.56 ± 0.13 1.00<br />
NGC 4649 18 190.93189 11.53865 1.08 −8.702 ± 0.016 −9.557 ± 0.021 2.62 ± 0.11 1.00<br />
NGC 4649 20 190.93488 11.54396 1.04 −5.402 ± 0.256 −6.370 ± 0.169 3.79 ± 1.01 0.84<br />
NGC 4649 21 190.92660 11.52909 1.34 −6.500 ± 0.041 −7.737 ± 0.040 1.82 ± 0.24 0.99<br />
NGC 4649 22 190.94317 11.55944 1.40 −9.114 ± 0.020 −10.607 ± 0.020 2.64 ± 0.16 1.00<br />
NGC 4649 25 190.93342 11.54183 1.03 −6.405 ± 0.031 −7.848 ± 1.391 2.17 ± 0.25 1.00<br />
NGC 4649 26 190.93227 11.53987 1.05 −8.216 ± 0.024 −9.150 ± 0.017 2.42 ± 0.10 1.00<br />
NGC 4649 27 190.92459 11.52629 1.45 −6.797 ± 0.063 −7.624 ± 0.048 3.50 ± 0.19 0.97<br />
NGC 4649 28 190.93306 11.54155 1.03 −8.226 ± 0.043 −9.227 ± 0.657 2.57 ± 0.47 1.00<br />
NGC 4649 31 190.94635 11.56611 1.68 −7.935 ± 0.019 −9.555 ± 0.014 2.50 ± 0.12 1.00<br />
NGC 4649 32 190.93834 11.55180 1.11 −7.428 ± 0.037 −8.923 ± 0.027 1.92 ± 0.13 1.00<br />
NGC 4649 34 190.93390 11.54422 0.99 −7.524 ± 0.029 −8.461 ± 0.027 1.59 ± 0.13 1.00<br />
NGC 4649 35 190.92955 11.53651 1.08 −9.756 ± 0.147 −11.327 ± 0.039 2.28 ± 0.26 1.00<br />
NGC 4649 36 190.92784 11.53363 1.15 −9.904 ± 0.012 −10.931 ± 0.014 2.82 ± 0.10 1.00<br />
NGC 4649 37 190.92328 11.52537 1.47 −7.339 ± 0.019 −8.759 ± 0.020 1.85 ± 0.16 1.00<br />
NGC 4649 38 190.92956 11.53680 1.07 −6.877 ± 0.061 −8.465 ± 0.048 1.82 ± 0.39 1.00<br />
NGC 4649 40 190.92411 11.52770 1.37 −7.465 ± 0.028 −8.853 ± 0.019 2.31 ± 0.17 1.00<br />
NGC 4649 41 190.93462 11.54676 0.97 −7.348 ± 0.036 −8.272 ± 0.038 2.06 ± 0.21 1.00<br />
NGC 4649 43 190.93672 11.55063 1.04 −7.311 ± 0.022 −8.915 ± 0.031 2.97 ± 0.16 1.00<br />
NGC 4649 44 190.93216 11.54259 0.96 −6.345 ± 0.047 −7.663 ± 0.948 1.81 ± 0.33 0.99<br />
NGC 4649 45 190.92634 11.53249 1.17 −6.064 ± 0.064 −6.807 ± 0.104 2.05 ± 0.39 0.99<br />
NGC 4649 46 190.92985 11.53879 1.00 −9.799 ± 0.017 −11.274 ± 0.010 2.27 ± 0.12 1.00<br />
NGC 4649 48 190.92597 11.53204 1.19 −7.802 ± 0.017 −9.129 ± 0.014 1.65 ± 0.14 1.00<br />
NGC 4649 49 190.93822 11.55405 1.11 −6.478 ± 0.080 −7.926 ± 0.444 1.29 ± 0.44 0.97<br />
NGC 4649 51 190.92582 11.53200 1.19 −6.719 ± 0.032 −7.763 ± 0.046 2.23 ± 0.26 1.00<br />
NGC 4649 52 190.93109 11.54177 0.94 −5.991 ± 0.368 −7.413 ± 0.095 2.13 ± 0.43 0.99<br />
NGC 4649 53 190.92992 11.53996 0.96 −7.318 ± 0.041 −8.677 ± 0.019 1.68 ± 0.20 1.00<br />
NGC 4649 55 190.92430 11.52988 1.26 −7.630 ± 0.025 −8.520 ± 0.020 2.75 ± 0.11 1.00<br />
NGC 4649 56 190.92699 11.53469 1.09 −5.914 ± 0.068 −7.347 ± 0.052 2.62 ± 0.34 0.99<br />
NGC 4649 59 190.92740 11.53557 1.06 −4.772 ± 0.110 −6.596 ± 0.318 3.38 ± 0.96 0.91<br />
NGC 4649 62 190.93077 11.54227 0.91 −6.298 ± 0.046 −7.063 ± 0.297 2.21 ± 0.39 0.99<br />
NGC 4649 63 190.92985 11.54067 0.93 −7.898 ± 0.020 −9.190 ± 0.018 1.47 ± 0.09 0.98<br />
NGC 4649 64 190.93665 11.55295 1.03 −7.918 ± 0.021 −9.548 ± 0.015 2.50 ± 0.12 1.00<br />
NGC 4649 65 190.94434 11.56683 1.60 −8.436 ± 0.021 −9.850 ± 0.016 2.49 ± 0.10 1.00<br />
NGC 4649 66 190.94311 11.56486 1.50 −5.725 ± 0.094 −6.477 ± 0.120 2.48 ± 0.50 0.97<br />
NGC 4649 68 190.93738 11.55467 1.07 −5.830 ± 0.062 −7.342 ± 0.113 2.77 ± 0.51 0.98<br />
NGC 4649 69 190.93048 11.54250 0.89 −6.839 ± 0.424 −8.483 ± 0.034 1.21 ± 0.19 0.95<br />
NGC 4649 70 190.93843 11.55695 1.14 −7.899 ± 0.020 −8.878 ± 0.039 2.63 ± 0.19 1.00<br />
NGC 4649 71 190.94316 11.56547 1.51 −8.485 ± 0.020 −9.725 ± 0.013 2.36 ± 0.11 1.00<br />
NGC 4649 73 190.92105 11.52605 1.42 −8.596 ± 0.015 −9.807 ± 0.020 2.31 ± 0.10 1.00<br />
NGC 4649 74 190.93301 11.54753 0.88 −7.513 ± 0.027 −8.983 ± 0.038 1.41 ± 0.22 0.97<br />
NGC 4649 77 190.93643 11.55418 1.02 −9.180 ± 0.016 −10.692 ± 0.012 2.40 ± 0.09 1.00<br />
NGC 4649 78 190.94151 11.56337 1.39 −5.690 ± 0.082 −7.327 ± 0.057 2.57 ± 0.38 0.99<br />
NGC 4649 79 190.92820 11.53962 0.91 −6.807 ± 0.296 −8.190 ± 0.703 2.30 ± 0.63 1.00<br />
NGC 4649 81 190.93782 11.55779 1.12 −7.436 ± 0.032 −8.464 ± 0.016 2.04 ± 0.18 1.00<br />
Continued on Next Page. . .<br />
385
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4649 82 190.93087 11.54541 0.82 −8.908 ± 0.029 −10.372 ± 0.014 1.92 ± 0.14 1.00<br />
NGC 4649 83 190.93280 11.54898 0.85 −9.976 ± 0.017 −11.162 ± 0.018 4.39 ± 0.09 0.96<br />
NGC 4649 84 190.91992 11.52598 1.41 −8.810 ± 0.018 −10.368 ± 0.015 2.77 ± 0.09 1.00<br />
NGC 4649 85 190.93582 11.55481 0.99 −8.949 ± 0.023 −10.454 ± 0.026 2.21 ± 0.12 1.00<br />
NGC 4649 88 190.93216 11.54840 0.83 −8.965 ± 0.022 −10.087 ± 0.014 2.32 ± 0.12 1.00<br />
NGC 4649 89 190.92624 11.53765 0.93 −7.073 ± 0.043 −8.283 ± 0.044 3.40 ± 0.20 1.00<br />
NGC 4649 90 190.93971 11.56189 1.28 −7.024 ± 0.035 −8.293 ± 1.568 2.07 ± 0.22 1.00<br />
NGC 4649 91 190.93622 11.55568 1.01 −6.994 ± 0.038 −8.456 ± 0.037 1.84 ± 0.18 1.00<br />
NGC 4649 92 190.92921 11.54313 0.82 −7.725 ± 0.022 −9.098 ± 0.017 1.86 ± 0.18 1.00<br />
NGC 4649 93 190.92810 11.54117 0.84 −7.028 ± 0.032 −8.006 ± 0.065 2.06 ± 0.25 1.00<br />
NGC 4649 94 190.92814 11.54126 0.84 −6.386 ± 0.067 −7.797 ± 0.050 1.94 ± 0.40 1.00<br />
NGC 4649 95 190.93800 11.55916 1.14 −6.695 ± 0.042 −7.954 ± 0.035 2.02 ± 0.17 1.00<br />
NGC 4649 96 190.94292 11.56804 1.57 −6.678 ± 0.039 −7.655 ± 0.063 2.10 ± 0.26 1.00<br />
NGC 4649 97 190.93805 11.55929 1.15 −6.766 ± 0.142 −8.566 ± 0.135 7.70 ± 1.28 0.66<br />
NGC 4649 98 190.93685 11.55726 1.06 −7.157 ± 0.033 −8.236 ± 0.037 2.21 ± 0.15 1.00<br />
NGC 4649 99 190.93645 11.55669 1.04 −6.577 ± 0.106 −8.345 ± 0.058 2.56 ± 0.36 1.00<br />
NGC 4649 100 190.91751 11.52285 1.57 −5.151 ± 0.182 −6.464 ± 0.346 2.03 ± 0.71 0.98<br />
NGC 4649 101 190.93623 11.55655 1.02 −6.901 ± 0.054 −8.445 ± 0.044 1.55 ± 0.27 1.00<br />
NGC 4649 102 190.91906 11.52590 1.41 −9.162 ± 0.015 −10.109 ± 0.014 2.48 ± 0.14 1.00<br />
NGC 4649 103 190.93515 11.55479 0.95 −8.532 ± 0.023 −10.050 ± 0.017 1.92 ± 0.14 1.00<br />
NGC 4649 104 190.92538 11.53724 0.93 −6.573 ± 0.053 −7.660 ± 0.101 2.86 ± 0.49 0.99<br />
NGC 4649 106 190.93693 11.55822 1.08 −7.022 ± 0.028 −7.969 ± 0.037 2.02 ± 0.23 1.00<br />
NGC 4649 107 190.93175 11.54898 0.80 −7.689 ± 0.018 −8.763 ± 0.037 2.53 ± 0.18 1.00<br />
NGC 4649 109 190.94019 11.56421 1.35 −6.725 ± 0.056 −7.989 ± 0.028 1.87 ± 0.31 1.00<br />
NGC 4649 110 190.91710 11.52285 1.57 −5.911 ± 0.081 −6.779 ± 0.173 5.02 ± 0.84 0.54<br />
NGC 4649 111 190.92313 11.53393 1.04 −7.864 ± 0.035 −9.482 ± 0.031 2.07 ± 0.23 1.00<br />
NGC 4649 113 190.94046 11.56526 1.38 −7.725 ± 0.026 −8.689 ± 0.025 2.42 ± 0.12 1.00<br />
NGC 4649 118 190.93552 11.55670 0.99 −6.008 ± 0.596 −7.476 ± 0.058 1.41 ± 0.39 0.97<br />
NGC 4649 119 190.92271 11.53391 1.04 −8.552 ± 0.017 −9.606 ± 0.014 2.66 ± 0.09 1.00<br />
NGC 4649 120 190.93478 11.55557 0.94 −7.592 ± 0.035 −8.843 ± 0.299 1.86 ± 0.23 1.00<br />
NGC 4649 122 190.92515 11.53885 0.85 −10.376 ± 0.018 −11.376 ± 0.024 5.00 ± 0.09 0.93<br />
NGC 4649 124 190.92688 11.54205 0.77 −8.719 ± 0.049 −10.139 ± 0.029 0.78 ± 0.12 0.65<br />
NGC 4649 125 190.93103 11.54989 0.75 −7.429 ± 0.029 −8.970 ± 0.034 2.02 ± 0.27 1.00<br />
NGC 4649 126 190.93321 11.55411 0.85 −7.483 ± 0.027 −8.489 ± 0.035 1.99 ± 0.19 1.00<br />
NGC 4649 127 190.92427 11.53813 0.86 −8.738 ± 0.015 −9.910 ± 0.015 2.00 ± 0.09 1.00<br />
NGC 4649 128 190.92070 11.53177 1.12 −5.965 ± 0.120 −7.081 ± 0.113 3.75 ± 0.75 0.89<br />
NGC 4649 129 190.93487 11.55735 0.96 −6.791 ± 0.038 −8.112 ± 0.042 1.09 ± 0.28 0.93<br />
NGC 4649 130 190.92426 11.53836 0.85 −8.561 ± 0.047 −10.002 ± 0.016 1.20 ± 0.17 0.93<br />
NGC 4649 132 190.93655 11.56054 1.10 −5.980 ± 0.293 −7.366 ± 1.090 0.98 ± 0.40 0.88<br />
NGC 4649 133 190.93504 11.55790 0.98 −7.063 ± 0.038 −8.505 ± 0.033 2.05 ± 0.27 1.00<br />
NGC 4649 134 190.92170 11.53388 1.02 −5.989 ± 0.057 −7.077 ± 0.673 1.28 ± 0.32 0.94<br />
NGC 4649 135 190.92279 11.53599 0.93 −7.060 ± 0.025 −8.149 ± 0.061 3.08 ± 0.28 1.00<br />
NGC 4649 136 190.92988 11.54887 0.71 −6.829 ± 0.033 −8.330 ± 0.040 2.03 ± 0.23 1.00<br />
NGC 4649 137 190.92509 11.54026 0.79 −7.573 ± 0.016 −8.826 ± 0.028 2.44 ± 0.15 1.00<br />
NGC 4649 138 190.94202 11.57078 1.61 −7.702 ± 0.024 −8.940 ± 0.025 2.17 ± 0.17 1.00<br />
NGC 4649 139 190.93207 11.55288 0.79 −7.605 ± 0.036 −8.997 ± 0.025 2.00 ± 0.19 1.00<br />
NGC 4649 140 190.92560 11.54123 0.76 −5.961 ± 0.069 −7.486 ± 0.070 2.19 ± 0.36 0.99<br />
NGC 4649 145 190.93205 11.55307 0.79 −7.982 ± 0.020 −9.436 ± 0.017 2.00 ± 0.10 1.00<br />
NGC 4649 146 190.91699 11.52627 1.39 −7.195 ± 0.032 −8.210 ± 0.042 2.61 ± 0.20 1.00<br />
NGC 4649 147 190.92180 11.53506 0.96 −9.175 ± 0.012 −10.245 ± 0.018 2.56 ± 0.10 1.00<br />
NGC 4649 148 190.93350 11.55615 0.88 −6.449 ± 0.385 −8.324 ± 0.038 1.34 ± 0.28 0.97<br />
NGC 4649 149 190.93542 11.55970 1.03 −5.562 ± 0.140 −7.298 ± 0.139 3.30 ± 0.70 0.96<br />
NGC 4649 151 190.92992 11.54995 0.70 −7.730 ± 0.025 −9.259 ± 0.021 1.56 ± 0.10 1.00<br />
NGC 4649 152 190.92230 11.53618 0.92 −6.900 ± 0.401 −8.074 ± 0.037 2.00 ± 0.27 1.00<br />
NGC 4649 154 190.93269 11.55494 0.83 −7.037 ± 0.036 −8.017 ± 0.030 2.01 ± 0.17 1.00<br />
NGC 4649 155 190.91593 11.52504 1.45 −5.838 ± 0.261 −7.221 ± 0.297 1.40 ± 0.41 0.96<br />
NGC 4649 156 190.92574 11.54265 0.71 −6.377 ± 0.164 −7.914 ± 0.054 1.35 ± 0.33 0.97<br />
NGC 4649 157 190.93101 11.55224 0.74 −5.980 ± 0.404 −7.485 ± 0.042 1.70 ± 0.47 0.99<br />
NGC 4649 158 190.93119 11.55272 0.74 −7.336 ± 0.039 −8.128 ± 0.042 2.07 ± 0.25 1.00<br />
NGC 4649 160 190.92188 11.53619 0.91 −6.383 ± 0.152 −7.379 ± 0.061 1.98 ± 0.36 0.99<br />
NGC 4649 161 190.91791 11.52922 1.23 −6.145 ± 0.049 −7.658 ± 0.054 2.85 ± 0.24 0.99<br />
NGC 4649 162 190.91451 11.52324 1.55 −8.312 ± 0.021 −9.392 ± 0.017 2.48 ± 0.10 1.00<br />
Continued on Next Page. . .<br />
386
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4649 163 190.93299 11.55642 0.86 −8.002 ± 0.022 −8.877 ± 0.021 2.09 ± 0.20 1.00<br />
NGC 4649 164 190.92935 11.54984 0.67 −7.087 ± 0.097 −8.558 ± 0.299 1.70 ± 0.34 1.00<br />
NGC 4649 165 190.92781 11.54713 0.64 −7.433 ± 0.044 −8.402 ± 0.047 1.74 ± 0.25 1.00<br />
NGC 4649 166 190.91980 11.53270 1.06 −6.472 ± 0.045 −7.534 ± 0.047 1.62 ± 0.22 0.98<br />
NGC 4649 167 190.93310 11.55678 0.87 −8.800 ± 0.014 −9.916 ± 0.016 2.74 ± 0.12 1.00<br />
NGC 4649 168 190.92137 11.53581 0.92 −9.941 ± 0.016 −10.999 ± 0.013 2.49 ± 0.09 1.00<br />
NGC 4649 169 190.92782 11.54733 0.64 −6.984 ± 0.043 −8.033 ± 0.875 1.82 ± 0.40 1.00<br />
NGC 4649 170 190.93551 11.56122 1.06 −6.879 ± 0.043 −8.357 ± 0.032 1.98 ± 0.20 1.00<br />
NGC 4649 171 190.92221 11.53747 0.85 −9.087 ± 0.018 −10.059 ± 0.013 2.14 ± 0.14 1.00<br />
NGC 4649 172 190.91831 11.53038 1.18 −6.545 ± 0.049 −7.583 ± 0.075 2.87 ± 0.29 0.99<br />
NGC 4649 174 190.91939 11.53251 1.07 −8.707 ± 0.021 −9.549 ± 0.017 2.24 ± 0.16 1.00<br />
NGC 4649 177 190.93176 11.55478 0.78 −6.692 ± 0.172 −8.264 ± 0.037 1.67 ± 0.26 1.00<br />
NGC 4649 178 190.93601 11.56243 1.11 −7.942 ± 0.018 −9.227 ± 0.017 2.20 ± 0.10 1.00<br />
NGC 4649 180 190.93539 11.56143 1.06 −5.752 ± 0.069 −7.306 ± 0.700 1.18 ± 0.35 0.93<br />
NGC 4649 181 190.91910 11.53227 1.08 −8.236 ± 0.016 −9.001 ± 0.018 2.66 ± 0.12 1.00<br />
NGC 4649 183 190.91860 11.53173 1.11 −6.830 ± 0.035 −8.191 ± 0.034 1.81 ± 0.22 1.00<br />
NGC 4649 184 190.93434 11.56014 0.99 −7.479 ± 0.033 −9.191 ± 0.022 1.67 ± 0.14 1.00<br />
NGC 4649 187 190.93224 11.55631 0.82 −5.039 ± 0.381 −6.178 ± 0.181 1.59 ± 0.68 0.97<br />
NGC 4649 188 190.92465 11.54304 0.65 −7.145 ± 0.037 −7.890 ± 0.058 2.63 ± 0.18 0.99<br />
NGC 4649 189 190.91856 11.53231 1.08 −8.718 ± 0.019 −9.752 ± 0.017 1.68 ± 0.10 1.00<br />
NGC 4649 190 190.92990 11.55269 0.68 −6.871 ± 0.044 −7.962 ± 0.054 1.50 ± 0.27 0.99<br />
NGC 4649 191 190.93424 11.56048 0.99 −6.330 ± 0.160 −7.019 ± 0.108 5.32 ± 1.00 0.55<br />
NGC 4649 192 190.93502 11.56201 1.06 −6.792 ± 0.033 −8.280 ± 0.033 1.41 ± 0.17 0.98<br />
NGC 4649 193 190.93293 11.55837 0.88 −7.325 ± 0.033 −8.451 ± 0.038 2.93 ± 0.28 1.00<br />
NGC 4649 194 190.92477 11.54365 0.63 −5.809 ± 0.139 −6.822 ± 0.101 2.48 ± 0.66 0.98<br />
NGC 4649 196 190.92529 11.54475 0.61 −6.661 ± 0.062 −7.426 ± 0.068 3.08 ± 0.44 0.98<br />
NGC 4649 197 190.93100 11.55506 0.75 −7.585 ± 0.030 −9.152 ± 0.032 1.80 ± 0.17 1.00<br />
NGC 4649 199 190.93341 11.55999 0.94 −7.484 ± 0.039 −9.018 ± 0.035 3.05 ± 0.19 1.00<br />
NGC 4649 200 190.92140 11.53851 0.79 −6.932 ± 0.042 −8.467 ± 0.049 2.08 ± 0.27 1.00<br />
NGC 4649 201 190.91508 11.52742 1.33 −7.704 ± 0.039 −8.539 ± 0.023 2.44 ± 0.15 1.00<br />
NGC 4649 205 190.92890 11.55264 0.63 −8.401 ± 0.103 −9.924 ± 0.037 2.02 ± 0.27 1.00<br />
NGC 4649 206 190.92040 11.53766 0.81 −7.592 ± 0.029 −8.733 ± 0.026 2.33 ± 0.18 1.00<br />
