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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 1264 187.71523 12.36441 1.07 −7.318 ± 0.033 −8.308 ± 0.055 3.25 ± 0.26 1.00 NGC 4486 1265 187.71519 12.41326 0.91 −5.141 ± 0.132 −6.783 ± 0.137 4.97 ± 0.58 0.73 NGC 4486 1266 187.71522 12.37015 0.87 −6.486 ± 0.043 −7.493 ± 0.085 2.80 ± 0.44 0.99 NGC 4486 1267 187.71526 12.37031 0.86 −6.853 ± 0.049 −8.399 ± 0.035 2.18 ± 0.35 1.00 NGC 4486 1268 187.71527 12.39727 0.42 −6.616 ± 0.068 −8.271 ± 0.141 2.62 ± 0.59 1.00 NGC 4486 1269 187.71532 12.40035 0.49 −8.789 ± 0.020 −9.820 ± 0.014 2.57 ± 0.14 1.00 NGC 4486 1270 187.71531 12.37586 0.68 −6.209 ± 0.058 −7.535 ± 0.114 2.43 ± 0.40 1.00 NGC 4486 1273 187.71548 12.38337 0.46 −8.376 ± 0.012 −9.734 ± 0.016 1.61 ± 0.17 1.00 NGC 4486 1274 187.71550 12.36903 0.91 −6.741 ± 0.048 −8.261 ± 0.031 1.53 ± 0.23 0.99 NGC 4486 1276 187.71552 12.38680 0.39 −7.438 ± 0.031 −8.790 ± 0.038 1.96 ± 0.19 1.00 NGC 4486 1277 187.71561 12.40023 0.50 −8.944 ± 0.018 −10.394 ± 0.019 2.62 ± 0.15 1.00 NGC 4486 1278 187.71559 12.40131 0.53 −8.188 ± 0.021 −9.330 ± 0.022 3.00 ± 0.14 1.00 NGC 4486 1279 187.71569 12.37617 0.67 −8.449 ± 0.070 −9.398 ± 0.073 7.49 ± 0.47 0.98 NGC 4486 1281 187.71576 12.39380 0.38 −7.278 ± 0.046 −8.359 ± 0.073 3.52 ± 0.34 1.00 NGC 4486 1282 187.71577 12.41269 0.90 −7.726 ± 0.024 −9.064 ± 0.030 3.12 ± 0.21 1.00 NGC 4486 1283 187.71557 12.39252 0.36 −6.784 ± 0.123 −8.373 ± 0.082 2.79 ± 0.43 1.00 NGC 4486 1284 187.71587 12.37923 0.58 −6.501 ± 0.066 −7.660 ± 0.112 3.60 ± 0.39 0.99 NGC 4486 1285 187.71590 12.40010 0.50 −8.043 ± 0.058 −9.516 ± 0.057 5.89 ± 0.38 1.00 NGC 4486 1287 187.71602 12.40714 0.71 −8.943 ± 0.019 −10.538 ± 0.011 2.34 ± 0.11 1.00 NGC 4486 1288 187.71593 12.41237 0.89 −5.113 ± 0.245 −6.415 ± 0.144 1.94 ± 0.55 0.98 NGC 4486 1289 187.71615 12.40865 0.77 −11.108 ± 0.023 −12.160 ± 0.015 5.46 ± 0.12 1.00 NGC 4486 1290 187.71602 12.39399 0.39 −7.255 ± 0.059 −8.383 ± 0.136 5.78 ± 0.91 0.94 NGC 4486 1291 187.71601 12.40843 0.76 −7.236 ± 0.045 −8.413 ± 0.040 3.21 ± 0.21 1.00 NGC 4486 1292 187.71600 12.40546 0.66 −5.764 ± 0.091 −7.336 ± 0.109 2.47 ± 0.47 1.00 NGC 4486 1295 187.71614 12.38107 0.54 −9.503 ± 0.015 −11.028 ± 0.017 2.56 ± 0.09 1.00 NGC 4486 1296 187.71608 12.38612 0.42 −6.667 ± 0.216 −8.248 ± 0.058 1.81 ± 0.30 1.00 NGC 4486 1297 187.71616 12.37982 0.57 −9.312 ± 0.021 −10.468 ± 0.015 2.43 ± 0.21 1.00 NGC 4486 1298 187.71611 12.39264 0.38 −6.952 ± 0.079 −8.286 ± 0.101 3.88 ± 0.43 1.00 NGC 4486 1300 187.71617 12.36663 1.00 −7.962 ± 0.031 −9.408 ± 0.020 1.69 ± 0.12 1.00 NGC 4486 1301 187.71616 12.38251 0.50 −7.458 ± 0.042 −8.317 ± 0.052 3.31 ± 0.29 1.00 NGC 4486 1302 187.71617 12.38041 0.56 −7.955 ± 0.024 −9.350 ± 0.026 1.86 ± 0.13 1.00 NGC 4486 1303 187.71616 12.41861 1.11 −6.698 ± 0.063 −7.738 ± 0.099 3.94 ± 0.51 0.99 NGC 4486 1304 187.71608 12.36848 0.94 −5.967 ± 0.075 −7.085 ± 0.151 3.68 ± 0.64 0.96 NGC 4486 1305 187.71628 12.39031 0.38 −7.278 ± 0.046 −8.196 ± 0.054 2.40 ± 0.31 1.00 NGC 4486 1306 187.71625 12.39193 0.38 −5.682 ± 0.183 −6.541 ± 0.722 1.34 ± 0.46 0.94 NGC 4486 1307 187.71634 12.36346 1.12 −8.221 ± 0.030 −9.669 ± 0.022 1.96 ± 0.20 1.00 NGC 4486 1308 187.71633 12.40969 0.80 −5.362 ± 0.107 −6.003 ± 0.149 2.79 ± 0.49 0.98 NGC 4486 1309 187.71639 12.38708 0.42 −7.303 ± 0.138 −8.554 ± 0.089 1.42 ± 0.25 0.98 NGC 4486 1310 187.71639 12.38875 0.40 −6.926 ± 0.048 −8.267 ± 0.145 4.55 ± 0.78 0.99 NGC 4486 1311 187.71640 12.41506 0.99 −6.427 ± 0.055 −7.240 ± 0.075 4.89 ± 0.29 0.87 NGC 4486 1312 187.71642 12.36732 0.98 −7.659 ± 0.028 −8.631 ± 0.025 2.39 ± 0.16 1.00 NGC 4486 1313 187.71644 12.39951 0.50 −8.315 ± 0.027 −9.783 ± 0.017 2.70 ± 0.17 1.00 NGC 4486 1314 187.71644 12.39999 0.51 −7.088 ± 0.038 −8.540 ± 0.052 3.09 ± 0.24 1.00 NGC 4486 1315 187.71646 12.39979 0.51 −5.783 ± 1.139 −7.228 ± 0.072 2.39 ± 0.59 1.00 NGC 4486 1316 187.71648 12.39279 0.40 −6.253 ± 0.076 −7.778 ± 0.067 2.62 ± 0.34 1.00 NGC 4486 1317 187.71653 12.41362 0.94 −6.445 ± 0.050 −7.717 ± 0.042 1.71 ± 0.27 0.99 NGC 4486 1318 187.71663 12.40203 0.57 −6.220 ± 0.073 −7.279 ± 0.100 2.49 ± 0.42 1.00 NGC 4486 1319 187.71669 12.41409 0.96 −9.835 ± 0.019 −10.982 ± 0.040 6.03 ± 0.17 1.00 NGC 4486 1320 187.71673 12.38954 0.40 −7.253 ± 0.031 −8.779 ± 0.037 2.14 ± 0.19 1.00 NGC 4486 1321 187.71675 12.40843 0.77 −7.840 ± 0.028 −8.852 ± 0.027 2.62 ± 0.16 1.00 NGC 4486 1322 187.71673 12.41615 1.03 −6.428 ± 0.119 −7.499 ± 0.115 4.60 ± 0.57 0.94 NGC 4486 1323 187.71674 12.38210 0.53 −6.051 ± 0.055 −7.444 ± 0.046 2.23 ± 0.29 1.00 NGC 4486 1324 