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

More documents

Recommendations

Info

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 1855 187.73450 12.38748 1.07 −6.548 ± 0.049 −8.062 ± 0.053 3.02 ± 0.32 1.00 NGC 4486 1856 187.73454 12.38431 1.09 −7.441 ± 0.024 −8.532 ± 0.039 3.13 ± 0.18 1.00 NGC 4486 1857 187.73406 12.36648 1.40 −7.040 ± 0.030 −8.616 ± 0.039 2.15 ± 0.18 1.00 NGC 4486 1859 187.73476 12.40977 1.28 −9.406 ± 0.012 −10.459 ± 0.012 3.56 ± 0.09 1.00 NGC 4486 1860 187.73474 12.40709 1.23 −8.743 ± 0.045 −9.922 ± 0.036 3.54 ± 0.29 1.00 NGC 4486 1862 187.73482 12.40953 1.28 −8.506 ± 0.014 −9.595 ± 0.015 3.76 ± 0.12 1.00 NGC 4486 1865 187.73494 12.37252 1.29 −5.719 ± 0.132 −6.627 ± 0.131 3.04 ± 0.86 0.98 NGC 4486 1866 187.73403 12.40875 1.24 −5.767 ± 0.081 −6.962 ± 0.044 1.74 ± 0.23 0.99 NGC 4486 1870 187.73508 12.39125 1.08 −6.202 ± 0.092 −7.799 ± 0.054 2.10 ± 0.28 1.00 NGC 4486 1871 187.73507 12.36825 1.39 −5.517 ± 0.065 −6.610 ± 0.353 2.31 ± 0.44 0.99 NGC 4486 1872 187.73513 12.40839 1.26 −8.138 ± 0.031 −9.672 ± 0.017 1.77 ± 0.14 1.00 NGC 4486 1874 187.73520 12.36682 1.42 −7.183 ± 0.025 −8.637 ± 0.032 2.08 ± 0.20 1.00 NGC 4486 1875 187.73520 12.38901 1.09 −8.021 ± 0.030 −8.670 ± 0.036 5.36 ± 0.23 0.98 NGC 4486 1876 187.73523 12.38406 1.12 −5.633 ± 0.635 −7.305 ± 0.069 1.73 ± 0.41 0.99 NGC 4486 1877 187.73526 12.37968 1.17 −6.297 ± 0.039 −7.384 ± 0.050 1.76 ± 0.29 0.99 NGC 4486 1878 187.73531 12.37815 1.19 −5.116 ± 0.114 −6.698 ± 0.066 1.91 ± 0.56 0.99 NGC 4486 1880 187.73552 12.41308 1.38 −9.401 ± 0.015 −10.568 ± 0.016 2.49 ± 0.10 1.00 NGC 4486 1882 187.73556 12.40395 1.20 −6.942 ± 0.053 −8.183 ± 0.410 2.50 ± 0.68 1.00 NGC 4486 1883 187.73564 12.38558 1.12 −8.921 ± 0.012 −10.225 ± 0.016 2.28 ± 0.11 1.00 NGC 4486 1884 187.73566 12.39022 1.10 −8.369 ± 0.025 −9.268 ± 0.027 3.02 ± 0.14 1.00 NGC 4486 1885 187.73563 12.38235 1.15 −7.028 ± 0.026 −8.001 ± 0.048 2.07 ± 0.30 1.00 NGC 4486 1886 187.73572 12.41954 1.54 −5.374 ± 0.153 −6.831 ± 0.444 2.63 ± 0.78 0.99 NGC 4486 1888 187.73584 12.37938 1.19 −6.981 ± 0.041 −8.605 ± 0.025 2.25 ± 0.20 1.00 NGC 4486 1889 187.73592 12.38053 1.18 −9.218 ± 0.018 −10.699 ± 0.020 3.86 ± 0.17 1.00 NGC 4486 1890 