NGC 4649 207 190.92967 11.55444 0.67 −8.032 ± 0.761 −9.653 ± 0.026 1.97 ± 0.23 1.00<br />
NGC 4649 208 190.93530 11.56469 1.14 −7.298 ± 0.033 −8.924 ± 0.015 1.88 ± 0.15 1.00<br />
NGC 4649 209 190.93073 11.55687 0.75 −8.715 ± 0.014 −9.810 ± 0.019 2.01 ± 0.11 1.00<br />
NGC 4649 210 190.92518 11.54691 0.53 −7.637 ± 0.041 −8.866 ± 0.061 3.61 ± 0.31 1.00<br />
NGC 4649 211 190.92362 11.54423 0.57 −9.403 ± 0.014 −10.332 ± 0.015 2.91 ± 0.08 1.00<br />
NGC 4649 212 190.91716 11.53285 1.04 −9.704 ± 0.018 −10.975 ± 0.013 3.09 ± 0.12 1.00<br />
NGC 4649 213 190.92394 11.54492 0.55 −7.146 ± 0.036 −8.687 ± 0.039 1.43 ± 0.31 0.98<br />
NGC 4649 214 190.91782 11.53387 0.99 −6.429 ± 0.068 −7.444 ± 0.139 3.81 ± 0.74 0.94<br />
NGC 4649 215 190.92716 11.55076 0.55 −6.284 ± 0.623 −6.994 ± 0.280 1.39 ± 0.45 0.95<br />
NGC 4649 216 190.92168 11.54093 0.67 −5.949 ± 0.339 −7.626 ± 0.114 2.86 ± 0.61 0.99<br />
NGC 4649 217 190.92205 11.54179 0.64 −6.979 ± 0.050 −8.198 ± 0.038 2.16 ± 0.26 1.00<br />
NGC 4649 219 190.91733 11.53339 1.02 −6.842 ± 0.039 −7.639 ± 0.052 2.52 ± 0.28 0.99<br />
NGC 4649 220 190.91725 11.53345 1.01 −6.654 ± 0.037 −7.555 ± 0.040 2.16 ± 0.24 1.00<br />
NGC 4649 221 190.93327 11.56206 0.98 −5.927 ± 0.084 −6.933 ± 0.153 3.89 ± 0.65 0.85<br />
NGC 4649 222 190.92349 11.54467 0.55 −9.307 ± 0.011 −10.437 ± 0.013 2.30 ± 0.08 1.00<br />
NGC 4649 223 190.93154 11.55925 0.83 −7.834 ± 0.029 −9.239 ± 0.027 1.51 ± 0.21 0.98<br />
NGC 4649 224 190.91931 11.53734 0.82 −7.487 ± 0.079 −8.772 ± 0.212 7.77 ± 1.92 0.73<br />
NGC 4649 225 190.93016 11.55701 0.73 −8.722 ± 0.016 −10.130 ± 0.100 1.76 ± 0.23 1.00<br />
NGC 4649 226 190.93003 11.55677 0.72 −6.927 ± 0.033 −8.128 ± 0.050 2.02 ± 0.25 1.00<br />
NGC 4649 228 190.92732 11.55204 0.55 −8.490 ± 0.017 −9.952 ± 0.017 2.06 ± 0.15 1.00<br />
NGC 4649 231 190.92543 11.54898 0.49 −8.962 ± 0.018 −10.252 ± 0.021 2.39 ± 0.10 1.00<br />
NGC 4649 234 190.91499 11.53046 1.17 −8.349 ± 0.027 −9.637 ± 0.021 1.72 ± 0.19 1.00<br />
NGC 4649 235 190.92354 11.54583 0.51 −8.830 ± 0.019 −9.853 ± 0.021 2.16 ± 0.14 1.00<br />
NGC 4649 236 190.92573 11.54988 0.49 −9.184 ± 0.016 −10.469 ± 0.009 1.85 ± 0.04 1.00<br />
NGC 4649 238 190.91315 11.52737 1.34 −8.979 ± 0.012 −9.922 ± 0.016 2.30 ± 0.09 1.00<br />
NGC 4649 240 190.93052 11.55885 0.78 −5.187 ± 0.856 −6.962 ± 0.104 2.00 ± 0.57 0.99<br />
NGC 4649 241 190.93488 11.56685 1.19 −7.168 ± 0.041 −8.205 ± 0.036 2.51 ± 0.19 1.00<br />
NGC 4649 242 190.92683 11.55246 0.52 −6.023 ± 0.089 −7.887 ± 0.070 3.08 ± 0.40 0.99<br />
NGC 4649 243 190.92409 11.54757 0.47 −7.354 ± 0.027 −8.327 ± 0.068 2.69 ± 0.30 1.00<br />
NGC 4649 244 190.91659 11.53412 0.98 −6.860 ± 0.041 −7.933 ± 0.030 2.71 ± 0.21 0.99<br />
Continued on Next Page. . .<br />
387
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4649 245 190.91929 11.53897 0.73 −6.623 ± 0.045 −7.946 ± 0.597 2.23 ± 0.30 1.00<br />
NGC 4649 246 190.92088 11.54186 0.61 −5.972 ± 0.195 −7.405 ± 0.075 1.31 ± 0.36 0.96<br />
NGC 4649 247 190.91760 11.53610 0.87 −7.992 ± 0.027 −8.735 ± 0.023 1.77 ± 0.17 1.00<br />
NGC 4649 248 190.93079 11.55983 0.81 −7.851 ± 0.022 −8.957 ± 0.032 3.62 ± 0.15 1.00<br />
NGC 4649 249 190.91580 11.53303 1.04 −6.951 ± 0.029 −7.987 ± 0.047 2.50 ± 0.23 1.00<br />
NGC 4649 250 190.92860 11.55619 0.64 −6.818 ± 0.030 −7.658 ± 0.051 2.35 ± 0.26 1.00<br />
NGC 4649 252 190.92534 11.55056 0.46 −6.459 ± 0.431 −7.655 ± 0.168 2.48 ± 0.81 0.99<br />
NGC 4649 253 190.92458 11.54924 0.45 −7.644 ± 0.027 −9.200 ± 0.025 1.38 ± 0.14 0.97<br />
NGC 4649 255 190.92964 11.55843 0.73 −6.090 ± 0.077 −7.780 ± 0.147 3.79 ± 0.82 0.97<br />
NGC 4649 256 190.92253 11.54567 0.48 −7.360 ± 0.025 −8.333 ± 0.032 2.03 ± 0.12 1.00<br />
NGC 4649 258 190.92169 11.54450 0.50 −7.298 ± 0.034 −8.675 ± 0.026 1.94 ± 0.13 1.00<br />
NGC 4649 259 190.91536 11.53311 1.03 −6.108 ± 0.242 −7.630 ± 0.049 1.80 ± 0.32 0.99<br />
NGC 4649 260 190.92947 11.55880 0.73 −7.892 ± 0.024 −9.351 ± 0.038 1.40 ± 0.17 0.97<br />
NGC 4649 261 190.92204 11.54539 0.47 −5.830 ± 0.127 −7.352 ± 0.087 2.15 ± 0.48 0.99<br />
NGC 4649 263 190.92177 11.54534 0.47 −7.596 ± 0.036 −8.389 ± 0.057 2.49 ± 0.27 1.00<br />
NGC 4649 264 190.92375 11.54900 0.41 −7.533 ± 0.035 −8.821 ± 0.027 1.65 ± 0.20 1.00<br />
NGC 4649 268 190.93459 11.56854 1.24 −7.554 ± 0.030 −8.484 ± 0.033 3.21 ± 0.17 1.00<br />
NGC 4649 269 190.92431 11.55018 0.41 −6.687 ± 0.093 −8.170 ± 0.058 2.17 ± 0.40 1.00<br />
NGC 4649 270 190.93702 11.57328 1.50 −5.934 ± 0.087 −7.275 ± 0.057 2.66 ± 0.33 0.98<br />
NGC 4649 274 190.92169 11.54625 0.43 −7.297 ± 0.055 −8.614 ± 0.035 2.07 ± 0.17 1.00<br />
NGC 4649 276 190.91785 11.53962 0.69 −5.732 ± 0.141 −7.127 ± 0.050 3.31 ± 0.52 0.94<br />
NGC 4649 278 190.92029 11.54416 0.49 −7.795 ± 0.031 −9.287 ± 0.019 1.98 ± 0.17 1.00<br />
NGC 4649 279 190.93010 11.56196 0.84 −8.137 ± 0.024 −9.154 ± 0.049 3.95 ± 0.19 1.00<br />
NGC 4649 280 190.92037 11.54442 0.48 −5.957 ± 0.252 −6.775 ± 1.400 1.20 ± 0.37 0.91<br />
NGC 4649 281 190.93193 11.56523 1.02 −5.334 ± 0.599 −6.252 ± 0.291 1.46 ± 0.67 0.96<br />
NGC 4649 282 190.92306 11.54938 0.37 −6.000 ± 0.326 −7.655 ± 0.073 2.47 ± 0.46 0.99<br />
NGC 4649 283 190.92520 11.55352 0.44 −8.240 ± 0.020 −9.573 ± 0.017 1.95 ± 0.09 1.00<br />
NGC 4649 285 190.91847 11.54167 0.59 −8.113 ± 0.018 −9.551 ± 0.017 2.08 ± 0.10 1.00<br />
NGC 4649 286 190.92336 11.55050 0.36 −7.845 ± 0.022 −9.148 ± 0.042 2.20 ± 0.22 1.00<br />
NGC 4649 288 190.92302 11.54999 0.36 −6.350 ± 0.058 −7.811 ± 0.064 1.91 ± 0.39 1.00<br />
NGC 4649 289 190.91502 11.53576 0.89 −7.316 ± 0.042 −8.894 ± 0.025 2.79 ± 0.24 1.00<br />
NGC 4649 290 190.92593 11.55535 0.49 −8.127 ± 0.021 −9.047 ± 0.017 2.13 ± 0.22 1.00<br />
NGC 4649 291 190.92149 11.54769 0.36 −7.819 ± 0.030 −8.877 ± 0.030 2.71 ± 0.20 1.00<br />
NGC 4649 292 190.91820 11.54172 0.58 −8.100 ± 0.019 −9.250 ± 0.027 2.12 ± 0.12 1.00<br />
NGC 4649 294 190.91626 11.53833 0.76 −7.487 ± 0.036 −8.879 ± 0.018 1.62 ± 0.18 1.00<br />
NGC 4649 295 190.92034 11.54568 0.42 −6.289 ± 0.115 −7.723 ± 0.083 2.16 ± 0.46 1.00<br />
NGC 4649 298 190.92932 11.56194 0.81 −5.157 ± 0.115 −6.376 ± 0.465 3.33 ± 3.94 0.92<br />
NGC 4649 299 190.92712 11.55788 0.60 −6.812 ± 0.037 −8.384 ± 0.304 1.25 ± 0.31 0.96<br />
NGC 4649 300 190.93012 11.56359 0.89 −7.215 ± 0.365 −8.851 ± 0.036 1.88 ± 0.30 1.00<br />
NGC 4649 301 190.91470 11.53585 0.89 −6.091 ± 0.238 −7.505 ± 0.469 1.49 ± 0.42 0.98<br />
NGC 4649 302 190.93499 11.57238 1.39 −6.660 ± 0.049 −7.778 ± 0.063 3.27 ± 0.21 0.98<br />
NGC 4649 303 190.92865 11.56108 0.75 −7.129 ± 0.042 −8.212 ± 0.038 2.74 ± 0.25 1.00<br />
NGC 4649 304 190.91312 11.53316 1.04 −8.238 ± 0.016 −9.709 ± 0.019 1.90 ± 0.18 1.00<br />
NGC 4649 305 190.91656 11.53939 0.70 −8.106 ± 0.018 −9.627 ± 0.017 1.59 ± 0.15 1.00<br />
NGC 4649 306 190.92290 11.55102 0.33 −6.867 ± 0.130 −8.611 ± 0.037 2.49 ± 0.35 1.00<br />
NGC 4649 307 190.90909 11.52623 1.44 −4.955 ± 0.245 −6.648 ± 0.126 4.98 ± 1.42 0.52<br />
NGC 4649 308 190.91597 11.53892 0.73 −10.304 ± 0.009 −11.888 ± 0.012 2.84 ± 0.10 1.00<br />
NGC 4649 309 190.92745 11.55976 0.66 −9.135 ± 0.017 −10.035 ± 0.019 2.32 ± 0.16 1.00<br />
NGC 4649 310 190.92656 11.55815 0.58 −9.428 ± 0.015 −11.019 ± 0.013 2.17 ± 0.14 1.00<br />
NGC 4649 313 190.91281 11.53344 1.03 −6.506 ± 0.046 −7.284 ± 0.072 2.75 ± 0.27 0.98<br />
NGC 4649 314 190.92812 11.56110 0.73 −8.946 ± 0.015 −10.054 ± 0.015 1.92 ± 0.10 1.00<br />
NGC 4649 315 190.91119 11.53060 1.19 −5.658 ± 0.391 −6.705 ± 1.027 4.64 ± 22.85 0.63<br />
NGC 4649 317 190.93033 11.56518 0.96 −6.700 ± 0.045 −8.042 ± 0.021 1.89 ± 0.19 1.00<br />
NGC 4649 318 190.90892 11.52674 1.42 −6.763 ± 0.042 −8.142 ± 0.051 2.64 ± 0.38 1.00<br />
NGC 4649 319 190.91984 11.54602 0.39 −6.957 ± 0.042 −8.632 ± 0.054 2.27 ± 0.25 1.00<br />
NGC 4649 322 190.91014 11.52897 1.29 −6.663 ± 0.063 −7.635 ± 0.046 2.68 ± 0.23 0.99<br />
NGC 4649 323 190.92762 11.56049 0.69 −7.179 ± 0.067 −8.750 ± 0.035 1.70 ± 0.19 1.00<br />
NGC 4649 324 190.93022 11.56545 0.96 −7.953 ± 0.018 −9.337 ± 0.016 2.02 ± 0.16 1.00<br />
NGC 4649 326 190.91220 11.53330 1.05 −7.961 ± 0.029 −8.844 ± 0.034 3.07 ± 0.13 1.00<br />
NGC 4649 327 190.92703 11.56000 0.65 −7.582 ± 0.023 −9.237 ± 0.024 2.44 ± 0.16 1.00<br />
NGC 4649 328 190.92307 11.55289 0.33 −8.034 ± 0.025 −9.031 ± 0.042 2.13 ± 0.19 1.00<br />
NGC 4649 330 190.92753 11.56139 0.72 −6.897 ± 0.051 −8.378 ± 0.069 2.75 ± 0.28 1.00<br />
Continued on Next Page. . .<br />
388
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4649 332 190.92018 11.54839 0.29 −8.098 ± 0.033 −9.423 ± 0.033 2.79 ± 0.17 1.00<br />
NGC 4649 333 190.93146 11.56875 1.13 −7.418 ± 0.031 −8.871 ± 0.024 1.99 ± 0.15 1.00<br />
NGC 4649 335 190.91207 11.53423 1.00 −8.113 ± 0.025 −9.304 ± 0.018 1.99 ± 0.16 1.00<br />
NGC 4649 336 190.92108 11.55046 0.26 −7.647 ± 0.031 −8.988 ± 0.035 1.76 ± 0.21 1.00<br />
NGC 4649 337 190.91756 11.54418 0.45 −6.689 ± 0.959 −8.124 ± 0.116 1.66 ± 0.45 1.00<br />
NGC 4649 341 190.91987 11.54858 0.27 −9.246 ± 0.025 −10.172 ± 0.037 4.85 ± 0.12 1.00<br />
NGC 4649 342 190.92266 11.55375 0.31 −7.421 ± 0.028 −8.402 ± 0.057 2.16 ± 0.26 1.00<br />
NGC 4649 344 190.92975 11.56672 0.99 −6.112 ± 0.069 −7.094 ± 0.052 2.50 ± 0.44 0.99<br />
NGC 4649 345 190.92474 11.55782 0.49 −8.856 ± 0.022 −10.400 ± 0.016 2.10 ± 0.12 1.00<br />
NGC 4649 346 190.91193 11.53478 0.97 −7.726 ± 0.018 −8.858 ± 0.020 1.98 ± 0.14 1.00<br />
NGC 4649 347 190.92110 11.55124 0.24 −7.257 ± 0.106 −8.878 ± 0.125 2.09 ± 0.35 1.00<br />
NGC 4649 348 190.92456 11.55760 0.48 −8.104 ± 0.023 −9.151 ± 0.038 2.99 ± 0.17 1.00<br />
NGC 4649 350 190.91979 11.54931 0.24 −7.367 ± 0.037 −8.174 ± 0.052 1.54 ± 0.22 1.00<br />
NGC 4649 352 190.92801 11.56435 0.84 −4.957 ± 0.201 −6.798 ± 0.325 5.13 ± 3.78 0.51<br />
NGC 4649 353 190.91576 11.54242 0.54 −7.842 ± 0.021 −9.160 ± 0.021 2.51 ± 0.12 1.00<br />
NGC 4649 355 190.92372 11.55676 0.42 −8.650 ± 0.015 −9.634 ± 0.028 2.70 ± 0.13 1.00<br />
NGC 4649 357 190.91942 11.54935 0.23 −9.611 ± 0.016 −10.638 ± 0.020 2.61 ± 0.10 1.00<br />
NGC 4649 358 190.90715 11.52736 1.42 −8.131 ± 0.028 −9.000 ± 0.029 2.68 ± 0.19 1.00<br />
NGC 4649 359 190.91902 11.54869 0.25 −7.837 ± 0.340 −9.259 ± 0.040 1.54 ± 0.23 1.00<br />
NGC 4649 360 190.92276 11.55565 0.35 −8.734 ± 0.021 −10.334 ± 0.031 2.15 ± 0.19 1.00<br />
NGC 4649 362 190.91704 11.54555 0.38 −6.247 ± 0.043 −7.324 ± 0.715 1.73 ± 0.50 0.98<br />
NGC 4649 363 190.92280 11.55602 0.36 −7.668 ± 0.026 −8.429 ± 0.043 2.41 ± 0.24 1.00<br />
NGC 4649 364 190.90820 11.52983 1.28 −7.631 ± 0.037 −8.932 ± 0.021 2.06 ± 0.18 1.00<br />
NGC 4649 366 190.91051 11.53413 1.03 −8.414 ± 0.025 −9.624 ± 0.021 1.57 ± 0.10 1.00<br />
NGC 4649 367 190.92381 11.55799 0.46 −8.754 ± 0.020 −10.254 ± 0.017 1.44 ± 0.13 0.98<br />
NGC 4649 368 190.91911 11.54969 0.20 −6.646 ± 2.200 −8.350 ± 0.567 1.69 ± 0.51 1.00<br />
NGC 4649 369 190.91066 11.53449 1.01 −5.101 ± 0.368 −6.447 ± 0.083 2.21 ± 0.50 0.98<br />
NGC 4649 371 190.91902 11.54961 0.20 −8.679 ± 0.023 −10.146 ± 0.015 1.56 ± 0.14 1.00<br />
NGC 4649 373 190.91953 11.55018 0.20 −9.237 ± 0.021 −10.319 ± 0.015 3.12 ± 0.11 1.00<br />
NGC 4649 375 190.92134 11.55397 0.25 −8.108 ± 0.022 −8.935 ± 0.043 1.80 ± 0.23 1.00<br />
NGC 4649 376 190.92395 11.55884 0.49 −7.784 ± 0.080 −8.982 ± 0.094 6.34 ± 0.62 0.93<br />
NGC 4649 378 190.91504 11.54289 0.52 −7.753 ± 0.039 −8.645 ± 0.043 2.87 ± 0.18 1.00<br />
NGC 4649 379 190.92044 11.55266 0.19 −7.768 ± 0.057 −9.001 ± 0.064 3.31 ± 0.29 1.00<br />
NGC 4649 380 190.91585 11.54445 0.44 −8.441 ± 0.030 −9.739 ± 0.019 2.63 ± 0.16 1.00<br />
NGC 4649 381 190.92706 11.56464 0.82 −7.889 ± 0.021 −9.354 ± 0.026 2.50 ± 0.19 1.00<br />
NGC 4649 385 190.92624 11.56347 0.75 −9.570 ± 0.017 −10.871 ± 0.015 2.48 ± 0.15 1.00<br />
NGC 4649 386 190.91237 11.53865 0.77 −6.759 ± 0.048 −8.197 ± 0.051 2.42 ± 0.37 1.00<br />
NGC 4649 387 190.91990 11.55226 0.17 −9.003 ± 0.023 −10.409 ± 0.019 1.72 ± 0.16 1.00<br />
NGC 4649 388 190.91976 11.55228 0.16 −9.672 ± 0.019 −10.827 ± 0.018 2.45 ± 0.14 1.00<br />
NGC 4649 390 190.92030 11.55317 0.19 −6.125 ± 0.870 −7.746 ± 0.088 1.55 ± 0.46 0.99<br />
NGC 4649 392 190.91551 11.54469 0.43 −6.763 ± 0.062 −7.657 ± 0.070 2.74 ± 0.31 0.99<br />
NGC 4649 393 190.91684 11.54714 0.29 −7.825 ± 0.026 −9.105 ± 0.037 2.12 ± 0.23 1.00<br />
NGC 4649 394 190.91212 11.53868 0.77 −5.706 ± 0.059 −6.937 ± 0.089 2.61 ± 0.37 0.98<br />
NGC 4649 397 190.91960 11.55241 0.15 −7.756 ± 0.064 −8.881 ± 0.091 3.44 ± 0.34 1.00<br />
NGC 4649 398 190.91872 11.55087 0.14 −9.092 ± 0.022 −10.276 ± 0.034 3.16 ± 0.15 1.00<br />
