PhD Thesis (PDF) - Department of Astronomy - University of Virginia

More documents

Recommendations

Info

References Angelini, L., Loewenstein, M., & Mushotzky, R. F. 2001, ApJ, 557, L35 Baggett, W. E., Baggett, S. M., & Anderson, K. S. J. 1998, AJ, 116, 1626 Barton, E., Geller, M., Ramella, M., Marzke, R. O., & da Costa, L. N. 1996, AJ, 112, 871 Bassino, L. P., Cellone, S. A., Forte, J. C., & Dirsch, B. 2003, A&A, 399, 489 Begelman, M. C. 2002, ApJ, 568, L97 Belian, R. D., Conner, J. P., & Evans, W. D. 1976, ApJ, 206, L135 Bellazzini, M., Pasquali, A., Federici, L., Ferraro, F. R., & Pecci, F. F. 1995, ApJ, 439, 687 Bhattacharya, D. & Srinivasan, G. 1995, in X-ray Binaries, ed. W. H. G. Lewin, J. van Paradijs, & E. P. J. van den Heuvel (Cambridge: Cambridge University Press), 495 Bildsten, L. & Deloye, C. J. 2004, ApJ, 607, L119 Binney, J. & Merrifield, M. 1998, Galactic Astronomy (Princeton: Princeton Univer- sity Press) Birkinshaw, M. & Davies, R. L. 1985, ApJ, 291, 32 406
Blanton, E. L., Sarazin, C. L., & Irwin, J. A. 2001, ApJ, 552, 106 Brandt, W. N. et al. 2000, AJ, 119, 2349 —. 2001, AJ, 122, 2810 Bregman, J. N., Irwin, J. A., Seitzer, P., & Flores, M. 2006, ApJ, 640, 282 Brighenti, F. & Mathews, W. G. 1996, ApJ, 470, 747 Brown, B. A. & Bregman, J. N. 1998, ApJ, 495, L75+ Bruzual, G. & Charlot, S. 2003, MNRAS, 344, 1000 Buote, D. A. & Fabian, A. C. 1998, MNRAS, 296, 977 Canizares, C. R., Fabbiano, G., & Trinchieri, G. 1987, ApJ, 312, 503 Clark, G. W. 1975, ApJ, 199, L143 Colbert, E. J. M. & Mushotzky, R. F. 1999, ApJ, 519, 89 Condon, J. J. & Broderick, J. J. 1991, AJ, 102, 1663 Côté, P. et al. 2004, ApJS, 153, 223 Cutri, R. M. et al. 2001, Explanatory Supplement to the 2MASS Second In- cremental Data Release, The Two Micron All Sky Survey at IPAC Website: http://www.ipac.caltech.edu/2mass/releases/second/doc/explsup.html Davis, D. S. & White, R. E. 1996, ApJ, 470, L35+ de Vaucouleurs, G., de Vaucouleurs, A., Corwin, H. G., Buta, R. J., Paturel, G., & Fouque, P. 1992, Third Reference Catalogue of Bright Galaxies (RC3) 407
Page 1 and 2:
LOW-MASS X-RAY BINARIES, DIFFUSE GA
Page 3 and 4:
smaller GCs are more likely to cont
Page 5 and 6:
GO2-3099X, GO3-4099X, AR3-4005X, GO
Page 7 and 8:
her room (my apologies to her offic
Page 9 and 10:
US Court expert from India), for al
Page 11 and 12:
Table of contents Abstract ii Ackno
Page 13 and 14:
5.2.1 Chandra X-ray Observatory . .
Page 15 and 16:
List of Figures 1.1 Hubble Tuning F
Page 17 and 18:
List of Tables 1.1 Galactic Low-Mas
Page 19 and 20:
Chapter 1 General Introduction 1.1
Page 21 and 22:
Fig. 1.1.— Hubble Tuning Fork, co
Page 23 and 24:
2000). In most HMXBs, the accreted
Page 25 and 26:
not get a complete picture of the L
Page 27 and 28:
this, the result of dynamical inter
Page 29 and 30:
is the Advanced CCD Imaging Spectro
Page 31 and 32:
Chapter 2 Chandra Observations of L
Page 33 and 34:
keV (Sarazin et al. 2000, 2001). Wi
Page 35 and 36:
agreed with positions from the USNO
Page 37 and 38:
24:00 22:00 7:20:00 18:00 16:00 18:
Page 39 and 40:
Table 2.1. Discrete X-ray Sources i
Page 41 and 42:
Table 2.1—Continued Source d Coun
Page 43 and 44:
Page 45 and 46:
Table 2.2—Continued Source d Coun
Page 47 and 48:
optical/IR positions of R.A. = 12 h
Page 49 and 50:
log N(>L) 2.0 1.5 1.0 0.5 0.0 NGC 4
Page 51 and 52:
luminosity function for luminositie
Page 53 and 54:
H31 1.0 0.5 0.0 -0.5 -1.0 NGC 4365
Page 55 and 56:
2.4.5 Variability We searched for v
Page 57 and 58:
Number 10 8 6 4 2 NGC 4365 Optical
Page 59 and 60:
LMXBs has an effective radius of 12
Page 61 and 62:
component (“MEKAL”) was used fo
Page 63 and 64:
Table 2.4. X-ray Spectral Fits of N
Page 65 and 66:
Fig. 2.9.— Top panels: Cumulative
Page 67 and 68:
we extended the spectrum down to 0.
