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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 1405 187.71982 12.40643 0.78 −10.946 ± 0.022 −12.157 ± 0.023 6.27 ± 0.14 1.00 NGC 4486 1407 187.71971 12.41668 1.10 −6.838 ± 0.040 −8.118 ± 0.035 1.73 ± 0.19 1.00 NGC 4486 1408 187.71979 12.38811 0.53 −5.318 ± 0.539 −6.943 ± 0.182 0.81 ± 0.50 0.76 NGC 4486 1409 187.71981 12.38906 0.52 −5.772 ± 0.064 −7.003 ± 0.386 2.86 ± 0.49 0.99 NGC 4486 1412 187.71973 12.41747 1.12 −8.512 ± 0.036 −9.460 ± 0.026 1.88 ± 0.31 1.00 NGC 4486 1414 187.71997 12.41011 0.89 −7.538 ± 0.030 −9.047 ± 0.022 1.70 ± 0.16 1.00 NGC 4486 1415 187.71999 12.40187 0.66 −5.610 ± 0.143 −7.105 ± 0.167 2.59 ± 0.83 0.99 NGC 4486 1416 187.72002 12.36701 1.05 −5.889 ± 0.081 −7.740 ± 0.155 4.02 ± 0.92 0.98 NGC 4486 1417 187.72009 12.39010 0.53 −7.332 ± 0.044 −8.810 ± 0.022 1.98 ± 0.18 1.00 NGC 4486 1418 187.72017 12.41257 0.97 −9.714 ± 0.027 −10.622 ± 0.027 3.20 ± 0.15 1.00 NGC 4486 1419 187.72013 12.36423 1.15 −7.791 ± 0.024 −9.048 ± 0.022 2.19 ± 0.12 1.00 NGC 4486 1420 187.72012 12.40781 0.82 −5.728 ± 0.157 −6.502 ± 0.665 2.33 ± 0.67 0.99 NGC 4486 1421 187.72012 12.37485 0.81 −6.230 ± 0.053 −7.362 ± 0.088 2.43 ± 0.37 1.00 NGC 4486 1422 187.72012 12.39881 0.60 −5.614 ± 0.115 −6.495 ± 0.368 2.44 ± 0.59 0.99 NGC 4486 1423 187.72017 12.37059 0.94 −7.488 ± 0.025 −8.638 ± 0.033 2.29 ± 0.21 1.00 NGC 4486 1424 187.72013 12.38255 0.62 −5.667 ± 0.086 −7.390 ± 0.124 2.44 ± 0.51 1.00 NGC 4486 1426 187.72020 12.38987 0.53 −6.532 ± 0.069 −7.553 ± 0.088 2.66 ± 0.50 1.00 NGC 4486 1427 187.72018 12.39516 0.55 −6.754 ± 0.089 −7.289 ± 0.035 2.07 ± 0.25 1.00 NGC 4486 1428 187.72038 12.37422 0.84 −10.161 ± 0.029 −11.133 ± 0.021 4.91 ± 0.14 0.98 NGC 4486 1429 187.72023 12.37484 0.81 −6.763 ± 0.033 −7.549 ± 0.057 3.48 ± 0.22 0.99 NGC 4486 1430 187.72034 12.40067 0.65 −7.364 ± 0.029 −8.371 ± 0.041 2.60 ± 0.16 1.00 NGC 4486 1431 187.72035 12.40533 0.76 −7.304 ± 0.031 −8.640 ± 0.032 2.54 ± 0.17 1.00 NGC 4486 1432 187.72042 12.37666 0.77 −7.549 ± 0.041 −8.655 ± 0.052 3.35 ± 0.34 1.00 NGC 4486 1433 187.72052 12.36561 1.11 −6.878 ± 0.049 −8.260 ± 0.041 2.65 ± 0.23 1.00 NGC 4486 1434 187.72052 12.38598 0.57 −7.328 ± 0.040 −8.327 ± 0.108 4.45 ± 0.51 0.99 NGC 4486 1435 187.72052 12.39401 0.55 −7.063 ± 0.027 −8.279 ± 0.031 1.88 ± 0.18 1.00 NGC 4486 1436 187.72053 12.38228 0.64 −6.693 ± 0.088 −8.178 ± 0.025 1.28 ± 0.24 0.97 NGC 4486 1437 187.72056 12.39697 0.59 −5.672 ± 0.078 −6.679 ± 0.121 2.80 ± 0.40 0.98 NGC 4486 1438 187.72060 12.40102 0.66 −6.526 ± 0.090 −7.912 ± 0.036 1.84 ± 0.38 1.00 NGC 4486 1440 187.72069 12.40433 0.74 −9.123 ± 0.013 −10.033 ± 0.013 2.80 ± 0.12 1.00 NGC 4486 1441 187.72077 12.40660 0.80 −7.577 ± 0.022 −9.236 ± 0.017 2.07 ± 0.11 1.00 NGC 4486 1443 187.72077 12.39093 0.55 −6.713 ± 0.189 −7.956 ± 0.113 6.58 ± 1.20 0.78 NGC 4486 1444 187.72078 12.39288 0.55 −7.775 ± 0.028 −9.293 ± 0.026 2.46 ± 0.15 1.00 NGC 4486 1447 187.72087 12.40546 0.78 −7.479 ± 0.021 −8.998 ± 0.020 2.23 ± 0.11 1.00 NGC 4486 1448 187.72095 12.41495 1.06 −7.134 ± 0.036 −8.182 ± 0.035 2.05 ± 0.22 1.00 NGC 4486 1449 187.72097 12.38221 0.65 −5.399 ± 0.266 −7.215 ± 0.461 5.31 ± 11.59 0.80 NGC 4486 1450 187.72103 12.38608 0.59 −8.033 ± 0.021 −9.506 ± 0.025 2.44 ± 0.18 1.00 NGC 4486 1451 187.72107 12.41453 1.05 −8.592 ± 0.023 −9.406 ± 0.029 2.95 ± 0.16 1.00 NGC 4486 1452 187.72075 12.39683 0.59 −9.229 ± 0.020 −10.536 ± 0.012 2.59 ± 0.12 1.00 NGC 4486 1453 187.72109 12.41652 1.12 −6.757 ± 0.062 −7.887 ± 0.083 3.54 ± 0.48 0.99 NGC 4486 1454 187.72115 12.40714 0.83 −6.251 ± 0.099 −7.538 ± 0.087 3.32 ± 0.37 0.99 NGC 4486 1455 187.72115 12.39355 0.57 −7.217 ± 0.026 −8.631 ± 0.288 1.25 ± 0.21 0.96 NGC 4486 1456 187.72126 12.39379 0.58 −9.143 ± 0.017 −10.405 ± 0.010 2.79 ± 0.07 1.00 NGC 4486 1457 187.72138 12.39380 0.58 −8.056 ± 0.024 −9.270 ± 0.019 2.09 ± 0.16 1.00 NGC 4486 1458 187.72119 12.38949 0.57 −6.778 ± 0.034 −8.251 ± 0.044 2.67 ± 0.22 1.00 NGC 4486 1459 187.72122 12.37964 0.71 −6.485 ± 0.059 −7.617 ± 0.071 3.46 ± 0.33 0.99 NGC 4486 1460 187.72125 12.37277 0.90 −7.030 ± 0.031 −8.561 ± 0.033 2.03 ± 0.19 1.00 NGC 4486 1461 187.72127 12.39903 0.64 −6.944 ± 0.079 −8.145 ± 0.047 3.11 ± 0.41 1.00 NGC 4486 1462 187.72127 12.41592 1.10 −7.548 ± 0.024 −9.058 ± 0.049 3.39 ± 0.29 1.00 NGC 4486 1463 187.72132 12.40734 0.84 −8.767 ± 0.023 −9.833 ± 0.022 2.25 ± 0.19 1.00 NGC 4486 1464 187.72135 12.40144 0.69 −6.507 ± 