NGC 4649 401 190.92785 11.56735 0.96 −5.459 ± 0.072 −7.115 ± 0.058 2.22 ± 0.41 0.99<br />
NGC 4649 402 190.91073 11.53669 0.90 −7.837 ± 0.044 −8.817 ± 0.064 4.99 ± 0.33 0.98<br />
NGC 4649 404 190.91564 11.54570 0.37 −6.367 ± 0.112 −7.008 ± 0.347 3.04 ± 0.60 0.96<br />
NGC 4649 406 190.92163 11.55645 0.32 −6.087 ± 0.565 −7.679 ± 0.579 1.90 ± 0.51 0.99<br />
NGC 4649 407 190.92386 11.56063 0.55 −9.426 ± 0.023 −10.707 ± 0.014 2.14 ± 0.20 1.00<br />
NGC 4649 408 190.91897 11.55178 0.13 −7.010 ± 0.237 −8.287 ± 0.229 3.97 ± 1.81 1.00<br />
NGC 4649 409 190.91971 11.55311 0.16 −7.386 ± 0.038 −8.941 ± 0.050 1.97 ± 0.29 1.00<br />
NGC 4649 410 190.91009 11.53600 0.94 −9.090 ± 0.014 −10.437 ± 0.025 2.85 ± 0.12 1.00<br />
NGC 4649 411 190.93103 11.57359 1.32 −6.903 ± 0.050 −7.899 ± 0.032 2.89 ± 0.26 0.99<br />
NGC 4649 413 190.91620 11.54711 0.30 −6.504 ± 0.085 −7.714 ± 0.532 1.24 ± 0.31 0.96<br />
NGC 4649 414 190.91486 11.54470 0.43 −8.285 ± 0.032 −9.275 ± 0.026 2.94 ± 0.15 1.00<br />
NGC 4649 417 190.92979 11.57166 1.20 −5.658 ± 0.066 −6.954 ± 0.369 2.61 ± 0.52 0.98<br />
NGC 4649 419 190.91333 11.54242 0.57 −8.020 ± 0.022 −9.562 ± 0.021 2.21 ± 0.21 1.00<br />
NGC 4649 421 190.90928 11.53534 0.99 −7.452 ± 0.023 −8.320 ± 0.034 3.44 ± 0.21 1.00<br />
NGC 4649 422 190.92076 11.55606 0.27 −6.968 ± 0.056 −7.975 ± 0.043 1.87 ± 0.30 1.00<br />
NGC 4649 423 190.91599 11.54783 0.26 −7.533 ± 0.046 −8.736 ± 0.045 3.18 ± 0.20 1.00<br />
NGC 4649 424 190.91395 11.54413 0.47 −7.809 ± 0.018 −9.183 ± 0.026 2.64 ± 0.14 1.00<br />
Continued on Next Page. . .<br />
389
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4649 425 190.91931 11.55389 0.15 −8.461 ± 0.036 −9.387 ± 0.031 2.03 ± 0.19 1.00<br />
NGC 4649 427 190.92694 11.56788 0.95 −8.625 ± 0.027 −10.043 ± 0.019 2.80 ± 0.11 1.00<br />
NGC 4649 428 190.91392 11.54445 0.46 −6.241 ± 0.228 −7.124 ± 0.059 4.10 ± 1.19 0.85<br />
NGC 4649 429 190.91365 11.54407 0.48 −6.780 ± 0.070 −7.762 ± 0.064 3.26 ± 0.36 0.98<br />
NGC 4649 430 190.91802 11.55225 0.07 −7.000 ± 0.516 −8.407 ± 0.342 1.77 ± 1.78 1.00<br />
NGC 4649 431 190.92754 11.56947 1.04 −6.510 ± 0.055 −7.485 ± 0.298 2.59 ± 0.43 0.99<br />
NGC 4649 433 190.92131 11.55863 0.39 −7.657 ± 0.065 −8.892 ± 0.256 7.17 ± 2.30 0.85<br />
NGC 4649 434 190.93112 11.57628 1.44 −6.945 ± 0.042 −7.819 ± 0.038 2.92 ± 0.28 0.99<br />
NGC 4649 436 190.91805 11.55294 0.07 −8.184 ± 0.046 −9.563 ± 0.311 2.23 ± 0.24 1.00<br />
NGC 4649 437 190.91533 11.54809 0.25 −8.474 ± 0.023 −9.400 ± 0.027 2.08 ± 0.18 1.00<br />
NGC 4649 439 190.92971 11.57431 1.31 −7.290 ± 0.328 −8.990 ± 0.021 1.59 ± 0.34 1.00<br />
NGC 4649 440 190.91122 11.54121 0.67 −6.921 ± 0.047 −8.285 ± 0.050 2.70 ± 0.22 1.00<br />
NGC 4649 441 190.91188 11.54262 0.59 −8.105 ± 0.021 −9.236 ± 0.028 2.98 ± 0.14 1.00<br />
NGC 4649 443 190.91442 11.54769 0.29 −6.862 ± 0.048 −8.436 ± 0.039 2.76 ± 0.23 1.00<br />
NGC 4649 444 190.90510 11.53101 1.29 −5.782 ± 0.090 −7.415 ± 0.085 2.47 ± 0.43 0.99<br />
NGC 4649 445 190.91169 11.54290 0.58 −6.625 ± 0.032 −8.091 ± 0.049 2.21 ± 0.33 1.00<br />
NGC 4649 446 190.91685 11.55217 0.03 −8.395 ± 0.072 −10.017 ± 0.042 1.82 ± 0.26 1.00<br />
NGC 4649 447 190.91711 11.55223 0.04 −8.635 ± 0.626 −10.020 ± 1.331 1.85 ± 0.62 1.00<br />
NGC 4649 451 190.90757 11.53571 1.01 −7.238 ± 0.031 −7.982 ± 0.030 1.99 ± 0.25 1.00<br />
NGC 4649 452 190.91924 11.55689 0.25 −6.989 ± 0.541 −7.928 ± 0.227 1.37 ± 0.32 0.98<br />
NGC 4649 454 190.90743 11.53586 1.00 −9.444 ± 0.015 −10.544 ± 0.013 2.57 ± 0.08 1.00<br />
NGC 4649 456 190.92094 11.56020 0.45 −6.611 ± 0.038 −8.336 ± 0.057 2.29 ± 0.32 1.00<br />
NGC 4649 457 190.92172 11.56168 0.53 −7.662 ± 0.464 −9.110 ± 0.029 1.37 ± 0.22 0.97<br />
NGC 4649 458 190.92381 11.56555 0.76 −6.428 ± 0.059 −7.706 ± 0.081 2.55 ± 0.31 0.99<br />
NGC 4649 459 190.91234 11.54494 0.47 −6.447 ± 0.055 −7.303 ± 0.183 1.19 ± 0.25 0.93<br />
NGC 4649 460 190.92334 11.56470 0.71 −6.743 ± 0.050 −7.597 ± 0.071 2.90 ± 0.39 0.99<br />
NGC 4649 461 190.91737 11.55400 0.07 −8.094 ± 0.194 −9.492 ± 0.034 1.86 ± 0.34 1.00<br />
NGC 4649 462 190.92463 11.56712 0.86 −7.305 ± 0.035 −8.537 ± 0.042 2.79 ± 0.24 1.00<br />
NGC 4649 464 190.92023 11.55949 0.40 −8.092 ± 0.024 −9.625 ± 0.025 1.39 ± 0.18 0.97<br />
NGC 4649 466 190.91392 11.54799 0.29 −7.480 ± 0.044 −9.025 ± 0.028 2.09 ± 0.22 1.00<br />
NGC 4649 469 190.92230 11.56333 0.62 −6.610 ± 0.043 −8.009 ± 0.074 1.92 ± 0.32 1.00<br />
NGC 4649 470 190.91188 11.54503 0.47 −7.040 ± 0.040 −7.826 ± 0.044 2.58 ± 0.24 0.99<br />
NGC 4649 471 190.91966 11.55906 0.36 −6.184 ± 0.112 −7.466 ± 0.444 2.34 ± 0.47 0.99<br />
NGC 4649 472 190.91493 11.55081 0.14 −9.820 ± 0.021 −11.311 ± 0.009 2.34 ± 0.16 1.00<br />
NGC 4649 473 190.91039 11.54269 0.62 −6.907 ± 0.034 −8.360 ± 0.045 1.95 ± 0.27 1.00<br />
NGC 4649 474 190.91660 11.55392 0.06 −9.696 ± 0.014 −10.822 ± 0.019 1.95 ± 0.14 1.00<br />
NGC 4649 475 190.91115 11.54418 0.53 −10.079 ± 0.017 −11.074 ± 0.012 3.45 ± 0.10 1.00<br />
NGC 4649 476 190.91804 11.55657 0.21 −8.446 ± 1.615 −9.597 ± 0.760 0.82 ± 0.32 0.75<br />
NGC 4649 477 190.91449 11.55022 0.17 −9.084 ± 0.021 −10.405 ± 0.011 1.59 ± 0.12 1.00<br />
NGC 4649 478 190.91782 11.55623 0.19 −7.512 ± 0.059 −8.818 ± 0.105 3.19 ± 0.59 1.00<br />
NGC 4649 479 190.91409 11.54949 0.22 −6.693 ± 0.088 −7.897 ± 0.133 1.93 ± 0.65 1.00<br />
NGC 4649 480 190.91083 11.54377 0.56 −5.370 ± 0.466 −6.429 ± 0.289 2.14 ± 0.64 0.98<br />
NGC 4649 481 190.92495 11.56930 0.96 −6.872 ± 0.027 −7.762 ± 0.035 2.60 ± 0.21 0.99<br />
NGC 4649 482 190.91370 11.54941 0.23 −11.033 ± 0.025 −12.692 ± 0.018 4.80 ± 0.15 0.98<br />
NGC 4649 483 190.91180 11.54579 0.44 −7.886 ± 0.031 −9.106 ± 0.022 2.38 ± 0.17 1.00<br />
NGC 4649 484 190.92763 11.57439 1.26 −6.984 ± 0.049 −8.410 ± 0.026 2.46 ± 0.22 1.00<br />
NGC 4649 485 190.92445 11.56853 0.92 −5.095 ± 0.797 −6.541 ± 0.281 0.94 ± 0.45 0.84<br />
NGC 4649 487 190.91119 11.54464 0.51 −6.897 ± 0.131 −8.383 ± 0.034 1.73 ± 0.31 1.00<br />
NGC 4649 488 190.90793 11.53923 0.84 −6.040 ± 0.085 −6.664 ± 0.387 2.05 ± 0.49 0.99<br />
NGC 4649 489 190.91008 11.54319 0.61 −7.783 ± 0.020 −9.071 ± 0.016 1.83 ± 0.17 1.00<br />
NGC 4649 491 190.90541 11.53502 1.09 −8.461 ± 0.016 −9.224 ± 0.021 2.52 ± 0.15 1.00<br />
NGC 4649 493 190.90634 11.53683 0.99 −8.454 ± 0.022 −9.871 ± 0.017 2.60 ± 0.13 1.00<br />
NGC 4649 494 190.90674 11.53756 0.95 −7.258 ± 0.034 −8.819 ± 0.025 2.78 ± 0.13 1.00<br />
NGC 4649 495 190.91892 11.55957 0.37 −7.707 ± 0.032 −9.001 ± 0.030 2.69 ± 0.24 1.00<br />
NGC 4649 496 190.91658 11.55510 0.12 −6.835 ± 0.052 −8.478 ± 0.085 2.37 ± 0.31 1.00<br />
NGC 4649 497 190.92661 11.57366 1.21 −8.612 ± 0.037 −9.542 ± 0.025 3.92 ± 0.14 1.00<br />
NGC 4649 498 190.92616 11.57282 1.16 −7.577 ± 0.642 −9.208 ± 0.032 2.30 ± 0.56 1.00<br />
NGC 4649 500 190.91099 11.54567 0.47 −6.379 ± 0.169 −7.669 ± 0.340 3.04 ± 0.85 0.99<br />
NGC 4649 501 190.92711 11.57472 1.27 −6.071 ± 0.075 −7.221 ± 0.051 1.71 ± 0.26 0.98<br />
NGC 4649 503 190.92673 11.57445 1.25 −6.555 ± 0.088 −7.669 ± 0.074 4.81 ± 0.39 0.87<br />
NGC 4649 504 190.92073 11.56363 0.61 −6.436 ± 0.061 −7.825 ± 0.075 3.13 ± 0.45 0.99<br />
NGC 4649 505 190.91391 11.55141 0.16 −8.421 ± 0.031 −9.819 ± 0.022 2.35 ± 0.16 1.00<br />
Continued on Next Page. . .<br />
390
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4649 506 190.91572 11.55498 0.13 −8.997 ± 0.021 −10.396 ± 0.019 2.08 ± 0.15 1.00<br />
NGC 4649 507 190.90703 11.53940 0.86 −6.120 ± 0.062 −7.621 ± 0.043 2.03 ± 0.24 1.00<br />
NGC 4649 508 190.91009 11.54504 0.53 −6.145 ± 0.053 −7.283 ± 0.077 2.08 ± 0.28 0.99<br />
NGC 4649 509 190.92007 11.56313 0.57 −7.209 ± 0.048 −7.951 ± 0.057 1.75 ± 0.43 0.99<br />
NGC 4649 511 190.90786 11.54140 0.75 −7.635 ± 0.070 −8.225 ± 0.108 3.58 ± 0.47 1.00<br />
NGC 4649 512 190.92222 11.56733 0.81 −7.240 ± 0.043 −8.097 ± 0.068 3.11 ± 0.35 1.00<br />
NGC 4649 513 190.92302 11.56877 0.90 −7.308 ± 0.035 −8.242 ± 0.053 3.06 ± 0.29 1.00<br />
NGC 4649 514 190.91052 11.54639 0.46 −8.801 ± 0.022 −10.331 ± 0.013 2.36 ± 0.12 1.00<br />
NGC 4649 515 190.90944 11.54445 0.57 −5.302 ± 0.298 −6.780 ± 0.484 2.84 ± 1.75 0.96<br />
NGC 4649 516 190.91367 11.55220 0.16 −8.699 ± 0.023 −10.109 ± 0.021 2.86 ± 0.12 1.00<br />
NGC 4649 517 190.91971 11.56311 0.56 −8.151 ± 0.034 −9.075 ± 0.047 4.03 ± 0.20 1.00<br />
NGC 4649 518 190.91475 11.55436 0.13 −9.397 ± 0.017 −10.445 ± 0.019 2.60 ± 0.10 1.00<br />
NGC 4649 519 190.90840 11.54304 0.66 −8.549 ± 0.047 −9.811 ± 0.090 7.36 ± 0.71 1.00<br />
NGC 4649 521 190.90605 11.53878 0.91 −8.525 ± 0.020 −9.558 ± 0.018 2.91 ± 0.16 1.00<br />
NGC 4649 522 190.90587 11.53840 0.93 −6.420 ± 0.083 −8.198 ± 0.059 3.42 ± 0.32 1.00<br />
NGC 4649 523 190.91954 11.56310 0.56 −7.583 ± 0.026 −8.818 ± 0.028 1.82 ± 0.17 1.00<br />
NGC 4649 524 190.92005 11.56430 0.63 −6.356 ± 0.107 −6.947 ± 0.062 2.64 ± 0.38 0.98<br />
NGC 4649 529 190.90466 11.53660 1.05 −5.430 ± 0.489 −6.911 ± 0.356 2.23 ± 0.50 0.99<br />
NGC 4649 530 190.92587 11.57480 1.25 −7.072 ± 0.062 −8.060 ± 0.104 5.02 ± 0.46 0.93<br />
NGC 4649 533 190.91656 11.55815 0.28 −9.650 ± 0.015 −10.617 ± 0.015 2.99 ± 0.14 1.00<br />
NGC 4649 534 190.90188 11.53186 1.33 −6.983 ± 0.043 −7.973 ± 0.060 2.02 ± 0.32 1.00<br />
NGC 4649 535 190.91400 11.55405 0.15 −7.885 ± 0.042 −9.321 ± 0.036 1.90 ± 0.19 1.00<br />
NGC 4649 538 190.91562 11.55715 0.24 −6.555 ± 0.174 −7.802 ± 0.100 3.89 ± 0.69 0.97<br />
NGC 4649 539 190.90619 11.54031 0.85 −7.966 ± 0.021 −9.459 ± 0.032 2.24 ± 0.18 1.00<br />
NGC 4649 540 190.91077 11.54862 0.37 −8.958 ± 0.020 −9.938 ± 0.022 2.82 ± 0.13 1.00<br />
NGC 4649 541 190.91940 11.56410 0.61 −7.156 ± 0.051 −8.173 ± 0.304 1.92 ± 0.31 1.00<br />
NGC 4649 542 190.91133 11.54960 0.32 −8.130 ± 0.017 −9.457 ± 0.019 2.18 ± 0.13 1.00<br />
NGC 4649 543 190.91315 11.55326 0.18 −6.855 ± 0.128 −8.424 ± 0.349 4.69 ± 2.46 0.98<br />
NGC 4649 545 190.91987 11.56545 0.68 −6.659 ± 0.041 −7.586 ± 0.317 1.74 ± 0.27 0.99<br />
NGC 4649 546 190.90766 11.54374 0.66 −8.198 ± 0.033 −9.235 ± 0.040 3.16 ± 0.14 1.00<br />
NGC 4649 547 190.91864 11.56357 0.57 −9.589 ± 0.015 −10.483 ± 0.012 4.33 ± 0.05 1.00<br />
NGC 4649 549 190.91173 11.55126 0.27 −9.741 ± 0.014 −10.850 ± 0.010 3.06 ± 0.06 1.00<br />
NGC 4649 550 190.90208 11.53400 1.24 −8.077 ± 0.021 −9.063 ± 0.023 2.95 ± 0.18 1.00<br />
NGC 4649 551 190.90152 11.53309 1.29 −5.825 ± 0.065 −7.137 ± 0.241 5.71 ± 2.03 0.52<br />
NGC 4649 552 190.90636 11.54198 0.77 −5.587 ± 0.177 −7.288 ± 0.190 4.01 ± 1.10 0.90<br />
NGC 4649 553 190.91540 11.55838 0.30 −8.664 ± 0.015 −9.634 ± 0.026 3.21 ± 0.11 1.00<br />
NGC 4649 554 190.91087 11.55060 0.32 −10.392 ± 0.024 −11.269 ± 0.019 9.78 ± 0.17 1.00<br />
NGC 4649 555 190.91094 11.55076 0.31 −7.601 ± 0.036 −8.922 ± 0.036 2.57 ± 0.29 1.00<br />
NGC 4649 556 190.91191 11.55238 0.24 −8.796 ± 0.016 −9.777 ± 0.033 3.10 ± 0.15 1.00<br />
NGC 4649 557 190.91456 11.55715 0.25 −7.185 ± 0.044 −8.115 ± 0.104 2.62 ± 0.40 1.00<br />
NGC 4649 559 190.91021 11.54951 0.37 −7.430 ± 0.034 −8.468 ± 0.065 2.70 ± 0.38 1.00<br />
NGC 4649 560 190.90516 11.54079 0.86 −7.166 ± 0.034 −8.349 ± 0.031 2.02 ± 0.23 1.00<br />
NGC 4649 561 190.89949 11.53072 1.45 −7.667 ± 0.018 −9.302 ± 0.019 2.15 ± 0.11 1.00<br />
NGC 4649 562 190.91463 11.55804 0.30 −7.965 ± 0.029 −9.399 ± 0.023 2.07 ± 0.17 1.00<br />
NGC 4649 563 190.92474 11.57653 1.31 −8.795 ± 0.045 −9.865 ± 0.025 2.63 ± 0.25 1.00<br />
NGC 4649 564 190.92424 11.57564 1.26 −8.065 ± 0.022 −9.132 ± 0.023 2.66 ± 0.15 1.00<br />
NGC 4649 566 190.91115 11.55213 0.29 −8.600 ± 0.028 −10.126 ± 0.019 2.11 ± 0.12 1.00<br />
NGC 4649 567 190.92349 11.57440 1.19 −9.557 ± 0.018 −11.037 ± 0.010 1.76 ± 0.10 1.00<br />
NGC 4649 568 190.91228 11.55413 0.24 −8.378 ± 0.017 −9.939 ± 0.017 2.18 ± 0.16 1.00<br />
NGC 4649 569 190.91675 11.56264 0.52 −7.211 ± 0.024 −8.047 ± 1.201 2.16 ± 0.39 1.00<br />
NGC 4649 570 190.91356 11.55703 0.27 −8.314 ± 0.035 −9.326 ± 0.055 3.72 ± 0.26 1.00<br />
NGC 4649 571 190.91417 11.55810 0.31 −6.589 ± 0.085 −8.202 ± 0.046 2.07 ± 0.38 1.00<br />
NGC 4649 572 190.92262 11.57341 1.12 −6.872 ± 0.042 −8.409 ± 0.050 2.87 ± 0.28 1.00<br />
NGC 4649 573 190.90286 11.53790 1.05 −7.521 ± 0.027 −8.579 ± 0.059 2.72 ± 0.25 1.00<br />
NGC 4649 574 190.91669 11.56313 0.54 −7.399 ± 0.030 −8.422 ± 0.040 1.92 ± 0.21 1.00<br />
NGC 4649 575 190.90970 11.55056 0.38 −8.411 ± 0.023 −9.369 ± 0.021 2.57 ± 0.10 1.00<br />
NGC 4649 576 190.90350 11.53971 0.96 −7.919 ± 0.018 −9.288 ± 0.019 2.44 ± 0.12 1.00<br />
NGC 4649 579 190.90544 11.54324 0.76 −6.036 ± 0.074 −7.451 ± 0.418 2.12 ± 0.37 0.99<br />
