NGC 5139 / C1323-472 / Omega Centauri (Updated February 2017) RA: 13:26:47.24 DEC: -47:28:46.5 (J2000) ============================================================ Bytes Format Explanation 1-8 A8 Star ID 10-32 A11,1x,A11 Position 34-35 A2 Units for position R0 denotes RA, DEC in the J2000 coordinates R5 denotes RA, DEC in the 1950 coordinates XA denotes X, Y in arcseconds XP denotes X, Y in pixels 37-44 F8.4 Period (days) 46-51 F6.3 Mean magnitude (or maximum magnitude if "max" is indicated in the remarks column) 53-57 F5.3 Light amplitude (range of variability) 59 A1 Colour for mean magnitude and amplitude e.g. B, V, R, I, J, K or P (for photographic). 61-65 A5 Type of variable (draft 2006 GCVS classifications) CST denotes non variable stars previously designated as variables 67-80 A19 Notes and Remarks (f denotes field star) "--" or "----" indicates no data available ========================================================================= ID Position Period ampl C Type Notes/ RA/X Dec/Y Units Remarks ========================================================================= 1 13:26:05.26 -47:23:42.8 R0 29.3479 10.89 1.15 V RV DC 2 13:26:12.65 -47:24:41.9 R0 242.0 -- -- M f;Fea 3 13:25:56.15 -47:25:53.8 R0 0.8413 14.389 0.75 V RR0 4 13:26:12.93 -47:24:18.8 R0 0.6273 14.453 1.04 V RR0 5 13:26:18.33 -47:23:12.4 R0 0.5153 14.745 1.15 V RR0 6 13:26:30.24 -47:24:28.4 R0 110.0 12.26 1.2 V SR DFL 7 13:27:00.90 -47:14:00.5 R0 0.7130 14.590 0.93 V RR0 K97b 8 13:27:48.45 -47:28:20.3 R0 0.5213 14.683 1.26 V RR0 9 13:25:59.58 -47:26:24.0 R0 0.5235 14.756 1.09 V RR0 10 13:26:06.99 -47:24:36.6 R0 0.3750 14.484 0.37 V RR1 11 13:26:30.59 -47:23:01.6 R0 0.5648 14.534 0.65 V RR0 12 13:26:27.21 -47:24:06.2 R0 0.3868 14.522 0.43 V RR1 13 13:25:58.18 -47:25:21.6 R0 0.6690 14.465 0.95 V RR0 14 13:25:59.74 -47:39:09.6 R0 0.3771 14.514 0.47 V RR1 15 13:26:27.11 -47:24:38.0 R0 0.8106 14.397 0.70 V RR0 16 13:27:37.69 -47:37:34.8 R0 0.3302 14.562 0.49 V RR1 17 13:27:37.77 -47:25:17.0 R0 60.0 12.68 0.8 V SR DFL 18 13:27:45.11 -47:24:56.6 R0 0.6217 14.570 1.14 V RR0 19 13:27:30.14 -47:28:05.2 R0 0.2996 14.830 0.45 V RR1 Note 20 13:27:14.05 -47:28:06.3 R0 0.6156 14.579 1.12 V RR0 21 13:26:11.17 -47:25:58.8 R0 0.3808 14.356 0.46 V RR1 Note 22 13:27:41.04 -47:34:07.6 R0 0.3961 14.547 0.45 V RR1 23 13:26:46.50 -47:24:39.5 R0 0.5109 14.869 1.05 V RR0 24 13:27:38.32 -47:34:14.5 R0 0.4623 14.478 0.39 V RR1 25 13:26:25.52 -47:28:23.3 R0 0.5884 14.478 0.92 V RR0 26 13:26:23.64 -47:26:59.4 R0 0.7847 14.502 0.59 V RR0 27 13:26:26.04 -47:28:16.5 R0 0.6157 14.757 0.59 V RR0 28 CST Note 29 13:26:27.28 -47:28:47.4 R0 14.7338 11.82 0.91 V CW DC 30 13:26:15.94 -47:29:56.0 R0 0.4044 14.483 0.38 V RR1 31 CST 32 13:27:03.32 -47:21:38.9 R0 0.6204 14.530 1.17 V RR0 33 13:25:51.60 -47:29:05.8 R0 0.6023 14.544 1.17 V RR0 34 13:26:07.21 -47:33:10.4 R0 0.7340 14.481 0.79 V RR0 35 13:26:53.21 -47:22:34.7 R0 0.3868 14.563 0.45 V RR1 36 13:27:10.11 -47:15:29.8 R0 0.3798 14.55 0.49 V RR1 K97b 37 CST 38 13:27:03.30 -47:36:30.2 R0 0.7791 14.478 0.59 V RR0 39 13:27:59.77 -47:34:42.3 R0 0.3934 14.565 0.48 V RR1 40 13:26:24.56 -47:30:46.2 R0 0.6341 14.519 1.11 V RR0 41 13:27:01.41 -47:31:01.7 R0 0.6629 14.537 0.97 V RR0 42 13:26:46.38 -47:29:30.9 R0 149.4 12.5 3.3 V SR f?;DFL;Note 43 13:26:34.55 -47:26:57.3 R0 1.1569 13.779 0.94 V CW 44 13:26:22.39 -47:34:35.3 R0 0.5675 14.732 0.98 V RR0 45 13:25:30.88 -47:27:21.0 R0 0.5891 14.531 1.03 V RR0 46 13:25:30.23 -47:25:51.8 R0 0.6870 14.501 0.92 V RR0 47 13:25:56.46 -47:24:12.0 R0 0.4853 14.344 0.41 V RR1 48 13:26:37.82 -47:30:25.2 R0 4.4752 12.69 0.61 V CW DC 49 13:26:07.78 -47:37:55.5 R0 0.6046 14.609 0.90 V RR0 50 13:25:53.94 -47:27:35.8 R0 0.3862 14.633 0.45 V RR1 51 13:26:42.66 -47:24:21.4 R0 0.5742 14.564 1.18 V RR0 52 13:26:35.19 -47:28:03.8 R0 0.6604 13.765 0.54 V RR0 Note 53 13:25:58.79 -47:36:09.8 R0 ---- 11.87 -- V CST? DFL;Note 54 13:26:23.54 -47:18:47.7 R0 0.7729 14.419 0.65 V RR0 55 13:25:45.00 -47:42:18.0 R0 0.5817 14.70 0.96 V RR0 GSz 56 13:25:55.53 -47:37:44.1 R0 0.5680 14.762 0.80 V RR0 Note 57 13:27:49.38 -47:36:50.5 R0 0.7944 14.471 0.58 V RR0 58 13:26:13.05 -47:24:03.0 R0 0.3699 14.474 0.28 V RR1 59 13:26:18.43 -47:29:46.7 R0 0.5185 14.741 0.70 V RR0 60 13:26:35.69 -47:32:48.1 R0 1.3495 13.707 0.98 V CW 61 13:27:13.99 -47:27:30.5 R0 2.2736 13.667 0.55 V CW 62 13:26:26.59 -47:27:55.4 R0 0.6198 14.474 1.07 V RR0 63 13:25:07.96 -47:36:54.1 R0 0.8259 14.48 0.51 V RR0 GSz 64 13:26:02.22 -47:36:19.2 R0 0.3445 14.555 0.49 V RR1 65 13:26:01.61 -47:36:35.7 R0 0.0627 14.922 0.18 V SXPHE f;Note 66 13:26:33.08 -47:22:25.2 R0 0.4073 14.488 0.40 V RR1 67 13:26:28.62 -47:18:46.9 R0 0.5645 14.681 1.04 V RR0 68 13:26:12.80 -47:19:35.7 R0 0.5346 14.242 0.38 V RR1? Note 69 13:25:11.02 -47:37:33.5 R0 0.6532 14.49 0.92 V RR0 GSz 70 13:27:27.76 -47:33:42.7 R0 0.3907 14.558 0.41 V RR1 71 13:27:08.08 -47:27:51.6 R0 0.3575 14.532 0.44 V RR1 72 13:27:33.11 -47:16:22.9 R0 0.3845 14.48 0.62 V RR1 GSz 73 13:25:53.75 -47:16:10.8 R0 0.5752 14.49 1.19 V RR0 GSz 74 13:27:07.22 -47:17:33.9 R0 0.5032 14.626 1.16 V RR0 75 13:27:19.70 -47:18:46.5 R0 0.4222 14.476 0.39 V RR1 76 13:26:57.23 -47:20:07.7 R0 0.3380 14.517 0.37 V RR1 77 13:27:20.89 -47:22:05.6 R0 0.4263 14.569 0.42 V RR1 78 13:27:44.07 -47:26:09.4 R0 1.1681 -- 0.66 V EA f;Note 79 13:28:24.99 -47:29:25.2 R0 0.6083 14.60 1.08 V RR0 K97b 80 13:28:55.06 -47:30:16.4 R0 0.3772 13.360 -- K RR1 Nav;Note 81 13:27:36.68 -47:24:48.3 R0 0.3894 14.608 0.44 V RR1 82 13:27:35.61 -47:26:30.3 R0 0.3358 14.563 0.39 V RR1 83 13:27:08.42 -47:21:34.1 R0 0.3566 14.585 0.48 V RR1 84 13:24:47.45 -47:29:56.5 R0 0.5799 14.27 0.66 V RR0 f;K97b;Note 85 13:25:06.49 -47:23:34.0 R0 0.7427 14.470 0.74 V RR0 K97b 86 13:27:15.19 -47:26:11.1 R0 0.6478 14.541 1.00 V RR0 87 13:26:57.47 -47:25:35.4 R0 0.3965 14.593 0.47 V RR1 88 13:26:55.91 -47:25:16.3 R0 0.6902 14.500 0.85 V RR0 89 13:26:45.98 -47:26:01.0 R0 0.3751 14.635 0.46 V RR1 90 13:26:45.76 -47:26:23.4 R0 0.6034 14.525 1.09 V RR0 91 13:26:50.61 -47:26:15.6 R0 0.8952 14.335 0.58 V RR0 92 13:26:14.84 -47:21:14.4 R0 1.3460 13.947 0.33 V CW 93 CST 94 13:25:57.06 -47:22:46.1 R0 0.2539 14.764 0.30 V RR1 95 13:25:24.95 -47:28:53.2 R0 0.4051 14.558 0.41 V RR1 96 13:26:39.31 -47:27:03.0 R0 0.6245 14.344 0.87 V RR0 97 13:27:08.49 -47:25:30.9 R0 0.6919 14.534 0.89 V RR0 98 13:27:05.85 -47:26:56.5 R0 0.2806 14.782 0.47 V RR1 99 13:27:02.16 -47:27:48.8 R0 0.7662 14.244 1.07 V RR0 100 13:27:04.04 -47:27:33.4 R0 0.5527 14.789 1.10 V RR0 101 13:27:30.24 -47:29:51.0 R0 0.3409 14.610 0.41 V RR1 102 13:27:22.11 -47:30:12.3 R0 0.6914 14.554 0.96 V RR0 103 13:27:14.29 -47:28:36.3 R0 0.3289 14.538 0.29 V RR1 104 13:28:07.76 -47:33:44.9 R0 0.8665 14.515 0.38 V RR0 105 13:27:46.02 -47:32:43.9 R0 0.3353 14.746 0.49 V RR1 106 13:26:59.19 -47:28:12.5 R0 0.5699 14.518 