187.73587 12.39039 1.11 −6.856 ± 0.046 −8.365 ± 0.032 2.20 ± 0.23 1.00 NGC 4486 1891 187.73591 12.39525 1.12 −7.194 ± 0.062 −8.497 ± 0.042 5.01 ± 0.40 0.99 NGC 4486 1892 187.73592 12.38859 1.12 −7.533 ± 0.028 −8.765 ± 0.029 3.07 ± 0.18 1.00 NGC 4486 1893 187.73600 12.37400 1.29 −6.003 ± 0.061 −7.176 ± 0.059 1.89 ± 0.39 0.99 NGC 4486 1894 187.73621 12.38852 1.13 −6.231 ± 0.058 −7.193 ± 0.100 3.50 ± 0.52 0.97 NGC 4486 1895 187.73632 12.36706 1.45 −6.843 ± 0.043 −8.170 ± 0.044 3.41 ± 0.25 1.00 NGC 4486 1897 187.73653 12.39180 1.13 −8.529 ± 0.024 −9.453 ± 0.024 3.02 ± 0.19 1.00 NGC 4486 1898 187.73650 12.38868 1.14 −6.776 ± 0.044 −7.527 ± 0.062 2.72 ± 0.27 1.00 NGC 4486 1900 187.73661 12.39466 1.14 −8.259 ± 0.023 −9.122 ± 0.032 3.97 ± 0.15 1.00 NGC 4486 1901 187.73661 12.40189 1.21 −7.908 ± 0.018 −8.972 ± 0.017 2.58 ± 0.12 1.00 NGC 4486 1902 187.73678 12.37908 1.23 −8.589 ± 0.028 −9.989 ± 0.021 2.55 ± 0.12 1.00 NGC 4486 1903 187.73680 12.38864 1.15 −8.202 ± 0.019 −9.297 ± 0.026 2.78 ± 0.16 1.00 NGC 4486 1904 187.73677 12.39154 1.14 −6.519 ± 0.055 −7.421 ± 0.066 3.35 ± 0.31 0.99 NGC 4486 1905 187.73678 12.41509 1.46 −5.862 ± 0.086 −6.783 ± 0.059 1.57 ± 0.38 0.97 NGC 4486 1906 187.73684 12.38325 1.18 −7.299 ± 0.035 −8.649 ± 0.025 2.78 ± 0.18 1.00 NGC 4486 1907 187.73691 12.36967 1.41 −6.459 ± 0.037 −7.762 ± 0.034 1.46 ± 0.17 0.98 NGC 4486 1908 187.73703 12.38439 1.18 −7.264 ± 0.054 −8.416 ± 0.032 3.66 ± 0.19 1.00 NGC 4486 1909 187.73708 12.36813 1.45 −6.975 ± 0.036 −8.331 ± 0.031 2.45 ± 0.22 1.00 NGC 4486 1910 187.73715 12.41444 1.46 −5.452 ± 0.165 −6.387 ± 0.393 2.75 ± 0.68 0.98 NGC 4486 1911 187.73718 12.38198 1.21 −6.968 ± 0.033 −8.066 ± 0.044 2.56 ± 0.18 1.00 NGC 4486 1912 187.73723 12.37752 1.27 −5.112 ± 0.132 −6.209 ± 0.090 2.31 ± 0.50 0.99 NGC 4486 1913 187.73732 12.39215 1.16 −9.465 ± 0.015 −10.469 ± 0.015 2.73 ± 0.10 1.00 NGC 4486 1914 187.73732 12.39614 1.18 −7.010 ± 0.027 −7.980 ± 1.790 2.03 ± 0.31 1.00 NGC 4486 1915 187.73746 12.38809 1.17 −8.482 ± 0.021 −9.332 ± 0.025 2.57 ± 0.20 1.00 NGC 4486 1916 187.73749 12.36671 1.49 −8.209 ± 0.021 −9.407 ± 0.023 2.56 ± 0.23 1.00 NGC 4486 1917 187.73743 12.40110 1.23 −5.933 ± 0.067 −7.455 ± 0.960 1.97 ± 0.42 1.00 