0.092 −7.142 ± 0.370 5.95 ± 3.66 0.65 NGC 4486 1466 187.72157 12.40288 0.73 −6.057 ± 0.082 −7.537 ± 0.105 2.30 ± 0.60 1.00 NGC 4486 1467 187.72159 12.40837 0.87 −7.581 ± 0.023 −8.804 ± 0.027 2.55 ± 0.12 1.00 NGC 4486 1469 187.72166 12.37145 0.95 −6.571 ± 0.035 −8.027 ± 0.026 1.72 ± 0.28 0.99 NGC 4486 1470 187.72168 12.39370 0.59 −7.021 ± 0.049 −8.365 ± 0.050 2.12 ± 0.24 1.00 NGC 4486 1472 187.72170 12.41549 1.09 −6.910 ± 0.030 −8.283 ± 0.029 1.84 ± 0.22 1.00 NGC 4486 1473 187.72170 12.39155 0.58 −6.767 ± 0.047 −8.113 ± 0.029 2.30 ± 0.29 1.00 NGC 4486 1474 187.72174 12.40668 0.83 −7.586 ± 0.033 −8.671 ± 0.029 2.65 ± 0.22 1.00 NGC 4486 1475 187.72175 12.37846 0.76 −7.800 ± 0.026 −8.923 ± 0.030 2.73 ± 0.16 1.00 NGC 4486 1476 187.72179 12.39513 0.61 −8.099 ± 0.026 −9.021 ± 0.030 2.55 ± 0.22 1.00 NGC 4486 1477 187.72177 12.40852 0.88 −6.746 ± 0.050 −7.587 ± 0.063 3.92 ± 0.34 0.98 NGC 4486 1478 187.72183 12.36983 1.00 −6.516 ± 0.105 −7.299 ± 0.056 3.85 ± 0.42 0.97 Continued on Next Page. . . 362
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 1479 187.72189 12.38182 0.69 −6.549 ± 0.059 −7.936 ± 0.058 2.97 ± 0.33 1.00 NGC 4486 1481 187.72186 12.40247 0.73 −6.595 ± 0.039 −8.191 ± 0.040 1.95 ± 0.27 1.00 NGC 4486 1482 187.72194 12.39505 0.61 −6.356 ± 0.091 −7.917 ± 0.086 3.72 ± 0.45 0.99 NGC 4486 1483 187.72202 12.40157 0.72 −9.036 ± 0.014 −10.170 ± 0.017 2.58 ± 0.07 1.00 NGC 4486 1484 187.72196 12.40850 0.89 −6.336 ± 0.076 −7.909 ± 0.050 1.95 ± 0.33 1.00 NGC 4486 1485 187.72217 12.39161 0.60 −7.004 ± 0.039 −8.334 ± 0.016 2.21 ± 0.27 1.00 NGC 4486 1486 187.72220 12.37812 0.78 −7.000 ± 0.044 −8.309 ± 0.031 2.26 ± 0.27 1.00 NGC 4486 1487 187.72193 12.40881 0.90 −6.982 ± 0.046 −8.732 ± 0.023 1.96 ± 0.21 1.00 NGC 4486 1488 187.72218 12.38101 0.71 −5.686 ± 0.079 −7.000 ± 0.359 5.98 ± 3.84 0.59 NGC 4486 1489 187.72217 12.38251 0.68 −5.992 ± 0.059 −7.093 ± 0.067 2.53 ± 0.35 0.99 NGC 4486 1490 187.72223 12.38265 0.68 −7.991 ± 0.049 −8.828 ± 0.258 2.05 ± 0.33 1.00 NGC 4486 1491 187.72221 12.41105 0.97 −5.202 ± 0.575 −7.012 ± 0.070 1.86 ± 0.66 0.99 NGC 4486 1493 187.72223 12.37839 0.77 −4.810 ± 0.488 −6.055 ± 0.182 2.09 ± 0.68 0.99 NGC 4486 1494 187.72231 12.40008 0.70 −7.141 ± 0.041 −8.754 ± 0.038 3.56 ± 0.17 1.00 NGC 4486 1495 187.72231 12.38757 0.62 −7.055 ± 0.088 −8.379 ± 0.100 4.40 ± 0.60 1.00 NGC 4486 1496 187.72235 12.40565 0.82 −9.190 ± 0.018 −10.505 ± 0.015 2.40 ± 0.10 1.00 NGC 4486 1497 187.72235 12.38046 0.73 −5.970 ± 1.388 −7.514 ± 0.109 1.78 ± 0.34 0.99 NGC 4486 1498 187.72238 12.36886 1.04 −5.283 ± 0.085 −6.833 ± 0.098 1.86 ± 0.55 0.99 NGC 4486 1499 187.72252 12.40261 0.75 −8.769 ± 0.018 −9.826 ± 0.017 2.44 ± 0.09 1.00 NGC 4486 1500 187.72255 12.36575 1.14 −5.936 ± 0.097 −7.494 ± 0.125 6.15 ± 0.90 0.75 NGC 4486 1501 187.72254 12.39228 0.62 −7.075 ± 0.089 −7.685 ± 0.126 4.43 ± 0.49 0.96 NGC 4486 1502 187.72254 12.40119 0.72 −5.835 ± 0.556 −7.213 ± 0.051 1.08 ± 0.42 0.91 NGC 4486 1504 187.72272 12.40652 0.85 −5.188 ± 0.188 −6.237 ± 0.193 4.95 ± 0.94 0.71 NGC 4486 1507 187.72282 12.37580 0.85 −8.665 ± 0.021 −10.035 ± 0.022 3.16 ± 0.14 1.00 NGC 4486 1508 187.72285 12.39377 0.64 −7.156 ± 0.029 −8.446 ± 0.052 2.77 ± 0.31 1.00 NGC 4486 1509 187.72287 12.38866 0.63 −6.409 ± 0.046 −7.801 ± 0.068 2.25 ± 0.35 1.00 NGC 4486 1510 187.72292 12.39730 0.67 −7.423 ± 0.063 −8.727 ± 0.099 8.11 ± 0.81 0.85 NGC 4486 1512 187.72305 12.38114 0.74 −8.133 ± 0.022 −9.003 ± 0.021 2.51 ± 0.12 1.00 NGC 4486 1513 187.72303 12.37080 1.00 −6.330 ± 0.055 −7.856 ± 0.081 2.74 ± 0.37 1.00 NGC 4486 1514 187.72312 12.36381 1.22 −8.709 ± 0.021 −10.189 ± 0.030 2.23 ± 0.13 1.00 NGC 4486 1516 187.72310 12.39204 0.64 −7.538 ± 0.028 −8.480 ± 0.045 2.94 ± 0.21 1.00 NGC 4486 1517 187.72316 12.39841 0.70 −7.953 ± 0.028 −9.330 ± 0.036 2.65 ± 0.26 1.00 NGC 4486 1518 187.72315 12.40283 0.78 −8.953 ± 0.019 −10.053 ± 0.018 3.22 ± 0.19 1.00 NGC 4486 1521 187.72318 12.38054 0.75 −7.626 ± 0.042 −8.535 ± 0.050 4.22 ± 0.32 1.00 NGC 4486 1522 187.72319 12.36832 1.08 −7.417 ± 0.031 −8.649 ± 0.028 2.57 ± 0.16 1.00 NGC 4486 1523 187.72330 12.38929 0.65 −8.714 ± 0.024 −10.241 ± 0.020 2.49 ± 0.16 1.00 NGC 4486 1524 187.72329 12.39982 0.72 −8.207 ± 0.037 −9.040 ± 0.032 4.61 ± 0.14 1.00 NGC 4486 1525 187.72310 12.41775 1.19 −4.803 ± 0.173 −6.508 ± 0.203 3.66 ± 1.09 0.93 NGC 4486 1526 187.72330 12.41628 1.15 −8.706 ± 0.025 −9.720 ± 0.017 2.29 ± 0.12 1.00 NGC 4486 1527 187.72339 12.39014 