NGC 4649 580 190.91444 11.55949 0.37 −6.658 ± 0.058 −7.694 ± 0.056 2.12 ± 0.29 1.00<br />
NGC 4649 581 190.90853 11.54889 0.46 −5.705 ± 0.153 −7.603 ± 0.403 3.93 ± 1.31 0.95<br />
NGC 4649 582 190.91475 11.56011 0.40 −5.976 ± 0.204 −7.246 ± 0.133 2.40 ± 0.51 0.99<br />
NGC 4649 583 190.90714 11.54648 0.59 −6.188 ± 0.085 −7.873 ± 0.053 2.39 ± 0.37 1.00<br />
Continued on Next Page. . .<br />
391
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4649 584 190.90465 11.54212 0.83 −5.333 ± 0.521 −6.713 ± 0.130 3.19 ± 1.22 0.93<br />
NGC 4649 585 190.91511 11.56111 0.44 −7.918 ± 0.400 −8.974 ± 0.026 1.93 ± 0.20 1.00<br />
NGC 4649 586 190.90700 11.54586 0.61 −9.280 ± 0.038 −10.243 ± 0.028 5.26 ± 0.16 1.00<br />
NGC 4649 587 190.91533 11.56165 0.47 −7.117 ± 0.039 −8.516 ± 0.269 2.96 ± 0.55 1.00<br />
NGC 4649 588 190.91055 11.55325 0.31 −7.122 ± 0.050 −8.430 ± 0.063 3.43 ± 0.30 1.00<br />
NGC 4649 589 190.92004 11.57040 0.94 −6.658 ± 0.044 −8.191 ± 0.074 1.56 ± 0.28 1.00<br />
NGC 4649 590 190.91193 11.55580 0.29 −6.749 ± 0.938 −8.374 ± 0.052 1.09 ± 0.32 0.93<br />
NGC 4649 591 190.91310 11.55816 0.34 −10.662 ± 0.036 −11.892 ± 0.022 5.50 ± 0.16 1.00<br />
NGC 4649 592 190.90725 11.54776 0.55 −5.886 ± 0.436 −6.893 ± 0.599 0.94 ± 0.43 0.82<br />
NGC 4649 593 190.91345 11.55908 0.37 −5.990 ± 0.812 −7.412 ± 0.057 1.56 ± 0.31 0.98<br />
NGC 4649 594 190.90538 11.54472 0.72 −9.261 ± 0.021 −10.782 ± 0.014 2.60 ± 0.18 1.00<br />
NGC 4649 595 190.90466 11.54392 0.77 −8.766 ± 0.038 −9.638 ± 0.038 4.64 ± 0.25 1.00<br />
NGC 4649 597 190.90107 11.53746 1.13 −7.276 ± 0.037 −8.130 ± 0.028 2.04 ± 0.19 1.00<br />
NGC 4649 599 190.91068 11.55489 0.33 −6.992 ± 0.063 −8.659 ± 0.054 2.52 ± 0.25 1.00<br />
NGC 4649 600 190.90287 11.54106 0.94 −6.025 ± 0.061 −7.594 ± 0.059 3.21 ± 0.35 0.98<br />
NGC 4649 601 190.91381 11.56091 0.45 −5.793 ± 0.142 −6.381 ± 0.472 2.56 ± 0.66 0.97<br />
NGC 4649 602 190.90434 11.54408 0.78 −8.375 ± 0.034 −9.513 ± 0.032 2.90 ± 0.23 1.00<br />
NGC 4649 603 190.90826 11.55127 0.44 −7.488 ± 0.032 −8.995 ± 0.122 1.63 ± 0.26 1.00<br />
NGC 4649 604 190.90604 11.54792 0.60 −8.312 ± 0.026 −9.529 ± 0.025 2.17 ± 0.17 1.00<br />
NGC 4649 606 190.90503 11.54638 0.68 −7.972 ± 0.056 −9.334 ± 0.020 2.28 ± 0.22 1.00<br />
NGC 4649 607 190.89888 11.53532 1.29 −6.732 ± 0.051 −7.548 ± 0.040 2.41 ± 0.28 0.99<br />
NGC 4649 608 190.89800 11.53380 1.38 −6.209 ± 0.046 −7.539 ± 0.055 2.46 ± 0.28 0.99<br />
NGC 4649 609 190.91713 11.56848 0.82 −7.658 ± 0.015 −8.554 ± 0.032 2.33 ± 0.18 1.00<br />
NGC 4649 610 190.92290 11.57884 1.40 −7.106 ± 0.350 −8.607 ± 1.214 2.66 ± 0.59 1.00<br />
NGC 4649 613 190.91216 11.55994 0.44 −8.876 ± 0.017 −9.869 ± 0.011 2.21 ± 0.12 1.00<br />
NGC 4649 614 190.91701 11.56890 0.85 −6.313 ± 0.065 −7.803 ± 0.043 2.65 ± 0.37 0.99<br />
NGC 4649 615 190.91623 11.56762 0.78 −9.345 ± 0.024 −10.669 ± 0.011 1.97 ± 0.18 1.00<br />
NGC 4649 616 190.91468 11.56479 0.64 −8.973 ± 0.015 −10.259 ± 0.020 1.56 ± 0.14 1.00<br />
NGC 4649 617 190.92037 11.57502 1.18 −7.839 ± 0.040 −9.270 ± 0.021 2.02 ± 0.17 1.00<br />
NGC 4649 618 190.91034 11.55702 0.39 −7.603 ± 0.032 −9.007 ± 0.024 2.10 ± 0.19 1.00<br />
NGC 4649 619 190.89845 11.53577 1.29 −8.162 ± 0.024 −9.442 ± 0.042 2.27 ± 0.19 1.00<br />
NGC 4649 620 190.91252 11.56112 0.49 −9.477 ± 0.015 −10.405 ± 0.011 2.51 ± 0.13 1.00<br />
NGC 4649 621 190.90874 11.55442 0.42 −9.102 ± 0.047 −10.209 ± 0.024 2.47 ± 0.25 1.00<br />
NGC 4649 622 190.90863 11.55446 0.42 −7.533 ± 0.033 −8.874 ± 0.313 1.44 ± 0.23 0.98<br />
NGC 4649 623 190.91862 11.57250 1.04 −6.869 ± 0.033 −7.947 ± 0.061 3.09 ± 0.31 0.99<br />
NGC 4649 624 190.90874 11.55499 0.42 −7.895 ± 0.029 −9.604 ± 0.035 3.52 ± 0.14 1.00<br />
NGC 4649 625 190.91101 11.55905 0.44 −6.144 ± 0.177 −7.751 ± 0.125 4.81 ± 0.97 0.89<br />
NGC 4649 626 190.90460 11.54765 0.67 −8.843 ± 0.020 −10.269 ± 0.011 2.40 ± 0.17 1.00<br />
NGC 4649 627 190.90919 11.55606 0.42 −7.736 ± 0.029 −9.274 ± 0.024 2.14 ± 0.22 1.00<br />
NGC 4649 628 190.91933 11.57425 1.13 −7.849 ± 0.027 −8.859 ± 0.030 2.76 ± 0.16 1.00<br />
NGC 4649 629 190.90674 11.55162 0.51 −8.048 ± 0.016 −9.045 ± 0.044 3.61 ± 0.20 1.00<br />
NGC 4649 630 190.90761 11.55323 0.47 −5.699 ± 0.310 −7.090 ± 0.085 2.62 ± 0.73 0.98<br />
NGC 4649 631 190.91217 11.56159 0.52 −7.540 ± 0.034 −9.145 ± 0.035 1.91 ± 0.19 1.00<br />
NGC 4649 632 190.90341 11.54619 0.76 −6.024 ± 0.106 −7.155 ± 0.073 2.57 ± 0.45 0.98<br />
NGC 4649 633 190.91449 11.56612 0.71 −5.607 ± 0.135 −6.327 ± 0.684 2.27 ± 1.17 0.98<br />
NGC 4649 634 190.90382 11.54708 0.72 −7.196 ± 0.080 −7.791 ± 0.054 4.53 ± 0.27 0.92<br />
NGC 4649 635 190.90714 11.55320 0.49 −6.113 ± 0.210 −7.711 ± 0.305 2.67 ± 0.45 0.99<br />
NGC 4649 636 190.91634 11.56984 0.89 −6.758 ± 0.084 −8.048 ± 0.054 2.62 ± 0.52 1.00<br />
NGC 4649 637 190.91870 11.57413 1.12 −7.227 ± 0.037 −8.142 ± 0.031 2.66 ± 0.19 1.00<br />
NGC 4649 640 190.90489 11.54954 0.63 −7.976 ± 0.025 −9.411 ± 0.023 2.66 ± 0.14 1.00<br />
NGC 4649 641 190.91223 11.56286 0.58 −9.032 ± 0.018 −10.411 ± 0.014 1.36 ± 0.09 0.96<br />
NGC 4649 642 190.89848 11.53805 1.21 −5.666 ± 0.085 −7.060 ± 0.396 1.36 ± 0.37 0.95<br />
NGC 4649 643 190.90797 11.55533 0.47 −8.611 ± 0.019 −9.925 ± 0.015 2.04 ± 0.09 1.00<br />
NGC 4649 644 190.92087 11.57852 1.37 −7.750 ± 0.024 −8.683 ± 0.023 2.34 ± 0.18 1.00<br />
NGC 4649 645 190.90752 11.55453 0.48 −7.342 ± 0.063 −8.797 ± 0.119 3.41 ± 0.43 1.00<br />
NGC 4649 647 190.90532 11.55037 0.60 −7.834 ± 0.024 −9.255 ± 0.019 1.89 ± 0.16 1.00<br />
NGC 4649 648 190.91156 11.56194 0.55 −7.292 ± 0.036 −8.496 ± 0.147 4.67 ± 0.72 0.99<br />
NGC 4649 649 190.89819 11.53812 1.22 −9.246 ± 0.018 −10.271 ± 0.009 2.74 ± 0.08 1.00<br />
NGC 4649 650 190.90947 11.55834 0.47 −8.998 ± 0.014 −10.505 ± 0.015 2.67 ± 0.08 1.00<br />
NGC 4649 651 190.91092 11.56101 0.52 −6.544 ± 0.050 −7.982 ± 0.103 2.54 ± 0.49 1.00<br />
NGC 4649 652 190.89655 11.53521 1.38 −5.265 ± 0.095 −6.164 ± 0.641 3.63 ± 0.65 0.89<br />
NGC 4649 653 190.90550 11.55150 0.58 −8.674 ± 0.013 −10.212 ± 0.021 2.52 ± 0.10 1.00<br />
Continued on Next Page. . .<br />
392
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4649 654 190.89981 11.54118 1.06 −7.931 ± 0.019 −8.894 ± 0.022 2.58 ± 0.15 1.00<br />
NGC 4649 655 190.89511 11.53298 1.52 −7.550 ± 0.049 −8.868 ± 0.023 3.47 ± 0.20 1.00<br />
NGC 4649 656 190.90512 11.55096 0.60 −6.876 ± 0.063 −8.217 ± 0.043 3.12 ± 0.21 1.00<br />
NGC 4649 659 190.92110 11.57999 1.44 −6.973 ± 0.056 −8.067 ± 0.066 3.15 ± 0.34 0.99<br />
NGC 4649 660 190.90669 11.55412 0.52 −7.100 ± 0.048 −8.221 ± 0.081 4.07 ± 0.32 1.00<br />
NGC 4649 661 190.91791 11.57447 1.14 −6.741 ± 0.041 −8.141 ± 0.031 2.03 ± 0.21 1.00<br />
NGC 4649 662 190.90216 11.54623 0.82 −6.891 ± 0.073 −7.676 ± 0.062 3.31 ± 0.32 0.98<br />
NGC 4649 664 190.91515 11.56983 0.90 −7.279 ± 0.025 −8.182 ± 0.042 2.51 ± 0.22 1.00<br />
NGC 4649 665 190.89473 11.53328 1.52 −6.552 ± 0.056 −7.867 ± 0.031 1.77 ± 0.27 0.99<br />
NGC 4649 666 190.89608 11.53566 1.39 −5.771 ± 0.651 −6.514 ± 0.074 0.94 ± 0.24 0.84<br />
NGC 4649 668 190.90172 11.54600 0.85 −7.321 ± 0.048 −8.710 ± 0.021 1.53 ± 0.23 0.99<br />
NGC 4649 669 190.91063 11.56206 0.58 −5.320 ± 0.141 −6.587 ± 0.737 2.39 ± 0.79 0.98<br />
NGC 4649 670 190.89704 11.53773 1.28 −8.158 ± 0.038 −9.594 ± 0.035 2.48 ± 0.23 1.00<br />
NGC 4649 671 190.91219 11.56514 0.69 −8.700 ± 0.024 −9.797 ± 0.019 2.01 ± 0.16 1.00<br />
NGC 4649 672 190.90260 11.54794 0.77 −6.400 ± 0.083 −7.855 ± 0.070 2.85 ± 0.37 0.99<br />
NGC 4649 673 190.90512 11.55265 0.59 −5.983 ± 0.220 −6.935 ± 0.120 3.85 ± 1.25 0.85<br />
NGC 4649 674 190.91016 11.56184 0.58 −6.452 ± 0.134 −7.700 ± 0.165 2.08 ± 0.35 1.00<br />
NGC 4649 675 190.90113 11.54573 0.88 −8.817 ± 0.022 −10.339 ± 0.019 2.53 ± 0.14 1.00<br />
NGC 4649 676 190.90987 11.56157 0.58 −8.856 ± 0.013 −10.006 ± 0.014 2.42 ± 0.07 1.00<br />
NGC 4649 678 190.90603 11.55506 0.56 −7.509 ± 0.033 −9.057 ± 0.026 1.91 ± 0.14 1.00<br />
NGC 4649 679 190.90449 11.55243 0.63 −7.278 ± 0.030 −8.841 ± 0.025 1.76 ± 0.21 1.00<br />
NGC 4649 681 190.89410 11.53393 1.52 −7.283 ± 0.033 −8.461 ± 0.049 3.33 ± 0.26 1.00<br />
NGC 4649 682 190.91279 11.56768 0.81 −6.248 ± 0.070 −7.431 ± 0.061 1.93 ± 0.46 0.99<br />
NGC 4649 684 190.89487 11.53560 1.44 −7.057 ± 0.026 −7.792 ± 0.028 2.38 ± 0.20 1.00<br />
NGC 4649 685 190.91887 11.57894 1.38 −5.408 ± 0.370 −6.723 ± 0.328 2.63 ± 0.55 0.97<br />
NGC 4649 686 190.90602 11.55616 0.57 −6.628 ± 0.735 −8.113 ± 0.044 1.38 ± 0.35 0.98<br />
NGC 4649 688 190.91193 11.56684 0.78 −6.869 ± 0.031 −8.197 ± 0.802 1.88 ± 0.25 1.00<br />
NGC 4649 689 190.91211 11.56718 0.79 −5.699 ± 0.081 −7.174 ± 0.244 3.30 ± 1.18 0.95<br />
NGC 4649 690 190.90812 11.56001 0.58 −6.580 ± 0.203 −7.920 ± 0.651 2.15 ± 0.37 1.00<br />
NGC 4649 691 190.89455 11.53570 1.45 −6.016 ± 0.115 −6.909 ± 0.117 3.91 ± 0.58 0.84<br />
NGC 4649 692 190.91771 11.57724 1.28 −5.856 ± 0.056 −7.593 ± 0.050 3.84 ± 0.27 0.95<br />
NGC 4649 693 190.90439 11.55340 0.63 −6.467 ± 0.091 −7.771 ± 0.195 5.76 ± 1.40 0.81<br />
NGC 4649 694 190.90496 11.55456 0.61 −7.682 ± 0.042 −8.658 ± 0.032 2.61 ± 0.20 1.00<br />
NGC 4649 696 190.89810 11.54238 1.10 −5.827 ± 0.096 −7.255 ± 0.091 3.16 ± 0.48 0.96<br />
NGC 4649 697 190.91684 11.57622 1.23 −7.982 ± 0.014 −9.220 ± 0.024 2.37 ± 0.15 1.00<br />
NGC 4649 698 190.91464 11.57223 1.02 −6.791 ± 0.080 −8.269 ± 0.036 1.27 ± 0.24 0.96<br />
NGC 4649 701 190.90082 11.54752 0.86 −7.950 ± 0.021 −9.593 ± 0.027 2.98 ± 0.14 1.00<br />
NGC 4649 703 190.89371 11.53487 1.51 −5.916 ± 0.105 −7.397 ± 0.048 3.62 ± 0.27 0.94<br />
NGC 4649 704 190.90351 11.55258 0.68 −6.266 ± 0.118 −7.393 ± 0.495 2.08 ± 1.33 0.99<br />
NGC 4649 706 190.91652 11.57627 1.23 −5.508 ± 0.331 −7.051 ± 0.068 2.35 ± 0.57 0.99<br />
NGC 4649 707 190.90776 11.56061 0.61 −8.014 ± 0.028 −8.897 ± 0.033 2.30 ± 0.19 1.00<br />
NGC 4649 708 190.91703 11.57739 1.29 −5.493 ± 0.234 −6.944 ± 0.065 3.16 ± 1.72 0.94<br />
NGC 4649 709 190.91308 11.57043 0.94 −8.175 ± 0.027 −9.842 ± 0.018 2.38 ± 0.17 1.00<br />
NGC 4649 711 190.91084 11.56696 0.80 −8.481 ± 0.017 −9.340 ± 0.032 3.49 ± 0.13 1.00<br />
NGC 4649 712 190.89647 11.54133 1.20 −7.934 ± 0.022 −9.397 ± 0.016 1.96 ± 0.07 1.00<br />
NGC 4649 713 190.90365 11.55425 0.67 −6.145 ± 0.069 −7.425 ± 0.072 3.32 ± 0.40 0.96<br />
NGC 4649 715 190.91508 11.57495 1.16 −5.471 ± 0.463 −6.848 ± 0.218 2.54 ± 1.15 0.98<br />
NGC 4649 716 190.90611 11.55894 0.63 −8.393 ± 0.023 −9.328 ± 0.037 3.48 ± 0.18 1.00<br />
NGC 4649 717 190.89815 11.54462 1.04 −6.930 ± 0.034 −8.400 ± 0.041 2.16 ± 0.21 1.00<br />
NGC 4649 718 190.91263 11.57079 0.97 −9.049 ± 0.011 −10.076 ± 0.016 1.76 ± 0.09 1.00<br />
NGC 4649 720 190.90655 11.55994 0.64 −6.440 ± 0.053 −7.957 ± 0.050 1.35 ± 0.31 0.97<br />
NGC 4649 721 190.91070 11.56744 0.83 −5.981 ± 0.114 −6.665 ± 0.097 1.46 ± 0.34 0.95<br />
NGC 4649 722 190.89586 11.54079 1.24 −6.526 ± 0.036 −7.930 ± 0.087 2.63 ± 0.34 1.00<br />
NGC 4649 723 190.91294 11.57160 1.00 −6.374 ± 0.088 −7.463 ± 0.123 4.24 ± 0.60 0.90<br />
NGC 4649 724 190.90332 11.55436 0.69 −7.712 ± 0.017 −8.966 ± 0.025 1.58 ± 0.18 1.00<br />
NGC 4649 725 190.91268 11.57169 1.01 −6.398 ± 0.051 −7.806 ± 0.066 3.01 ± 0.37 0.99<br />
NGC 4649 726 190.91639 11.57844 1.34 −4.802 ± 0.273 −6.318 ± 0.233 3.18 ± 1.44 0.94<br />
NGC 4649 729 190.91219 11.57135 1.00 −7.290 ± 0.851 −8.213 ± 0.728 1.70 ± 0.61 1.00<br />
NGC 4649 730 190.90550 11.55930 0.67 −6.704 ± 0.037 −7.940 ± 0.076 1.92 ± 0.31 1.00<br />
NGC 4649 731 190.90699 11.56211 0.70 −6.489 ± 0.136 −7.732 ± 0.572 1.27 ± 0.33 0.96<br />
NGC 4649 733 190.90746 11.56332 0.73 −6.351 ± 0.065 −7.824 ± 0.158 4.02 ± 0.80 0.97<br />
NGC 4649 735 190.91313 11.57376 1.11 −4.881 ± 0.302 −6.283 ± 0.327 2.78 ± 0.61 0.96<br />
Continued on Next Page. . .<br />
393
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4649 736 190.89586 11.54277 1.19 −4.751 ± 0.199 −6.391 ± 0.178 2.66 ± 0.99 0.96<br />
NGC 4649 737 190.91250 11.57275 1.07 −6.903 ± 0.039 −8.323 ± 0.037 1.93 ± 0.22 1.00<br />
NGC 4649 738 190.90597 11.56110 0.70 −6.433 ± 0.097 −7.720 ± 0.082 3.54 ± 0.48 0.97<br />
NGC 4649 739 190.91403 11.57564 1.21 −5.778 ± 0.559 −7.129 ± 0.051 1.56 ± 0.34 0.97<br />
NGC 4649 741 190.89450 11.54092 1.30 −9.424 ± 0.017 −10.394 ± 0.015 3.78 ± 0.08 1.00<br />
NGC 4649 743 190.91618 11.58002 1.43 −6.632 ± 0.041 −7.933 ± 0.070 2.15 ± 0.30 1.00<br />
NGC 4649 744 190.89691 11.54548 1.08 −7.052 ± 0.036 −8.635 ± 0.056 3.55 ± 0.28 1.00<br />
NGC 4649 745 190.90889 11.56713 0.85 −7.307 ± 0.074 −8.845 ± 0.046 4.44 ± 0.33 1.00<br />