NGC 4486 1918 187.73746 12.38145 1.22 −5.903 ± 0.082 −6.804 ± 0.121 2.35 ± 0.61 0.99 NGC 4486 1919 187.73752 12.40334 1.26 −7.658 ± 0.039 −8.611 ± 0.035 3.33 ± 0.22 1.00 NGC 4486 1921 187.73761 12.40708 1.32 −8.112 ± 0.018 −8.925 ± 0.020 3.23 ± 0.09 1.00 NGC 4486 1922 187.73760 12.37044 1.41 −5.505 ± 0.784 −6.792 ± 0.539 1.09 ± 0.65 0.89 NGC 4486 1923 187.73769 12.36591 1.52 −9.848 ± 0.012 −10.907 ± 0.014 3.48 ± 0.07 1.00 NGC 4486 1924 187.73763 12.38677 1.19 −6.768 ± 0.034 −8.113 ± 0.038 1.94 ± 0.22 1.00 NGC 4486 1926 187.73773 12.38564 1.20 −6.637 ± 0.033 −7.811 ± 0.040 2.48 ± 0.16 1.00 NGC 4486 1928 187.73776 12.41139 1.41 −7.668 ± 0.026 −8.526 ± 0.032 2.70 ± 0.20 1.00 NGC 4486 1931 187.73796 12.41298 1.45 −7.845 ± 0.034 −9.265 ± 0.025 2.36 ± 0.14 1.00 NGC 4486 1933 187.73789 12.39090 1.18 −8.762 ± 0.026 −9.856 ± 0.017 2.85 ± 0.17 1.00 NGC 4486 1934 187.73796 12.40053 1.24 −9.233 ± 0.012 −10.198 ± 0.020 3.03 ± 0.13 1.00 NGC 4486 1935 187.73799 12.41861 1.58 −9.334 ± 0.025 −10.215 ± 0.021 5.12 ± 0.13 1.00 Continued on Next Page. . . 368
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 1936 187.73801 12.42004 1.62 −9.501 ± 0.024 −10.628 ± 0.012 3.18 ± 0.12 1.00 NGC 4486 1937 187.73793 12.41279 1.44 −5.702 ± 0.074 −6.469 ± 0.124 2.71 ± 0.38 0.98 NGC 4486 1938 187.73792 12.39349 1.19 −6.024 ± 0.086 −7.346 ± 0.088 3.62 ± 0.52 0.98 NGC 4486 1939 187.73827 12.38881 1.20 −9.729 ± 0.018 −10.801 ± 0.013 3.63 ± 0.08 1.00 NGC 4486 1940 187.73807 12.40726 1.34 −8.053 ± 0.020 −9.048 ± 0.033 3.04 ± 0.19 1.00 NGC 4486 1941 187.73837 12.41097 1.42 −7.336 ± 0.024 −8.517 ± 0.026 2.35 ± 0.15 1.00 NGC 4486 1943 187.73848 12.37110 1.43 −5.662 ± 0.074 −6.926 ± 0.188 5.00 ± 0.96 0.76 NGC 4486 1945 187.73859 12.37961 1.29 −7.872 ± 0.015 −9.279 ± 0.019 2.19 ± 0.14 1.00 NGC 4486 1948 187.73876 12.36988 1.46 −7.236 ± 0.067 −7.900 ± 0.097 5.06 ± 0.50 0.96 NGC 4486 1949 187.73883 12.38049 1.28 −7.944 ± 0.027 −9.055 ± 0.028 2.89 ± 0.17 1.00 NGC 4486 1950 187.73889 12.38117 1.28 −8.626 ± 0.022 −9.424 ± 0.021 3.24 ± 0.15 1.00 NGC 4486 1951 187.73888 12.41304 1.48 −7.506 ± 0.030 −8.700 ± 0.031 2.62 ± 0.22 1.00 NGC 4486 1954 187.73897 12.41912 1.62 −7.055 ± 0.427 −8.473 ± 0.383 2.23 ± 0.56 