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

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et al. 2001; Kundu et al. 2002); early-type galaxies can provide the large number of GCs containing LMXBs necessary to probe LMXB formation and evolution in GCs. Early samples have shown that GCs that are brighter and redder are more likely to contain LMXBs (e.g. Kundu et al. 2003; Sarazin et al. 2003); however, the use of resolution limited ground-based data or field-of-view (FOV) limited space-based data suppressed the numbers of GCs that could clearly be identified. By observing nearby early-type galaxies with the Hubble Space Telescope Ad- vanced Camera for Surveys (HST-ACS), which has a 3. ′ 2 × 3. ′ 2 FOV and can resolve GCs in nearby galaxies, one can construct accurate and comprehensive lists of GCs. In particular, the measurement of GC size allows better discrimination against un- resolved background sources with GC colors, while providing a GC property that is crucially important to probing the structural parameters of GCs that contain LMXBs. The ACS Virgo Cluster Survey (ACSVCS) has observed the centers of 100 early-type galaxies (Côté et al. 2004) and provides excellent GC data. Some of its initial work ex- plored the GC-LMXB connection in NGC 4486 (M87, Jordán et al. 2004b, hereafter ACSVCS3). In this work, we expand upon this analysis exploring the GC-LMXB connection in 10 ACSVCS galaxies and an additional galaxy observed following the ACSVCS observational setup. We identify 270 GCs that contain LMXBs; this is one of the largest such samples to date, and the largest sample that includes information about GC size. 232
6.2 Sample 6.2.1 Galaxy Sample Table 6.1. Galaxy Properties of Sample Type reff DSBF MB Galaxy (RC3) (arcsec) (Mpc) (mag) (1) (2) (3) (4) (5) NGC 4365 E3 49.8 23.2 -21.46 NGC 4374 E1 51.0 18.7 -21.45 NGC 4382 S0 54.6 17.9 -21.46 NGC 4406 E3 104.0 18.0 -21.56 NGC 4472 E2 104.0 16.8 -21.98 NGC 4486 E0 94.9 15.7 -21.70 NGC 4526 S0 44.4 16.1 -20.60 NGC 4552 E0 29.3 16.1 -20.55 NGC 4621 E5 40.5 15.0 -20.37 NGC 4649 E2 68.7 16.4 -21.39 NGC 4697 E6 72.0 11.3 -20.29 We selected our sample from early-type Virgo galaxies with central detections of LMXBs using CXO and GCs using HST-ACS. Since the most massive galaxies are the most likely to have large populations of both LMXBs and GCs, we concentrated on galaxies with MB < −20.25. Our sample includes the ten brightest ACSVCS galaxies (NGC 4472, 4486, 4406, 4365, 4382, 4374, 4649, 4526, 4552, and 4621) and NGC 4697, a similarly bright galaxy, which we observed with nearly the same setup as the ACSVCS. Table 6.1 summarizes some properties of the galaxies in our 233
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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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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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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
Page 207 and 208: 5.9 Spectral Analysis We performed
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Page 217 and 218: 5.10.1 Intraobservation Variability
Page 219 and 220: Fig. 5.14.— Binned lightcurve usi
Page 221 and 222: Table 5.10. Possible Flaring Source
Page 223 and 224: Fig. 5.16.— Cumulative lightcurve
Page 225 and 226: pairs of observations. In Figure 5.
Page 227 and 228: Table 5.11—Continued Source PL,AB
Page 229 and 230: Fig. 5.17.— Percentage of Analysi
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Page 233 and 234: Table 5.12—Continued Source Obs.S
Page 235 and 236: of states as transient candidates.
Page 237 and 238: Long-Term Hardness Ratio Variabilit
Page 239 and 240: In the final observation, there wer
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Page 249: in the field of the Milky Way and a
Page 253 and 254: Table 6.2. Properties of Chandra Ob
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Page 257 and 258: the QE degradation in the ACIS dete
Page 259 and 260: Table 6.3—Continued Galaxy NX LX,
Page 261 and 262: The positions of the GCs were used
Page 263 and 264: Fig. 6.2.— Scatter plot of GC gal
Page 265 and 266: Fig. 6.3.— Scatter plot of estima
Page 267 and 268: Fig. 6.5.— Scatter plot of estima
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Page 271 and 272: 6.3.1 Luminosity and Mass Prior obs
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Page 281 and 282: Fig. 6.9.— Identical to Figure 6.
Page 283 and 284: We used the indices from our best-f
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Page 289 and 290: Fig. 6.11.— (Left:) Two-dimension
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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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