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

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86 47:00.0 30.0 83 -5:48:00.0 78 30.0 49:00.0 30.0 76 74 65 66 64 85 82 68 67 63 58 57 52 56 46 71 50 49 28 29 31 19 41 26 20 16 40 15 23 39 53 9 12 8 7 55 14 30 34 79 21 18 10 5 2 1 4 35 62 33 59 61 138 40.0 38.0 36.0 34.0 32.0 12:48:30.0 Fig. 5.2.— Chandra S3 image (0.3–6 keV) of the central 3 ′ × 3 ′ of NGC 4697 from all five observations. The optical center of NGC 4697 lies within the circle for Source 1. The gray scale is the same as in Figure 5.1. The positions of detected sources in the image are indicated by their source numbers in Table 5.1 11 6 3 13 24 47 32 25 17 27 42 43 22 84 36 37 51 38 44 60 45 48 54 77 81 69 70 73 72 75 80
Fig. 5.3.— Adaptively smoothed Chandra true-color S3 image (with red = 0.3– 1 keV, green = 1–2 keV, and blue = 2–6 keV) of NGC 4697 (all five observations), corrected for exposure and blank-sky background. The intensity scale for the colors is logarithmic and ranges from 5 × 10 −7 to 1 × 10 −5 count s −1 arcsec −2 in total surface brightness. The D25 ellipse is shown. 139
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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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Page 109 and 110: tion), and βouter = 0.36 +0.01 −
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Page 113 and 114: group, we assumed that they were at
Page 115 and 116: the group gas than we calculate fro
Page 117 and 118: 04:55 -5:05:00 05 -5:05:10 15 -5:05
Page 119 and 120: for the spectrum: “Field” impli
Page 121 and 122: 90% confidence level errors. Bracke
Page 123 and 124: we adopted the power-law model as o
Page 125 and 126: sources could be a non-trivial sour
Page 127 and 128: jection to include the emission fro
Page 129 and 130: Fig. 3.13.— Estimated gas and gra
Page 131 and 132: ackground source population cannot
Page 133 and 134: NGC 1600 that has a small spatial s
Page 135 and 136: (HMXBs). LMC X-4, an HMXB pulsar, h
Page 137 and 138: searched for the shortest time tn o
Page 139 and 140: 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
Page 145 and 146: to persistent rate for short flares
Page 147 and 148: Chapter 5 Multi-Epoch Chandra X-ray
Page 149 and 150: the field, these different populati
Page 151 and 152: luminous (MB < −20) elliptical (E
Page 153 and 154: Although Chandra is known to encoun
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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
Page 185 and 186: dependence are allowed to vary. Var
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 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
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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-
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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
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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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