187.71683 12.41136 0.87 −6.748 ± 0.060 −7.689 ± 0.133 5.91 ± 0.81 0.86 NGC 4486 1325 187.71683 12.39333 0.41 −6.407 ± 0.309 −7.661 ± 0.091 5.53 ± 1.97 0.90 NGC 4486 1326 187.71691 12.40276 0.60 −8.285 ± 0.022 −9.695 ± 0.022 2.51 ± 0.18 1.00 NGC 4486 1327 187.71681 12.38400 0.49 −5.247 ± 1.531 −6.628 ± 0.937 0.82 ± 1.20 0.80 NGC 4486 1328 187.71686 12.38429 0.48 −7.524 ± 0.026 −8.609 ± 0.048 2.64 ± 0.19 1.00 NGC 4486 1329 187.71686 12.39096 0.41 −7.843 ± 0.094 −8.919 ± 0.106 4.68 ± 0.52 1.00 NGC 4486 1330 187.71693 12.36446 1.09 −6.876 ± 0.096 −7.881 ± 0.203 3.15 ± 0.43 1.00 NGC 4486 1331 187.71698 12.36972 0.91 −8.603 ± 0.030 −9.562 ± 0.024 3.89 ± 0.14 1.00 NGC 4486 1332 187.71700 12.36326 1.13 −8.164 ± 0.030 −9.423 ± 0.023 3.00 ± 0.21 1.00 NGC 4486 1333 187.71698 12.37563 0.72 −5.185 ± 0.833 −6.702 ± 0.477 1.07 ± 0.75 0.88 Continued on Next Page. . . 360
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 1334 187.71705 12.36453 1.09 −5.759 ± 0.118 −7.058 ± 0.160 3.44 ± 0.87 0.97 NGC 4486 1335 187.71712 12.40321 0.62 −10.469 ± 0.020 −11.978 ± 0.010 2.83 ± 0.11 1.00 NGC 4486 1336 187.71712 12.39915 0.51 −9.033 ± 0.015 −10.353 ± 0.016 2.46 ± 0.10 1.00 NGC 4486 1337 187.71715 12.41599 1.03 −8.258 ± 0.033 −9.644 ± 0.018 2.10 ± 0.13 1.00 NGC 4486 1339 187.71717 12.40116 0.56 −8.679 ± 0.022 −9.640 ± 0.017 2.07 ± 0.17 1.00 NGC 4486 1340 187.71725 12.39691 0.47 −8.113 ± 0.029 −9.334 ± 0.019 2.66 ± 0.12 1.00 NGC 4486 1341 187.71738 12.38633 0.46 −8.055 ± 0.029 −9.260 ± 0.034 1.59 ± 0.19 1.00 NGC 4486 1342 187.71739 12.41260 0.92 −5.342 ± 0.076 −6.928 ± 0.264 1.86 ± 0.51 0.99 NGC 4486 1343 187.71743 12.39509 0.45 −7.064 ± 0.046 −8.544 ± 0.117 4.39 ± 0.69 1.00 NGC 4486 1344 187.71746 12.36969 0.92 −6.439 ± 0.063 −7.820 ± 0.049 2.31 ± 0.35 1.00 NGC 4486 1345 187.71752 12.38536 0.48 −5.932 ± 0.127 −7.405 ± 0.124 4.68 ± 0.61 0.92 NGC 4486 1346 187.71758 12.37908 0.63 −7.026 ± 0.047 −8.208 ± 0.051 2.44 ± 0.29 1.00 NGC 4486 1347 187.71760 12.38237 0.55 −6.743 ± 0.130 −8.221 ± 0.312 1.68 ± 0.37 1.00 NGC 4486 1348 187.71767 12.37758 0.67 −5.676 ± 0.079 −7.111 ± 0.163 2.20 ± 0.31 1.00 NGC 4486 1350 187.71775 12.38029 0.60 −7.181 ± 0.036 −8.598 ± 0.039 1.86 ± 0.21 1.00 NGC 4486 1351 187.71776 12.40084 0.57 −7.470 ± 0.043 −8.847 ± 0.027 2.03 ± 0.19 