Page 69 and 70:
We also examined whether the unreso
Page 71 and 72:
esolved sources in the galaxy. This
Page 73 and 74:
temperature ∼0.3 keV. Matsumoto e
Page 75 and 76:
log I X (counts/sec/arcmin 2 ) -1.0
Page 77 and 78:
∼45% of the counts are resolved i
Page 79 and 80:
Chapter 3 Chandra Observations of D
Page 81 and 82:
noninteracting members (de Vaucoule
Page 83 and 84:
used for spectroscopic analysis. We
Page 85 and 86:
02:00.0 03:00.0 04:00.0 05:00.0 06:
Page 87 and 88:
Page 89 and 90:
Table 3.1—Continued d a Count Rat
Page 91 and 92:
We also attempted detections in mul
Page 93 and 94:
sociated with extended X-ray or opt
Page 95 and 96:
Fig. 3.3.— Histogram of the obser
Page 97 and 98:
chip. The number of ULX candidates
Page 99 and 100:
these luminosities among previously
Page 101 and 102:
to 2-6 keV. Since the 6-10 keV rang
Page 103 and 104:
absorption and varying power-law in
Page 105 and 106:
counts occur within ∼ 4 ks. Sourc
Page 107 and 108:
log I X (counts/sec/arcmin 2 ) 0.5
Page 109 and 110:
tion), and βouter = 0.36 +0.01 −
Page 111 and 112:
the east and northeast of NGC 1600.
Page 113 and 114:
group, we assumed that they were at
Page 115 and 116:
the group gas than we calculate fro
Page 117 and 118:
04:55 -5:05:00 05 -5:05:10 15 -5:05
Page 119 and 120:
for the spectrum: “Field” impli
Page 121 and 122:
90% confidence level errors. Bracke
Page 123 and 124:
we adopted the power-law model as o
Page 125 and 126:
sources could be a non-trivial sour
Page 127 and 128:
jection to include the emission fro
Page 129 and 130:
Fig. 3.13.— Estimated gas and gra
Page 131 and 132:
ackground source population cannot
Page 133 and 134:
NGC 1600 that has a small spatial s
Page 135 and 136:
(HMXBs). LMC X-4, an HMXB pulsar, h
Page 137 and 138:
searched for the shortest time tn o
Page 139 and 140:
with NGC 4697. Columns (1)-(4) list
Page 141 and 142:
duration, ∆tflat, beginning at a
Page 143 and 144:
the uncertainties quoted do not inc
Page 145 and 146:
to persistent rate for short flares
Page 147 and 148:
Chapter 5 Multi-Epoch Chandra X-ray
Page 149 and 150:
the field, these different populati
Page 151 and 152:
luminous (MB < −20) elliptical (E
Page 153 and 154:
Although Chandra is known to encoun
Page 155 and 156:
42:00.0 44:00.0 46:00.0 48:00.0 -5:
Page 157 and 158:
Fig. 5.3.— Adaptively smoothed Ch
Page 159 and 160:
1 × 10 −5 count s −1 arcsec
Page 161 and 162:
Table 5.1—Continued Source R.A. D
Page 163 and 164:
Page 165 and 166:
Page 167 and 168:
source list against which to regist
Page 169 and 170:
ate from Observation 0784 alone (Pa
Page 171 and 172:
Table 5.2. : Optical Properties of
Page 173 and 174:
actually be an AGN. Sources 79, 80,
Page 175 and 176:
two potential GC counterparts. We l
Page 177 and 178:
Table 5.3—Continued X-ray Source
Page 179 and 180:
Fig. 5.6.— Color (G475−Z850) -
Page 181 and 182:
mass segregation of GCs with the sa
Page 183 and 184:
Table 5.4. Fits to the Expected Num
Page 185 and 186:
dependence are allowed to vary. Var
Page 187 and 188:
NGC 4697 to convert the observed so
Page 189 and 190:
Table 5.6—Continued Source LA LB
Page 191 and 192:
Table 5.6—Continued Source LA LB
Page 193 and 194:
Table 5.7. Combined Luminosities &
Page 195 and 196:
Table 5.7—Continued Source Not De
Page 197 and 198:
Fig. 5.8.— Cumulative luminosity
Page 199 and 200:
LF, there are enough datapoints tha
Page 201 and 202:
Fig. 5.10.— Cumulative luminosity
Page 203 and 204:
Fig. 5.11.— Merged luminosities (
Page 205 and 206:
Fig. 5.12.— X-ray color-color dia
Page 207 and 208:
5.9 Spectral Analysis We performed
Page 209 and 210:
some data loss, it allows for direc
Page 211 and 212:
for 2 dof and the f-test indicates
Page 213 and 214:
ple to LMXBs interior to that semi-
Page 215 and 216:
est-fit (χ 2 = 56.4 for 65 dof) by
Page 217 and 218:
5.10.1 Intraobservation Variability
Page 219 and 220:
Fig. 5.14.— Binned lightcurve usi
Page 221 and 222:
Table 5.10. Possible Flaring Source
Page 223 and 224:
Fig. 5.16.— Cumulative lightcurve
Page 225 and 226:
pairs of observations. In Figure 5.
Page 227 and 228:
Table 5.11—Continued Source PL,AB
Page 229 and 230:
Fig. 5.17.— Percentage of Analysi
Page 231 and 232:
dofs and the number of combinations
Page 233 and 234:
Table 5.12—Continued Source Obs.S
Page 235 and 236:
of states as transient candidates.
Page 237 and 238:
Long-Term Hardness Ratio Variabilit
Page 239 and 240:
In the final observation, there wer
Page 241 and 242:
limits). The 0.3-10 keV X-ray lumin
Page 243 and 244:
atio is expected only from the most
Page 245 and 246:
eak (Kim et al. 2006a). We find mar
Page 247 and 248:
LMXBs in Galactic GCs (Heinke et al
Page 249 and 250:
in the field of the Milky Way and a
Page 251 and 252:
6.2 Sample 6.2.1 Galaxy Sample Tabl
Page 253 and 254:
Table 6.2. Properties of Chandra Ob
Page 255 and 256:
identification of point sources, AC
Page 257 and 258:
the QE degradation in the ACIS dete
Page 259 and 260:
Table 6.3—Continued Galaxy NX LX,
Page 261 and 262:
The positions of the GCs were used
Page 263 and 264:
Fig. 6.2.— Scatter plot of GC gal
Page 265 and 266:
Fig. 6.3.— Scatter plot of estima
Page 267 and 268:
Fig. 6.5.— Scatter plot of estima
Page 269 and 270:
isophote from the galaxy optical su
Page 271 and 272:
6.3.1 Luminosity and Mass Prior obs
Page 273 and 274:
compare their χ 2 fits to test whi
Page 275 and 276:
GCs without LMXBs; however, there a
Page 277 and 278:
following dependence on GC properti
Page 279 and 280:
of this probability with individual
Page 281 and 282:
Fig. 6.9.— Identical to Figure 6.
Page 283 and 284:
We used the indices from our best-f
Page 285 and 286:
(20.3 for half-mass radius, both wi
Page 287 and 288:
most are steeper than Z ∼0.4 . Ei
Page 289 and 290:
Fig. 6.11.— (Left:) Two-dimension
Page 291 and 292:
differently by the properties of th
Page 293 and 294:
dependent IMF (Grindlay 1987), or e
Page 295 and 296:
a 1.4M⊙ neutron star (NS). They s
Page 297 and 298:
equivalent to a dependence on the b
Page 299 and 300:
variability timescale, but it is no
Page 301 and 302:
7.2.1 X-ray Properties of the GC-LM
Page 303 and 304:
of the metallicity dependence. As i
Page 305 and 306:
Appendix A Encounter Rate Parameter
Page 307 and 308:
Fig. A.1.— Dimensionless quantity
Page 309 and 310:
and four; these positions do not in
Page 311 and 312:
Table B.1—Continued RA Dec. d GC
Page 313 and 314:
Page 315 and 316:
Table B.2. Optical Properties of Gl
Page 317 and 318:
Page 319 and 320:
Page 321 and 322:
Page 323 and 324:
Page 325 and 326:
Page 327 and 328:
Page 329 and 330:
Page 331 and 332:
Page 333 and 334:
Page 335 and 336:
Page 337 and 338:
Page 339 and 340:
Page 341 and 342:
Page 343 and 344:
Page 345 and 346:
Page 347 and 348:
Page 349 and 350:
Page 351 and 352:
Page 353 and 354:
Page 355 and 356:
Page 357 and 358:
Page 359 and 360:
Page 361 and 362:
Page 363 and 364:
Page 365 and 366:
Page 367 and 368:
Page 369 and 370:
Page 371 and 372:
Page 373 and 374: Table B.2—Continued RA Dec. d GC
Page 421 and 422: investigations into improving the h
Page 423: C.4 Sivakoff Signature Soy Sauce Sk
Page 427 and 428: Frogel, J. A., Persson, S. E., Matt
Page 429 and 430: Johnston, H. M. & Verbunt, F. 1996,
Page 431 and 432: Makishima, K. et al. 2000, ApJ, 535
Page 433 and 434: Porter, A. C. 1993, PASP, 105, 1250
Page 435: Verner, D. A., Ferland, G. J., Kori
show all

PhD Thesis (PDF) - Department of Astronomy - University of Virginia

You also want an ePaper? Increase the reach of your titles

Delete template?

Save as template?