1.00 NGC 4486 1955 187.73903 12.40807 1.39 −6.188 ± 0.085 −7.793 ± 0.057 3.03 ± 0.45 1.00 NGC 4486 1959 187.73935 12.41059 1.44 −8.278 ± 0.020 −9.155 ± 0.035 3.29 ± 0.15 1.00 NGC 4486 1960 187.73937 12.36363 1.62 −9.268 ± 0.017 −10.170 ± 0.024 2.98 ± 0.17 1.00 NGC 4486 1961 187.73938 12.39933 1.28 −8.118 ± 0.018 −9.557 ± 0.017 2.51 ± 0.10 1.00 NGC 4486 1962 187.73937 12.41138 1.46 −5.615 ± 0.068 −6.787 ± 0.071 2.57 ± 0.36 0.99 NGC 4486 1963 187.73813 12.38181 1.24 −7.937 ± 0.028 −9.231 ± 0.020 2.68 ± 0.15 1.00 NGC 4486 1964 187.73950 12.38662 1.26 −8.527 ± 0.009 −9.869 ± 0.014 2.49 ± 0.09 1.00 NGC 4486 1967 187.73966 12.41413 1.52 −7.530 ± 0.031 −8.927 ± 0.021 2.66 ± 0.19 1.00 NGC 4486 1968 187.73979 12.38900 1.26 −6.129 ± 0.046 −7.635 ± 0.055 2.19 ± 0.29 1.00 NGC 4486 1969 187.73981 12.40566 1.37 −5.423 ± 0.420 −6.929 ± 0.059 2.05 ± 0.34 0.99 NGC 4486 1970 187.73996 12.38074 1.32 −8.940 ± 0.036 −9.773 ± 0.016 2.83 ± 0.15 1.00 NGC 4486 1972 187.74007 12.38188 1.31 −6.511 ± 0.045 −7.541 ± 0.103 4.50 ± 0.58 0.95 NGC 4486 1974 187.74036 12.39128 1.28 −9.209 ± 0.010 −10.167 ± 0.016 3.01 ± 0.09 1.00 NGC 4486 1975 187.74036 12.39629 1.29 −8.181 ± 0.022 −9.602 ± 0.020 2.36 ± 0.13 1.00 NGC 4486 1976 187.74045 12.40608 1.40 −6.732 ± 0.059 −7.974 ± 0.051 3.15 ± 0.22 1.00 NGC 4486 1977 187.74052 12.38545 1.30 −9.067 ± 0.020 −9.956 ± 0.016 3.42 ± 0.15 1.00 NGC 4486 1979 187.74060 12.37369 1.45 −9.174 ± 0.014 −10.163 ± 0.020 2.81 ± 0.09 1.00 NGC 4486 1981 187.74056 12.36385 1.65 −5.913 ± 0.128 −7.133 ± 0.126 5.64 ± 0.72 0.71 NGC 4486 1982 187.74063 12.38663 1.30 −7.252 ± 0.040 −8.048 ± 0.047 3.51 ± 0.24 0.99 NGC 4486 1983 187.74066 12.39003 1.29 −6.898 ± 0.046 −7.829 ± 0.058 4.16 ± 0.26 0.98 NGC 4486 1984 187.74071 12.39224 1.29 −8.206 ± 0.023 −9.580 ± 0.019 3.06 ± 0.12 1.00 NGC 4486 1985 187.74075 12.40296 1.37 −8.013 ± 0.046 −8.965 ± 0.067 5.16 ± 0.28 0.99 NGC 4486 1986 187.74088 12.41522 1.59 −9.058 ± 0.280 −10.432 ± 0.032 2.28 ± 0.34 1.00 NGC 4486 1987 187.74093 12.38786 1.30 −9.533 ± 0.020 −10.802 ± 0.021 3.62 ± 0.13 1.00 NGC 4486 1988 187.74095 12.36578 1.62 −8.522 ± 0.045 −9.752 ± 0.038 4.48 ± 0.26 1.00 NGC 4486 1990 187.74107 12.37790 1.40 −8.512 ± 0.020 −9.584 ± 0.019 2.84 ± 0.13 1.00 NGC 4486 1991 187.74115 12.40751 1.45 −9.101 ± 0.022 −10.640 ± 0.016 4.97 ± 0.15 1.00 NGC 4486 1992 187.74124 12.38213 1.35 −8.174 ± 0.028 −9.021 ± 0.038 3.29 ± 0.19 1.00 NGC 4486 1993 187.74135 12.41719 1.64 −7.728 ± 0.057 −9.027 ± 0.105 3.11 ± 0.35 1.00 NGC 4486 1995 187.74132 12.41939 1.69 −5.118 ± 0.162 −6.247 ± 0.295 4.95 ± 1.72 0.70 NGC 4486 1996 187.74149 12.40747 1.46 −9.693 ± 0.016 −10.915 ± 0.013 3.07 ± 0.09 1.00 NGC 4486 1997 187.74154 12.41713 1.65 −8.024 ± 0.027 −9.175 ± 0.031 3.48 ± 0.17 1.00 NGC 4526 1 188.53656 7.69903 1.94 −6.872 ± 0.111 −8.270 ± 0.057 4.67 ± 0.53 0.92 NGC 4526 2 188.54054 7.71130 2.46 −6.777 ± 0.069 −7.739 ± 0.204 4.49 ± 1.21 0.79 NGC 4526 10 188.53103 7.68715 1.79 −4.867 ± 0.465 −6.641 ± 0.177 3.08 ± 4.83 0.76 NGC 4526 12 188.53250 7.69182 1.72 −6.605 ± 0.685 −7.321 ± 0.681 1.77 ± 0.68 0.86 NGC 4526 14 188.53311 7.69415 1.71 −9.344 ± 0.026 −10.272 ± 0.033 4.49 ± 0.16 1.00 NGC 4526 22 188.53184 7.69171 1.68 −7.586 ± 0.033 −9.119 ± 0.026 2.62 ± 0.14 1.00 NGC 4526 24 188.53134 7.69111 1.66 −5.666 ± 0.189 −7.403 ± 0.175 4.38 ± 1.20 0.70 NGC 4526 25 188.53283 7.69590 1.66 −8.447 ± 0.018 −9.292 ± 0.027 2.56 ± 0.14 1.00 NGC 4526 31 188.53610 7.70586 1.97 −8.200 ± 0.036 −9.473 ± 0.025 4.56 ± 0.18 1.00 NGC 4526 32 188.53461 7.70160 1.79 −6.575 ± 0.071 −7.404 ± 0.089 3.57 ± 0.42 0.86 NGC 4526 33 188.52916 7.68661 1.70 −7.143 ± 0.092 −8.243 ± 0.030 5.72 ± 0.36 0.63 NGC 4526 36 188.52941 7.68807 1.64 −6.236 ± 0.060 −7.601 ± 0.086 2.95 ± 0.37 0.95 NGC 4526 37 188.53346 7.69981 1.69 −8.169 ± 0.026 −9.545 ± 0.027 3.98 ± 0.18 1.00 NGC 4526 38 188.52792 7.68404 1.76 −7.015 ± 0.036 −8.009 ± 0.060 3.29 ± 0.27 0.96 NGC 4526 50 188.53276 7.70021 1.64 −6.789 ± 0.046 −8.037 ± 0.066 3.90 ± 0.32 0.95 NGC 4526 54 188.52884 7.68980 1.53 −5.669 ± 0.136 −7.343 ± 0.231 4.34 ± 2.54 0.68 Continued on Next Page. . . 369
Page 1 and 2:
LOW-MASS X-RAY BINARIES, DIFFUSE GA
Page 3 and 4:
smaller GCs are more likely to cont
Page 5 and 6:
GO2-3099X, GO3-4099X, AR3-4005X, GO
Page 7 and 8:
her room (my apologies to her offic
Page 9 and 10:
US Court expert from India), for al
Page 11 and 12:
Table of contents Abstract ii Ackno
Page 13 and 14:
5.2.1 Chandra X-ray Observatory . .
Page 15 and 16:
List of Figures 1.1 Hubble Tuning F
Page 17 and 18:
List of Tables 1.1 Galactic Low-Mas
Page 19 and 20:
Chapter 1 General Introduction 1.1
Page 21 and 22:
Fig. 1.1.— Hubble Tuning Fork, co
Page 23 and 24:
2000). In most HMXBs, the accreted
Page 25 and 26:
not get a complete picture of the L
Page 27 and 28:
this, the result of dynamical inter
Page 29 and 30:
is the Advanced CCD Imaging Spectro
Page 31 and 32:
Chapter 2 Chandra Observations of L
Page 33 and 34:
keV (Sarazin et al. 2000, 2001). Wi
Page 35 and 36:
agreed with positions from the USNO
Page 37 and 38:
24:00 22:00 7:20:00 18:00 16:00 18:
Page 39 and 40:
Table 2.1. Discrete X-ray Sources i
Page 41 and 42:
Table 2.1—Continued Source d Coun
Page 43 and 44:
Page 45 and 46:
Table 2.2—Continued Source d Coun
Page 47 and 48:
optical/IR positions of R.A. = 12 h
Page 49 and 50:
log N(>L) 2.0 1.5 1.0 0.5 0.0 NGC 4
Page 51 and 52:
luminosity function for luminositie
Page 53 and 54:
H31 1.0 0.5 0.0 -0.5 -1.0 NGC 4365
Page 55 and 56:
2.4.5 Variability We searched for v
Page 57 and 58:
Number 10 8 6 4 2 NGC 4365 Optical
Page 59 and 60:
LMXBs has an effective radius of 12
Page 61 and 62:
component (“MEKAL”) was used fo
Page 63 and 64:
Table 2.4. X-ray Spectral Fits of N
Page 65 and 66:
Fig. 2.9.— Top panels: Cumulative
Page 67 and 68:
we extended the spectrum down to 0.
Page 69 and 70:
We also examined whether the unreso
Page 71 and 72:
esolved sources in the galaxy. This
Page 73 and 74:
temperature ∼0.3 keV. Matsumoto e
Page 75 and 76:
log I X (counts/sec/arcmin 2 ) -1.0
Page 77 and 78:
∼45% of the counts are resolved i
Page 79 and 80:
Chapter 3 Chandra Observations of D
Page 81 and 82:
noninteracting members (de Vaucoule
Page 83 and 84:
used for spectroscopic analysis. We
Page 85 and 86:
02:00.0 03:00.0 04:00.0 05:00.0 06:
Page 87 and 88:
Page 89 and 90:
Table 3.1—Continued d a Count Rat
Page 91 and 92:
We also attempted detections in mul
Page 93 and 94:
sociated with extended X-ray or opt
Page 95 and 96:
Fig. 3.3.— Histogram of the obser
Page 97 and 98:
chip. The number of ULX candidates
Page 99 and 100:
these luminosities among previously
Page 101 and 102:
to 2-6 keV. Since the 6-10 keV rang
Page 103 and 104:
absorption and varying power-law in
Page 105 and 106:
counts occur within ∼ 4 ks. Sourc
Page 107 and 108:
log I X (counts/sec/arcmin 2 ) 0.5
Page 109 and 110:
tion), and βouter = 0.36 +0.01 −
Page 111 and 112:
the east and northeast of NGC 1600.
Page 113 and 114:
group, we assumed that they were at
Page 115 and 116:
the group gas than we calculate fro
Page 117 and 118:
04:55 -5:05:00 05 -5:05:10 15 -5:05
Page 119 and 120:
for the spectrum: “Field” impli
Page 121 and 122:
90% confidence level errors. Bracke
Page 123 and 124:
we adopted the power-law model as o
Page 125 and 126:
sources could be a non-trivial sour
Page 127 and 128:
jection to include the emission fro
Page 129 and 130:
Fig. 3.13.— Estimated gas and gra
Page 131 and 132:
ackground source population cannot
Page 133 and 134:
NGC 1600 that has a small spatial s
Page 135 and 136:
(HMXBs). LMC X-4, an HMXB pulsar, h
Page 137 and 138:
searched for the shortest time tn o
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
Page 149 and 150:
the field, these different populati
Page 151 and 152:
luminous (MB < −20) elliptical (E
Page 153 and 154:
Although Chandra is known to encoun
Page 155 and 156:
42:00.0 44:00.0 46:00.0 48:00.0 -5:
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 163 and 164:
Page 165 and 166:
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 and 174:
actually be an AGN. Sources 79, 80,
Page 175 and 176:
two potential GC counterparts. We l
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
Page 185 and 186:
dependence are allowed to vary. Var
Page 187 and 188:
NGC 4697 to convert the observed so
Page 189 and 190:
Table 5.6—Continued Source LA LB
Page 191 and 192:
Table 5.6—Continued Source LA LB
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
Page 199 and 200:
LF, there are enough datapoints tha
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
Page 209 and 210:
some data loss, it allows for direc
Page 211 and 212:
for 2 dof and the f-test indicates
Page 213 and 214:
ple to LMXBs interior to that semi-
Page 215 and 216:
est-fit (χ 2 = 56.4 for 65 dof) by
Page 217 and 218:
5.10.1 Intraobservation Variability
Page 219 and 220:
Fig. 5.14.— Binned lightcurve usi
Page 221 and 222:
Table 5.10. Possible Flaring Source
Page 223 and 224:
Fig. 5.16.— Cumulative lightcurve
Page 225 and 226:
pairs of observations. In Figure 5.