1.15 V RR0 107 13:27:14.05 -47:30:57.9 R0 0.5141 14.864 1.22 V RR0 108 13:27:04.71 -47:29:25.7 R0 0.5945 14.532 1.11 V RR0 109 13:27:01.56 -47:29:36.6 R0 0.7441 14.446 0.95 V RR0 110 13:27:02.08 -47:30:06.6 R0 0.3321 14.616 0.49 V RR1 111 13:26:49.03 -47:28:40.4 R0 0.7629 14.393 0.65 V RR0 112 13:26:54.28 -47:30:23.2 R0 0.4744 14.490 1.00 V RR0 113 13:26:56.34 -47:31:47.6 R0 0.5734 14.563 1.16 V RR0 114 13:26:50.12 -47:30:21.1 R0 0.6753 14.467 0.87 V RR0 115 13:26:12.30 -47:34:17.5 R0 0.6305 14.535 1.06 V RR0 116 13:26:35.50 -47:28:07.0 R0 0.7201 14.392 0.69 V RR0 117 13:26:19.91 -47:29:21.0 R0 0.4216 14.474 0.41 V RR1 118 13:26:40.56 -47:30:19.1 R0 0.6116 14.458 1.04 V RR0 119 13:26:38.29 -47:31:18.0 R0 0.3059 14.686 0.31 V RR1 120 13:26:25.52 -47:32:48.6 R0 0.5485 14.764 0.98 V RR0 121 13:26:28.17 -47:31:50.5 R0 0.3042 14.588 0.28 V RR1 122 13:26:30.31 -47:33:02.2 R0 0.6349 14.554 1.07 V RR0 123 13:26:51.17 -47:37:13.2 R0 0.4742 14.452 0.38 V RR1 124 13:26:54.49 -47:39:07.5 R0 0.3319 14.561 0.51 V RR1 125 13:26:48.92 -47:41:03.7 R0 0.5929 14.58 1.17 V RR0 K97b 126 13:28:08.03 -47:40:46.7 R0 0.3420 14.60 0.46 V RR1 K97b 127 13:25:19.36 -47:28:37.6 R0 0.3053 14.63 0.32 V RR1 K97b 128 13:26:17.75 -47:30:13.0 R0 0.8350 14.391 0.58 V RR0 129 13:27:05.32 -47:29:04.7 R0 ---- -- -- V SR f;DFL 130 13:26:09.93 -47:13:40.0 R0 0.4932 14.74 0.67 V RR0 K97b 131 13:26:30.07 -47:29:40.7 R0 0.3923 14.493 0.41 V RR1 132 13:26:39.22 -47:29:09.8 R0 0.6557 14.452 0.93 V RR0 133 13:23:38.06 -47:11:07.0 R0 0.3171 14.13 0.79 P EW f;vG 134 13:25:13.42 -47:12:28.7 R0 0.6529 14.46 0.84 V RR0 GSz 135 13:26:28.14 -47:29:17.6 R0 0.6326 14.513 0.83 V RR0 136 13:26:31.09 -47:27:40.5 R0 0.3919 14.376 0.41 V RR1 137 13:26:31.55 -47:27:04.3 R0 0.3342 14.557 0.47 V RR1 138 13:26:35.44 -47:31:48.4 R0 ---- 11.35 0.4 V SR DFL 139 13:26:37.76 -47:27:35.2 R0 0.6769 14.361 0.83 V RR0 140 13:26:42.16 -47:30:07.1 R0 0.6198 14.463 0.70 V RR0 141 13:26:40.91 -47:29:27.9 R0 0.6974 14.494 0.71 V RR0 142 13:26:42.67 -47:28:42.7 R0 0.3758 14.587 0.40 V RR01? Note 143 13:26:42.64 -47:27:28.8 R0 0.8207 14.400 0.60 V RR0 144 13:26:43.06 -47:28:17.9 R0 0.8353 14.401 0.46 V RR0 145 13:26:51.26 -47:31:08.6 R0 0.3732 14.519 0.41 V RR1 146 13:26:52.87 -47:29:27.9 R0 0.6331 14.480 1.04 V RR0 147 13:27:15.86 -47:31:09.2 R0 0.4227 14.490 0.43 V RR1 148 13:27:15.85 -47:27:54.0 R0 ---- 11.60 0.5 V SR DFL 149 13:27:32.94 -47:13:43.6 R0 0.6827 14.38 0.80 V RR0 GSz 150 13:27:40.21 -47:36:00.1 R0 0.8993 14.284 0.77 V RR0 151 13:28:25.40 -47:16:00.2 R0 0.4078 14.63 0.42 P RR1 Mar;Note 152 13:26:47.71 -47:29:28.4 R0 ---- 11.3 0.5 V SR DFL 153 13:26:49.69 -47:26:23.7 R0 0.3862 14.578 0.42 V RR1 154 13:27:03.15 -47:30:32.6 R0 0.3223 14.537 0.15 V RR1 155 13:26:53.63 -47:24:42.5 R0 0.4139 14.516 0.41 V RR1 156 13:26:47.92 -47:31:52.5 R0 0.3591 14.522 0.40 V RR1 157 13:26:46.49 -47:27:17.5 R0 0.4064 14.585 0.46 V RR1 158 13:26:45.34 -47:30:40.2 R0 0.3673 14.509 0.35 V RR1 159 13:23:24.44 -47:43:33.1 R0 0.3431 14.68 0.57 P RR1 vG 160 13:25:36.16 -47:12:32.5 R0 0.3973 14.51 0.49 V RR1 GSz 161 13:26:36.85 -47:30:50.0 R0 ---- 11.67 0.4 V SR DFL 162 13:26:07.67 -47:32:54.1 R0 ---- 11.75 -- V CST? DFL;Note 163 13:25:49.42 -47:20:21.5 R0 0.3132 14.554 0.22 V RR1 164 13:27:01.16 -47:20:40.7 R0 ---- 12.10 0.3 V SR DFL 165 13:26:39.44 -47:26:56.1 R0 0.5008 14.642 1.16 V RR0 166 13:26:46.00 -47:26:15.3 R0 0.3402 14.501 0.20 