NGC 4649 746 190.89951 11.55043 0.89 −7.514 ± 0.033 −8.773 ± 0.030 2.27 ± 0.27 1.00<br />
NGC 4649 747 190.91113 11.57146 1.02 −8.056 ± 0.029 −9.671 ± 0.021 2.56 ± 0.15 1.00<br />
NGC 4649 748 190.89574 11.54378 1.17 −7.650 ± 0.035 −8.521 ± 0.045 4.42 ± 0.15 0.99<br />
NGC 4649 749 190.90203 11.55517 0.76 −8.035 ± 0.023 −9.442 ± 0.022 1.95 ± 0.14 1.00<br />
NGC 4649 750 190.91269 11.57445 1.15 −8.796 ± 0.020 −9.825 ± 0.016 2.24 ± 0.17 1.00<br />
NGC 4649 751 190.90149 11.55435 0.78 −6.456 ± 0.032 −7.965 ± 0.071 2.74 ± 0.30 0.99<br />
NGC 4649 752 190.90645 11.56332 0.76 −7.452 ± 0.026 −8.790 ± 0.159 1.42 ± 0.26 0.98<br />
NGC 4649 753 190.90480 11.56037 0.73 −6.770 ± 0.058 −7.711 ± 0.079 2.07 ± 0.47 1.00<br />
NGC 4649 754 190.89770 11.54779 1.01 −7.731 ± 0.039 −8.703 ± 0.040 3.84 ± 0.21 1.00<br />
NGC 4649 755 190.90267 11.55674 0.75 −7.456 ± 0.037 −8.374 ± 0.044 3.42 ± 0.14 1.00<br />
NGC 4649 756 190.91608 11.58086 1.47 −6.045 ± 0.523 −7.738 ± 0.085 2.43 ± 0.96 1.00<br />
NGC 4649 757 190.89508 11.54345 1.21 −9.796 ± 0.023 −11.181 ± 0.022 2.66 ± 0.14 1.00<br />
NGC 4649 758 190.89595 11.54510 1.14 −7.735 ± 0.026 −8.731 ± 0.032 2.79 ± 0.22 1.00<br />
NGC 4649 759 190.90045 11.55312 0.83 −5.590 ± 0.714 −7.083 ± 0.058 2.33 ± 0.43 0.99<br />
NGC 4649 760 190.90465 11.56075 0.75 −6.706 ± 0.319 −7.944 ± 0.080 1.48 ± 0.34 0.98<br />
NGC 4649 761 190.89894 11.55079 0.92 −9.285 ± 0.014 −10.219 ± 0.016 2.95 ± 0.14 1.00<br />
NGC 4649 762 190.90403 11.55983 0.75 −5.936 ± 0.206 −6.819 ± 0.152 2.03 ± 0.62 0.99<br />
NGC 4649 763 190.90475 11.56144 0.76 −9.342 ± 0.012 −10.417 ± 0.016 2.87 ± 0.08 1.00<br />
NGC 4649 764 190.90593 11.56370 0.79 −5.679 ± 0.096 −7.147 ± 0.994 1.71 ± 0.41 0.98<br />
NGC 4649 765 190.91685 11.58346 1.61 −5.672 ± 0.116 −6.591 ± 0.715 4.66 ± 17.52 0.60<br />
NGC 4649 766 190.90738 11.56651 0.86 −8.381 ± 0.017 −9.528 ± 0.020 2.51 ± 0.12 1.00<br />
NGC 4649 767 190.90044 11.55417 0.84 −7.090 ± 0.030 −8.207 ± 0.320 2.93 ± 0.59 1.00<br />
NGC 4649 769 190.91529 11.58102 1.48 −8.990 ± 0.029 −9.917 ± 0.013 2.64 ± 0.19 1.00<br />
NGC 4649 770 190.91260 11.57634 1.25 −10.865 ± 0.020 −12.174 ± 0.021 3.40 ± 0.15 1.00<br />
NGC 4649 771 190.91637 11.58321 1.59 −5.394 ± 0.161 −6.581 ± 0.147 3.04 ± 1.16 0.94<br />
NGC 4649 772 190.91096 11.57400 1.15 −7.576 ± 0.048 −8.912 ± 0.035 2.52 ± 0.24 1.00<br />
NGC 4649 773 190.89507 11.54547 1.17 −5.537 ± 0.461 −6.709 ± 0.082 1.78 ± 0.37 0.98<br />
NGC 4649 774 190.89702 11.54919 1.03 −8.467 ± 0.056 −9.403 ± 0.040 4.36 ± 0.22 1.00<br />
NGC 4649 776 190.91496 11.58160 1.51 −7.769 ± 0.022 −9.071 ± 0.024 2.66 ± 0.16 1.00<br />
NGC 4649 777 190.89070 11.53809 1.54 −6.003 ± 1.344 −7.634 ± 0.050 1.41 ± 0.31 0.97<br />
NGC 4649 780 190.89830 11.55199 0.94 −5.691 ± 0.077 −7.042 ± 0.342 1.63 ± 0.43 0.97<br />
NGC 4649 781 190.90230 11.55934 0.81 −6.358 ± 0.114 −7.563 ± 0.252 4.96 ± 2.12 0.83<br />
NGC 4649 782 190.91402 11.58041 1.45 −6.195 ± 0.045 −7.149 ± 0.086 2.65 ± 0.32 0.98<br />
NGC 4649 783 190.90746 11.56884 0.97 −8.553 ± 0.020 −9.459 ± 0.027 2.28 ± 0.17 1.00<br />
NGC 4649 784 190.89854 11.55273 0.93 −5.074 ± 0.408 −6.934 ± 0.208 2.83 ± 0.99 0.97<br />
NGC 4649 785 190.89303 11.54292 1.32 −6.966 ± 0.030 −8.618 ± 0.037 3.04 ± 0.24 1.00<br />
NGC 4649 786 190.89851 11.55296 0.93 −9.807 ± 0.028 −10.810 ± 0.033 3.79 ± 0.16 1.00<br />
NGC 4649 787 190.90460 11.56382 0.85 −6.910 ± 0.046 −8.257 ± 0.042 1.99 ± 0.27 1.00<br />
NGC 4649 788 190.91455 11.58197 1.53 −8.283 ± 0.017 −9.270 ± 0.023 3.29 ± 0.14 1.00<br />
NGC 4649 789 190.88893 11.53601 1.67 −7.692 ± 0.026 −8.620 ± 0.055 3.35 ± 0.19 1.00<br />
NGC 4649 790 190.89769 11.55178 0.98 −6.616 ± 0.038 −7.818 ± 0.130 3.79 ± 0.61 0.98<br />
NGC 4649 791 190.90899 11.57226 1.09 −6.551 ± 0.057 −7.669 ± 0.047 1.48 ± 0.25 0.98<br />
NGC 4649 792 190.88911 11.53667 1.65 −7.935 ± 0.043 −8.821 ± 0.126 2.46 ± 0.42 1.00<br />
NGC 4649 793 190.90473 11.56482 0.88 −7.575 ± 0.029 −8.478 ± 0.038 2.06 ± 0.25 1.00<br />
NGC 4649 795 190.90360 11.56331 0.87 −8.351 ± 0.020 −9.920 ± 0.016 2.23 ± 0.14 1.00<br />
NGC 4649 797 190.90426 11.56493 0.90 −6.227 ± 0.082 −7.700 ± 0.120 6.23 ± 0.62 0.69<br />
NGC 4649 798 190.89700 11.55205 1.01 −9.515 ± 0.011 −10.514 ± 0.015 3.18 ± 0.11 1.00<br />
NGC 4649 799 190.90992 11.57536 1.23 −8.427 ± 0.025 −10.087 ± 0.027 2.43 ± 0.21 1.00<br />
NGC 4649 801 190.89946 11.55680 0.91 −6.810 ± 0.046 −7.412 ± 0.068 4.94 ± 0.27 0.79<br />
NGC 4649 802 190.90348 11.56404 0.90 −6.006 ± 0.209 −6.904 ± 0.110 4.43 ± 0.98 0.72<br />
NGC 4649 803 190.89679 11.55204 1.02 −7.074 ± 0.037 −8.470 ± 0.025 1.18 ± 0.22 0.95<br />
NGC 4649 806 190.90741 11.57164 1.10 −7.681 ± 0.018 −8.426 ± 0.022 2.83 ± 0.15 1.00<br />
NGC 4649 807 190.90593 11.56936 1.03 −7.102 ± 0.219 −8.628 ± 0.025 1.83 ± 0.31 1.00<br />
NGC 4649 808 190.89209 11.54464 1.33 −6.263 ± 0.045 −7.570 ± 0.051 1.83 ± 0.31 0.99<br />
Continued on Next Page. . .<br />
394
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4649 809 190.88875 11.53864 1.61 −6.655 ± 0.065 −7.553 ± 0.086 3.31 ± 0.47 0.97<br />
NGC 4649 812 190.90189 11.56244 0.91 −6.497 ± 0.057 −7.516 ± 0.045 2.00 ± 0.27 0.99<br />
NGC 4649 814 190.89523 11.55063 1.11 −7.030 ± 0.029 −8.501 ± 0.038 2.09 ± 0.23 1.00<br />
NGC 4649 815 190.90712 11.57216 1.13 −8.217 ± 0.016 −9.630 ± 0.020 2.06 ± 0.15 1.00<br />
NGC 4649 816 190.89711 11.55424 1.01 −8.090 ± 0.019 −8.979 ± 0.053 2.69 ± 0.18 1.00<br />
NGC 4649 817 190.90892 11.57547 1.25 −7.500 ± 0.031 −8.448 ± 0.033 2.82 ± 0.15 1.00<br />
NGC 4649 819 190.91303 11.58303 1.60 −7.299 ± 0.025 −8.731 ± 0.026 2.40 ± 0.12 1.00<br />
NGC 4649 821 190.91002 11.57776 1.35 −5.247 ± 0.516 −6.158 ± 0.564 1.78 ± 0.67 0.98<br />
NGC 4649 822 190.89740 11.55514 1.00 −5.554 ± 0.093 −6.899 ± 0.072 1.71 ± 0.41 0.98<br />
NGC 4649 824 190.91207 11.58170 1.53 −8.648 ± 0.018 −9.554 ± 0.014 2.27 ± 0.12 1.00<br />
NGC 4649 825 190.91159 11.58060 1.48 −5.771 ± 0.454 −6.985 ± 0.369 1.41 ± 0.53 0.95<br />
NGC 4649 827 190.88840 11.53935 1.61 −6.052 ± 0.095 −7.358 ± 0.138 4.16 ± 0.56 0.89<br />
NGC 4649 832 190.89525 11.55213 1.10 −6.341 ± 0.053 −8.003 ± 0.053 2.35 ± 0.34 1.00<br />
NGC 4649 834 190.90959 11.57830 1.39 −6.810 ± 0.040 −7.663 ± 0.055 2.67 ± 0.21 0.99<br />
NGC 4649 835 190.89632 11.55439 1.05 −5.591 ± 0.143 −7.015 ± 0.075 1.95 ± 0.46 0.99<br />
NGC 4649 837 190.90713 11.57411 1.22 −8.057 ± 0.059 −9.102 ± 0.048 4.55 ± 0.35 1.00<br />
NGC 4649 839 190.89587 11.55389 1.07 −6.949 ± 0.038 −8.015 ± 0.054 1.67 ± 0.19 0.99<br />
NGC 4649 840 190.89555 11.55382 1.09 −7.870 ± 0.022 −8.968 ± 0.030 2.14 ± 0.19 1.00<br />
NGC 4649 841 190.89543 11.55368 1.09 −7.477 ± 0.026 −9.098 ± 0.033 3.13 ± 0.19 1.00<br />
NGC 4649 842 190.89826 11.55876 1.00 −8.263 ± 0.019 −9.720 ± 0.013 1.87 ± 0.13 1.00<br />
NGC 4649 843 190.88916 11.54260 1.51 −7.659 ± 0.034 −9.417 ± 0.026 3.67 ± 0.14 1.00<br />
NGC 4649 844 190.89856 11.55955 0.99 −8.044 ± 0.024 −9.585 ± 0.018 1.56 ± 0.11 1.00<br />
NGC 4649 845 190.89265 11.54903 1.25 −7.438 ± 0.034 −8.298 ± 0.036 2.37 ± 0.20 1.00<br />
NGC 4649 846 190.90540 11.57194 1.16 −6.249 ± 1.942 −7.503 ± 0.082 1.87 ± 0.41 0.99<br />
NGC 4649 847 190.89081 11.54593 1.37 −7.597 ± 0.028 −8.560 ± 0.033 2.81 ± 0.25 1.00<br />
NGC 4649 848 190.90329 11.56867 1.08 −7.958 ± 0.020 −9.561 ± 0.018 2.05 ± 0.08 1.00<br />
NGC 4649 849 190.90067 11.56395 1.01 −6.825 ± 0.041 −7.926 ± 0.392 1.87 ± 0.34 1.00<br />
NGC 4649 850 190.88893 11.54322 1.51 −9.373 ± 0.017 −10.481 ± 0.013 3.09 ± 0.12 1.00<br />
NGC 4649 851 190.90127 11.56530 1.03 −6.192 ± 0.043 −7.681 ± 0.127 1.51 ± 0.28 0.98<br />
NGC 4649 852 190.89740 11.55848 1.03 −7.767 ± 0.022 −8.783 ± 0.041 2.20 ± 0.25 1.00<br />
NGC 4649 853 190.90475 11.57169 1.16 −7.214 ± 0.147 −8.429 ± 0.055 6.93 ± 0.98 0.71<br />
NGC 4649 858 190.90628 11.57497 1.28 −7.266 ± 0.043 −8.290 ± 0.023 2.57 ± 0.21 1.00<br />
NGC 4649 859 190.89444 11.55374 1.14 −5.442 ± 0.165 −6.822 ± 0.485 3.89 ± 6.99 0.83<br />
NGC 4649 862 190.88871 11.54365 1.51 −7.047 ± 0.055 −8.387 ± 0.043 2.88 ± 0.31 1.00<br />
NGC 4649 864 190.89262 11.55116 1.24 −8.447 ± 0.025 −9.448 ± 0.024 2.66 ± 0.13 1.00<br />
NGC 4649 865 190.89821 11.56110 1.04 −6.689 ± 0.445 −8.082 ± 0.033 1.26 ± 0.33 0.96<br />
NGC 4649 866 190.89629 11.55770 1.08 −6.410 ± 1.132 −7.985 ± 0.056 2.14 ± 0.46 1.00<br />
NGC 4649 867 190.88805 11.54313 1.55 −8.643 ± 0.020 −9.529 ± 0.018 2.35 ± 0.09 1.00<br />
NGC 4649 870 190.90587 11.57525 1.30 −6.581 ± 0.043 −7.768 ± 0.046 2.86 ± 0.26 0.99<br />
NGC 4649 871 190.89389 11.55378 1.17 −8.043 ± 0.064 −9.071 ± 0.203 7.86 ± 1.86 0.84<br />
NGC 4649 872 190.88673 11.54092 1.66 −5.776 ± 0.054 −7.135 ± 0.042 1.17 ± 0.30 0.92<br />
NGC 4649 873 190.89995 11.56478 1.06 −5.809 ± 0.339 −7.061 ± 0.431 1.76 ± 0.46 0.98<br />
NGC 4649 875 190.88890 11.54512 1.48 −8.650 ± 0.030 −9.546 ± 0.018 2.51 ± 0.13 1.00<br />
NGC 4649 876 190.90427 11.57290 1.23 −5.857 ± 0.060 −6.766 ± 0.090 2.84 ± 0.27 0.96<br />
NGC 4649 877 190.89952 11.56458 1.08 −5.538 ± 0.505 −6.675 ± 0.931 1.05 ± 0.52 0.87<br />
NGC 4649 879 190.89573 11.55751 1.10 −7.206 ± 0.027 −8.733 ± 0.022 2.24 ± 0.16 1.00<br />
NGC 4649 880 190.90039 11.56646 1.10 −7.573 ± 0.019 −9.075 ± 0.019 2.07 ± 0.14 1.00<br />
NGC 4649 882 190.90158 11.56904 1.15 −9.116 ± 0.019 −10.225 ± 0.019 2.68 ± 0.13 1.00<br />
NGC 4649 883 190.88804 11.54456 1.53 −6.385 ± 0.047 −7.430 ± 0.077 3.38 ± 0.35 0.96<br />
NGC 4649 890 190.90406 11.57448 1.31 −7.948 ± 0.021 −8.953 ± 0.031 3.05 ± 0.17 1.00<br />
NGC 4649 892 190.89341 11.55533 1.20 −5.900 ± 0.139 −6.936 ± 0.078 2.38 ± 0.65 0.99<br />
NGC 4649 894 190.88454 11.53974 1.78 −8.612 ± 0.014 −9.841 ± 0.023 2.87 ± 0.13 1.00<br />
NGC 4649 895 190.91071 11.58671 1.80 −7.174 ± 0.033 −8.484 ± 0.030 1.81 ± 0.19 1.00<br />
NGC 4649 896 190.90761 11.58124 1.56 −7.314 ± 0.037 −8.737 ± 0.027 2.71 ± 0.18 1.00<br />
NGC 4649 897 190.88989 11.54964 1.38 −5.117 ± 0.168 −6.531 ± 0.110 4.15 ± 0.71 0.72<br />
NGC 4649 899 190.89871 11.56561 1.14 −5.661 ± 0.124 −6.784 ± 0.628 1.50 ± 0.51 0.96<br />
NGC 4649 900 190.88295 11.53740 1.91 −8.248 ± 0.025 −9.462 ± 0.019 2.15 ± 0.13 1.00<br />
NGC 4649 901 190.89218 11.55393 1.26 −6.724 ± 0.037 −7.727 ± 0.025 2.27 ± 0.18 1.00<br />
NGC 4649 902 190.90584 11.57847 1.46 −4.764 ± 0.997 −6.055 ± 0.470 2.31 ± 0.60 0.98<br />
NGC 4649 905 190.90396 11.57534 1.35 −5.058 ± 0.155 −6.426 ± 1.745 2.34 ± 0.62 0.98<br />
NGC 4649 906 190.89591 11.56112 1.15 −9.443 ± 0.026 −10.823 ± 0.015 1.86 ± 0.14 1.00<br />
NGC 4649 908 190.88374 11.53922 1.83 −5.431 ± 0.886 −6.367 ± 0.184 0.86 ± 0.43 0.83<br />
Continued on Next Page. . .<br />
395
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4649 910 190.90794 11.58289 1.64 −5.533 ± 0.120 −6.421 ± 0.085 2.83 ± 0.36 0.96<br />
NGC 4649 911 190.90774 11.58261 1.63 −6.016 ± 0.100 −6.811 ± 0.077 5.12 ± 0.44 0.52<br />
NGC 4649 914 190.90340 11.57531 1.36 −7.361 ± 0.035 −8.674 ± 0.042 3.25 ± 0.17 1.00<br />
NGC 4649 917 190.88336 11.53980 1.84 −7.041 ± 0.053 −8.347 ± 0.136 4.32 ± 1.10 0.99<br />
NGC 4649 918 190.89860 11.56724 1.20 −5.052 ± 0.367 −6.472 ± 0.175 4.06 ± 0.72 0.74<br />
NGC 4649 919 190.89617 11.56302 1.18 −5.415 ± 0.703 −7.039 ± 0.401 1.08 ± 0.40 0.89<br />
NGC 4649 920 190.90037 11.57094 1.27 −8.652 ± 0.017 −9.911 ± 0.015 1.77 ± 0.12 1.00<br />
NGC 4649 926 190.89235 11.55713 1.27 −8.680 ± 0.019 −9.507 ± 0.027 2.71 ± 0.15 1.00<br />
NGC 4649 927 190.88683 11.54724 1.56 −7.229 ± 0.029 −8.351 ± 0.031 2.08 ± 0.16 1.00<br />
NGC 4649 928 190.89885 11.56910 1.25 −7.558 ± 0.037 −8.810 ± 0.022 2.41 ± 0.19 1.00<br />
NGC 4649 929 190.89460 11.56150 1.22 −8.660 ± 0.018 −9.931 ± 0.025 2.10 ± 0.15 1.00<br />
NGC 4649 930 190.89668 11.56544 1.22 −6.607 ± 0.076 −7.547 ± 0.048 2.91 ± 0.31 0.99<br />
NGC 4649 931 190.89539 11.56359 1.23 −8.753 ± 0.016 −9.718 ± 0.017 2.98 ± 0.11 1.00<br />
NGC 4649 932 190.89253 11.55833 1.27 −5.301 ± 0.175 −7.000 ± 0.263 4.56 ± 1.73 0.73<br />
NGC 4649 933 190.89682 11.56645 1.25 −7.307 ± 0.050 −8.969 ± 0.037 4.64 ± 0.18 1.00<br />
NGC 4649 935 190.88977 11.55394 1.38 −7.978 ± 0.022 −8.943 ± 0.024 2.38 ± 0.13 1.00<br />
NGC 4649 937 190.89139 11.55692 1.32 −7.604 ± 0.024 −9.245 ± 0.027 1.97 ± 0.13 1.00<br />
NGC 4649 939 190.89861 11.57040 1.31 −7.823 ± 0.018 −9.353 ± 0.018 1.76 ± 0.11 1.00<br />
NGC 4649 941 190.88658 11.54892 1.56 −9.221 ± 0.019 −10.490 ± 0.015 2.32 ± 0.09 1.00<br />
NGC 4649 943 190.89939 11.57227 1.35 −8.134 ± 0.023 −9.385 ± 0.021 1.76 ± 0.18 1.00<br />
NGC 4649 944 190.88496 11.54632 1.66 −5.269 ± 0.396 −5.948 ± 0.188 5.41 ± 2.48 0.54<br />
