Extragalactic abstracts - IRSA - California Institute of Technology
Extragalactic abstracts - IRSA - California Institute of Technology
Extragalactic abstracts - IRSA - California Institute of Technology
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Spitzer_Approved_<strong>Extragalactic</strong><br />
Mar 25, 10 16:24 Page 397/742<br />
Spitzer Space Telescope − General Observer Proposal #30603<br />
Probing the Distribution <strong>of</strong> Star Formation and Dust in a Unique, Transforming<br />
Spiral Galaxy<br />
Principal Investigator: Todd Tripp<br />
Institution: University <strong>of</strong> Massachusetts<br />
Technical Contact: Todd Tripp, University <strong>of</strong> Massachusetts<br />
Co−Investigators:<br />
Limin Song, University <strong>of</strong> Massachusetts<br />
Min Yun, University <strong>of</strong> Massachusetts<br />
David Bowen, Princeton University<br />
Science Category: interacting/merging galaxies<br />
Observing Modes: IracMap MipsPhot<br />
Hours Approved: 2.7<br />
Abstract:<br />
We have identified a spiral galaxy (NGC4319) that appears to be in the process<br />
<strong>of</strong> transforming into an S0 galaxy. This spiral is embedded in X−ray emitting hot<br />
gas in the NGC4291 group, and it appears that ram pressure has stripped most <strong>of</strong><br />
the H~I out <strong>of</strong> the galaxy making it H~I deficient and molecule−rich. Using a<br />
background Seyfert galaxy behind NGC4319, we have detected an array <strong>of</strong><br />
ultraviolet absorption lines from the ISM <strong>of</strong> NGC4319 using high−resolution<br />
spectrographs on HST and FUSE. We find that the H~I column density is<br />
surprisingly low, but nevertheless we detect 17 absorption lines <strong>of</strong> H_2 from the<br />
J = 0, 1, 2, and 3 rotational levels. We have also observed the galaxy with the<br />
FCRAO 14m telescope, and we detect CO emission from the barred center. Here we<br />
propose to map NGC4319 and 3 nearby companion galaxies (in the same group) with<br />
IRAC and MIPS to investigate the following questions: (1) How does ram pressure<br />
and tidal stripping affect star formation in NGC4319? (2) Is there hidden spiral<br />
structure in the 3 companion S0 and elliptical galaxies (e.g., as observed by<br />
Pahre et al. in other lenticulars)? (3) How has ram pressure and tidal stripping<br />
affected the dust in these galaxies? (4) Is dust being ejected into the IGM <strong>of</strong><br />
the group? Combined with our unique information from ultraviolet spectroscopy<br />
already obtained, this program will provide valuable insight on the effects <strong>of</strong><br />
ram pressure and tidal stripping on galaxy evolution.<br />
Spitzer_Approved_<strong>Extragalactic</strong><br />
Printed_by_SSC<br />
Mar 25, 10 16:24 Page 398/742<br />
Spitzer Space Telescope − General Observer Proposal #3187<br />
The Evolution <strong>of</strong> Activity in Massive Gas−Rich Mergers<br />
Principal Investigator: Sylvain Veilleux<br />
Institution: University <strong>of</strong> Maryland<br />
Technical Contact: Sylvain Veilleux, University <strong>of</strong> Maryland<br />
Co−Investigators:<br />
Reinhard Genzel, MPE, UC Berkeley [co−PI]<br />
Eckhard Sturm, MPE [Project Scientist]<br />
Dieter Lutz, MPE<br />
Linda Tacconi, MPE<br />
Matthew Lehnert, MPE<br />
Alessandra Contursi, MPE<br />
David Sanders, University <strong>of</strong> Hawaii, <strong>Institute</strong> for Astronomy<br />
Robert Joseph, University <strong>of</strong> Hawaii, <strong>Institute</strong> for Astronomy<br />
Alan Stockton, University <strong>of</strong> Hawaii, <strong>Institute</strong> for Astronomy<br />
Josh Barnes, University <strong>of</strong> Hawaii, <strong>Institute</strong> for Astronomy<br />
Joe Mazzarella, IPAC, Caltech<br />
Steve Lord, IPAC, Caltech<br />
Hagai Netzer, Tel Aviv University<br />
Amiel Sternberg, Tel Aviv University<br />
Chris Mihos, Case Western Reserve University<br />
Olivier Guyon, Subaru Telescope<br />
Kaliopi Dasyra, MPE<br />
Science Category: interacting/merging galaxies<br />
Observing Modes: IrsStare<br />
Hours Approved: 95.3<br />
Abstract:<br />
We wish to study in detail the basic physical processes involved in creating<br />
massive early type hosts on the one hand, and growing/feeding embedded massive<br />
black holes on the other hand, in major galaxy mergers. This is an important<br />
question since 50% <strong>of</strong> cosmic star formation at high−z and most <strong>of</strong> the big BHs<br />
appear to be formed in this process, which we need to better understand in a<br />
local laboratory, in order to apply this knowledge to high z. We want to test<br />
the ‘Sanders’ (1988) scenario that massive ellipticals as well as QSO−like (><br />
10^8 Msun) black holes are formed when two big, gas rich galaxies merge. We want<br />
to understand how and at what rate during the various stages <strong>of</strong> the merger black<br />
holes are fed and grow in mass. We want to verify whether the output BHs are<br />
typical <strong>of</strong> QSOs and whether this process adheres to the local BHmass−sigma<br />
relationship. Our approach is unique and goes much beyond the proposed GTO and<br />
Legacy programs in this area. Taking an unbiased set <strong>of</strong> 54 local Universe active<br />
mergers and QSOs, we first need to fully understand the structural properties <strong>of</strong><br />
each galaxy merger as well as the time/phase at which we see it. This we get<br />
from our near−IR/optical data sets, which is the first such complete<br />
investigation. Then we need to assign to each system the amount <strong>of</strong><br />
radiation/energy produced in star formation and BH accretion. This information<br />
we get (and only can obtain) from mid−IR spectroscopic data which will be<br />
acquired with SST. The SST data we propose to get for the first time allow<br />
obtaining the key fine−structure line diagnostics for a large sample, and for<br />
the first time, for QSOs. With our previous ISO spectroscopy we have pioneered<br />
the basic technique. Here we wish to apply these techniques to a full sample<br />
that allows the exploration <strong>of</strong> evolution.<br />
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