V RR1 167 13:26:11.56 -47:34:02.8 R0 ---- 13.30 -- V CST? f;Note 168 13:25:52.78 -47:32:02.9 R0 0.3213 15.134 0.45 V RR1 f;Note 169 13:27:20.47 -47:23:59.1 R0 0.3191 14.641 0.23 V RR1 Note 170 13:25:21.41 -47:36:54.4 R0 ---- 11.57 0.25 V SR Eg 171 13:22:58.93 -46:47:24.8 R0 ---- -- -- RR0 Wil 172 13:27:55.14 -47:04:38.7 R0 0.7380 14.31 0.82 V RR0 Note 173 13:29:43.24 -47:16:54.1 R0 0.3590 13.360 -- K RR1 Nav 174 13:28:10.22 -47:02:29.9 R0 1.8984 -- -- E? Wil 175 13:22:23.02 -48:19:04.2 R0 0.3161 13.22 -- RR1 f?;Note 176 13:27:01.12 -47:29:47.4 R0 ---- -- -- CST 177 13:29:04.27 -47:36:21.5 R0 0.3147 13.479 -- K RR1 Nav;Note 178 13:31:50.27 -47:18:22.4 R0 ---- -- -- RR0 Wil 179 13:23:45.51 -48:17:52.9 R0 ---- -- -- RR0 Wil 180 13:24:15.32 -47:40:32.4 R0 0.3901 12.839 -- K EW Nav 181 13:30:00.45 -47:48:45.6 R0 0.5884 14.535 -- K RR0 f;Nav 182 13:32:13.42 -47:06:18.6 R0 0.5454 -- -- RR0? HSH3;Note 183 13:29:39.55 -47:30:18.9 R0 0.2960 14.449 -- K RR1 f;Nav;Note 184 13:27:28.50 -47:31:35.4 R0 0.3034 14.661 0.22 V RR1 185 13:26:04.13 -47:21:45.0 R0 0.3330 14.56 0.17 V RR1 K97b 186 13:26:05.41 -47:28:20.4 R0 ---- 12.43 0.5 V SR Note 187 13:27:49.57 -47:32:57.3 R0 ---- -- -- CST 188 13:27:19.82 -47:30:17.9 R0 ---- -- -- CST 189 13:27:34.36 -47:29:34.8 R0 ---- -- -- CST 190 13:28:01.88 -47:26:11.1 R0 ---- -- -- CST 191 13:27:35.63 -47:23:03.3 R0 ---- -- -- CST 192 13:27:19.34 -47:21:52.2 R0 1.3762 16.01 1.17 V EA max 193 13:27:07.03 -47:21:54.9 R0 ---- -- -- CST 194 13:27:53.94 -47:31:53.9 R0 0.0472 17.016 0.51 V SXPHE 195 13:27:15.64 -47:24:34.3 R0 0.0655 16.780 0.38 V SXPHE 196 13:25:01.10 -47:25:29.9 R0 0.0574 17.000 0.23 V SXPHE K97a 197 13:26:20.46 -47:31:59.2 R0 0.0471 16.850 0.13 V SXPHE 198 13:26:34.56 -47:31:03.5 R0 0.0482 17.533 0.15 V SXPHE 199 13:26:28.66 -47:28:37.9 R0 0.0623 16.689 0.73 V SXPHE 200 13:27:06.92 -47:26:10.0 R0 0.0495 16.568 0.28 V SXPHE 201 13:26:11.04 -47:15:53.9 R0 0.0507 17.200 0.19 V SXPHE K96 202 13:26:38.85 -47:11:51.5 R0 0.0464 17.170 0.12 V SXPHE K96 203 13:27:19.91 -47:15:21.1 R0 0.0418 16.750 0.25 V SXPHE K96 204 13:27:07.96 -47:37:05.1 R0 0.0494 16.881 0.40 V SXPHE 205 13:26:33.36 -47:23:00.0 R0 0.3687 17.15 0.29 V EA max 206 13:27:06.89 -47:36:02.8 R0 0.3074 17.09 0.32 V EW max 207 13:26:56.06 -47:23:17.6 R0 0.2759 17.72 0.34 V EW max 208 13:27:10.54 -47:26:06.9 R0 0.3055 17.01 0.28 V EW max 209 13:26:17.28 -47:23:16.8 R0 0.8344 16.56 0.25 V EA max 210 13:26:47.35 -47:36:00.1 R0 1.4966 16.90 0.50 V EA max 211 13:26:47.41 -47:23:16.0 R0 0.5762 18.11 1.25 V EA max 212 13:27:21.73 -47:23:32.6 R0 2.4669 17.24 0.31 V EA max 213 13:27:02.67 -47:08:49.1 R0 0.3982 16.22 0.29 V EW max;K96 214 13:27:21.82 -47:37:19.0 R0 0.3418 16.54 0.16 V EW max 215 13:26:30.08 -47:41:44.3 R0 0.2493 17.86 0.19 V EW max;K96 216 13:26:08.25 -47:30:32.2 R0 23.7370 15.105 0.07 V ? Note 217 13:26:16.93 -47:27:25.3 R0 0.0533 17.038 0.10 V SXPHE 218 13:26:11.22 -47:17:53.6 R0 0.0437 17.095 0.07 V SXPHE 219 13:26:08.42 -47:19:24.2 R0 0.0387 17.303 0.08 V SXPHE 220 13:26:48.64 -47:21:42.3 R0 0.0529 16.986 0.12 V SXPHE 221 13:27:15.99 -47:21:48.7 R0 0.0361 16.680 0.05 V SXPHE 222 13:26:18.45 -47:41:12.6 R0 0.0389 17.310 0.05 V SXPHE K96 223 13:26:53.17 -47:18:22.6 R0 23.6950 14.975 0.27 V ? f;Note 224 13:26:23.80 -47:19:12.8 R0 37.8860 15.141 0.04 V ? Note 225 13:27:02.29 -47:24:36.5 R0 0.0486 16.845 0.22 V SXPHE 226 13:26:10.49 -47:29:56.8 R0 