NGC 4649 945 190.89569 11.56526 1.26 −6.319 ± 0.068 −7.374 ± 0.099 2.76 ± 0.47 0.98<br />
NGC 4649 947 190.88800 11.55218 1.47 −5.937 ± 0.087 −6.992 ± 0.106 3.55 ± 0.58 0.91<br />
NGC 4649 948 190.88597 11.54865 1.59 −7.344 ± 0.030 −8.304 ± 0.028 2.51 ± 0.18 1.00<br />
NGC 4649 949 190.88366 11.54469 1.75 −9.366 ± 0.016 −10.892 ± 0.019 2.72 ± 0.13 1.00<br />
NGC 4649 950 190.88750 11.55151 1.50 −7.741 ± 0.080 −8.771 ± 0.042 2.21 ± 0.35 1.00<br />
NGC 4649 951 190.89856 11.57144 1.35 −7.867 ± 0.017 −8.873 ± 0.027 2.07 ± 0.12 1.00<br />
NGC 4649 952 190.89845 11.57151 1.36 −8.447 ± 0.019 −9.556 ± 0.030 1.70 ± 0.20 1.00<br />
NGC 4649 954 190.89342 11.56253 1.30 −9.215 ± 0.042 −10.149 ± 0.049 6.93 ± 0.26 1.00<br />
NGC 4649 955 190.89801 11.57086 1.35 −8.874 ± 0.015 −9.928 ± 0.011 2.39 ± 0.15 1.00<br />
NGC 4649 956 190.90643 11.58607 1.82 −6.988 ± 0.043 −8.558 ± 0.035 2.74 ± 0.24 1.00<br />
NGC 4649 958 190.89744 11.56998 1.34 −5.204 ± 0.061 −6.012 ± 0.818 1.40 ± 0.44 0.96<br />
NGC 4649 959 190.89116 11.55885 1.35 −5.752 ± 0.211 −7.291 ± 0.091 1.45 ± 0.43 0.96<br />
NGC 4649 960 190.88547 11.54860 1.62 −5.095 ± 0.158 −6.712 ± 0.048 2.36 ± 0.33 0.98<br />
NGC 4649 961 190.88506 11.54788 1.64 −6.838 ± 0.453 −7.559 ± 0.117 1.02 ± 0.29 0.90<br />
NGC 4649 962 190.88199 11.54246 1.86 −7.600 ± 0.023 −8.893 ± 0.018 1.88 ± 0.11 1.00<br />
NGC 4649 963 190.89328 11.56291 1.31 −9.095 ± 0.013 −10.105 ± 0.013 2.19 ± 0.13 1.00<br />
NGC 4649 964 190.90569 11.58529 1.79 −6.645 ± 0.056 −7.541 ± 0.051 2.95 ± 0.24 0.99<br />
NGC 4649 965 190.89377 11.56402 1.31 −6.633 ± 0.045 −7.960 ± 0.032 2.34 ± 0.29 1.00<br />
NGC 4649 966 190.89472 11.56618 1.33 −9.691 ± 0.017 −10.710 ± 0.016 3.14 ± 0.10 1.00<br />
NGC 4649 967 190.88612 11.55091 1.57 −9.056 ± 0.016 −10.138 ± 0.017 3.04 ± 0.09 1.00<br />
NGC 4649 969 190.88735 11.55373 1.51 −6.457 ± 0.041 −7.972 ± 0.055 2.00 ± 0.27 1.00<br />
NGC 4649 971 190.88287 11.54606 1.77 −6.387 ± 0.049 −7.377 ± 0.247 4.14 ± 0.37 0.90<br />
NGC 4649 973 190.89578 11.56957 1.39 −8.880 ± 0.028 −10.316 ± 0.015 2.30 ± 0.20 1.00<br />
NGC 4649 975 190.88524 11.55076 1.62 −5.315 ± 0.103 −6.904 ± 0.056 3.01 ± 0.43 0.96<br />
NGC 4649 976 190.89212 11.56343 1.38 −5.321 ± 0.237 −6.647 ± 0.516 1.86 ± 0.58 0.98<br />
NGC 4649 977 190.88402 11.55006 1.68 −7.926 ± 0.022 −8.832 ± 0.022 2.30 ± 0.12 1.00<br />
NGC 4649 978 190.89302 11.56625 1.40 −6.971 ± 0.074 −8.500 ± 0.140 6.98 ± 1.13 0.72<br />
NGC 4649 980 190.87920 11.54171 2.01 −7.719 ± 0.029 −8.709 ± 0.037 2.84 ± 0.17 1.00<br />
NGC 4649 984 190.89112 11.56425 1.44 −6.009 ± 0.069 −6.862 ± 0.105 4.07 ± 0.37 0.79<br />
NGC 4649 985 190.89290 11.56769 1.45 −5.708 ± 0.071 −7.040 ± 0.341 4.11 ± 0.61 0.82<br />
NGC 4649 989 190.87680 11.54061 2.14 −5.171 ± 0.296 −5.932 ± 0.400 4.41 ± 2.86 0.72<br />
NGC 4649 990 190.87867 11.54409 2.00 −5.210 ± 1.025 −6.484 ± 0.765 0.93 ± 0.47 0.84<br />
NGC 4649 991 190.89076 11.56610 1.50 −8.308 ± 0.015 −9.576 ± 0.017 2.30 ± 0.15 1.00<br />
NGC 4649 992 190.88483 11.55608 1.64 −7.972 ± 0.026 −8.910 ± 0.049 2.80 ± 0.44 1.00<br />
NGC 4649 993 190.89099 11.56720 1.52 −7.028 ± 0.041 −8.349 ± 0.034 2.33 ± 0.45 1.00<br />
NGC 4649 994 190.88737 11.56061 1.56 −6.901 ± 0.495 −8.300 ± 0.337 1.49 ± 0.59 0.99<br />
NGC 4649 995 190.90311 11.58926 2.03 −7.286 ± 0.080 −8.753 ± 0.034 4.60 ± 0.32 0.99<br />
NGC 4649 996 190.88398 11.55494 1.68 −6.133 ± 0.078 −6.948 ± 0.128 3.54 ± 0.59 0.90<br />
NGC 4649 997 190.88147 11.55046 1.81 −7.295 ± 0.043 −8.684 ± 0.031 2.63 ± 0.22 1.00<br />
NGC 4649 998 190.88520 11.55735 1.63 −6.920 ± 0.051 −7.556 ± 0.046 4.76 ± 0.20 0.85<br />
NGC 4649 1000 190.89070 11.56770 1.55 −6.397 ± 0.047 −7.739 ± 0.040 1.91 ± 0.21 1.00<br />
Continued on Next Page. . .<br />
396
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4649 1002 190.88938 11.56610 1.57 −7.477 ± 0.383 −8.918 ± 0.290 2.17 ± 0.43 1.00<br />
NGC 4649 1005 190.87895 11.54806 1.95 −7.282 ± 0.038 −8.451 ± 0.048 3.78 ± 0.24 1.00<br />
NGC 4649 1006 190.88244 11.55449 1.76 −6.515 ± 0.036 −8.118 ± 0.029 1.96 ± 0.19 1.00<br />
NGC 4649 1009 190.90190 11.59002 2.09 −5.469 ± 0.073 −6.309 ± 0.082 3.06 ± 0.41 0.94<br />
NGC 4649 1010 190.88258 11.55538 1.75 −6.632 ± 0.051 −7.732 ± 0.110 3.89 ± 0.51 0.97<br />
NGC 4649 1016 190.88415 11.55882 1.70 −7.109 ± 0.037 −8.411 ± 0.033 2.55 ± 0.16 1.00<br />
NGC 4649 1017 190.88908 11.56805 1.63 −7.996 ± 0.024 −8.891 ± 0.027 2.74 ± 0.16 1.00<br />
NGC 4649 1018 190.88435 11.55959 1.70 −7.417 ± 0.030 −8.786 ± 0.025 2.39 ± 0.14 1.00<br />
NGC 4649 1019 190.88270 11.55660 1.75 −6.681 ± 0.035 −7.632 ± 0.037 2.71 ± 0.20 0.99<br />
NGC 4649 1021 190.88693 11.56451 1.65 −5.669 ± 0.382 −7.099 ± 0.047 1.70 ± 0.47 0.98<br />
NGC 4649 1025 190.88576 11.56323 1.68 −7.236 ± 0.040 −9.022 ± 0.034 10.23 ± 0.27 0.62<br />
NGC 4649 1026 190.88368 11.55950 1.73 −6.303 ± 0.075 −7.846 ± 0.067 2.63 ± 0.35 0.99<br />
NGC 4649 1027 190.87964 11.55238 1.90 −7.009 ± 0.048 −8.185 ± 0.076 5.82 ± 0.45 0.83<br />
NGC 4649 1028 190.88807 11.56769 1.66 −7.521 ± 0.032 −8.431 ± 0.030 3.17 ± 0.18 1.00<br />
NGC 4649 1029 190.87401 11.54228 2.26 −6.083 ± 0.070 −7.532 ± 0.054 2.83 ± 0.25 0.99<br />
NGC 4649 1030 190.88438 11.56109 1.71 −8.268 ± 0.026 −9.608 ± 0.024 1.87 ± 0.20 1.00<br />
NGC 4649 1034 190.87935 11.55477 1.92 −4.756 ± 0.314 −6.475 ± 0.142 3.66 ± 1.32 0.87<br />
NGC 4649 1035 190.88599 11.56680 1.74 −5.218 ± 0.535 −6.103 ± 0.817 2.12 ± 2.24 0.98<br />
NGC 4649 1036 190.87532 11.54777 2.14 −9.230 ± 0.021 −10.243 ± 0.014 2.80 ± 0.12 1.00<br />
NGC 4649 1038 190.88640 11.56771 1.74 −6.641 ± 0.078 −7.745 ± 0.077 4.62 ± 0.34 0.91<br />
NGC 4649 1043 190.87198 11.54274 2.35 −5.334 ± 0.072 −6.437 ± 0.918 1.92 ± 0.40 0.98<br />
NGC 4649 1045 190.87797 11.55455 1.99 −7.257 ± 0.030 −8.793 ± 0.022 2.84 ± 0.15 1.00<br />
NGC 4649 1047 190.88385 11.56629 1.83 −5.554 ± 0.683 −6.849 ± 0.269 2.55 ± 0.58 0.98<br />
NGC 4649 1048 190.89798 11.59182 2.26 −4.921 ± 0.171 −5.945 ± 0.469 3.39 ± 0.92 0.94<br />
NGC 4649 1049 190.88305 11.56512 1.84 −6.178 ± 0.159 −7.786 ± 1.007 4.24 ± 0.80 0.95<br />
NGC 4649 1051 190.87975 11.55951 1.93 −6.345 ± 0.048 −7.892 ± 0.045 1.65 ± 0.23 0.99<br />
NGC 4649 1052 190.87393 11.54930 2.20 −6.161 ± 0.116 −8.056 ± 0.162 6.64 ± 1.01 0.69<br />
NGC 4649 1053 190.87892 11.55847 1.96 −9.078 ± 0.016 −10.329 ± 0.015 2.02 ± 0.11 1.00<br />
NGC 4649 1054 190.87547 11.55252 2.11 −6.480 ± 0.054 −7.130 ± 0.089 4.55 ± 0.36 0.77<br />
NGC 4649 1058 190.87031 11.54375 2.43 −5.824 ± 0.117 −6.729 ± 0.076 3.51 ± 0.59 0.90<br />
NGC 4649 1059 190.87903 11.55985 1.97 −8.469 ± 0.027 −9.570 ± 0.017 2.58 ± 0.17 1.00<br />
NGC 4649 1060 190.87077 11.54493 2.39 −6.365 ± 0.074 −7.825 ± 0.035 2.89 ± 0.32 0.99<br />
NGC 4649 1061 190.87053 11.54487 2.40 −6.238 ± 0.060 −7.790 ± 0.043 3.43 ± 0.27 0.98<br />
NGC 4649 1062 190.87171 11.54710 2.33 −7.288 ± 0.026 −8.645 ± 0.021 2.97 ± 0.18 1.00<br />
NGC 4649 1064 190.87944 11.56132 1.96 −8.747 ± 0.025 −9.913 ± 0.025 2.97 ± 0.23 1.00<br />
NGC 4697 2 192.11877 -5.81460 1.68 −7.221 ± 0.050 −8.587 ± 0.055 3.19 ± 0.18 1.00<br />
NGC 4697 3 192.11728 -5.81817 1.83 −6.704 ± 0.046 −7.578 ± 0.045 1.81 ± 0.08 1.00<br />
NGC 4697 4 192.12007 -5.81209 1.57 −7.807 ± 0.040 −9.099 ± 0.020 1.80 ± 0.07 1.00<br />
NGC 4697 6 192.12139 -5.80962 1.47 −6.803 ± 0.055 −7.664 ± 0.032 1.89 ± 0.09 1.00<br />
NGC 4697 11 192.12839 -5.79461 1.10 −7.197 ± 0.101 −8.294 ± 0.179 3.69 ± 0.87 0.95<br />
NGC 4697 12 192.12844 -5.79497 1.09 −6.585 ± 0.039 −8.069 ± 0.028 1.30 ± 0.09 1.00<br />
NGC 4697 18 192.13261 -5.78801 1.06 −9.840 ± 0.047 −10.729 ± 0.055 3.72 ± 0.17 1.00<br />
NGC 4697 24 192.13280 -5.79103 0.96 −8.449 ± 0.060 −9.319 ± 0.033 2.93 ± 0.13 1.00<br />
NGC 4697 26 192.12988 -5.79803 0.99 −5.777 ± 0.052 −6.911 ± 0.110 1.74 ± 0.30 0.94<br />
NGC 4697 30 192.13120 -5.79575 0.95 −7.381 ± 0.044 −8.852 ± 0.022 2.21 ± 0.08 1.00<br />
NGC 4697 31 192.12918 -5.80064 1.01 −7.637 ± 0.041 −8.732 ± 0.026 2.13 ± 0.10 1.00<br />
NGC 4697 32 192.12110 -5.81991 1.71 −8.950 ± 0.073 −10.201 ± 0.030 2.63 ± 0.16 1.00<br />
NGC 4697 34 192.13318 -5.79136 0.94 −7.872 ± 0.090 −9.084 ± 0.043 1.89 ± 0.22 1.00<br />
NGC 4697 40 192.13027 -5.79996 0.96 −8.776 ± 0.048 −9.659 ± 0.036 2.72 ± 0.14 1.00<br />
NGC 4697 42 192.13176 -5.79702 0.91 −7.272 ± 0.025 −8.189 ± 0.045 5.02 ± 0.12 0.56<br />
NGC 4697 43 192.12851 -5.80463 1.07 −5.343 ± 0.076 −6.840 ± 0.066 3.07 ± 0.22 0.64<br />
NGC 4697 45 192.12867 -5.80451 1.06 −8.219 ± 0.034 −9.410 ± 0.022 1.46 ± 0.07 1.00<br />
NGC 4697 47 192.13246 -5.79559 0.89 −7.338 ± 0.031 −8.066 ± 0.024 1.65 ± 0.06 1.00<br />
NGC 4697 48 192.13727 -5.78434 1.02 −8.085 ± 0.055 −8.826 ± 0.030 2.56 ± 0.14 1.00<br />
NGC 4697 55 192.12692 -5.81010 1.22 −6.758 ± 0.124 −7.812 ± 0.058 2.85 ± 0.37 0.95<br />
NGC 4697 58 192.12697 -5.81079 1.23 −5.296 ± 0.170 −6.267 ± 0.145 2.26 ± 0.68 0.69<br />
NGC 4697 61 192.12404 -5.81845 1.55 −5.923 ± 0.085 −6.707 ± 0.087 2.00 ± 0.18 0.90<br />
NGC 4697 63 192.13423 -5.79497 0.82 −6.680 ± 0.034 −7.935 ± 0.030 1.31 ± 0.08 1.00<br />
NGC 4697 72 192.13199 -5.80167 0.88 −4.880 ± 0.238 −6.045 ± 0.712 1.52 ± 5.22 0.67<br />
NGC 4697 73 192.13011 -5.80627 1.01 −6.674 ± 0.040 −7.752 ± 0.035 1.29 ± 0.08 1.00<br />
NGC 4697 76 192.13509 -5.79474 0.78 −6.049 ± 0.036 −7.711 ± 0.072 2.18 ± 0.19 1.00<br />
Continued on Next Page. . .<br />
397
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4697 80 192.13141 -5.80432 0.92 −6.127 ± 0.121 −7.338 ± 0.072 2.25 ± 0.30 1.00<br />
NGC 4697 81 192.14068 -5.78249 1.01 −6.585 ± 0.083 −7.795 ± 0.039 2.02 ± 0.23 1.00<br />
NGC 4697 83 192.12439 -5.82164 1.63 −8.193 ± 0.040 −9.186 ± 0.066 3.97 ± 0.23 0.94<br />
NGC 4697 84 192.12982 -5.80867 1.06 −5.562 ± 0.072 −7.251 ± 0.112 3.19 ± 0.29 0.75<br />
NGC 4697 85 192.13082 -5.80656 0.98 −7.763 ± 0.052 −9.041 ± 0.028 2.45 ± 0.13 1.00<br />
NGC 4697 88 192.12809 -5.81297 1.23 −7.841 ± 0.022 −8.711 ± 0.024 1.83 ± 0.07 1.00<br />
NGC 4697 92 192.13486 -5.79840 0.74 −6.863 ± 0.048 −7.894 ± 0.039 2.01 ± 0.12 1.00<br />
NGC 4697 94 192.13426 -5.80021 0.76 −6.219 ± 0.059 −7.611 ± 0.042 1.07 ± 0.14 1.00<br />
NGC 4697 95 192.13631 -5.79592 0.70 −6.553 ± 0.080 −7.477 ± 0.074 2.37 ± 0.20 1.00<br />
NGC 4697 96 192.12951 -5.81233 1.15 −7.775 ± 0.037 −9.246 ± 0.025 2.31 ± 0.09 1.00<br />
NGC 4697 98 192.13527 -5.79956 0.71 −8.089 ± 0.057 −8.907 ± 0.034 2.52 ± 0.12 1.00<br />
NGC 4697 99 192.14560 -5.77574 1.26 −8.204 ± 0.043 −9.242 ± 0.016 2.23 ± 0.11 1.00<br />
NGC 4697 101 192.13609 -5.79899 0.68 −6.747 ± 0.054 −8.009 ± 0.078 2.30 ± 0.21 1.00<br />
NGC 4697 103 192.14169 -5.78626 0.82 −6.695 ± 0.030 −8.055 ± 0.013 1.22 ± 0.08 1.00<br />
NGC 4697 105 192.13106 -5.81184 1.08 −7.028 ± 0.080 −7.755 ± 0.071 2.85 ± 0.23 0.94<br />
NGC 4697 107 192.13419 -5.80512 0.80 −8.114 ± 0.033 −8.794 ± 0.030 2.38 ± 0.11 1.00<br />
NGC 4697 111 192.13498 -5.80405 0.74 −9.549 ± 0.026 −10.441 ± 0.016 2.24 ± 0.07 1.00<br />
NGC 4697 112 192.12802 -5.82045 1.46 −8.322 ± 0.085 −9.270 ± 0.048 3.23 ± 0.24 1.00<br />
NGC 4697 115 192.13305 -5.80868 0.91 −8.457 ± 0.029 −9.242 ± 0.016 1.74 ± 0.05 1.00<br />
NGC 4697 116 192.14353 -5.78393 0.89 −7.440 ± 0.035 −8.601 ± 0.020 1.86 ± 0.08 1.00<br />
NGC 4697 117 192.14374 -5.78357 0.91 −7.810 ± 0.025 −8.627 ± 0.021 1.62 ± 0.07 1.00<br />
NGC 4697 121 192.14267 -5.78654 0.79 −7.494 ± 0.033 −8.905 ± 0.025 1.56 ± 0.07 1.00<br />
NGC 4697 125 192.13497 -5.80604 0.77 −5.760 ± 0.055 −6.964 ± 0.159 1.99 ± 0.41 0.95<br />
NGC 4697 130 192.13354 -5.81029 0.93 −7.517 ± 0.056 −8.922 ± 0.045 2.02 ± 0.19 1.00<br />
NGC 4697 135 192.15014 -5.77219 1.43 −7.939 ± 0.101 −9.444 ± 0.059 3.84 ± 0.34 0.96<br />
NGC 4697 139 192.13838 -5.80089 0.56 −8.361 ± 0.041 −9.815 ± 0.016 2.21 ± 0.12 1.00<br />
NGC 4697 141 192.13618 -5.80625 0.72 −7.032 ± 0.045 −7.883 ± 0.064 2.11 ± 0.11 1.00<br />
NGC 4697 142 192.13857 -5.80068 0.55 −8.499 ± 0.026 −9.823 ± 0.021 1.41 ± 0.08 1.00<br />
NGC 4697 144 192.14613 -5.78336 0.88 −7.157 ± 0.034 −8.388 ± 0.028 1.36 ± 0.10 1.00<br />
NGC 4697 149 192.14503 -5.78689 0.73 −8.223 ± 0.032 −9.526 ± 0.015 2.08 ± 0.07 1.00<br />
NGC 4697 151 192.14007 -5.79939 0.48 −8.181 ± 0.030 −9.295 ± 0.025 1.72 ± 0.06 1.00<br />
NGC 4697 154 192.14090 -5.79838 0.45 −7.213 ± 0.109 −8.371 ± 0.059 2.68 ± 0.24 1.00<br />
NGC 4697 155 192.13393 -5.81505 1.06 −8.456 ± 0.034 −9.370 ± 0.022 2.25 ± 0.07 1.00<br />
NGC 4697 157 192.14190 -5.79629 0.44 −9.090 ± 0.029 −10.477 ± 0.011 2.17 ± 0.08 1.00<br />
NGC 4697 159 192.13426 -5.81478 1.04 −4.981 ± 0.095 −5.866 ± 0.095 2.07 ± 0.21 0.56<br />
NGC 4697 160 192.13895 -5.80372 0.55 −7.376 ± 0.089 −8.770 ± 0.072 3.08 ± 0.31 1.00<br />
