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

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Table 5.7—Continued Source Not Detected Not in FOV Lall H21 0 all H31 0 all H32 0 all (1) (2) (3) (4) (5) (6) (7) 133 B · · · 5.0±0.7 +0.14 +0.17 −0.18 134 · · · · · · 171.7±3.8 +0.62 +0.03 −0.03 135 ABCD · · · 1.0±0.5 −0.64 +0.33 −0.28 136 E BCD 2.9±1.0 +0.56 +0.44 −0.98 137 · · · · · · 9.4±1.0 −0.27 +0.11 −0.10 138 ABCDE · · · 1.1±0.5 −0.30 +1.30 −0.70 139 BDE · · · 2.4±0.6 −0.13 +0.24 −0.21 140 ABCDE · · · 2.1±0.6 −0.23 +0.30 −0.23 141 BCD · · · 3.2±0.7 −0.50 +0.19 −0.16 142 BCD E 2.8±0.7 −0.40 +0.24 −0.21 143 · · · BCD 67.2±5.2 −0.37 +0.07 −0.07 144 BD · · · 5.1±0.8 +0.03 +0.19 −0.17 145 ABCDE · · · 0.6±0.4 +0.13 +0.87 −1.12 146 CDE · · · 3.4±0.9 +0.39 +0.35 −0.32 147 B A 6.5±1.0 −0.10 +0.16 −0.15 148 · · · ABCD 8.2±2.3 +1.00 +0.00 −0.22 149 · · · BCD 8.1±1.7 −0.06 +0.24 −0.21 150 BCDE · · · 2.2±0.6 +0.46 +0.26 −0.25 151 · · · BCD 11.5±2.1 −0.23 +0.16 −0.16 152 ABCD · · · 2.4±0.8 +0.22 +0.48 −0.36 153 · · · BCD 10.5±1.9 +0.60 +0.21 −0.23 154 · · · ABCD 36.5±4.3 −0.15 +0.13 −0.12 155 · · · AE 101.1±4.1 −0.02 +0.05 −0.05 156 · · · AE 90.0±3.9 −0.79 +0.02 −0.02 157 · · · ABCD 4.5±2.2 +0.05 +0.55 −0.45 158 BCD AE 6.0±1.7 +0.99 +0.01 −0.45 −0.06+0.19 −0.18 +0.60+0.03 −0.03 −0.78+0.31 −0.22 +0.90+0.10 −0.41 −0.38+0.11 −0.10 +0.70+0.30 −0.47 −0.42+0.26 −0.22 −0.49+0.29 −0.23 −0.52+0.18 −0.16 −0.47+0.23 −0.22 −0.65+0.06 −0.06 −0.17+0.20 −0.18 +0.58+0.42 −0.64 +0.41+0.34 −0.33 −0.66+0.15 −0.13 +1.00+0.00 −0.09 −0.33+0.26 −0.22 −0.36+0.49 −0.42 −0.65+0.17 −0.14 −0.30+0.67 −0.46 +0.51+0.26 −0.27 −0.37+0.13 −0.12 −0.30+0.05 −0.05 −1.00+0.01 −0.00 −0.13+0.60 −0.51 +0.98+0.02 −0.64 −0.19 +0.15 −0.14 −0.03 +0.02 −0.02 −0.28 +0.79 −0.72 +0.68 +0.21 −0.25 −0.12 +0.12 −0.12 +0.83 +0.17 −0.33 −0.31 +0.25 −0.25 −0.29 +0.30 −0.29 −0.03 +0.27 −0.28 −0.09 +0.30 −0.33 −0.37 +0.09 −0.09 −0.20 +0.16 −0.15 +0.49 +0.51 −0.54 +0.02 +0.22 −0.22 −0.60 +0.15 −0.14 +0.43 +0.20 −0.22 −0.27 +0.21 −0.21 −0.71 +0.22 −0.20 −0.49 +0.20 −0.19 −0.49 +0.31 −0.33 −0.14 +0.16 −0.16 −0.24 +0.13 −0.12 −0.28 +0.04 −0.04 −0.99 +0.06 −0.01 −0.18 +0.45 −0.44 −0.22 +0.22 −0.22 NOTE.—Luminosities are in units of 10 37 ergs s −1 . Observations 0784, 4727, 4728, 4729, 4730 are indicated by A, B, C, D, and E, respectively. If an observation is listed in the “Not in FOV” column, it means the source was not in the S3 FOV for that observation, and thus could not possibly be detected. If an observation is listed in the “Not Detected” column, it means the source was in the FOV for that observation, but was not detected by wavdetect in that individual observation. Sources with ABCDE in the “Not Detected” were not detected in any individual observation, only in the combined sum of the observations. t Source is a transient candidate. 178
Fig. 5.8.— Cumulative luminosity function of the constant sources (LX = Lconstant) detected within a < 220 ′′ using their cumulative luminosity for all observations. The continuous curves are the sum of the best-fit LMXB luminosity functions (to sources detected at the 3σ level) and the expected background source counts. The broken power law is the best fit model; however, a cutoff power law is acceptable according to the K-S test. 179
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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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Page 147 and 148: Chapter 5 Multi-Epoch Chandra X-ray
Page 149 and 150: the field, these different populati
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Page 153 and 154: Although Chandra is known to encoun
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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 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
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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: Table 5.7—Continued Source Not De
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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 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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LMXBs in Galactic GCs (Heinke et al
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in the field of the Milky Way and a
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6.2 Sample 6.2.1 Galaxy Sample Tabl
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Table 6.2. Properties of Chandra Ob
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identification of point sources, AC
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the QE degradation in the ACIS dete
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Table 6.3—Continued Galaxy NX LX,
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The positions of the GCs were used
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Fig. 6.2.— Scatter plot of GC gal
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Fig. 6.3.— Scatter plot of estima
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Fig. 6.5.— Scatter plot of estima
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isophote from the galaxy optical su
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6.3.1 Luminosity and Mass Prior obs
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compare their χ 2 fits to test whi
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GCs without LMXBs; however, there a
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following dependence on GC properti
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of this probability with individual
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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.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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