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

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that v ∝ (Mc/rc) 1/2 ∝ rc ρ 1/2 0 , where Mc is the core mass of the GC. This is a valid assumption as the empirically defined fundamental plane of GCs appears to reproduce this relation (McLaughlin 2000). Then, the encounter rate is typically written as 288 Γ ∝ ρ 3/2 0 r 2 c. (A.3) Since the central densities and core radii of extragalactic GCs are difficult to accurately measure, particularly for those at distances beyond 10 Mpc, it is desirable to recast the encounter rate in terms of the larger scale properties of the cluster. A more easily determined radius is the half-mass radius r ′ h . If r′ h and the total luminosity can be measured, then is is straightforward to determine the average surface mass density within r ′ h , which is σh ≡ (1/2)M/[π(r ′ h )2 ]. Using the dimensionless quantities L = M/ρ0r 3 c and R = r ′ h /rc, we find Γ ∝ R5/2 L 3/2 M 3/2 (r ′ , (A.4) h )5/2 where both L and R depend on the concentration, c = log(rt/rc). If two samples of extragalactic GCs have the same distributions of concentrations, one can compare more easily the following encounter rate parameter, Γh ≡ σ 3/2 h (r ′ h) 1/2 ∝ M 3/2 (r ′ h) −5/2 . (A.5) The GC concentration affects the accuracy of Γh as a proxy for the encounter rate through the quantity R 5/2 L −3/2 . This quantity can be calculated given the polynomial relationships in Appendix B of McLaughlin (2000) that apply over the range 0.5 c 3.6 (Figure A.1). Since R 5/2 L −3/2 varies only between 0.07 and 0.14
Fig. A.1.— Dimensionless quantity R 5/2 L −3/2 as a function of concentration, c, for GCs using the expressions in McLaughlin (2000). This quantity connects estimates of the encounter rate based on core and half-mass radius values, Γ ∝ R 5/2 L −3/2 Γh. The diamonds (non-core-collapse Galactic GCs) and asterisks (core-collapse Galactic GCs) indicate comparisons of Γ and Γh from the February 2003 revision of Harris (1996). The catalog Harris (1996) is based on arbitrarily adopted c = 2.5 for corecollapse Galactic GCs. The use of the large scale encounter rate parameter Γh will underestimate the encounter rate for globular clusters with high concentrations (c 1.6). for 0.5 c 1.6, Γh is a relatively good proxy for the encounter rate Γ over that concentration range. The use of Γh will underestimate the encounter rate in GCs with higher concentrations (c 1.6). 289
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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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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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Page 259 and 260: Table 6.3—Continued Galaxy NX LX,
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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.
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Page 301 and 302: 7.2.1 X-ray Properties of the GC-LM
Page 303 and 304: of the metallicity dependence. As i
Page 305: Appendix A Encounter Rate Parameter
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Table B.2—Continued RA Dec. d GC
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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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