NGC 4697 162 192.13666 -5.80943 0.78 −8.676 ± 0.025 −9.542 ± 0.016 1.79 ± 0.07 1.00<br />
NGC 4697 163 192.13285 -5.81848 1.22 −8.984 ± 0.034 −10.088 ± 0.013 1.76 ± 0.07 1.00<br />
NGC 4697 164 192.14833 -5.78224 0.93 −7.022 ± 0.055 −8.120 ± 0.058 1.91 ± 0.12 1.00<br />
NGC 4697 165 192.13752 -5.80825 0.71 −8.315 ± 0.057 −9.651 ± 0.023 2.89 ± 0.18 1.00<br />
NGC 4697 167 192.13750 -5.80851 0.72 −6.966 ± 0.056 −8.198 ± 0.027 2.32 ± 0.10 1.00<br />
NGC 4697 168 192.14964 -5.78001 1.04 −9.590 ± 0.031 −10.424 ± 0.029 5.26 ± 0.14 1.00<br />
NGC 4697 169 192.14517 -5.79057 0.55 −8.638 ± 0.024 −9.825 ± 0.020 1.78 ± 0.06 1.00<br />
NGC 4697 170 192.14824 -5.78333 0.87 −5.685 ± 0.058 −6.831 ± 0.072 1.11 ± 0.17 0.86<br />
NGC 4697 175 192.14081 -5.80135 0.44 −6.436 ± 0.054 −7.593 ± 0.259 1.74 ± 0.15 1.00<br />
NGC 4697 176 192.14542 -5.79073 0.54 −7.370 ± 0.034 −8.753 ± 0.020 1.16 ± 0.09 1.00<br />
NGC 4697 178 192.13293 -5.82045 1.29 −6.625 ± 0.043 −7.818 ± 0.032 1.47 ± 0.12 1.00<br />
NGC 4697 179 192.14311 -5.79641 0.39 −7.609 ± 0.034 −8.564 ± 0.025 1.55 ± 0.08 1.00<br />
NGC 4697 181 192.14074 -5.80227 0.45 −6.663 ± 0.078 −7.921 ± 0.075 1.91 ± 0.18 1.00<br />
NGC 4697 182 192.13151 -5.82407 1.47 −5.387 ± 0.063 −6.866 ± 0.057 1.74 ± 0.16 0.93<br />
NGC 4697 183 192.14600 -5.79058 0.54 −7.850 ± 0.036 −8.956 ± 0.021 2.26 ± 0.09 1.00<br />
NGC 4697 186 192.13749 -5.81098 0.79 −7.026 ± 0.063 −8.391 ± 0.053 2.73 ± 0.16 1.00<br />
NGC 4697 187 192.14165 -5.80174 0.40 −7.307 ± 0.099 −7.908 ± 0.114 3.98 ± 0.49 0.80<br />
NGC 4697 188 192.14534 -5.79312 0.43 −7.330 ± 0.028 −8.241 ± 0.050 1.99 ± 0.09 1.00<br />
NGC 4697 189 192.14233 -5.80023 0.36 −4.670 ± 0.511 −6.164 ± 0.566 1.36 ± 1.75 0.70<br />
NGC 4697 191 192.14452 -5.79529 0.37 −8.490 ± 0.030 −9.353 ± 0.015 1.83 ± 0.07 1.00<br />
NGC 4697 192 192.14264 -5.79982 0.35 −7.783 ± 0.037 −9.168 ± 0.032 1.21 ± 0.14 1.00<br />
NGC 4697 193 192.14185 -5.80187 0.39 −8.461 ± 0.029 −9.327 ± 0.027 2.03 ± 0.07 1.00<br />
NGC 4697 197 192.13356 -5.82148 1.31 −7.094 ± 0.057 −8.049 ± 0.079 3.76 ± 0.27 0.88<br />
NGC 4697 199 192.13767 -5.81263 0.84 −6.061 ± 0.073 −7.490 ± 0.141 2.58 ± 0.36 1.00<br />
NGC 4697 202 192.13908 -5.81026 0.71 −6.725 ± 0.059 −7.442 ± 0.035 1.47 ± 0.14 1.00<br />
NGC 4697 203 192.14259 -5.80209 0.35 −6.294 ± 0.058 −7.803 ± 0.040 1.14 ± 0.15 1.00<br />
Continued on Next Page. . .<br />
398
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4697 205 192.15101 -5.78256 0.91 −7.807 ± 0.056 −8.693 ± 0.025 2.37 ± 0.13 1.00<br />
NGC 4697 209 192.15042 -5.78412 0.83 −8.101 ± 0.034 −8.937 ± 0.026 1.62 ± 0.09 1.00<br />
NGC 4697 211 192.14014 -5.80875 0.62 −5.108 ± 0.202 −6.372 ± 0.115 2.01 ± 0.52 0.80<br />
NGC 4697 212 192.13724 -5.81581 0.97 −7.252 ± 0.054 −8.618 ± 0.039 2.51 ± 0.12 1.00<br />
NGC 4697 213 192.15029 -5.78509 0.78 −7.228 ± 0.057 −8.111 ± 0.062 2.59 ± 0.20 1.00<br />
NGC 4697 214 192.13776 -5.81495 0.92 −7.119 ± 0.044 −8.278 ± 0.083 1.71 ± 0.28 1.00<br />
NGC 4697 216 192.15136 -5.78258 0.91 −6.419 ± 0.035 −7.785 ± 0.031 4.11 ± 0.09 0.72<br />
NGC 4697 217 192.14871 -5.78968 0.55 −9.042 ± 0.036 −10.223 ± 0.017 2.51 ± 0.12 1.00<br />
NGC 4697 220 192.14026 -5.80951 0.64 −7.209 ± 0.137 −7.994 ± 0.071 3.28 ± 0.50 0.93<br />
NGC 4697 221 192.14827 -5.79089 0.50 −9.685 ± 0.032 −10.861 ± 0.018 2.20 ± 0.08 1.00<br />
NGC 4697 222 192.15021 -5.78686 0.69 −6.756 ± 0.126 −8.372 ± 0.149 5.11 ± 0.92 0.74<br />
NGC 4697 223 192.15163 -5.78444 0.82 −10.622 ± 0.068 −11.559 ± 0.042 2.68 ± 0.13 1.00<br />
NGC 4697 224 192.14348 -5.80357 0.34 −6.441 ± 0.060 −7.701 ± 0.431 0.89 ± 0.14 0.79<br />
NGC 4697 230 192.14830 -5.79382 0.35 −8.945 ± 0.023 −9.770 ± 0.018 2.03 ± 0.04 1.00<br />
NGC 4697 231 192.14934 -5.79158 0.46 −9.360 ± 0.031 −10.520 ± 0.017 1.87 ± 0.06 1.00<br />
NGC 4697 234 192.14406 -5.80418 0.32 −7.868 ± 0.032 −9.385 ± 0.023 1.14 ± 0.09 1.00<br />
NGC 4697 236 192.14808 -5.79484 0.30 −7.190 ± 0.035 −8.533 ± 0.024 1.42 ± 0.08 1.00<br />
NGC 4697 237 192.14812 -5.79507 0.29 −6.702 ± 0.038 −7.948 ± 0.040 1.57 ± 0.09 1.00<br />
NGC 4697 238 192.15401 -5.78129 1.00 −6.277 ± 0.176 −8.005 ± 0.243 3.66 ± 1.30 0.88<br />
NGC 4697 246 192.14847 -5.79542 0.27 −6.895 ± 0.082 −8.259 ± 0.097 2.24 ± 0.25 1.00<br />
NGC 4697 247 192.14815 -5.79662 0.22 −8.029 ± 0.033 −9.054 ± 0.021 1.64 ± 0.07 1.00<br />
NGC 4697 250 192.14813 -5.79694 0.20 −7.063 ± 0.036 −8.549 ± 0.036 1.25 ± 0.08 1.00<br />
NGC 4697 252 192.15392 -5.78380 0.87 −4.581 ± 0.137 −6.043 ± 0.317 2.18 ± 1.23 0.60<br />
NGC 4697 256 192.14389 -5.80840 0.48 −8.184 ± 0.029 −9.142 ± 0.020 1.51 ± 0.08 1.00<br />
NGC 4697 258 192.14061 -5.81651 0.91 −9.047 ± 0.044 −9.893 ± 0.029 1.99 ± 0.11 1.00<br />
NGC 4697 259 192.14784 -5.79952 0.10 −7.618 ± 0.057 −8.776 ± 0.027 1.51 ± 0.11 1.00<br />
NGC 4697 260 192.15397 -5.78486 0.82 −4.262 ± 0.532 −6.119 ± 0.250 1.58 ± 0.69 0.70<br />
NGC 4697 261 192.15225 -5.79033 0.54 −7.889 ± 0.046 −9.113 ± 0.036 1.56 ± 0.12 1.00<br />
NGC 4697 264 192.14902 -5.79879 0.10 −6.016 ± 0.128 −7.248 ± 0.744 0.99 ± 0.18 0.87<br />
NGC 4697 266 192.15023 -5.79577 0.25 −8.685 ± 0.048 −9.770 ± 0.041 2.08 ± 0.10 1.00<br />
NGC 4697 269 192.15085 -5.79499 0.29 −5.777 ± 0.155 −6.674 ± 0.121 2.18 ± 0.37 0.88<br />
NGC 4697 271 192.15082 -5.79541 0.27 −8.475 ± 0.050 −9.806 ± 0.024 1.90 ± 0.12 1.00<br />
NGC 4697 275 192.15315 -5.79008 0.56 −7.137 ± 0.133 −8.250 ± 0.040 3.12 ± 0.40 0.98<br />
NGC 4697 278 192.14566 -5.80861 0.44 −7.984 ± 0.026 −9.380 ± 0.024 1.60 ± 0.09 1.00<br />
NGC 4697 287 192.14662 -5.80744 0.37 −6.632 ± 0.075 −8.104 ± 0.249 2.08 ± 0.28 1.00<br />
NGC 4697 290 192.15762 -5.78229 1.01 −8.087 ± 0.043 −9.449 ± 0.030 1.78 ± 0.11 1.00<br />
NGC 4697 293 192.15496 -5.78869 0.66 −7.915 ± 0.031 −8.781 ± 0.025 1.69 ± 0.07 1.00<br />
NGC 4697 295 192.15302 -5.79419 0.37 −6.390 ± 0.081 −7.955 ± 0.051 3.16 ± 0.17 0.94<br />
NGC 4697 296 192.15550 -5.78829 0.69 −4.113 ± 0.444 −5.692 ± 0.320 1.93 ± 1.23 0.54<br />
NGC 4697 300 192.15294 -5.79464 0.35 −6.831 ± 0.039 −8.250 ± 0.033 1.28 ± 0.11 1.00<br />
NGC 4697 302 192.14920 -5.80373 0.15 −7.209 ± 0.147 −7.911 ± 0.128 2.91 ± 0.46 0.96<br />
NGC 4697 306 192.14681 -5.80998 0.48 −7.035 ± 0.059 −7.724 ± 0.063 1.75 ± 0.14 1.00<br />
NGC 4697 308 192.15726 -5.78639 0.81 −8.594 ± 0.031 −9.872 ± 0.015 1.65 ± 0.07 1.00<br />
NGC 4697 310 192.14866 -5.79793 0.15 −9.030 ± 0.061 −9.914 ± 0.032 2.39 ± 0.15 1.00<br />
NGC 4697 313 192.15253 -5.79850 0.18 −8.022 ± 0.049 −9.475 ± 0.028 2.00 ± 0.09 1.00<br />
NGC 4697 318 192.14846 -5.80891 0.41 −6.477 ± 0.045 −8.284 ± 0.168 5.03 ± 1.38 0.64<br />
NGC 4697 319 192.16183 -5.77745 1.31 −7.584 ± 0.067 −8.361 ± 0.056 2.26 ± 0.22 1.00<br />
NGC 4697 320 192.14632 -5.81443 0.71 −7.527 ± 0.063 −8.376 ± 0.043 2.88 ± 0.20 0.99<br />
NGC 4697 322 192.15283 -5.79914 0.18 −8.159 ± 0.036 −9.522 ± 0.021 1.31 ± 0.09 1.00<br />
NGC 4697 323 192.15295 -5.79889 0.19 −8.193 ± 0.033 −9.690 ± 0.022 1.39 ± 0.07 1.00<br />
NGC 4697 330 192.15526 -5.78250 0.95 −8.531 ± 0.039 −9.755 ± 0.019 2.07 ± 0.08 1.00<br />
NGC 4697 331 192.15688 -5.79109 0.60 −8.784 ± 0.056 −9.732 ± 0.043 2.63 ± 0.16 1.00<br />
NGC 4697 333 192.15180 -5.80331 0.17 −6.039 ± 0.112 −7.243 ± 0.075 1.22 ± 0.30 0.94<br />
NGC 4697 335 192.15502 -5.79594 0.36 −8.592 ± 0.060 −10.080 ± 0.019 2.45 ± 0.14 1.00<br />
NGC 4697 338 192.15518 -5.79581 0.37 −6.499 ± 0.088 −7.382 ± 0.127 2.38 ± 0.26 1.00<br />
NGC 4697 343 192.15589 -5.79509 0.42 −7.363 ± 0.065 −8.718 ± 0.085 3.09 ± 0.30 1.00<br />
NGC 4697 344 192.15486 -5.79754 0.31 −7.570 ± 0.056 −8.666 ± 0.059 2.58 ± 0.15 1.00<br />
NGC 4697 346 192.15184 -5.80468 0.23 −5.571 ± 0.085 −6.984 ± 0.101 2.47 ± 0.20 0.90<br />
NGC 4697 347 192.15329 -5.80154 0.19 −8.838 ± 0.052 −10.171 ± 0.018 1.91 ± 0.08 1.00<br />
NGC 4697 349 192.15382 -5.80063 0.21 −8.442 ± 0.050 −9.396 ± 0.021 1.57 ± 0.08 1.00<br />
NGC 4697 351 192.15201 -5.80526 0.26 −6.420 ± 0.291 −7.930 ± 0.079 3.61 ± 1.38 0.86<br />
NGC 4697 357 192.15417 -5.80053 0.23 −7.024 ± 0.038 −7.896 ± 0.218 1.69 ± 0.16 1.00<br />
Continued on Next Page. . .<br />
399
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4697 360 192.16045 -5.78589 0.92 −7.434 ± 0.069 −8.904 ± 0.051 2.88 ± 0.17 1.00<br />
NGC 4697 366 192.16254 -5.78176 1.15 −4.827 ± 0.186 −6.657 ± 0.316 2.66 ± 1.59 0.75<br />
NGC 4697 367 192.15253 -5.80562 0.29 −9.401 ± 0.029 −10.337 ± 0.015 2.93 ± 0.05 1.00<br />
NGC 4697 368 192.14955 -5.81321 0.63 −7.920 ± 0.031 −9.071 ± 0.016 1.23 ± 0.08 1.00<br />
NGC 4697 369 192.15114 -5.80952 0.45 −7.099 ± 0.036 −8.190 ± 0.026 1.56 ± 0.10 1.00<br />
NGC 4697 374 192.15674 -5.79702 0.40 −8.517 ± 0.037 −9.650 ± 0.016 1.86 ± 0.08 1.00<br />
NGC 4697 375 192.15883 -5.79049 0.69 −7.047 ± 0.060 −7.811 ± 0.070 2.31 ± 0.17 1.00<br />
NGC 4697 377 192.15490 -5.80160 0.27 −8.123 ± 0.071 −8.984 ± 0.057 2.51 ± 0.17 1.00<br />
NGC 4697 379 192.15988 -5.78971 0.75 −6.021 ± 0.066 −6.694 ± 0.518 0.96 ± 0.19 0.70<br />
NGC 4697 381 192.15446 -5.80333 0.28 −7.975 ± 0.028 −9.250 ± 0.020 1.47 ± 0.09 1.00<br />
NGC 4697 382 192.15924 -5.79217 0.64 −7.993 ± 0.041 −9.306 ± 0.013 1.57 ± 0.09 1.00<br />
NGC 4697 384 192.15709 -5.79786 0.40 −7.422 ± 0.123 −8.347 ± 0.065 2.81 ± 0.25 1.00<br />
NGC 4697 388 192.14712 -5.82221 1.08 −4.234 ± 0.241 −5.623 ± 1.442 1.73 ± 0.67 0.55<br />
NGC 4697 391 192.15447 -5.80555 0.34 −7.369 ± 0.038 −8.742 ± 0.031 1.56 ± 0.11 1.00<br />
NGC 4697 396 192.15694 -5.80038 0.37 −6.461 ± 0.093 −7.994 ± 0.062 2.20 ± 0.19 1.00<br />
NGC 4697 398 192.14763 -5.82299 1.12 −8.572 ± 0.075 −9.634 ± 0.040 3.28 ± 0.18 1.00<br />
NGC 4697 400 192.14903 -5.81986 0.96 −7.878 ± 0.023 −9.116 ± 0.019 1.21 ± 0.06 1.00<br />
NGC 4697 403 192.15082 -5.81632 0.78 −5.713 ± 0.155 −7.122 ± 0.097 2.56 ± 0.47 0.92<br />
NGC 4697 404 192.15965 -5.79539 0.57 −4.907 ± 0.286 −6.094 ± 0.547 1.05 ± 0.58 0.55<br />
NGC 4697 405 192.15306 -5.81130 0.56 −7.750 ± 0.027 −9.036 ± 0.018 1.43 ± 0.05 1.00<br />
NGC 4697 406 192.15882 -5.79771 0.48 −6.817 ± 0.219 −8.057 ± 0.111 3.08 ± 0.83 0.96<br />
NGC 4697 408 192.15146 -5.81566 0.75 −8.503 ± 0.020 −9.512 ± 0.015 1.70 ± 0.04 1.00<br />
NGC 4697 411 192.14960 -5.82092 1.01 −6.746 ± 0.048 −8.279 ± 0.039 5.41 ± 0.20 0.66<br />
NGC 4697 416 192.15918 -5.79928 0.48 −7.948 ± 0.031 −8.891 ± 0.034 1.68 ± 0.10 1.00<br />
NGC 4697 417 192.15076 -5.81919 0.93 −6.496 ± 0.124 −7.426 ± 0.127 3.09 ± 0.50 0.84<br />
NGC 4697 418 192.14647 -5.82976 1.46 −6.943 ± 0.053 −8.359 ± 0.035 1.64 ± 0.14 1.00<br />
NGC 4697 420 192.15740 -5.80404 0.42 −6.810 ± 0.056 −8.284 ± 0.063 1.81 ± 0.17 1.00<br />
NGC 4697 425 192.15581 -5.80878 0.51 −6.310 ± 0.034 −7.507 ± 0.035 1.09 ± 0.12 1.00<br />
NGC 4697 428 192.16389 -5.79027 0.88 −8.070 ± 0.059 −9.119 ± 0.028 2.76 ± 0.14 1.00<br />
NGC 4697 429 192.16368 -5.79091 0.86 −8.138 ± 0.036 −9.289 ± 0.028 2.29 ± 0.11 1.00<br />
NGC 4697 430 192.16108 -5.79735 0.60 −8.880 ± 0.047 −10.378 ± 0.568 1.83 ± 0.41 1.00<br />
NGC 4697 433 192.16204 -5.79556 0.67 −8.451 ± 0.035 −9.651 ± 0.018 1.87 ± 0.08 1.00<br />
NGC 4697 437 192.14931 -5.82639 1.28 −6.924 ± 0.048 −7.836 ± 0.042 2.02 ± 0.13 1.00<br />
NGC 4697 440 192.14795 -5.83010 1.47 −7.414 ± 0.051 −8.309 ± 0.032 2.26 ± 0.10 1.00<br />
NGC 4697 441 192.15431 -5.81506 0.76 −7.567 ± 0.023 −8.581 ± 0.020 1.75 ± 0.06 1.00<br />
NGC 4697 442 192.15653 -5.80976 0.57 −7.046 ± 0.037 −7.866 ± 0.029 1.46 ± 0.10 1.00<br />
NGC 4697 445 192.16687 -5.78638 1.12 −7.965 ± 0.130 −8.943 ± 0.104 3.72 ± 0.58 0.97<br />
NGC 4697 446 192.16018 -5.80219 0.53 −7.732 ± 0.073 −8.585 ± 0.082 4.27 ± 0.33 0.89<br />
NGC 4697 447 192.16225 -5.79734 0.65 −7.771 ± 0.022 −9.215 ± 0.022 1.26 ± 0.06 1.00<br />
NGC 4697 450 192.16863 -5.78276 1.31 −7.702 ± 0.052 −8.910 ± 0.033 1.67 ± 0.13 1.00<br />
NGC 4697 451 192.16509 -5.79142 0.90 −7.524 ± 0.039 −8.230 ± 0.032 1.89 ± 0.08 1.00<br />
NGC 4697 452 192.15791 -5.80837 0.57 −6.336 ± 0.143 −7.578 ± 0.107 2.87 ± 0.46 0.92<br />
NGC 4697 459 192.16936 -5.78334 1.31 −9.876 ± 0.072 −10.727 ± 0.036 3.25 ± 0.22 1.00<br />
NGC 4697 464 192.15876 -5.80977 0.64 −6.285 ± 0.131 −7.426 ± 0.124 3.16 ± 0.42 0.82<br />
NGC 4697 465 192.15654 -5.81510 0.80 −6.342 ± 0.086 −7.082 ± 0.110 2.30 ± 0.29 0.94<br />
NGC 4697 468 192.15529 -5.81879 0.95 −6.589 ± 0.075 −7.833 ± 0.095 3.75 ± 0.44 0.81<br />
NGC 4697 469 192.16178 -5.80353 0.62 −8.354 ± 0.046 −9.271 ± 0.052 2.77 ± 0.17 1.00<br />
NGC 4697 472 192.15038 -5.83074 1.50 −7.278 ± 0.071 −8.086 ± 0.050 2.73 ± 0.15 1.00<br />
NGC 4697 477 192.15433 -5.82188 1.09 −6.411 ± 0.045 −7.823 ± 0.062 2.46 ± 0.13 1.00<br />