1.00 NGC 4486 1352 187.71781 12.41446 0.99 −8.878 ± 0.022 −10.299 ± 0.016 2.09 ± 0.11 1.00 NGC 4486 1353 187.71788 12.37986 0.62 −7.404 ± 0.029 −8.747 ± 0.033 2.77 ± 0.19 1.00 NGC 4486 1354 187.71790 12.40814 0.78 −7.365 ± 0.026 −8.787 ± 0.035 2.35 ± 0.13 1.00 NGC 4486 1355 187.71796 12.37805 0.67 −8.792 ± 0.019 −9.850 ± 0.014 2.50 ± 0.12 1.00 NGC 4486 1356 187.71801 12.37753 0.68 −7.663 ± 0.034 −9.181 ± 0.025 3.57 ± 0.15 1.00 NGC 4486 1357 187.71797 12.39471 0.47 −6.596 ± 0.042 −7.683 ± 0.050 2.16 ± 0.28 1.00 NGC 4486 1358 187.71805 12.41744 1.09 −8.113 ± 0.023 −9.475 ± 0.017 3.12 ± 0.13 1.00 NGC 4486 1359 187.71806 12.40351 0.65 −8.023 ± 0.016 −8.835 ± 0.028 2.71 ± 0.15 1.00 NGC 4486 1360 187.71819 12.37450 0.78 −6.116 ± 0.072 −7.117 ± 0.251 2.71 ± 0.41 0.99 NGC 4486 1361 187.71822 12.40938 0.83 −6.580 ± 0.039 −7.752 ± 0.055 2.82 ± 0.30 1.00 NGC 4486 1363 187.71826 12.38516 0.51 −7.230 ± 0.043 −8.197 ± 0.039 2.61 ± 0.25 1.00 NGC 4486 1364 187.71825 12.40537 0.71 −4.856 ± 0.163 −6.678 ± 0.347 2.83 ± 0.59 0.98 NGC 4486 1365 187.71830 12.36811 0.99 −5.170 ± 0.266 −6.404 ± 0.218 4.45 ± 1.82 0.79 NGC 4486 1366 187.71831 12.37831 0.67 −6.377 ± 0.335 −8.047 ± 0.032 1.52 ± 0.35 0.99 NGC 4486 1367 187.71832 12.38536 0.51 −6.586 ± 0.067 −7.648 ± 0.397 2.02 ± 0.31 1.00 NGC 4486 1368 187.71843 12.39392 0.48 −6.665 ± 0.069 −8.200 ± 0.042 1.75 ± 0.34 1.00 NGC 4486 1369 187.71860 12.37167 0.87 −8.738 ± 0.046 −9.781 ± 0.047 3.53 ± 0.43 1.00 NGC 4486 1370 187.71857 12.40253 0.64 −6.169 ± 0.076 −7.488 ± 0.081 2.63 ± 0.38 1.00 NGC 4486 1371 187.71858 12.39414 0.48 −5.076 ± 0.514 −6.869 ± 0.715 2.61 ± 0.88 0.99 NGC 4486 1372 187.71866 12.40617 0.74 −7.870 ± 0.031 −9.192 ± 0.028 2.83 ± 0.16 1.00 NGC 4486 1373 187.71865 12.37886 0.66 −7.986 ± 0.022 −9.095 ± 0.032 2.78 ± 0.21 1.00 NGC 4486 1375 187.71866 12.39309 0.48 −7.259 ± 0.052 −8.369 ± 0.052 3.16 ± 0.22 1.00 NGC 4486 1376 187.71877 12.37207 0.87 −9.461 ± 0.026 −10.388 ± 0.020 3.82 ± 0.12 1.00 NGC 4486 1377 187.71872 12.38509 0.53 −7.254 ± 0.033 −8.296 ± 0.030 2.25 ± 0.22 1.00 NGC 4486 1378 187.71876 12.38888 0.48 −7.046 ± 0.078 −8.330 ± 0.056 2.99 ± 0.47 1.00 NGC 4486 1379 187.71883 12.39466 0.50 −5.538 ± 0.255 −6.273 ± 0.392 3.27 ± 1.67 0.96 NGC 4486 1380 187.71890 12.38412 0.55 −8.385 ± 