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

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Fig. 5.7.— Cumulative luminosity functions for each of the five observations of the sources detected at the > 3σ level within a < 220 ′′ . The two-sample K-S tests do not indicate that any two of the observations are drawn from different populations. 174
Table 5.7. Combined Luminosities & Hardness Ratios of X-ray Sources Source Not Detected Not in FOV Lall H21 0 all H31 0 all H32 0 all (1) (2) (3) (4) (5) (6) (7) 1 · · · · · · 35.8±1.8 −0.16 +0.05 −0.05 2 ABCDE · · · 8.4±0.9 −0.13 +0.12 −0.11 3 ABCDE · · · 3.9±0.7 −0.18 +0.18 −0.16 4 B · · · 10.6±1.0 −0.33 +0.09 −0.08 5 · · · · · · 10.1±1.0 −0.17 +0.11 −0.10 6 AE · · · 4.1±0.7 −0.29 +0.16 −0.14 7 · · · · · · 18.7±1.3 −0.24 +0.07 −0.07 8 ABCDE · · · 2.0±0.6 −0.31 +0.29 −0.21 9 BCD · · · 3.7±0.7 −0.17 +0.18 −0.16 10 · · · · · · 18.3±1.3 −0.11 +0.08 −0.08 11 t · · · · · · 9.9±1.0 −0.37 +0.08 −0.08 12 B · · · 4.1±0.7 −0.31 +0.16 −0.14 13 E · · · 4.3±0.7 −0.13 +0.18 −0.16 14 E · · · 4.9±0.7 −0.41 +0.12 −0.12 15 · · · · · · 14.9±1.2 −0.17 +0.08 −0.08 16 · · · · · · 3.3±0.7 +0.12 +0.25 −0.23 17 ABCDE · · · 1.3±0.5 −0.35 +0.34 −0.27 18 BCDE · · · 0.8±0.4 −0.41 +0.36 −0.29 19 · · · · · · 9.4±1.0 −0.98 +0.02 −0.01 20 BD · · · 3.3±0.6 −0.21 +0.18 −0.16 21 ABCDE · · · 0.8±0.4 −0.09 +0.62 −0.38 22 BCD · · · 2.6±0.6 −0.23 +0.25 −0.21 23 ABCD · · · 0.9±0.4 −1.00 +0.13 −0.00 24 ABCDE · · · 1.1±0.5 −0.40 +0.40 −0.29 25 · · · · · · 7.7±0.9 −0.95 +0.03 −0.03 26 ACDE · · · 0.8±0.4 −0.85 +0.33 −0.15 27 ABD · · · 3.1±0.6 −0.32 +0.19 −0.17 28 BCDE · · · 1.8±0.5 −0.32 +0.28 −0.24 29 · · · · · · 12.3±1.1 −0.17 +0.10 −0.09 30 B · · · 3.3±0.6 −0.01 +0.19 −0.18 31 · · · · · · 23.1±1.4 −0.18 +0.07 −0.07 32 · · · · · · 23.6±1.4 −0.03 +0.07 −0.07 33 ABCDE · · · 0.9±0.4 −0.46 +0.43 −0.26 34 · · · · · · 6.9±0.9 −0.00 +0.14 −0.14 35 · · · · · · 10.8±1.0 −0.07 +0.10 −0.10 36 ABCDE · · · 0.9±0.4 −0.07 +0.53 −0.37 37 t ABCD · · · 2.1±0.5 −0.16 +0.24 −0.21 38 ABC · · · 1.9±0.5 +0.06 +0.30 −0.26 39 · · · · · · 23.6±1.4 +0.02 +0.07 −0.07 40 ABCDE · · · 1.5±0.5 −0.61 +0.30 −0.24 41 t ADE · · · 2.7±0.6 −0.21 +0.23 −0.21 42 · · · · · · 10.5±1.0 −0.21 +0.10 −0.10 43 ABCDE · · · 0.7±0.4 −0.10 +0.61 −0.44 44 ADE · · · 2.2±0.5 −0.12 +0.36 −0.29 Continued on Next Page. . . −0.44+0.05 −0.05 −0.53+0.11 −0.10 −0.64+0.16 −0.12 −0.78+0.07 −0.06 −0.39+0.11 −0.10 −0.76+0.12 −0.10 −0.42+0.07 −0.07 −0.65+0.24 −0.19 −0.79+0.14 −0.11 −0.37+0.08 −0.07 −0.94+0.04 −0.03 −0.50+0.16 −0.13 −0.38+0.18 −0.16 −0.71+0.11 −0.09 −0.48+0.08 −0.07 +0.03+0.27 −0.24 −0.57+0.30 −0.22 −0.75+0.36 −0.25 −0.99+0.02 −0.01 −0.69+0.17 −0.13 −0.63+0.63 −0.28 −0.26+0.24 −0.20 −1.00+0.11 −0.00 −0.69+0.37 −0.21 −1.00+0.01 −0.00 −0.87+0.29 −0.13 −0.58+0.18 −0.14 −0.47+0.27 −0.21 −0.41+0.09 −0.09 −0.48+0.21 −0.17 −0.43+0.06 −0.06 −0.33+0.07 −0.07 −0.69+0.40 −0.25 −0.28+0.16 −0.14 −0.34+0.10 −0.10 −0.49+0.56 −0.34 −0.70+0.21 −0.15 −0.58+0.33 −0.23 −0.23+0.07 −0.07 −0.21+0.29 −0.25 −0.13+0.23 −0.21 −0.35+0.10 −0.09 −0.43+0.66 −0.37 +0.11+0.31 −0.28 −0.30 +0.05 −0.06 −0.43 +0.12 −0.11 −0.53 +0.17 −0.16 −0.60 +0.11 −0.10 −0.23 +0.11 −0.11 −0.60 +0.18 −0.15 −0.20 +0.08 −0.08 −0.43 +0.29 −0.27 −0.71 +0.17 −0.15 −0.27 +0.08 −0.07 −0.88 +0.08 −0.06 −0.22 +0.19 −0.18 −0.25 +0.17 −0.17 −0.43 +0.17 −0.16 −0.34 +0.09 −0.08 −0.10 +0.19 −0.19 −0.27 +0.39 −0.33 −0.49 +0.54 −0.51 −0.39 +0.66 −0.61 −0.56 +0.20 −0.18 −0.57 +0.42 −0.32 −0.04 +0.22 −0.23 +0.00 +1.00 −1.00 −0.40 +0.50 −0.37 −1.00 +0.51 −0.00 −0.06 +1.06 −0.94 −0.31 +0.22 −0.20 −0.17 +0.32 −0.29 −0.26 +0.09 −0.09 −0.47 +0.18 −0.16 −0.28 +0.07 −0.07 −0.30 +0.06 −0.06 −0.33 +0.51 −0.51 −0.28 +0.13 −0.13 −0.27 +0.10 −0.10 −0.43 +0.38 −0.37 −0.60 +0.23 −0.19 −0.62 +0.24 −0.20 −0.25 +0.07 −0.06 +0.46 +0.31 −0.33 +0.09 +0.21 −0.21 −0.15 +0.11 −0.10 −0.34 +0.49 −0.40 +0.23 +0.22 −0.23 175
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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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Page 147 and 148: Chapter 5 Multi-Epoch Chandra X-ray
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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
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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
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Page 195 and 196: 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
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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
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atio is expected only from the most
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eak (Kim et al. 2006a). We find mar
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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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