NGC 4697 478 192.17079 -5.78312 1.38 −7.504 ± 0.040 −8.720 ± 0.016 1.78 ± 0.07 1.00<br />
NGC 4697 479 192.16252 -5.80308 0.66 −7.711 ± 0.052 −8.741 ± 0.051 2.87 ± 0.20 1.00<br />
NGC 4697 481 192.15985 -5.80967 0.68 −6.502 ± 0.059 −7.540 ± 0.057 1.69 ± 0.19 1.00<br />
NGC 4697 484 192.15987 -5.81042 0.71 −7.226 ± 0.027 −8.380 ± 0.030 1.45 ± 0.08 1.00<br />
NGC 4697 488 192.16291 -5.80422 0.69 −7.524 ± 0.034 −8.475 ± 0.034 1.82 ± 0.08 1.00<br />
NGC 4697 494 192.16243 -5.80624 0.70 −6.213 ± 0.054 −7.050 ± 0.479 0.89 ± 0.33 0.71<br />
NGC 4697 495 192.15491 -5.82396 1.19 −4.465 ± 0.245 −6.063 ± 0.247 1.69 ± 0.57 0.69<br />
NGC 4697 497 192.17233 -5.78321 1.43 −4.638 ± 0.335 −5.939 ± 0.182 2.08 ± 0.73 0.59<br />
NGC 4697 498 192.16682 -5.79643 0.89 −6.965 ± 0.061 −7.646 ± 0.085 2.38 ± 0.23 1.00<br />
NGC 4697 500 192.15391 -5.82766 1.37 −4.540 ± 0.247 −6.315 ± 0.122 2.33 ± 0.66 0.69<br />
NGC 4697 503 192.16807 -5.79469 0.97 −7.385 ± 0.049 −8.833 ± 0.019 1.35 ± 0.10 1.00<br />
NGC 4697 504 192.15292 -5.83076 1.51 −7.853 ± 0.049 −9.033 ± 0.035 5.14 ± 0.20 0.99<br />
NGC 4697 505 192.17194 -5.78612 1.33 −8.688 ± 0.056 −10.035 ± 0.023 2.62 ± 0.14 1.00<br />
Continued on Next Page. . .<br />
400
Table B.2—Continued<br />
RA Dec. d GC G475 Z850 r h<br />
Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class<br />
(1) (2) (3) (4) (5) (6) (7) (8) (9)<br />
NGC 4697 506 192.16337 -5.80626 0.74 −6.093 ± 0.071 −7.510 ± 0.085 3.01 ± 0.19 0.88<br />
NGC 4697 510 192.16011 -5.81438 0.86 −6.486 ± 0.070 −7.380 ± 0.094 2.82 ± 0.22 1.00<br />
NGC 4697 512 192.16577 -5.80118 0.81 −7.369 ± 0.058 −8.054 ± 0.029 1.90 ± 0.13 1.00<br />
NGC 4697 514 192.16628 -5.80021 0.83 −9.055 ± 0.054 −9.828 ± 0.074 2.33 ± 0.27 1.00<br />
NGC 4697 515 192.16571 -5.80170 0.81 −7.119 ± 0.099 −8.456 ± 0.167 1.14 ± 0.21 1.00<br />
NGC 4697 516 192.16071 -5.81367 0.85 −7.503 ± 0.073 −8.718 ± 0.041 2.67 ± 0.17 1.00<br />
NGC 4697 526 192.16428 -5.80864 0.83 −7.430 ± 0.024 −8.749 ± 0.023 1.46 ± 0.08 1.00<br />
NGC 4697 527 192.16973 -5.79622 1.03 −7.021 ± 0.106 −7.900 ± 0.132 4.41 ± 0.56 0.70<br />
NGC 4697 529 192.17276 -5.78983 1.28 −7.834 ± 0.020 −9.251 ± 0.020 1.77 ± 0.08 1.00<br />
NGC 4697 531 192.16782 -5.80149 0.91 −6.308 ± 0.046 −7.693 ± 0.037 1.10 ± 0.12 1.00<br />
NGC 4697 539 192.16687 -5.80588 0.90 −8.140 ± 0.035 −8.942 ± 0.029 2.25 ± 0.10 1.00<br />
NGC 4697 541 192.16532 -5.81053 0.93 −6.544 ± 0.055 −7.702 ± 0.096 2.95 ± 0.31 0.92<br />
NGC 4697 549 192.15722 -5.83060 1.54 −8.441 ± 0.036 −9.359 ± 0.088 3.31 ± 0.26 1.00<br />
NGC 4697 551 192.17339 -5.79255 1.25 −6.033 ± 0.045 −7.063 ± 0.065 1.45 ± 0.21 0.94<br />
NGC 4697 552 192.17155 -5.79712 1.11 −5.253 ± 0.612 −5.814 ± 0.135 1.67 ± 0.36 0.60<br />
NGC 4697 557 192.17257 -5.79619 1.17 −5.994 ± 0.066 −7.514 ± 0.115 3.59 ± 0.35 0.69<br />
NGC 4697 558 192.16794 -5.80756 0.98 −7.420 ± 0.032 −8.625 ± 0.024 1.84 ± 0.10 1.00<br />
NGC 4697 563 192.16995 -5.80368 1.03 −8.327 ± 0.030 −9.217 ± 0.034 2.52 ± 0.12 1.00<br />
NGC 4697 564 192.16388 -5.81812 1.13 −7.147 ± 0.063 −7.875 ± 0.045 2.43 ± 0.15 1.00<br />
NGC 4697 567 192.17151 -5.80065 1.09 −9.020 ± 0.031 −9.891 ± 0.023 1.99 ± 0.08 1.00<br />
NGC 4697 568 192.17226 -5.79945 1.13 −8.516 ± 0.022 −9.965 ± 0.018 1.66 ± 0.06 1.00<br />
NGC 4697 569 192.16266 -5.82262 1.28 −7.963 ± 0.019 −9.281 ± 0.021 1.83 ± 0.07 1.00<br />
NGC 4697 571 192.17305 -5.79812 1.18 −8.590 ± 0.021 −9.461 ± 0.013 1.76 ± 0.05 1.00<br />
NGC 4697 572 192.17866 -5.78555 1.63 −9.420 ± 0.044 −10.780 ± 0.018 2.64 ± 0.13 1.00<br />
NGC 4697 574 192.16148 -5.82614 1.40 −5.126 ± 0.119 −6.024 ± 0.169 2.12 ± 0.47 0.61<br />
NGC 4697 575 192.15915 -5.83214 1.64 −6.843 ± 0.145 −7.573 ± 0.076 3.57 ± 0.44 0.73<br />
NGC 4697 595 192.16983 -5.81026 1.12 −6.423 ± 0.028 −7.718 ± 0.027 1.39 ± 0.06 1.00<br />
NGC 4697 596 192.17458 -5.79949 1.25 −5.806 ± 0.072 −6.893 ± 0.316 1.49 ± 0.21 0.93<br />
NGC 4697 597 192.15995 -5.83458 1.77 −4.944 ± 0.106 −6.323 ± 0.099 1.68 ± 0.29 0.78<br />
NGC 4697 598 192.17966 -5.78809 1.63 −6.492 ± 0.053 −7.872 ± 0.041 1.89 ± 0.12 1.00<br />
NGC 4697 599 192.16475 -5.82359 1.37 −6.921 ± 0.064 −8.423 ± 0.072 2.68 ± 0.21 1.00<br />
NGC 4697 600 192.17128 -5.80848 1.15 −7.196 ± 0.126 −7.884 ± 0.079 3.05 ± 0.33 0.94<br />
NGC 4697 603 192.16715 -5.81869 1.25 −6.686 ± 0.065 −7.713 ± 0.058 2.51 ± 0.17 1.00<br />
NGC 4697 608 192.17368 -5.80423 1.21 −7.768 ± 0.045 −8.947 ± 0.046 1.71 ± 0.15 1.00<br />
NGC 4697 609 192.16816 -5.81748 1.25 −6.541 ± 0.055 −7.089 ± 0.091 2.20 ± 0.17 0.95<br />
NGC 4697 613 192.16649 -5.82205 1.36 −8.045 ± 0.016 −9.233 ± 0.017 1.59 ± 0.05 1.00<br />
NGC 4697 616 192.17655 -5.79927 1.34 −5.306 ± 0.147 −6.476 ± 0.145 2.32 ± 0.50 0.78<br />
NGC 4697 617 192.17866 -5.79542 1.47 −6.641 ± 0.054 −7.589 ± 0.054 1.48 ± 0.13 1.00<br />
NGC 4697 618 192.16764 -5.82253 1.41 −6.597 ± 0.056 −7.370 ± 0.042 1.99 ± 0.13 1.00<br />
NGC 4697 626 192.17323 -5.81140 1.29 −6.353 ± 0.069 −7.464 ± 0.040 1.71 ± 0.12 1.00<br />
NGC 4697 629 192.18195 -5.79183 1.67 −7.859 ± 0.054 −8.777 ± 0.072 3.29 ± 0.19 1.00<br />
NGC 4697 636 192.18181 -5.79340 1.65 −7.817 ± 0.023 −8.839 ± 0.012 1.45 ± 0.06 1.00<br />
NGC 4697 644 192.17096 -5.82099 1.47 −8.329 ± 0.052 −9.245 ± 0.068 3.51 ± 0.20 0.99<br />
NGC 4697 654 192.16797 -5.83569 1.98 −8.263 ± 0.024 −8.970 ± 0.016 1.86 ± 0.06 1.00<br />
NGC 4697 664 192.16868 -5.83546 1.98 −7.004 ± 0.037 −8.190 ± 0.032 2.20 ± 0.07 1.00<br />
NGC 4697 672 192.17954 -5.81127 1.58 −8.052 ± 0.046 −9.383 ± 0.019 2.14 ± 0.12 1.00<br />
NGC 4697 685 192.18672 -5.79774 1.85 −5.071 ± 0.061 −6.212 ± 0.149 2.50 ± 0.41 0.55<br />
NGC 4697 698 192.17747 -5.82310 1.78 −7.038 ± 0.072 −7.943 ± 0.030 2.23 ± 0.16 1.00<br />
NGC 4697 700 192.18106 -5.81482 1.72 −6.427 ± 0.055 −7.608 ± 0.056 2.58 ± 0.16 1.00<br />
NGC 4697 702 192.18829 -5.79880 1.93 −8.727 ± 0.067 −9.639 ± 0.030 2.69 ± 0.16 1.00<br />
401
Appendix C<br />
Optimal Preparation <strong>of</strong> Bovine<br />
Diaphragm for Human<br />
Consumption<br />
C.1 Introduction<br />
There are many resources required to support proper astronomical inquiry; how-<br />
ever, discussion <strong>of</strong> such resources in the literature is limited. Heavy (and healthy)<br />
competition for some <strong>of</strong> these resources, e.g., telescope access, computing facilities,<br />
and research funding, suggest that the astronomical community understands the im-<br />
portance <strong>of</strong> these resources; such resources are unlikely to require further exposition.<br />
On the other hand, there are several resources that may be less universally recognized.<br />
These resources, for instance astronomer felicity, lack qualitative, let alone quanti-<br />
tative investigation. One might expect that astronomers who live satisfying lives<br />
outside <strong>of</strong> their workplace environment might be more productive the other 22 hours<br />
they spend at work. To that end, we have attempted one <strong>of</strong> the first quantitative<br />
402
investigations into improving the happiness level <strong>of</strong> astronomers and measuring its<br />
effect <strong>of</strong> productivity. Due to some restrictions on human-based research, we have had<br />
to limit our experiment sample to those directly involved in this research program,<br />
namely the <strong>University</strong> <strong>of</strong> <strong>Virginia</strong> <strong>Department</strong> <strong>of</strong> <strong>Astronomy</strong>.<br />
While there are many ongoing experiments, for instance “The Effect <strong>of</strong> Intramural<br />
Sports on Astronomical Productivity,” (Bary et al. in preparation) and “Science<br />
Fiction Dramas and the Astronomical Psyche: Battlestar Galactica,” (Wik et al. in<br />
preparation), this appendix concentrates on the astronomical pastime that uses direct<br />
heat methods for converting organic material into energy supplies (hereafter, grilling).<br />
C.2 Technique<br />
We have begun studies <strong>of</strong> this activity, which peaks in the summertime, by explor-<br />
ing the optimal preparation <strong>of</strong> bovine diaphragm (hereafter, skirt steak) for human<br />
consumption. We have employed a simple, but powerful metric to determine the effect<br />
<strong>of</strong> skirt steak on astronomer felicity; the rate <strong>of</strong> skirt steak consumption multiplied<br />
by the fraction <strong>of</strong> grill attendees who compliment the chef (on the skirt steak) R×fA.<br />
As bovines use their diaphragm continuously, skirt steak is characterized by stri-<br />
ated musculature. The marbling <strong>of</strong> fat in skirt steak make up for this complication<br />
to the enjoyment <strong>of</strong> this bovine product. Thus, it appeared obvious that addressing<br />
the stringiness <strong>of</strong> skirt steak might be the most pr<strong>of</strong>itable avenue for increasing as-<br />
tronomer felicity upon consumption. Our control experiment involved putting a plain<br />
skirt steak on the grill for about 240 s per side. The results were somewhat disap-<br />
pointing, R = 0.25 g s −1 and fA = 0. While proper cutting techniques (perpendicular<br />
to the grain) were found to mitigate stringiness (R = 0.38 g s −1 and fA = 0), it was<br />
clear that something had to be done to also address taste issues. A soy sauce mari-<br />
403
nade was a clear choice as this would simultaneously address stringiness and taste.<br />
A plain soy sauce marinade for 2700 s led to the first non-zero R × fA (R = 0.38 g s −1<br />
and fA = 0.25). Increased marinade times up to ∼ 4 × 10 4 s led to increases in<br />
both R and fA. As soy sauce can be overpowering, steps were taken to reduce the<br />
sodium level; the use <strong>of</strong> reduced sodium soy sauce and a one-to-one dilution with H2O<br />
(R = 0.5 g s −1 and fA = 0.55). After much experimentation, the addition <strong>of</strong> ginger<br />
and garlic were found to balance the sodium content (R = 1.0 g s −1 and fA = 0.95).<br />
Although there appears to be clear room for improvement in the rate, we note that<br />
the prevalence <strong>of</strong> vegetarians will limit fA 1 We encourage other scientists to duplicate<br />
and extend these experiments; however, for convenience we list the final recipe at the<br />
end <strong>of</strong> the appendix (we have converted the names and units into those more typical<br />
<strong>of</strong> the grill environment).<br />
C.3 Conclusions<br />
While we summarized the results measuring astronomer felicity above, we feel it<br />
is important to correlate those results with astronomer productivity. We chose to<br />
use number <strong>of</strong> doctoral dissertations completed by the chef to measure astronomer<br />
productivity. No doctoral dissertations were completed by the chef when R × fA <br />
0.9 g s −1 . On the other hand, the number <strong>of</strong> dissertations completed when R × fA <br />
0.9 g s −1 jumped infinitely to one. We believe this is suggestive, although not con-<br />
clusive pro<strong>of</strong> that optimal preparation <strong>of</strong> bovine diaphragm leads to happier, more<br />
productive astronomers. Clearly, more work needs to be done to verify this result.<br />
Bon appetit!<br />
1 While in press, we found that the addition <strong>of</strong> smoke chips to the grill yields fa = 0.97<br />
404
C.4 Sivak<strong>of</strong>f Signature Soy Sauce Skirt Steak<br />
• Ingredients<br />
– 1 Skirt Steak (∼ 2 lb)<br />
– 1 Cup Water<br />
– 1 Cup Reduced Sodium Soy Sauce<br />
– ∼ 1 tbs Ginger Powder<br />
– ∼ 1 tbs Garlic Powder<br />
• Directions<br />
1. Place minimally cut steak so it will lie flat in a dish.<br />
2. Mix other ingredients together.<br />
3. Adjust powdered ingredients to taste.<br />
4. Poor marinade over steak.<br />
5. Cover with plastic wrap.<br />
6. Put in refrigerator for 24–48 hours (substandard, but still edible, results<br />
are possible with less marinade time).<br />
7. Get a grill very hot (substandard, but still edible, results are possible on<br />
gas grills. Note that smoke chips enhance results.)<br />
8. Cook steak for about 3–4 minutes on one side.<br />
9. Flip steak and cook for another 3–4 minutes.<br />
10. Let sit for ∼ 5 minutes (this requires extreme patience).<br />
11. Cut steak in slices perpendicular to grain<br />
(thin slices atop potato bread rolls are an excellent serving choice).<br />
405
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