0.0379 17.299 0.17 V SXPHE 227 13:26:14.38 -47:23:53.7 R0 0.0382 17.272 0.05 V SXPHE 228 13:26:40.48 -47:33:46.4 R0 0.0399 17.199 0.08 V SXPHE 229 13:27:12.61 -47:23:58.8 R0 0.0375 17.407 0.09 V SXPHE 230 13:26:25.29 -47:46:40.9 R0 0.0339 16.550 0.03 V SXPHE K96 231 13:27:19.07 -47:35:53.8 R0 0.0375 17.419 0.05 V SXPHE 232 13:26:17.23 -47:11:49.9 R0 0.0370 17.590 0.04 V SXPHE K96 233 13:26:47.30 -47:20:31.9 R0 0.0365 17.210 0.10 V SXPHE 234 13:25:08.91 -47:30:24.9 R0 1.6200 16.62 0.09 V ELL max;K97a 235 13:25:19.23 -47:22:31.3 R0 1.0964 18.57 0.27 V EW max;K97a 236 13:25:52.15 -47:24:08.2 R0 0.2963 17.20 0.25 V EW max 237 13:25:52.87 -47:23:55.7 R0 0.0656 16.861 0.27 V SXPHE 238 13:27:33.98 -47:29:22.8 R0 0.0408 17.355 0.07 V SXPHE 239 13:27:28.56 -47:29:21.8 R0 1.1885 16.44 0.81 V EA max 240 13:27:28.68 -47:26:19.5 R0 0.3319 16.31 0.11 V EW max;f 241 13:27:36.22 -47:23:47.5 R0 0.3663 18.55 0.77 V EB max 242 13:27:45.13 -47:29:47.6 R0 4.6404 17.08 0.26 V EA max 243 13:28:23.28 -47:28:37.0 R0 0.4952 18.38 0.62 V EB max;K97a 244 13:28:37.19 -47:34:29.0 R0 0.2838 18.94 0.24 V EW max;K97a 245 13:28:32.82 -47:26:24.7 R0 0.4039 17.21 0.64 V EB max;K97a 246 13:28:06.77 -47:45:33.8 R0 0.2812 19.23 0.50 V EW max;K97a 247 13:28:08.31 -47:40:45.2 R0 0.4178 16.95 0.14 V EW max;f;K97a 248 13:25:02.01 -47:24:15.7 R0 0.4158 16.82 0.10 V EW max;K97a 249 13:25:46.28 -47:26:28.5 R0 0.0349 17.435 0.10 V SXPHE 250 13:27:31.75 -47:35:41.6 R0 0.0406 17.433 0.07 V SXPHE 251 13:27:28.02 -47:26:43.7 R0 0.9225 16.17 0.04 V EW max 252 13:27:29.73 -47:28:59.9 R0 0.0466 17.445 0.06 V SXPHE 253 13:27:22.15 -47:27:51.7 R0 0.0400 17.232 0.11 V SXPHE 254 13:27:28.61 -47:27:39.0 R0 0.3851 16.42 0.07 V EW max 255 13:28:35.29 -47:23:57.3 R0 0.5122 17.16 0.07 V EW max;K97a 256 =V231 257 13:25:04.92 -47:28:22.5 R0 0.2506 17.52 0.17 V EW max;f;K97a 258 13:25:38.19 -47:25:37.7 R0 0.6546 15.73 0.04 V ELL max 259 13:26:03.58 -47:29:30.6 R0 19.1200 15.702 0.03 V spot 260 13:24:52.62 -47:25:22.2 R0 0.0463 17.080 0.05 V SXPHE K97a 261 13:27:15.41 -47:21:29.5 R0 0.4025 14.562 0.10 V RR1 262 =V216 263 13:26:13.13 -47:26:09.7 R0 1.0122 14.304 0.23 V RR0 264 13:26:39.66 -47:30:28.2 R0 0.3214 14.743 0.41 V RR1 265 13:26:30.22 -47:28:45.2 R0 0.4226 14.462 0.31 V RR1 266 13:26:39.65 -47:28:01.7 R0 0.3523 14.509 0.18 V RR1 267 13:26:40.23 -47:26:35.8 R0 0.3158 14.486 0.24 V RR1 268 13:26:35.16 -47:26:10.9 R0 0.8129 14.544 0.46 V RR0 Note 269 13:26:31.55 -47:25:55.4 R0 145.0 13.799 0.83 V SR f;Note 270 13:26:56.57 -47:30:05.7 R0 0.3127 14.546 0.19 V RR1 271 13:26:47.13 -47:30:04.1 R0 0.4432 14.358 0.38 V RR1 272 13:26:42.95 -47:25:56.6 R0 0.3115 14.665 0.18 V RR1 273 13:26:54.34 -47:27:08.7 R0 0.3671 14.546 0.26 V RR1 274 13:26:43.73 -47:22:48.2 R0 0.3111 14.579 0.22 V RR1 275 13:26:49.75 -47:27:37.3 R0 0.3776 14.467 0.36 V RR1 276 13:27:16.51 -47:33:17.6 R0 0.3078 14.593 0.21 V RR1 277 13:26:59.97 -47:27:29.2 R0 0.3516 14.506 0.09 V RR1 278 CST 279 CST 280 13:27:09.33 -47:23:05.7 R0 0.2816 14.760 0.10 V RR1 281 13:27:06.29 -47:47:23.1 R0 0.2850 14.630 0.07 V RR1 K97b 282 13:27:27.19 -47:47:32.4 R0 0.664 15.20 0.09 V E max;f;Note 283 13:27:36.43 -47:46:40.0 R0 0.5173 18.100 1.08 V RR0 f;K97b 284 13:24:58.45 -47:36:08.2 R0 3.3207 18.560 0.40 V spot f;Note 285 13:25:40.20 -47:34:48.4 R0 0.3290 14.537 0.19 V RR1 286 =V94 287 =V169 288 13:28:10.32 -47:23:47.8 R0 0.2954 14.640 0.10 V RR1 K97b 289 13:28:03.68 -47:21:27.9 R0 0.3081 14.625 0.25 V RR1 Note 290 CST 291 13:26:38.52 -47:33:28.0 R0 0.3340 14.503 0.20 V RR1 292 13:27:08.46 -47:31:49.0 R0 46.6000 -- -- SR vL 293 13:26:34.87 -47:34:10.9 R0 98.8000 -- -- SR vL 294 13:27:32.06 -47:25:03.5 R0 0.0177 17.292 0.02 V SXPHE 295 13:27:27.71 -47:20:07.6 R0 0.0182 17.283 0.01 V SXPHE 296 13:26:17.41 -47:18:15.8 R0 0.0221 16.946 0.03 V SXPHE 297 13:26:43.78 -47:25:49.9 R0 0.0339 16.628 0.02 V SXPHE 298 13:26:50.30 -47:34:03.3 R0 0.0330 17.410 0.08 V SXPHE 299 13:27:00.31 -47:22:29.8 R0 0.0344 17.325 0.04 V SXPHE 300 13:25:46.53 -47:24:00.4 R0 0.0347 17.484 0.02 V SXPHE 301 13:27:25.23 -47:29:49.3 R0 0.0354 16.974 0.03 V SXPHE 302 13:26:47.04 -47:25:44.4 R0 0.0355 17.081 0.04 V SXPHE 303 13:26:31.33 -47:31:01.9 R0 0.0359 16.932 0.01 V SXPHE 304 13:26:19.60 -47:20:01.2 R0 0.0361 17.236 0.03 V SXPHE 305 13:27:51.50 -47:19:51.2 R0 0.0366 17.384 0.04 V SXPHE 306 13:27:11.02 -47:28:24.2 R0 0.0384 17.528 0.06 V SXPHE 307 13:27:03.02 -47:27:45.4 R0 0.0385 17.069 0.07 V SXPHE 308 13:27:50.11 -47:21:15.8 R0 0.0390 17.278 0.05 V SXPHE 309 13:26:20.15 -47:28:39.1 R0 0.0397 16.591 0.04 V SXPHE 310 13:26:31.79 -47:31:56.9 R0 0.0402 16.791 0.02 V SXPHE 311 13:26:58.70 -47:29:50.1 R0 0.0414 -- -- V SXPHE 312 13:26:40.40 -47:29:11.2 R0 0.0415 16.394 0.06 V SXPHE 313 13:26:38.30 -47:31:36.9 R0 0.0418 17.678 0.16 V SXPHE 314 13:27:08.92 -47:30:08.3 R0 0.0421 17.086 0.08 V SXPHE 315 13:26:46.03 -47:24:57.9 R0 0.0423 16.392 0.10 V SXPHE 316 13:26:14.87 -47:31:10.3 R0 0.0424 17.326 0.03 V SXPHE 317 13:28:06.01 -47:17:30.7 R0 0.0426 16.968 0.05 V SXPHE 318 13:26:28.68 -47:25:59.7 R0 0.0437 16.799 0.02 V SXPHE 319 13:26:28.55 -47:31:02.4 R0 0.0489 17.239 0.10 V SXPHE 320 13:26:49.45 -47:34:28.5 R0 0.0472 17.294 0.08 V SXPHE 321 13:26:44.55 -47:27:54.1 R0 0.0475 16.409 0.13 V SXPHE 322 13:26:38.88 -47:27:38.6 R0 0.0480 17.096 0.08 V SXPHE 323 13:26:43.38 -47:25:04.8 R0 0.0494 16.638 0.03 V SXPHE 324 13:26:18.15 -47:30:34.6 R0 0.0513 16.402 0.24 V SXPHE 325 13:26:35.08 -47:30:08.6 R0 0.0535 16.410 0.10 V SXPHE 326 13:26:40.24 -47:24:55.4 R0 0.0569 17.041 0.18 V SXPHE 327 13:26:45.21 -47:26:34.0 R0 0.0606 16.642 0.09 V SXPHE 328 13:27:01.29 -47:31:49.3 R0 0.0899 17.054 0.02 V SXPHE 329 13:26:46.70 -47:26:31.6 R0 0.1965 -- -- V EW? 330 13:26:52.06 -47:24:46.4 R0 0.2193 -- -- V EW 331 13:26:35.15 -47:26:06.3 R0 0.2213 18.06 0.12 V EW max 332 13:26:08.24 -47:31:26.5 R0 0.2474 17.73 0.06 V EW max 333 13:27:10.44 -47:28:43.3 R0 0.2553 -- -- V EW 334 13:27:23.39 -47:29:11.9 R0 0.2579 18.64 0.25 V EW max 335 13:27:13.59 -47:17:20.4 R0 0.2666 17.36 0.29 V EW max 336 13:25:52.03 -47:32:58.8 R0 0.2672 17.66 0.25 V EW max 337 13:27:13.82 -47:32:24.4 R0 0.2695 17.65 0.17 V EW? max;sdB? 338 13:26:41.59 -47:31:30.3 R0 0.2952 17.70 0.36 V EB max 339 13:26:29.67 -47:29:51.8 R0 0.3013 14.492 0.11 V RR1 340 13:26:38.95 -47:27:32.5 R0 0.3018 14.557 0.17 V RR1 341 13:26:54.61 -47:28:47.7 R0 0.3061 14.454 0.26 V RR1 342 13:27:18.69 -47:28:22.9 R0 0.3084 14.598 0.23 V RR1 343 13:26:47.79 -47:29:36.8 R0 0.3102 14.562 0.27 V RR1 344 13:26:38.09 -47:24:44.7 R0 0.3138 14.606 0.08 V RR1 345 13:26:36.90 -47:29:38.8 R0 0.3146 17.35 0.13 V EB max 346 13:26:46.93 -47:28:14.1 R0 0.3276 14.498 0.36 V RR1 347 13:26:50.88 -47:27:46.2 R0 0.3288 14.480 0.44 V RR1 348 13:26:44.19 -47:27:38.8 R0 0.3470 16.52 0.36 V EW max 349 13:26:51.80 -47:27:43.9 R0 0.3642 -- -- V