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

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coding red for soft, green for medium, and blue for hard. A logarithmic intensity scale was chosen to range between total band surface brightnesses of 5 × 10 −7 and 1 × 10 −3 counts arcsec −2 s −1 . In Figure 3.2 we show the corresponding Second Palomar Observatory Sky Survey (POSS II) optical (red) image using a linear gray scale. The field of view is the same as that in Figure 3.1. The largest galaxy near the upper center is NGC 1600 and corresponds to the brightest peak in the diffuse X-ray emission. Another group member, NGC 1603, lies to the east of NGC 1600. The galaxy north of NGC 1600 is the group member NGC 1601. In Figure 3.2 the overlaid regions indicate the positions of the X-ray sources discussed in § 3.4 and listed in Table 3.1. All of the sources with fluxes determined to more than 3 σ (squares) are clearly seen in the adaptively smoothed X-ray image (Fig. 3.1), except for the central three sources, which are embedded in strong diffuse emission. Very few of the weaker sources can be seen in Figure 3.1. The diffuse X-ray emission in Figure 3.1 shows several interesting structures. The central X-ray emission of NGC 1600 is elongated in a direction that is roughly aligned with the optical emission. However, there are some structures in the central X-ray emission, which are discussed below (§ 3.5.1). The emission around the elliptical galaxy NGC 1603 in the east appears somewhat extended, and there is a bridge of X-ray emission extending from NGC 1603 in the west toward NGC 1600. There is an X-ray source associated with the lenticular galaxy NGC 1601, but it is unclear whether it is extended in this image. On larger scales, there is a slightly elongated region of very extended X-ray surface brightness, with excess diffuse emission, to the northeast of NGC 1600. (Adaptively smoothed images with the sources replaced by Poisson noise do not affect the gross morphology of the diffuse X-ray emission; that 66
02:00.0 03:00.0 04:00.0 05:00.0 06:00.0 07:00.0 08:00.0 09:00.0 -5:10:00.0 55.0 50.0 45.0 4:31:40.0 35.0 30.0 25.0 Fig. 3.1.— Adaptively smoothed Chandra true-color S3 image (for 0.3–1 keV [red], 1–2 keV [green], 2–6 keV [blue]) of NGC 1600, corrected for exposure and background. The total intensity scale is logarithmic and ranges from 5 × 10 −7 to 1 × 10 −3 counts arcsec −2 s −1 . The surrounding white square is the field of view of the Chandra S3 image. 67
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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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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 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: used for spectroscopic analysis. We
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
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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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