0.017 −9.973 ± 0.022 3.08 ± 0.14 1.00 NGC 4486 1381 187.71886 12.41024 0.87 −6.934 ± 0.026 −8.315 ± 0.029 2.26 ± 0.21 1.00 NGC 4486 1382 187.71906 12.39873 0.57 −10.156 ± 0.077 −11.039 ± 0.100 6.96 ± 0.64 1.00 NGC 4486 1383 187.71901 12.38494 0.54 −7.785 ± 0.022 −9.249 ± 0.017 1.84 ± 0.12 1.00 NGC 4486 1384 187.71901 12.40015 0.59 −6.590 ± 0.051 −8.011 ± 0.041 1.89 ± 0.33 1.00 NGC 4486 1385 187.71910 12.40286 0.66 −7.308 ± 0.038 −8.196 ± 0.065 4.34 ± 0.24 0.99 NGC 4486 1386 187.71913 12.36801 1.00 −6.758 ± 0.043 −8.313 ± 0.039 2.16 ± 0.22 1.00 NGC 4486 1388 187.71912 12.41508 1.03 −5.373 ± 0.088 −6.932 ± 0.131 2.46 ± 0.51 0.99 NGC 4486 1389 187.71921 12.39515 0.52 −6.968 ± 0.031 −8.642 ± 0.028 2.07 ± 0.17 1.00 NGC 4486 1390 187.71929 12.39217 0.50 −6.990 ± 0.040 −8.198 ± 0.048 2.63 ± 0.24 1.00 NGC 4486 1392 187.71937 12.40066 0.62 −6.983 ± 0.055 −8.455 ± 0.049 2.92 ± 0.24 1.00 NGC 4486 1394 187.71945 12.40347 0.69 −5.721 ± 0.341 −6.862 ± 0.137 4.36 ± 2.37 0.86 NGC 4486 1395 187.71949 12.40136 0.64 −6.159 ± 0.089 −7.021 ± 0.188 3.11 ± 1.26 0.98 NGC 4486 1397 187.71897 12.39322 0.49 −6.570 ± 0.098 −7.487 ± 0.248 4.57 ± 1.59 0.94 NGC 4486 1398 187.71962 12.38113 0.63 −8.341 ± 0.028 −10.000 ± 0.025 2.85 ± 0.22 1.00 NGC 4486 1399 187.71956 12.38672 0.53 −5.148 ± 0.536 −6.566 ± 0.188 3.38 ± 0.85 0.96 NGC 4486 1401 187.71961 12.40137 0.64 −5.677 ± 0.069 −6.732 ± 0.097 2.59 ± 0.39 0.99 NGC 4486 1402 187.71963 12.40255 0.67 −4.997 ± 0.531 −6.214 ± 0.125 1.79 ± 0.97 0.98 NGC 4486 1403 187.71965 12.39658 0.55 −7.828 ± 0.031 −9.188 ± 0.024 2.33 ± 0.16 1.00 NGC 4486 1404 187.71968 12.41854 1.16 −6.327 ± 0.066 −7.230 ± 0.066 2.57 ± 0.30 0.99 Continued on Next Page. . . 361
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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Table B.2. Optical Properties of Gl
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Page 327 and 328: Table B.2—Continued RA Dec. d GC
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Page 421 and 422: investigations into improving the h
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Page 425 and 426: Blanton, E. L., Sarazin, C. L., & I
Page 427 and 428: 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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