0.65 −6.777 ± 0.058 −7.706 ± 0.074 3.43 ± 0.33 0.99 NGC 4486 1528 187.72346 12.40376 0.81 −9.051 ± 0.018 −10.153 ± 0.022 2.33 ± 0.14 1.00 NGC 4486 1530 187.72341 12.39221 0.65 −5.136 ± 0.200 −6.176 ± 1.130 1.39 ± 1.05 0.95 NGC 4486 1531 187.72350 12.40796 0.91 −7.579 ± 0.029 −9.211 ± 0.013 1.73 ± 0.16 1.00 NGC 4486 1532 187.72351 12.40302 0.79 −7.921 ± 0.016 −8.993 ± 0.023 2.02 ± 0.20 1.00 NGC 4486 1533 187.72356 12.39748 0.70 −8.972 ± 0.016 −10.097 ± 0.013 2.07 ± 0.09 1.00 NGC 4486 1534 187.72352 12.41369 1.08 −5.609 ± 0.112 −6.900 ± 0.140 3.80 ± 0.67 0.94 NGC 4486 1535 187.72354 12.41833 1.22 −7.154 ± 0.037 −7.933 ± 0.049 2.84 ± 0.26 1.00 NGC 4486 1536 187.72360 12.38901 0.66 −7.770 ± 0.018 −9.137 ± 0.020 1.94 ± 0.14 1.00 NGC 4486 1537 187.72363 12.37214 0.97 −6.002 ± 0.093 −7.569 ± 0.083 3.37 ± 0.50 0.99 NGC 4486 1538 187.72368 12.39507 0.67 −8.064 ± 0.025 −9.329 ± 0.029 2.98 ± 0.18 1.00 NGC 4486 1539 187.72367 12.39284 0.66 −7.620 ± 0.036 −8.408 ± 0.055 2.95 ± 0.21 1.00 NGC 4486 1540 187.72376 12.41318 1.07 −8.565 ± 0.018 −9.453 ± 0.030 3.86 ± 0.10 1.00 NGC 4486 1541 187.72377 12.41281 1.06 −7.819 ± 0.020 −8.732 ± 0.042 2.94 ± 0.22 1.00 NGC 4486 1542 187.72380 12.40471 0.84 −8.152 ± 0.027 −9.777 ± 0.019 2.13 ± 0.12 1.00 NGC 4486 1543 187.72386 12.38576 0.70 −6.921 ± 0.608 −8.405 ± 0.049 1.91 ± 0.59 1.00 NGC 4486 1544 187.72394 12.37575 0.89 −8.708 ± 0.025 −9.842 ± 0.020 2.64 ± 0.14 1.00 NGC 4486 1545 187.72415 12.37580 0.89 −9.617 ± 0.038 −10.585 ± 0.022 5.64 ± 0.24 1.00 NGC 4486 1546 187.72392 12.39180 0.67 −6.465 ± 0.063 −8.227 ± 0.080 2.38 ± 0.38 1.00 NGC 4486 1547 187.72391 12.41803 1.22 −7.390 ± 0.035 −8.283 ± 0.043 2.75 ± 0.17 1.00 NGC 4486 1548 187.72398 12.39705 0.71 −6.883 ± 0.046 −7.796 ± 0.114 1.88 ± 0.30 1.00 NGC 4486 1549 187.72397 12.40466 0.84 −8.693 ± 0.027 −9.626 ± 0.015 2.40 ± 0.15 1.00 NGC 4486 1550 187.72394 12.38949 0.67 −5.843 ± 0.107 −7.101 ± 0.073 1.84 ± 0.40 0.99 Continued on Next Page. . . 363
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 329 and 330: 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
Page 429 and 430: 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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