RR1? Note 350 13:26:56.40 -47:30:50.2 R0 0.3791 14.483 0.42 V RR1 351 13:26:42.66 -47:27:35.4 R0 0.3856 -- -- V RR1? Note 352 13:26:54.35 -47:29:11.3 R0 0.3975 14.179 0.30 V RR1 353 13:26:43.79 -47:27:56.6 R0 0.4010 14.471 0.41 V RR1 354 13:26:38.63 -47:25:09.9 R0 0.4199 14.537 0.42 V RR1 355 13:26:28.04 -47:28:33.2 R0 0.4467 17.50 0.26 V EB max 356 13:26:41.34 -47:28:02.6 R0 0.4647 -- -- V EA max 357 13:26:17.77 -47:30:23.4 R0 0.2978 14.562 0.05 V RR1 Note 358 13:27:20.18 -47:31:48.8 R0 0.5996 17.07 0.35 V EA max 359 13:26:52.79 -47:27:13.6 R0 0.6040 -- -- V EA max 360 13:26:02.06 -47:32:23.6 R0 0.6308 17.08 0.04 V ELL? max 361 13:27:17.81 -47:26:34.1 R0 0.6818 18.20 0.17 V EA max 362 13:27:29.47 -47:21:03.4 R0 0.7360 20.07 0.60 V EA max 363 13:26:22.76 -47:21:42.6 R0 0.8237 17.86 0.27 V EA max 364 13:26:56.22 -47:26:10.8 R0 0.8472 16.29 0.43 V EA max 365 13:27:11.63 -47:35:02.1 R0 0.9404 15.25 0.10 V EB f; max;Note 366 13:26:41.56 -47:31:42.0 R0 0.9999 14.145 0.46 V RR0 367 13:27:27.69 -47:19:07.1 R0 1.0138 14.721 0.07 V bin? f;Note 368 13:25:43.21 -47:19:13.1 R0 1.1525 15.092 0.03 V ? f;Note 369 13:27:21.60 -47:32:05.8 R0 1.7883 16.089 0.04 V ? f;Note 370 13:25:36.78 -47:17:55.4 R0 2.1703 14.364 0.05 V ? f;Note 371 13:26:41.09 -47:27:37.4 R0 2.1975 15.957 0.15 V ? 372 13:27:49.66 -47:23:43.0 R0 2.6489 18.770 0.10 V ? f_CM;Note 373 13:26:07.57 -47:23:05.6 R0 3.1698 19.207 0.26 V ? 374 13:26:24.39 -47:22:21.9 R0 3.3111 16.133 0.04 V ? 375 13:25:52.09 -47:19:08.2 R0 3.3462 14.781 0.13 V bin? f;Note 376 13:25:52.82 -47:28:52.7 R0 6.7533 17.527 0.27 V ? f;Note 377 13:27:10.10 -47:21:27.4 R0 3.6390 15.851 0.11 V IRR f;Note 378 13:26:38.53 -47:19:59.5 R0 2.0711 14.70 0.18 V EA f;max;Note 379 13:26:18.83 -47:21:09.6 R0 7.1040 16.218 0.06 V ? 380 13:26:22.59 -47:30:52.2 R0 7.8320 17.199 0.05 V bin? sdB? 381 13:25:40.47 -47:22:24.2 R0 8.0710 15.135 0.01 V ? f;Note 382 13:26:40.25 -47:19:49.1 R0 8.2180 17.252 0.06 V ? 383 13:27:08.43 -47:20:28.4 R0 8.6320 17.423 0.76 V ? f;Note 384 13:25:49.82 -47:36:59.9 R0 9.5270 16.975 0.43 V ? f_CM;Note 385 13:27:04.08 -47:38:04.6 R0 10.1060 17.369 0.05 V ? 386 13:26:31.44 -47:27:24.4 R0 14.4760 14.113 0.07 V ? 387 13:26:27.66 -47:28:49.7 R0 14.7060 18.527 0.15 V ? 388 13:25:40.55 -47:28:02.2 R0 14.9000 14.108 0.01 V ? f;Note 389 13:25:31.08 -47:29:49.4 R0 15.1900 17.071 0.08 V ? 390 13:27:24.45 -47:25:11.8 R0 15.7100 14.129 0.05 V ? 391 13:27:10.56 -47:36:59.4 R0 60.0000 -- -- ? 392 13:26:44.26 -47:35:19.0 R0 56.1000 -- -- ? 393 13:26:48.97 -47:38:00.5 R0 30.5400 15.504 0.04 V SR 394 13:26:55.57 -47:34:22.8 R0 ---- -- -- L 395 =V42;Note 396 13:26:17.57 -47:37:27.7 R0 ---- 15.33 0.34 V L 397 13:26:41.35 -47:26:08.0 R0 0.2736 16.098 0.02 V ? 398 13:26:41.05 -47:24:57.9 R0 0.3037 16.339 0.04 V ? 399 13:26:29.53 -47:30:02.6 R0 0.3098 14.581 0.05 V RR1 400 13:26:10.09 -47:31:50.3 R0 0.3185 16.566 0.01 V ? 401 13:26:09.02 -47:31:47.7 R0 0.3539 17.760 0.06 V ? 402 13:26:47.72 -47:36:30.1 R0 0.5201 17.614 0.04 V ? 403 13:27:57.40 -47:26:51.0 R0 0.5555 17.168 0.04 V ? f;Note 404 13:26:21.93 -47:26:05.2 R0 5.1650 17.391 0.05 V bin? sdB? 405 13:27:26.88 -47:25:44.9 R0 0.8629 17.384 0.02 V ? 