Page 227 and 228:
Table 5.11—Continued Source PL,AB
Page 229 and 230:
Fig. 5.17.— Percentage of Analysi
Page 231 and 232:
dofs and the number of combinations
Page 233 and 234:
Table 5.12—Continued Source Obs.S
Page 235 and 236:
of states as transient candidates.
Page 237 and 238:
Long-Term Hardness Ratio Variabilit
Page 239 and 240:
In the final observation, there wer
Page 241 and 242:
limits). The 0.3-10 keV X-ray lumin
Page 243 and 244:
atio is expected only from the most
Page 245 and 246:
eak (Kim et al. 2006a). We find mar
Page 247 and 248:
LMXBs in Galactic GCs (Heinke et al
Page 249 and 250:
in the field of the Milky Way and a
Page 251 and 252:
6.2 Sample 6.2.1 Galaxy Sample Tabl
Page 253 and 254:
Table 6.2. Properties of Chandra Ob
Page 255 and 256:
identification of point sources, AC
Page 257 and 258:
the QE degradation in the ACIS dete
Page 259 and 260:
Table 6.3—Continued Galaxy NX LX,
Page 261 and 262:
The positions of the GCs were used
Page 263 and 264:
Fig. 6.2.— Scatter plot of GC gal
Page 265 and 266:
Fig. 6.3.— Scatter plot of estima
Page 267 and 268:
Fig. 6.5.— Scatter plot of estima
Page 269 and 270:
isophote from the galaxy optical su
Page 271 and 272:
6.3.1 Luminosity and Mass Prior obs
Page 273 and 274:
compare their χ 2 fits to test whi
Page 275 and 276:
GCs without LMXBs; however, there a
Page 277 and 278:
following dependence on GC properti
Page 279 and 280:
of this probability with individual
Page 281 and 282:
Fig. 6.9.— Identical to Figure 6.
Page 283 and 284:
We used the indices from our best-f
Page 285 and 286:
(20.3 for half-mass radius, both wi
Page 287 and 288:
most are steeper than Z ∼0.4 . Ei
Page 289 and 290:
Fig. 6.11.— (Left:) Two-dimension
Page 291 and 292:
differently by the properties of th
Page 293 and 294:
dependent IMF (Grindlay 1987), or e
Page 295 and 296:
a 1.4M⊙ neutron star (NS). They s
Page 297 and 298:
equivalent to a dependence on the b
Page 299 and 300:
variability timescale, but it is no
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 and 306:
Appendix A Encounter Rate Parameter
Page 307 and 308:
Fig. A.1.— Dimensionless quantity
Page 309 and 310:
and four; these positions do not in
Page 311 and 312:
Table B.1—Continued RA Dec. d GC
Page 313 and 314:
Page 315 and 316:
Table B.2. Optical Properties of Gl
Page 317 and 318:
Page 319 and 320:
Page 321 and 322:
Page 323 and 324:
Page 325 and 326:
Page 327 and 328:
Page 329 and 330:
Page 331 and 332:
Page 333 and 334:
Page 335 and 336: Table B.2—Continued RA Dec. d GC
Page 385: Table B.2—Continued RA Dec. d GC
Page 421 and 422: investigations into improving the h
Page 423 and 424: C.4 Sivakoff Signature Soy Sauce Sk
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,
Page 431 and 432: Makishima, K. et al. 2000, ApJ, 535
Page 433 and 434: Porter, A. C. 1993, PASP, 105, 1250
Page 435: Verner, D. A., Ferland, G. J., Kori
show all

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

Create successful ePaper yourself

Delete template?

Save as template?