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Table B.2—Continued RA Dec. d GC G475 Z850 r h Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class (1) (2) (3) (4) (5) (6) (7) (8) (9) NGC 4486 278 187.69276 12.40219 0.64 −9.741 ± 0.014 −10.717 ± 0.018 3.36 ± 0.09 1.00 NGC 4486 279 187.69275 12.38140 0.61 −7.320 ± 0.035 −8.679 ± 0.034 2.27 ± 0.26 1.00 NGC 4486 281 187.69273 12.40316 0.67 −6.284 ± 0.088 −7.487 ± 0.440 2.32 ± 0.44 1.00 NGC 4486 282 187.69281 12.40580 0.74 −9.966 ± 0.048 −10.875 ± 0.035 6.92 ± 0.22 1.00 NGC 4486 283 187.69284 12.37914 0.66 −8.396 ± 0.017 −9.477 ± 0.024 3.40 ± 0.10 1.00 NGC 4486 284 187.69286 12.37050 0.92 −8.399 ± 0.022 −9.893 ± 0.021 2.46 ± 0.17 1.00 NGC 4486 286 187.69284 12.41184 0.92 −7.542 ± 0.024 −8.521 ± 0.022 2.50 ± 0.22 1.00 NGC 4486 287 187.69291 12.40710 0.77 −8.252 ± 0.015 −9.218 ± 0.024 2.46 ± 0.12 1.00 NGC 4486 288 187.69290 12.39809 0.55 −7.415 ± 0.042 −8.511 ± 0.041 2.83 ± 0.21 1.00 NGC 4486 291 187.69292 12.39098 0.48 −6.355 ± 0.060 −7.597 ± 0.546 1.60 ± 0.41 0.99 NGC 4486 292 187.69301 12.37849 0.68 −5.118 ± 0.361 −6.200 ± 0.488 3.82 ± 2.35 0.92 NGC 4486 293 187.69302 12.40155 0.62 −5.384 ± 0.152 −7.152 ± 0.206 3.57 ± 1.24 0.97 NGC 4486 294 187.69307 12.40965 0.85 −9.252 ± 0.026 −10.041 ± 0.020 3.80 ± 0.12 1.00 NGC 4486 295 187.69309 12.37566 0.76 −6.517 ± 0.063 −7.322 ± 0.062 2.78 ± 0.33 0.99 NGC 4486 296 187.69312 12.38956 0.48 −6.071 ± 0.132 −7.178 ± 0.093 3.78 ± 0.64 0.96 NGC 4486 297 187.69316 12.39110 0.47 −7.693 ± 0.031 −8.761 ± 0.030 1.81 ± 0.20 1.00 NGC 4486 298 187.69320 12.37168 0.88 −7.804 ± 0.031 −8.612 ± 0.027 2.49 ± 0.20 1.00 NGC 4486 299 187.69315 12.40347 0.67 −6.697 ± 0.198 −7.963 ± 0.056 1.95 ± 0.35 1.00 NGC 4486 300 187.69316 12.41158 0.91 −6.792 ± 0.057 −8.452 ± 0.071 2.78 ± 0.40 1.00 NGC 4486 301 187.69327 12.41768 1.11 −9.480 ± 0.026 −10.938 ± 0.012 2.45 ± 0.13 1.00 NGC 4486 302 187.69324 12.38767 0.49 −8.902 ± 0.034 −9.738 ± 0.043 5.04 ± 0.19 1.00 NGC 4486 303 187.69324 12.40898 0.82 −7.202 ± 0.032 −8.742 ± 0.034 2.48 ± 0.23 1.00 NGC 4486 304 187.69328 12.37405 0.80 −7.339 ± 0.031 −8.780 ± 0.032 2.46 ± 0.21 1.00 NGC 4486 305 187.69321 12.39450 0.49 −5.513 ± 0.511 −7.061 ± 0.288 1.29 ± 0.61 0.95 NGC 4486 306 187.69327 12.39515 0.49 −6.501 ± 0.131 −7.699 ± 0.148 5.64 ± 0.96 0.90 NGC 4486 308 187.69333 12.38484 0.52 −6.938 ± 0.036 −7.787 ± 0.102 2.32 ± 0.35 1.00 NGC 4486 310 187.69336 12.41454 1.00 −7.375 ± 0.031 −8.541 ± 0.032 2.68 ± 0.19 1.00 NGC 4486 311 187.69336 12.40067 0.59 −6.507 ± 0.055 −7.365 ± 0.050 2.19 ± 0.31 1.00 NGC 4486 312 187.69339 12.37150 0.88 −6.720 ± 0.039 −7.548 ± 0.291 1.92 ± 0.29 1.00 NGC 4486 313 187.69342 12.36619 1.05 −6.806 ± 0.055 −8.303 ± 0.038 2.84 ± 0.25 1.00 NGC 4486 314 187.69347 12.38353 0.54 −9.688 ± 0.019 −10.810 ± 0.019 1.83 ± 0.14 1.00 NGC 4486 315 187.69344 12.40475 0.69 −6.838 ± 0.047 −8.279 ± 0.028 1.67 ± 0.26 1.00 NGC 4486 316 187.69349 12.38663 0.49 −7.117 ± 0.032 −8.104 ± 0.077 2.29 ± 0.29 1.00 NGC 4486 317 187.69346 12.39958 0.56 −6.257 ± 0.059 −7.753 ± 0.047 2.51 ± 0.28 1.00 NGC 4486 318 187.69349 12.38467 0.52 −6.456 ± 0.054 −7.874 ± 0.067 1.93 ± 0.35 1.00 NGC 4486 319 187.69356 12.36448 1.11 −7.368 ± 0.029 −8.342 ± 0.025 2.73 ± 0.20 1.00 NGC 4486 320 187.69356 12.40010 0.57 −8.967 ± 0.010 −9.787 ± 0.017 2.84 ± 0.08 1.00 NGC 4486 321 187.69354 12.37786 0.68 −6.960 ± 0.027 −8.253 ± 0.036 2.30 ± 0.22 1.00 NGC 4486 322 187.69361 12.39092 0.46 −9.349 ± 0.031 −10.571 ± 0.013 2.12 ± 0.09 1.00 NGC 4486 323 187.69355 12.39239 0.46 −6.517 ± 0.058 −8.053 ± 0.236 4.93 ± 2.48 0.97 NGC 4486 324 187.69362 12.38818 0.47 −8.872 ± 0.020 −9.857 ± 0.021 2.55 ± 0.12 1.00 NGC 4486 328 187.69367 12.39110 0.45 −6.717 ± 0.050 −8.436 ± 0.069 3.07 ± 0.37 1.00 NGC 4486 329 187.69372 12.39216 0.45 −8.083 ± 0.034 −9.468 ± 0.021 2.46 ± 0.14 1.00 NGC 4486 330 187.69369 12.39387 0.47 −5.683 ± 0.091 −7.092 ± 0.107 2.92 ± 0.59 0.99 NGC 4486 331 187.69372 12.39413 0.47 −8.284 ± 0.027 −9.720 ± 0.020 2.74 ± 0.12 1.00 NGC 4486 332 187.69367 12.41037 0.86 −9.058 ± 0.014 −9.988 ± 0.013 2.62 ± 0.10 1.00 NGC 4486 333 187.69368 12.41439 0.99 −5.136 ± 0.093 −6.350 ± 0.556 2.91 ± 1.29 0.98 NGC 4486 334 187.69373 12.39942 0.55 −5.615 ± 0.115 −6.979 ± 0.121 2.41 ± 0.62 0.99 NGC 4486 335 187.69379 12.39555 0.48 −8.978 ± 0.020 −10.325 ± 0.024 2.26 ± 0.15 1.00 NGC 4486 336 187.69377 12.40194 0.61 −7.278 ± 0.044 −8.286 ± 0.029 2.05 ± 0.20 1.00 NGC 4486 337 187.69379 12.39588 0.48 −7.416 ± 0.030 −8.435 ± 0.039 2.41 ± 0.20 1.00 NGC 4486 341 187.69391 