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

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87 was near the limit of the S/N in Paper II. It was not detected in the individual reanalysis of Observation 0784, even when detections were made in the 0.3–10 keV range to match Paper II. 5.5.2 HST-ACS Identifications In our HST-ACS observation, we placed the center of NGC 4697 ∼ 20 ′′ from the center of the ACS FOV to avoid a chip boundary. Within this FOV, we can identify optical sources and separate out the GCs using a combination of magnitude, color, and spatial extent. This method is discussed in detail in Jordán et al. (2004a) and Jordán et al. (2006, in preparation). Out of 703 optical sources, there are 298 GCs. We registered the HST observation to the Chandra observation using all 703 optical sources detected by KINGPHOT. Through cross-correlation techniques, we determined that the HST coordinates required astrometric shifts of −0. ′′ 27 in R.A. and −0. ′′ 42 in Dec. Based on singly matched sources within 1 ′′ , we estimate a rel- ative astrometric error of 0. ′′ 21 and 0. ′′ 25 in R.A. and Dec., respectively, or 0. ′′ 32 in quadrature. Since most of these matches occur close to the X-ray pointing center, it is not surprising that this astrometric error is slightly smaller than the astrometric error derived from ground-based catalogs. After correcting the astrometry, we determined that the ACS FOV covers X-ray Sources 1–67, 69–87, 89, 94, and 108. Due to a prominent elliptical dust feature (≈ 7.0 ′′ × 1.7 ′′ or ≈ 384 pc × 93 pc), we did not attempt to detect optical sources in the region of X-ray Sources 1–5 and 8. X-ray Source 68 falls in the chip boundary. Adopting a search radius of 1 ′′ , we find 42 optical counterparts to 39 X-ray sources; three X-ray sources have two candidate optical counterparts within 1 ′′ . Thirty-three of the X-ray sources are associated with a single GC counterpart, while one X-ray source is likely to be associated with one of 156
two potential GC counterparts. We list the optical properties of the matched sources in Table 5.3. By randomizing the P.A. of a source list, assuming both a circular profile and a profile matching the galaxy’s elliptical isophotes, we have determined the percentage of false matches within a given radius. Randomizing the optical source list, we find that ≈ 6.8% of X-ray sources without a physically associated optical source will have a false optical match within 1 ′′ . This is consistent with only 3/39 of the X-ray/optical matches being false. If one considers only the GCs, ≈ 4.2% of X-ray sources will have a false match. This is consistent with only 2/34 of the X-ray/GC matches being false. Finally, comparing the optical source list to itself suggests that ≈ 1.8 X-ray sources will be matched to two optical sources within 1 ′′ by chance; we find three such matches. 157
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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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Page 129 and 130: Fig. 3.13.— Estimated gas and gra
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Page 135 and 136: (HMXBs). LMC X-4, an HMXB pulsar, h
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Page 139 and 140: with NGC 4697. Columns (1)-(4) list
Page 141 and 142: duration, ∆tflat, beginning at a
Page 143 and 144: the uncertainties quoted do not inc
Page 145 and 146: to persistent rate for short flares
Page 147 and 148: Chapter 5 Multi-Epoch Chandra X-ray
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Page 151 and 152: luminous (MB < −20) elliptical (E
Page 153 and 154: Although Chandra is known to encoun
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Page 157 and 158: Fig. 5.3.— Adaptively smoothed Ch
Page 159 and 160: 1 × 10 −5 count s −1 arcsec
Page 161 and 162: Table 5.1—Continued Source R.A. D
Page 167 and 168: source list against which to regist
Page 169 and 170: ate from Observation 0784 alone (Pa
Page 171 and 172: Table 5.2. : Optical Properties of
Page 173: actually be an AGN. Sources 79, 80,
Page 177 and 178: Table 5.3—Continued X-ray Source
Page 179 and 180: Fig. 5.6.— Color (G475−Z850) -
Page 181 and 182: mass segregation of GCs with the sa
Page 183 and 184: Table 5.4. Fits to the Expected Num
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Page 187 and 188: NGC 4697 to convert the observed so
Page 189 and 190: Table 5.6—Continued Source LA LB
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Page 193 and 194: Table 5.7. Combined Luminosities &
Page 195 and 196: Table 5.7—Continued Source Not De
Page 197 and 198: 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
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Page 221 and 222: Table 5.10. Possible Flaring Source
Page 223 and 224: 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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