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

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02:00 03:00 04:00 05:00 06:00 07:00 08:00 09:00 -5:10:00 71 60 59 40 17 18 23 13 8 7 10 55 4:31:50 45 4:31:40 35 4:31:30 25 Fig. 3.2.— Linear gray scale POSS II red optical image of NGC 1600. The squares and circles indicate the positions of the X-ray sources with S/N> 3 and S/N< 3 in Table 3.1, respectively. Sources mentioned in the text are labeled. The surrounding dark square is the field of view of the Chandra S3 image. 2 24 3 1 33 52 30 42 36 50 63 58 68
Table 3.1. Discrete X-ray Sources in NGC 1600 d a Count Rate Source Name R.A. Decl. (arcsec) (arcsec) (10 −4 s −1 ) S/N LX H21 0 H31 0 H32 0 Notes (1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13) 1 ....... CXOU J043139.8−050511 04 31 39.88 −05 05 11.4 0.9 1.0 38.91±3.10 12.55 160.3 −0.50 +0.11 −0.09 −0.96 +0.09 −0.03 −0.88 +0.22 −0.08 a,b,d,e 2 ....... CXOU J043140.0−050504 04 31 40.05 −05 05 04.7 6.4 6.5 15.00±1.94 7.75 61.8 −0.29 +0.25 −0.21 −0.88 +0.24 −0.09 −0.78 +0.36 −0.15 a,b 3 ....... CXOU J043139.7−050456 04 31 39.71 −05 04 56.6 14.1 15.5 7.31±1.42 5.16 30.1 −0.48 +0.28 −0.21 −0.91 +0.43 −0.08 −0.77 +0.77 −0.20 a,b 4 ....... CXOU J043138.1−050456 04 31 38.15 −05 04 56.9 29.0 42.3 1.78±0.70 2.55 7.3 −0.80 +1.09 −0.19 −0.67 +0.63 −0.25 +0.27 +0.67 −1.11 · · · 5 ....... CXOU J043140.1−050540 04 31 40.15 −05 05 40.7 30.6 33.2 4.26±1.05 4.05 17.5 −0.78 +0.66 −0.18 −0.48 +0.36 −0.25 +0.47 +0.42 −0.87 · · · 6 ....... CXOU J043139.7−050436 04 31 39.75 −05 04 36.3 34.2 36.1 1.55±0.65 2.37 6.4 +0.62 +0.36 −1.41 −0.22 +1.18 −0.76 −0.74 +0.98 −0.23 e 7 ....... CXOU J043138.3−050536 04 31 38.30 −05 05 36.7 35.2 39.2 7.48±1.35 5.52 30.8 +0.30 +0.33 −0.42 +0.12 +0.38 −0.42 −0.18 +0.24 −0.22 · · · 8 ....... CXOU J043141.2−050543 04 31 41.23 −05 05 43.0 38.4 49.1 4.77±1.10 4.33 19.7 −0.42 +0.34 −0.25 −0.67 +0.34 −0.19 −0.35 +0.47 −0.34 e 9 ....... CXOU J043137.3−050457 04 31 37.33 −05 04 57.2 40.2 59.4 3.48±0.93 3.73 14.3 −0.26 +0.41 −0.34 −0.67 +0.50 −0.23 −0.50 +0.57 −0.33 · · · 10...... CXOU J043139.8−050552 04 31 39.84 −05 05 52.3 41.9 43.4 8.32±1.42 5.87 34.3 −0.72 +0.17 −0.11 −0.86 +0.17 −0.08 −0.39 +0.48 −0.33 f 11...... CXOU J043137.3−050536 04 31 37.31 −05 05 36.0 46.0 56.6 1.43±0.61 2.36 5.9 −0.72 +1.05 −0.25 −0.50 +0.75 −0.37 +0.35 +0.59 −1.09 · · · 12...... CXOU J043141.9−050550 04 31 41.99 −05 05 50.8 51.3 68.0 2.03±0.73 2.78 8.4 +0.25 +0.50 −0.68 −0.65 +1.16 −0.32 −0.78 +0.93 −0.20 · · · 13...... CXOU J043141.5−050421 04 31 41.50 −05 04 21.0 55.1 56.3 1.52±0.63 2.40 6.3 +0.06 +0.62 −0.66 −1.00 +0.66 −0.00 −1.00 +0.59 −0.00 e 14...... CXOU J043139.8−050407 04 31 39.81 −05 04 07.1 63.4 66.1 3.65±0.94 3.90 15.0 −0.15 +0.42 −0.37 −0.53 +0.49 −0.29 −0.40 +0.48 −0.33 · · · 15...... CXOU J043136.0−050542 04 31 36.04 −05 05 42.2 65.5 83.2 1.66±0.65 2.56 6.9 −0.27 +0.91 −0.60 +0.01 +0.71 −0.72 +0.28 +0.51 −0.73 · · · 16...... CXOU J043135.1−050502 04 31 35.17 −05 05 02.6 70.7 103.9 9.47±1.51 6.26 39.0 −0.25 +0.22 −0.20 −0.61 +0.23 −0.16 −0.43 +0.27 −0.21 f 17...... CXOU J043143.2−050411 04 31 43.27 −05 04 11.3 78.0 86.3 5.49±1.18 4.63 22.6 −0.48 +0.24 −0.18 −1.00 +0.12 −0.00 −1.00 +0.33 −0.00 f 18...... CXOU J043145.0−050511 04 31 45.09 −05 05 11.1 78.0 113.5 1.66±0.65 2.54 6.8 −0.47 +0.59 −0.34 −0.81 +0.91 −0.17 −0.54 +1.12 −0.41 d 19...... CXOU J043145.0−050438 04 31 45.06 −05 04 38.1 84.0 111.0 1.24±0.56 2.20 5.1 −0.35 +0.87 −0.51 −0.40 +0.88 −0.47 −0.06 +0.77 −0.70 · · · 20...... CXOU J043139.9−050339 04 31 39.93 −05 03 39.2 91.3 94.6 1.48±0.60 2.45 6.1 −0.02 +0.89 −0.86 +0.26 +0.65 −1.00 +0.28 +0.51 −0.73 · · · 21...... CXOU J043134.2−050431 04 31 34.25 −05 04 31.1 92.7 136.0 5.54±1.15 4.82 22.8 −0.72 +0.22 −0.13 −0.95 +0.36 −0.04 −0.73 +1.00 −0.24 f 22...... CXOU J043143.6−050627 04 31 43.65 −05 06 27.6 95.6 125.5 3.75±0.97 3.85 15.5 +0.16 +0.54 −0.65 +0.04 +0.59 −0.62 −0.11 +0.40 −0.37 · · · 23...... CXOU J043141.7−050336 04 31 41.78 −05 03 36.9 97.9 97.9 2.73±0.83 3.30 11.2 −0.47 +0.67 −0.37 −0.60 +0.69 −0.30 −0.18 +0.75 −0.59 d 24...... CXOU J043141.2−050654 04 31 41.25 −05 06 54.3 105.8 117.5 2.80±0.82 3.43 11.5 +0.01 +0.61 −0.62 −0.16 +0.69 −0.56 −0.17 +0.51 −0.43 e 25...... CXOU J043141.6−050653 04 31 41.61 −05 06 53.5 106.3 120.4 12.63±1.71 7.38 52.0 +0.41 +0.25 −0.34 +0.36 +0.27 −0.34 −0.05 +0.17 −0.17 f 26...... CXOU J043132.6−050513 04 31 32.61 −05 05 13.1 108.5 156.9 1.52±0.62 2.46 6.3 −0.61 +0.83 −0.32 −0.59 +0.73 −0.31 +0.03 +0.76 −0.80 · · · Continued on Next Page. . . 69
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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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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
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: 02:00.0 03:00.0 04:00.0 05:00.0 06:
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
Page 97 and 98: chip. The number of ULX candidates
Page 99 and 100: these luminosities among previously
Page 101 and 102: to 2-6 keV. Since the 6-10 keV rang
Page 103 and 104: absorption and varying power-law in
Page 105 and 106: counts occur within ∼ 4 ks. Sourc
Page 107 and 108: log I X (counts/sec/arcmin 2 ) 0.5
Page 109 and 110: tion), and βouter = 0.36 +0.01 −
Page 111 and 112: the east and northeast of NGC 1600.
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
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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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