12.38182 0.57 −7.497 ± 0.040 −8.964 ± 0.020 2.10 ± 0.16 1.00 NGC 4486 342 187.69393 12.37516 0.75 −7.654 ± 0.038 −9.295 ± 0.021 2.47 ± 0.17 1.00 NGC 4486 343 187.69391 12.40067 0.57 −6.852 ± 0.052 −8.194 ± 0.268 1.84 ± 0.38 1.00 NGC 4486 344 187.69392 12.40148 0.59 −6.872 ± 0.065 −8.444 ± 0.076 3.39 ± 0.47 1.00 NGC 4486 345 187.69393 12.40316 0.64 −7.821 ± 0.021 −8.901 ± 0.035 2.91 ± 0.17 1.00 NGC 4486 346 187.69393 12.37567 0.74 −5.480 ± 0.350 −6.855 ± 0.178 5.51 ± 3.69 0.62 NGC 4486 348 187.69408 12.37697 0.69 −8.974 ± 0.022 −10.402 ± 0.018 2.68 ± 0.09 1.00 NGC 4486 349 187.69406 12.37074 0.89 −8.652 ± 0.020 −9.546 ± 0.027 3.44 ± 0.12 1.00 NGC 4486 350 187.69407 12.39609 0.48 −9.708 ± 0.015 −10.853 ± 0.010 2.57 ± 0.08 1.00 NGC 4486 351 187.69405 12.36929 0.94 −5.924 ± 0.161 −7.411 ± 0.059 5.09 ± 0.83 0.88 NGC 4486 352 187.69406 12.37537 0.74 −6.110 ± 0.083 −7.518 ± 0.108 4.01 ± 0.49 0.97 Continued on Next Page. . . 348
Table B.2—Continued RA Dec. d GC G475 Z850 r h Galaxy ACS ID (deg) (deg) (r eff ) (AB) (AB) (pc) Class (1) (2) (3) (4) (5) (6) (7) (8) (9) NGC 4486 354 187.69411 12.39575 0.47 −8.551 ± 0.016 −9.427 ± 0.034 2.56 ± 0.15 1.00 NGC 4486 355 187.69419 12.38943 0.44 −7.187 ± 0.035 −8.598 ± 0.033 1.82 ± 0.24 1.00 NGC 4486 357 187.69420 12.41572 1.03 −7.356 ± 0.047 −8.371 ± 0.076 6.90 ± 0.42 0.84 NGC 4486 358 187.69425 12.38920 0.44 −7.521 ± 0.027 −8.794 ± 0.032 2.11 ± 0.13 1.00 NGC 4486 359 187.69423 12.38643 0.47 −8.048 ± 0.019 −9.672 ± 0.026 1.60 ± 0.16 1.00 NGC 4486 360 187.69429 12.40655 0.73 −7.143 ± 0.040 −8.561 ± 0.034 2.32 ± 0.16 1.00 NGC 4486 362 187.69429 12.40718 0.75 −6.826 ± 0.042 −8.099 ± 0.056 3.55 ± 0.21 0.99 NGC 4486 363 187.69435 12.41321 0.94 −8.408 ± 0.069 −9.588 ± 0.025 2.30 ± 0.21 1.00 NGC 4486 364 187.69441 12.37609 0.71 −7.617 ± 0.030 −8.703 ± 0.029 2.38 ± 0.16 1.00 NGC 4486 365 187.69452 12.38854 0.43 −6.716 ± 0.067 −7.979 ± 0.060 2.36 ± 0.36 1.00 NGC 4486 366 187.69452 12.40041 0.55 −6.454 ± 0.214 −8.290 ± 0.138 7.11 ± 1.58 0.78 NGC 4486 367 187.69461 12.40046 0.55 −8.712 ± 0.021 −10.154 ± 0.014 2.12 ± 0.10 1.00 NGC 4486 368 187.69459 12.39551 0.45 −6.714 ± 0.055 −8.246 ± 0.039 1.96 ± 0.21 1.00 NGC 4486 369 187.69464 12.37124 0.86 −7.375 ± 0.028 −8.309 ± 0.038 2.94 ± 0.20 1.00 NGC 4486 