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

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Fig. 6.1.— Scatter plot of GC magnitudes (Z850) versus GC colors (G475 − Z850), with integrated histograms of the properties above and to the right of the scatter plot. GCs unmatched to LMXBs are indicated by small black dots and unfilled black histograms (scaled down by a factor of 10). Blue GCs with LMXBs are indicated by filled blue squares and histograms. Red GCs with LMXBs are indicated by filled red circles and histograms. The histograms of the GCs with LMXBs are stacked on each other. GCs that are redder and brighter are more likely to contain LMXBs. 244
Fig. 6.2.— Scatter plot of GC galactocentric distances (dGC) versus observed GC half-light radii (rh), with integrated histograms of the properties above and to the right of the scatter plot. The symbols follow that of Figure 6.1. GCs that are smaller in extent are more likely to contain LMXBs. The galactocentric distance does not appear to affect whether a GC contains an LMXB. 245
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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—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—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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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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mass segregation of GCs with the sa
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Table 5.4. Fits to the Expected Num
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dependence are allowed to vary. Var
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NGC 4697 to convert the observed so
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Table 5.6—Continued Source LA LB
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Table 5.6—Continued Source LA LB
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Table 5.7. Combined Luminosities &
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Table 5.7—Continued Source Not De
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Fig. 5.8.— Cumulative luminosity
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LF, there are enough datapoints tha
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Fig. 5.10.— Cumulative luminosity
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Fig. 5.11.— Merged luminosities (
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Fig. 5.12.— X-ray color-color dia
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5.9 Spectral Analysis We performed
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some data loss, it allows for direc
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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
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
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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
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: The positions of the GCs were used
Page 265 and 266: Fig. 6.3.— Scatter plot of estima
Page 267 and 268: Fig. 6.5.— Scatter plot of estima
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Page 271 and 272: 6.3.1 Luminosity and Mass Prior obs
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Page 281 and 282: Fig. 6.9.— Identical to Figure 6.
Page 283 and 284: We used the indices from our best-f
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Page 287 and 288: most are steeper than Z ∼0.4 . Ei
Page 289 and 290: Fig. 6.11.— (Left:) Two-dimension
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Page 293 and 294: dependent IMF (Grindlay 1987), or e
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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
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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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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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