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

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Table 2.2—Continued Source d Count Rate Number Name R.A. Decl. (arcsec) (10−4 s−1 ) S/N LX H21 H31 Notes (1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) 23........ CXOU J122518.4+181137 12 25 18.42 18 11 37.0 80.9 14.54±1.98 7.36 57.22 −0.20 +0.22 −0.20 −0.11+0.21 −0.20 24........ CXOU J122519.8+181235 12 25 19.82 18 12 35.3 91.8 3.61±1.01 3.59 14.19 +0.54 +0.30 −0.55 −0.07+0.73 −0.67 25........ CXOU J122520.7+180955 12 25 20.72 18 09 55.7 101.8 4.65±1.14 4.09 18.29 −0.12 +0.39 −0.36 −0.35+0.53 −0.37 26........ CXOU J122520.3+181301 12 25 20.32 18 13 01.7 109.5 40.73±3.37 12.10 160.27 +0.21 +0.10 −0.10 −0.60+0.15 −0.12 27........ CXOU J122525.5+180936 12 25 25.51 18 09 36.8 111.1 3.82±1.02 3.73 15.02 +0.67 +0.30 −1.09 +0.82+0.16 −0.89 28........ CXOU J122531.6+181051 12 25 31.68 18 10 51.8 114.1 5.66±1.26 4.49 22.26 −0.33 +0.35 −0.28 −0.47+0.41 −0.27 29........ CXOU J122527.4+181314 12 25 27.48 18 13 14.1 118.8 3.33±0.98 3.38 13.09 −0.48 +0.58 −0.34 −0.48+0.63 −0.35 30........ CXOU J122521.6+180929 12 25 21.61 18 09 29.0 121.9 21.55±2.39 9.01 84.78 +0.10 +0.16 −0.16 +0.02+0.17 −0.17 31........ CXOU J122518.1+181255 12 25 18.19 18 12 55.7 122.5 2.68±0.87 3.06 10.55 −0.41 +0.88 −0.47 −0.04+0.57 −0.54 32........ CXOU J122516.8+181234 12 25 16.82 18 12 34.3 123.5 8.37±1.51 5.53 32.93 +0.22 +0.23 −0.25 −0.57+0.46 −0.26 33........ CXOU J122530.4+181311 12 25 30.41 18 13 11.8 139.5 12.51±1.88 6.65 49.24 +0.47 +0.18 −0.23 +0.20+0.27 −0.30 34........ CXOU J122522.2+181344 12 25 22.22 18 13 44.0 140.5 7.37±1.46 5.04 28.99 +0.55 +0.24 −0.38 +0.47+0.28 −0.42 35........ CXOU J122515.0+181018 12 25 15.01 18 10 18.8 145.1 4.20±1.11 3.77 16.52 +0.71 +0.25 −0.79 +0.41+0.49 −0.95 36........ CXOU J122513.8+181248 12 25 13.80 18 12 48.9 167.9 2.70±0.88 3.05 10.62 −0.77 +0.98 −0.21 −0.35+0.50 −0.36 37........ CXOU J122517.6+181350 12 25 17.64 18 13 50.2 170.7 22.95±2.61 8.79 90.29 −0.05 +0.16 −0.16 −0.10+0.17 −0.17 38........ CXOU J122517.1+181346 12 25 17.17 18 13 46.8 171.6 156.44±7.25 21.60 615.56 −0.19 +0.05 −0.05 −0.59+0.06 −0.05 b,c 39........ CXOU J122512.9+181016 12 25 12.98 18 10 16.2 172.3 16.00±2.06 7.76 62.94 +0.00 +0.20 −0.20 −0.05+0.20 −0.20 40........ CXOU J122528.0+181417 12 25 28.06 18 14 17.2 180.7 3.56±1.04 3.42 14.08 −0.15 +0.60 −0.51 −0.15+0.56 −0.47 41........ CXOU J122518.1+180841 12 25 18.12 18 08 41.5 184.8 8.19±2.66 3.09 32.24 −0.14 +0.60 −0.51 −0.14+0.60 −0.51 d 42........ CXOU J122536.5+181002 12 25 36.58 18 10 02.6 197.2 6.43±1.37 4.70 25.31 −0.23 +0.31 −0.27 −0.49+0.43 −0.28 43........ CXOU J122511.1+181006 12 25 11.18 18 10 06.1 199.9 2.70±0.89 3.05 10.64 +0.47 +0.35 −0.59 −0.45+1.23 −0.51 44........ CXOU J122528.6+180808 12 25 28.66 18 08 08.6 208.0 3.20±0.94 3.39 12.59 −0.36 +0.63 −0.41 −0.26+0.57 −0.44 Continued on Next Page. . . 26
Table 2.2—Continued Source d Count Rate Number Name R.A. Decl. (arcsec) (10−4 s−1 ) S/N LX H21 H31 Notes (1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) 45........ CXOU J122523.3+180758 12 25 23.33 18 07 58.1 208.0 22.72±4.02 5.66 89.40 +0.00 +0.24 −0.24 −0.50+0.36 −0.24 d 46........ CXOU J122538.8+181137 12 25 38.83 18 11 37.1 211.1 5.71±1.41 4.06 22.48 +1.00 +0.00 −0.40 +1.00+0.00 −0.09 47........ CXOU J122522.4+181457 12 25 22.48 18 14 57.1 212.3 15.34±2.27 6.75 60.36 −0.24 +0.22 −0.20 −0.43+0.30 −0.23 48........ CXOU J122538.7+181205 12 25 38.75 18 12 05.1 213.2 6.64±1.53 4.33 26.13 +0.66 +0.26 −0.68 +0.67+0.25 −0.67 b 49........ CXOU J122512.8+181409 12 25 12.80 18 14 09.3 228.8 20.54±2.72 7.55 80.83 +0.10 +0.17 −0.18 −0.35+0.25 −0.21 50........ CXOU J122508.0+181229 12 25 08.00 18 12 29.9 237.3 3.75±1.11 3.37 14.73 +0.30 +0.34 −0.43 −0.65+1.25 −0.33 51........ CXOU J122540.6+181224 12 25 40.60 18 12 24.6 243.2 10.99±1.94 5.67 43.24 +0.13 +0.24 −0.25 −0.08+0.33 −0.32 52........ CXOU J122509.2+181336 12 25 09.27 18 13 36.7 247.8 9.67±2.13 4.55 38.07 +0.36 +0.31 −0.41 +0.28+0.35 −0.45 d 53........ CXOU J122506.1+181045 12 25 06.15 18 10 45.8 258.0 12.67±1.95 6.49 49.83 +0.11 +0.22 −0.23 −0.19+0.30 −0.27 b 54........ CXOU J122505.9+181158 12 25 05.91 18 11 58.9 260.5 9.25±1.67 5.53 36.41 +0.12 +0.25 −0.27 −0.48+0.57 −0.33 e 55........ CXOU J122504.7+181133 12 25 04.74 18 11 33.5 275.1 13.21±1.98 6.66 51.98 +0.58 +0.20 −0.30 +0.59+0.19 −0.29 56........ CXOU J122543.4+181048 12 25 43.44 18 10 48.3 278.9 8.82±2.98 3.02 34.69 +0.45 +0.36 −0.60 −0.14+0.88 −0.70 d 57........ CXOU J122503.7+181124 12 25 03.70 18 11 24.1 289.9 14.61±2.52 5.82 57.48 −0.12 +0.23 −0.22 −0.49+0.31 −0.22 b,d 58........ CXOU J122546.0+181302 12 25 46.05 18 13 02.9 328.3 12.11±2.49 4.86 47.65 +0.24 +0.32 −0.38 −0.40+1.03 −0.52 NOTE.—Units of right ascension are hours, minutes, and seconds, and units of declination are degrees, arcminutes, and arcseconds. The units for LX are 1037 ergs s−1 in the 0.3–10 keV band. a Sources near the center may be confused with nearby sources, making their positions, fluxes, and extents uncertain. b Source is noticeably more extended than PSF. c Possible faint optical counterpart. d Globular cluster is possible optical counterpart. e Source may be variable. f Source is at the edge of the S3 detector, and flux is uncertain due to large exposure correction. 27
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: Table 2.2. Discrete X-ray Sources i
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: Table 3.1. Discrete X-ray Sources i
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
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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
Page 131 and 132:
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
Page 141 and 142:
duration, ∆tflat, beginning at a
Page 143 and 144:
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
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
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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,
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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) -
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mass segregation of GCs with the sa
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Table 5.4. Fits to the Expected Num
Page 185 and 186:
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
Page 191 and 192:
Table 5.6—Continued Source LA LB
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Table 5.7. Combined Luminosities &
Page 195 and 196:
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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for 2 dof and the f-test indicates
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ple to LMXBs interior to that semi-
Page 215 and 216:
est-fit (χ 2 = 56.4 for 65 dof) by
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5.10.1 Intraobservation Variability
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Fig. 5.14.— Binned lightcurve usi
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Table 5.10. Possible Flaring Source
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Fig. 5.16.— Cumulative lightcurve
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pairs of observations. In Figure 5.
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Table 5.11—Continued Source PL,AB
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Fig. 5.17.— Percentage of Analysi
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dofs and the number of combinations
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Table 5.12—Continued Source Obs.S
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of states as transient candidates.
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Long-Term Hardness Ratio Variabilit
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In the final observation, there wer
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limits). The 0.3-10 keV X-ray lumin
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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
Page 251 and 252:
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
Page 259 and 260:
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
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
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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
Page 285 and 286:
(20.3 for half-mass radius, both wi
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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
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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
Page 303 and 304:
of the metallicity dependence. As i
Page 305 and 306:
Appendix A Encounter Rate Parameter
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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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