370 187.69464 12.38022 0.59 −7.685 ± 0.046 −8.652 ± 0.045 3.59 ± 0.28 1.00 NGC 4486 371 187.69467 12.37718 0.67 −7.577 ± 0.024 −8.812 ± 0.026 1.77 ± 0.19 1.00 NGC 4486 372 187.69474 12.38287 0.52 −9.759 ± 0.015 −10.568 ± 0.012 4.01 ± 0.06 1.00 NGC 4486 374 187.69475 12.38094 0.57 −9.351 ± 0.011 −10.309 ± 0.014 2.00 ± 0.11 1.00 NGC 4486 376 187.69480 12.37835 0.64 −6.805 ± 0.047 −8.271 ± 0.036 1.86 ± 0.20 1.00 NGC 4486 377 187.69489 12.37448 0.75 −8.905 ± 0.015 −9.859 ± 0.020 3.29 ± 0.11 1.00 NGC 4486 379 187.69489 12.36464 1.09 −8.712 ± 0.073 −9.364 ± 0.027 3.70 ± 0.28 1.00 NGC 4486 380 187.69498 12.38188 0.54 −6.087 ± 0.069 −7.611 ± 0.121 2.88 ± 0.52 1.00 NGC 4486 382 187.69507 12.40380 0.63 −8.295 ± 0.025 −9.325 ± 0.025 2.34 ± 0.18 1.00 NGC 4486 384 187.69509 12.41742 1.08 −7.276 ± 0.057 −8.527 ± 0.076 5.23 ± 0.36 0.98 NGC 4486 385 187.69516 12.39077 0.40 −7.306 ± 0.043 −8.626 ± 0.027 2.08 ± 0.25 1.00 NGC 4486 386 187.69519 12.39602 0.44 −8.390 ± 0.028 −9.247 ± 0.017 2.33 ± 0.15 1.00 NGC 4486 387 187.69524 12.36700 1.00 −6.279 ± 0.056 −7.984 ± 0.054 2.47 ± 0.31 1.00 NGC 4486 388 187.69525 12.40541 0.67 −7.762 ± 0.019 −9.111 ± 0.019 1.75 ± 0.15 1.00 NGC 4486 389 187.69530 12.38579 0.44 −8.096 ± 0.022 −9.007 ± 0.024 2.31 ± 0.16 1.00 NGC 4486 390 187.69529 12.38718 0.42 −6.300 ± 0.047 −7.752 ± 0.057 2.30 ± 0.35 1.00 NGC 4486 391 187.69531 12.37873 0.61 −5.914 ± 0.082 −7.262 ± 0.051 2.36 ± 0.41 1.00 NGC 4486 392 187.69543 12.40279 0.59 −7.494 ± 0.030 −8.994 ± 0.026 2.20 ± 0.14 1.00 NGC 4486 394 187.69544 12.37781 0.64 −7.210 ± 0.035 −8.596 ± 0.031 2.87 ± 0.22 1.00 NGC 4486 395 187.69541 12.39712 0.45 −6.483 ± 0.064 −7.646 ± 0.065 1.91 ± 0.32 1.00 NGC 4486 396 187.69547 12.38719 0.42 −8.029 ± 0.025 −8.994 ± 0.040 3.06 ± 0.25 1.00 NGC 4486 397 187.69547 12.39994 0.51 −7.396 ± 0.035 −8.699 ± 0.054 3.31 ± 0.32 1.00 NGC 4486 398 187.69554 12.37911 0.60 −8.413 ± 0.030 −9.733 ± 0.020 2.88 ± 0.15 1.00 NGC 4486 400 187.69553 12.40508 0.65 −8.836 ± 0.015 −10.303 ± 0.013 2.06 ± 0.07 1.00 NGC 4486 401 187.69552 12.40832 0.76 −6.002 ± 0.107 −7.074 ± 0.119 3.62 ± 0.59 0.96 NGC 4486 402 187.69556 12.37186 0.83 −7.117 ± 0.031 −8.831 ± 0.025 2.22 ± 0.17 1.00 NGC 4486 403 187.69555 12.39630 0.43 −7.314 ± 0.033 −8.337 ± 0.049 2.84 ± 