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LOW-MASS X-RAY BINARIES, DIFFUSE GA
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smaller GCs are more likely to cont
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GO2-3099X, GO3-4099X, AR3-4005X, GO
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her room (my apologies to her offic
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US Court expert from India), for al
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Table of contents Abstract ii Ackno
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5.2.1 Chandra X-ray Observatory . .
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List of Figures 1.1 Hubble Tuning F
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List of Tables 1.1 Galactic Low-Mas
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Chapter 1 General Introduction 1.1
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Fig. 1.1.— Hubble Tuning Fork, co
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2000). In most HMXBs, the accreted
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not get a complete picture of the L
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this, the result of dynamical inter
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is the Advanced CCD Imaging Spectro
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Chapter 2 Chandra Observations of L
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keV (Sarazin et al. 2000, 2001). Wi
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agreed with positions from the USNO
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24:00 22:00 7:20:00 18:00 16:00 18:
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Table 2.1. Discrete X-ray Sources i
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Table 2.1—Continued Source d Coun
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Table 2.2. Discrete X-ray Sources i
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Table 2.2—Continued Source d Coun
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optical/IR positions of R.A. = 12 h
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log N(>L) 2.0 1.5 1.0 0.5 0.0 NGC 4
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luminosity function for luminositie
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H31 1.0 0.5 0.0 -0.5 -1.0 NGC 4365
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2.4.5 Variability We searched for v
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Number 10 8 6 4 2 NGC 4365 Optical
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LMXBs has an effective radius of 12
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component (“MEKAL”) was used fo
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Table 2.4. X-ray Spectral Fits of N
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Fig. 2.9.— Top panels: Cumulative
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we extended the spectrum down to 0.
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We also examined whether the unreso
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esolved sources in the galaxy. This
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temperature ∼0.3 keV. Matsumoto e
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log I X (counts/sec/arcmin 2 ) -1.0
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∼45% of the counts are resolved i
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Chapter 3 Chandra Observations of D
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noninteracting members (de Vaucoule
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used for spectroscopic analysis. We
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02:00.0 03:00.0 04:00.0 05:00.0 06:
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Table 3.1. Discrete X-ray Sources i
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Table 3.1—Continued d a Count Rat
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We also attempted detections in mul
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sociated with extended X-ray or opt
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Fig. 3.3.— Histogram of the obser
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chip. The number of ULX candidates
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these luminosities among previously
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to 2-6 keV. Since the 6-10 keV rang
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absorption and varying power-law in
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counts occur within ∼ 4 ks. Sourc
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log I X (counts/sec/arcmin 2 ) 0.5
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tion), and βouter = 0.36 +0.01 −
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the east and northeast of NGC 1600.
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group, we assumed that they were at
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the group gas than we calculate fro
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04:55 -5:05:00 05 -5:05:10 15 -5:05
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for the spectrum: “Field” impli
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90% confidence level errors. Bracke
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we adopted the power-law model as o
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sources could be a non-trivial sour
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jection to include the emission fro
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Fig. 3.13.— Estimated gas and gra
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ackground source population cannot
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NGC 1600 that has a small spatial s
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(HMXBs). LMC X-4, an HMXB pulsar, h
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searched for the shortest time tn o
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with NGC 4697. Columns (1)-(4) list
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duration, ∆tflat, beginning at a
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the uncertainties quoted do not inc
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to persistent rate for short flares
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Chapter 5 Multi-Epoch Chandra X-ray
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the field, these different populati
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luminous (MB < −20) elliptical (E
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Although Chandra is known to encoun
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42:00.0 44:00.0 46:00.0 48:00.0 -5:
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Fig. 5.3.— Adaptively smoothed Ch
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1 × 10 −5 count s −1 arcsec
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Table 5.1—Continued Source R.A. D
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Table 5.1—Continued Source R.A. D
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Table 5.1—Continued Source R.A. D
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source list against which to regist
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ate from Observation 0784 alone (Pa
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Table 5.2. : Optical Properties of
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actually be an AGN. Sources 79, 80,
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two potential GC counterparts. We l
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Table 5.3—Continued X-ray Source
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Fig. 5.6.— Color (G475−Z850) -
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- 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
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- 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
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- 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
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- 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
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- Page 255 and 256: identification of point sources, AC
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- 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
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- Page 281 and 282: Fig. 6.9.— Identical to Figure 6.
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We used the indices from our best-f
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(20.3 for half-mass radius, both wi
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most are steeper than Z ∼0.4 . Ei
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Fig. 6.11.— (Left:) Two-dimension
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differently by the properties of th
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dependent IMF (Grindlay 1987), or e
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a 1.4M⊙ neutron star (NS). They s
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equivalent to a dependence on the b
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variability timescale, but it is no
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7.2.1 X-ray Properties of the GC-LM
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of the metallicity dependence. As i
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Appendix A Encounter Rate Parameter
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Fig. A.1.— Dimensionless quantity
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and four; these positions do not in
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Table B.1—Continued RA Dec. d GC
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Table B.1—Continued RA Dec. d GC
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Table B.2. Optical Properties of Gl
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Table B.2—Continued RA Dec. d GC
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Table B.2—Continued RA Dec. d GC
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Table B.2—Continued RA Dec. d GC
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Table B.2—Continued RA Dec. d GC
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Table B.2—Continued RA Dec. d GC
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Table B.2—Continued RA Dec. d GC
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Table B.2—Continued RA Dec. d GC
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Table B.2—Continued RA Dec. d GC
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Table B.2—Continued RA Dec. d GC
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Table B.2—Continued RA Dec. d GC
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Table B.2—Continued RA Dec. d GC
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Table B.2—Continued RA Dec. d GC
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Table B.2—Continued RA Dec. d GC
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Table B.2—Continued RA Dec. d GC
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Table B.2—Continued RA Dec. d GC
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Table B.2—Continued RA Dec. d GC
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Table B.2—Continued RA Dec. d GC
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Table B.2—Continued RA Dec. d GC
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Table B.2—Continued RA Dec. d GC
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Table B.2—Continued RA Dec. d GC
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Table B.2—Continued RA Dec. d GC
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Table B.2—Continued RA Dec. d GC
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Table B.2—Continued RA Dec. d GC
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Table B.2—Continued RA Dec. d GC
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Table B.2—Continued RA Dec. d GC
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Table B.2—Continued RA Dec. d GC
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Table B.2—Continued RA Dec. d GC
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Table B.2—Continued RA Dec. d GC
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Table B.2—Continued RA Dec. d GC
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Table B.2—Continued RA Dec. d GC
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Table B.2—Continued RA Dec. d GC
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Table B.2—Continued RA Dec. d GC
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Table B.2—Continued RA Dec. d GC
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Table B.2—Continued RA Dec. d GC
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Table B.2—Continued RA Dec. d GC
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Table B.2—Continued RA Dec. d GC
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Table B.2—Continued RA Dec. d GC
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investigations into improving the h
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C.4 Sivakoff Signature Soy Sauce Sk
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Blanton, E. L., Sarazin, C. L., & I
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Frogel, J. A., Persson, S. E., Matt
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Johnston, H. M. & Verbunt, F. 1996,
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Makishima, K. et al. 2000, ApJ, 535
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Porter, A. C. 1993, PASP, 105, 1250
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Verner, D. A., Ferland, G. J., Kori
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