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

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5.1 Raw X-ray Greyscale X-ray Image of NGC 4697: S3 FOV . . . . . . . 137 5.2 Raw X-ray Greyscale Image of NGC 4697: Central 3 ′ × 3 ′ FOV . . . 138 5.3 Adaptively Smoothed True-Color X-ray Image of NGC 4697: S3 FOV 139 5.4 Adaptively Smoothed True-Color X-ray Image of NGC 4697: Central 3 ′ × 3 ′ FOV . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 140 5.5 Percentage of GCs with an LMXB vs. Limiting X-ray Luminosity in NGC 4697 . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 160 5.6 Color Magnitude Diagram of GCs in NGC 4697 . . . . . . . . . . . . 161 5.7 Cumulative Luminosity Functions of Discrete X-ray Sources in NGC 4697: Individual Observations . . . . . . . . . . . . . . . . . . . . . . 174 5.8 Cumulative Luminosity Functions of Discrete X-ray Sources in NGC 4697: Constant Sources . . . . . . . . . . . . . . . . . . . . . . . . . . 179 5.9 Differential Instantaneous Luminosity Function of Discrete X-ray Sources in NGC 4697 . . . . . . . . . . . . . . . . . . . . . . . . . . 182 5.10 Cumulative Luminosity Functions of Discrete X-ray Sources in NGC 4697: GC-LMXBs vs. Field-LMXBs . . . . . . . . . . . . . . . . . . . 183 5.11 Luminosity and Hardness Ratios Spatial Functions of Discrete X-ray Sources in NGC 4697 . . . . . . . . . . . . . . . . . . . . . . . . . . . 185 5.12 Hardness Ratio Diagram of Discrete X-ray Sources in NGC 4697 . . . 187 5.13 X-ray Spectrum of LMXBs in NGC 4697 . . . . . . . . . . . . . . . . 192 5.14 X-ray Light Curve of Source 156 in NGC 4697 . . . . . . . . . . . . . 201 5.15 Photon Impulse Diagram of Source 57 in NGC 4697 . . . . . . . . . . 204 5.16 Accumulated Fractional X-ray Light Curve of Source 155 in NGC 4697 205 5.17 Percentages of Variable Discrete X-ray Sources in NGC 4697 . . . . . 211 6.1 Magnitudes and Colors of GCs . . . . . . . . . . . . . . . . . . . . . . 244 6.2 Galactocentric Distances and Sizes of GCs . . . . . . . . . . . . . . . 245 6.3 Corrected Sizes and Colors of GCs . . . . . . . . . . . . . . . . . . . 247 6.4 Relaxation Times and Magnitudes of GCs . . . . . . . . . . . . . . . 248 6.5 Corrected Sizes and Magnitudes of GCs . . . . . . . . . . . . . . . . . 249 6.6 Percentage of GCs with LMXBs: Base . . . . . . . . . . . . . . . . . 252 6.7 Percentage of Red-GCs and Blue-GCs with LMXBs . . . . . . . . . . 254 6.8 Percentage of GCs with LMXBs: GC Mass and Color Fit Overlaid . . 262 6.9 Percentage of GCs with LMXBs: GC Mass, Color, and Size Fit Overlaid263 6.10 Two-Dimensional Confidence Intervals of Mass and Radius Exponents 270 6.11 Two-Dimensional Confidence Intervals of Density and Metallicity Exponents . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 271 A.1 R 5/2 L −3/2 as a Function of GC Concentration . . . . . . . . . . . . . 289 xvi
List of Tables 1.1 Galactic Low-Mass X-ray Binaries in Globular Clusters . . . . . . . . 10 2.1 Discrete X-ray Sources in NGC 4365 . . . . . . . . . . . . . . . . . . 21 2.2 Discrete X-ray Sources in NGC 4382 . . . . . . . . . . . . . . . . . . 25 2.3 X-ray Spectral Fits of NGC 4365 . . . . . . . . . . . . . . . . . . . . 44 2.4 X-ray Spectral Fits of NGC 4382 . . . . . . . . . . . . . . . . . . . . 45 3.1 Discrete X-ray Sources in NGC 1600 . . . . . . . . . . . . . . . . . . 69 3.2 X-ray Spectral Fits of NGC 1600 . . . . . . . . . . . . . . . . . . . . 102 4.1 Observed Properties of Short-Timescale Flares in NGC 4697 . . . . . 122 4.2 Inferred Properties of Short-Timescale Flares in NGC 4697 . . . . . . 122 5.1 Discrete X-ray Sources in NGC 4697 . . . . . . . . . . . . . . . . . . 142 5.2 Optical Properties of Ground-Based Optical Sources Matched to X-ray Sources in NGC 4697 . . . . . . . . . . . . . . . . . . . . . . . . . . . 153 5.3 Optical Properties of HST Sources Matched with X-ray Sources in NGC 4697 . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 158 5.4 Fits to the Expected Number of LMXBs per GC (λ) . . . . . . . . . 165 5.5 X-ray Spectral Fits for Point Sources in NGC 4697 . . . . . . . . . . 168 5.6 Instantaneous Luminosities of X-ray Sources . . . . . . . . . . . . . . 170 5.7 Combined Luminosities & Hardness Ratios of X-ray Sources . . . . . 175 5.8 Possible Periodically Variable Sources . . . . . . . . . . . . . . . . . . 200 5.9 KS Test for Intraobservation Variability . . . . . . . . . . . . . . . . . 200 5.10 Possible Flaring Sources in NGC 4697 . . . . . . . . . . . . . . . . . . 203 5.11 Sources Which Vary between Pairs of Observations . . . . . . . . . . 208 5.12 States of Variable X-ray Sources . . . . . . . . . . . . . . . . . . . . . 214 6.1 Galaxy Properties of Sample . . . . . . . . . . . . . . . . . . . . . . . 233 6.2 Properties of Chandra Observations . . . . . . . . . . . . . . . . . . 235 6.3 GC-LMXB Matches by Galaxies . . . . . . . . . . . . . . . . . . . . 240 6.4 Fits of the Expected Number λt of LMXBs per GC . . . . . . . . . . 260 B.1 Optical Properties of Globular Clusters (With LMXBs) . . . . . . . 292 xvii
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: List of Figures 1.1 Hubble Tuning F
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 and 44: Table 2.2. Discrete X-ray Sources i
Page 45 and 46: Table 2.2—Continued Source d Coun
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
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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. Discrete X-ray Sources i
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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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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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