0.15 1.00 NGC 4486 404 187.69556 12.40596 0.68 −7.023 ± 0.043 −8.298 ± 0.045 2.22 ± 0.29 1.00 NGC 4486 405 187.69563 12.37313 0.78 −6.839 ± 0.081 −8.593 ± 0.062 4.67 ± 0.37 1.00 NGC 4486 406 187.69562 12.36999 0.89 −5.882 ± 0.052 −7.207 ± 0.046 1.63 ± 0.33 0.98 NGC 4486 408 187.69567 12.38919 0.39 −8.432 ± 0.022 −9.547 ± 0.032 2.91 ± 0.20 1.00 NGC 4486 409 187.69568 12.36237 1.16 −7.222 ± 0.047 −8.636 ± 0.032 2.53 ± 0.27 1.00 NGC 4486 410 187.69571 12.39734 0.45 −9.184 ± 0.016 −10.374 ± 0.013 2.14 ± 0.14 1.00 NGC 4486 411 187.69568 12.41200 0.88 −6.243 ± 0.039 −7.873 ± 0.059 2.76 ± 0.28 1.00 NGC 4486 412 187.69573 12.36260 1.15 −5.813 ± 0.074 −6.662 ± 0.088 2.65 ± 0.42 0.99 NGC 4486 414 187.69574 12.40229 0.57 −6.805 ± 0.031 −8.354 ± 0.053 2.72 ± 0.29 1.00 NGC 4486 415 187.69582 12.36601 1.02 −9.063 ± 0.012 −10.636 ± 0.025 2.76 ± 0.11 1.00 NGC 4486 416 187.69582 12.40626 0.69 −8.058 ± 0.025 −8.876 ± 0.023 2.55 ± 0.15 1.00 NGC 4486 417 187.69579 12.39888 0.48 −5.512 ± 0.996 −6.545 ± 0.389 1.23 ± 0.45 0.92 NGC 4486 418 187.69586 12.37676 0.66 −7.597 ± 0.032 −8.804 ± 0.033 2.13 ± 0.27 1.00 NGC 4486 419 187.69586 12.40208 0.56 −8.222 ± 0.030 −9.743 ± 0.025 3.24 ± 0.14 1.00 NGC 4486 420 187.69592 12.39619 0.42 −5.288 ± 0.734 −6.914 ± 0.600 1.86 ± 0.82 0.99 NGC 4486 421 187.69600 12.39993 0.50 −7.765 ± 0.014 −8.783 ± 0.019 1.86 ± 0.19 1.00 NGC 4486 422 187.69600 12.37355 0.76 −7.490 ± 0.028 −8.762 ± 0.025 2.39 ± 0.14 1.00 NGC 4486 424 187.69606 12.38721 0.39 −8.498 ± 0.021 −9.932 ± 0.012 2.17 ± 0.11 1.00 NGC 4486 426 187.69608 12.38489 0.44 −7.212 ± 0.040 −8.475 ± 0.030 2.19 ± 0.29 1.00 NGC 4486 427 187.69609 12.38271 0.48 −6.377 ± 0.074 −7.502 ± 0.142 3.42 ± 0.77 0.99 NGC 4486 428 187.69612 12.41154 0.86 −8.573 ± 0.024 −9.723 ± 0.024 3.22 ± 0.13 1.00 Continued on Next Page. . . 349
Page 1 and 2:
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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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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Page 315 and 316: Table B.2. Optical Properties of Gl
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Page 365: 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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