406 13:27:42.15 -47:23:34.5 R0 34.8 15.50 0.16 V EA? max;Note 407 13:27:30.02 -47:22:31.9 R0 ---- -- 0.85 V EA? 408 13:26:26.61 -47:26:35.1 R0 ---- -- -- V CV? 409 13:26:38.80 -47:21:39.8 R0 3.697 -- 0.16 V EA? 410 13:27:21.68 -47:29:21.2 R0 14.5070 14.504 0.02 V ? f;Note 411 13:26:40.77 -47:28:17.0 R0 0.8449 12.796 0.2 K RR0 Nav 412/W2 13:29:02.31 -47:04:25.8 R0 0.298 -- -- EC 413/W3 13:29:02.16 -47:03:45.5 R0 0.809 -- -- EC 414/W7 13:27:53.76 -47:13:18.5 R0 0.069 -- -- SXPhe 415/W9 13:27:42.15 -47:12:31.8 R0 8.4 -- -- L? 416/W13 13:27:29.62 -47:13:09.7 R0 0.287 -- -- EC 417/W14 13:27:59.82 -47:13:12.6 R0 0.290 -- -- EC 418/W16 13:27:15.73 -47:13:10.1 R0 23.79 -- -- L? 419/W22 13:28:53.57 -47:19:29.7 R0 0.041 -- -- SXPhe 420/W23 13:28:44.57 -47:24:51.0 R0 0.037 -- -- SXPhe 421/W26 13:28:25.94 -47:23:52.3 R0 0.426 -- -- EC 422/W28 13:28:18.70 -47:18:34.5 R0 0.311 -- -- EC 423/W29 13:28:23.48 -47:21:16.6 R0 18.09 -- -- L? 424/W44 13:27:35.42 -47:21:08.4 R0 8.463 -- -- ? 425/W46 13:27:19.48 -47:21:48.8 R0 1.374 -- -- EA 426/W52 13:28:59.84 -47:36:12.2 R0 4.337 -- -- L? 427/W54 13:28:53.72 -47:37:35.0 R0 1.901 -- -- EA 428/W55 13:28:51.95 -47:38:07.2 R0 ---- -- -- ? 429/W57 13:29:05.37 -47:39:49.9 R0 0.7425 -- -- EC 430/W71 13:27:08.30 -47:31:41.5 R0 6.110 -- -- EA 431/W72 13:27:08.05 -47:31:39.8 R0 8.41 -- -- ? 432/W73 13:29:04.61 -47:50:31.0 R0 0.2493 -- -- EC 433/W74 13:29:03.53 -47:48:58.3 R0 0.6671 -- -- ? f?;Note 434/W75 13:28:51.72 -47:48:19.1 R0 0.5663 -- -- EC 435/W76 13:28:51.35 -47:52:49.0 R0 19.6 -- -- L? 436/W77 13:28:07.59 -47:53:03.8 R0 5.070 -- -- L? 437/W79 13:28:06.34 -47:46:55.3 R0 0.509 -- -- EC 438/W81 13:27:38.59 -47:42:51.2 R0 2.733 -- -- L? 439/W83 13:27:35.03 -47:49:46.3 R0 6.033 -- -- L? 440/W85 13:26:44.60 -47:51:12.5 R0 0.382 -- -- EC 441/W87 13:26:31.41 -47:53:59.4 R0 24.39 -- -- L? 442/W89 13:26:20.52 -47:50:04.1 R0 9.26 -- -- ? 443/W94 13:25:03.82 -47:49:32.6 R0 0.337 -- -- EC 444/W96 13:24:57.89 -47:43:37.0 R0 0.338 -- -- EC 445/W131 13:24:54.09 -47:41:03.5 R0 0.047 -- -- SXPhe 446/W159 13:26:05.67 -47:23:54.5 R0 23.82 -- -- ? 447/W160 13:26:03.80 -47:23:36.8 R0 25.11 -- -- ? 448/W181 13:26:20.53 -47:04:27.6 R0 0.669 -- -- EA 449/W184 13:25:15.77 -47:03:54.9 R0 0.406 -- -- EC 450/W186 13:24:45.29 -47:09:17.9 R0 0.311 -- -- EC 451 13:27:11.77 -47:32:29.0 R0 0.0013 18.30 -- B sdOV Rand1 452 13:27:04.84 -47:32:32.3 R0 0.0012 18.44 -- B sdOV Rand2 453 13:26:24.74 -47:24:51.8 R0 0.0013 18.30 -- B sdOV Rand3 454 13:26:15.00 -47:33:05.8 R0 0.0014 18.21 -- B sdOV Rand4 455 13:27:53.94 -46:55:49.9 R0 0.9325 12.760 0.25 K RR0 456 13:22:53.94 -47:24:21.6 R0 0.3835 13.270 0.20 K RR1 457 13:26:46.25 -47:28:44.8 R0 ---- 15.82 0.15 I ? 458 13:26:46.10 -47:28:57.1 R0 ---- 10.21 0.04 I L 459 13:26:46.31 -47:28:40.3 R0 ---- 10.98 0.06 I L 460 13:27:15.0 -47:30:51 R0 0.0012 18.51 -- B sdOV Rand5 ====================================================================== Supplementary Notes The RA, dec and most of the elements listed for V1-410 in the above table are from the catalogue published by Kaluzny et al. (2004). In cases where they adopted the periods, magnitudes, amplitudes and classification from other sources because the stars' images were saturated on their frames or if they were outside their field of view, this is indicated in the remarks column where the source is indicated as follows: Bai refers to Bailey (1902) Mar refers to Martin (1938) vG refers to van Gent (1948) Fea refers to Feast (1965) Wil refers to Wilkens (1965) DC refers to Dickens & Carey (1967) DFL refers to Dickens et al. (1972) Eg refers to Eggen (1970) GSz refers to Geyer & Szeidl (1970) HSH3 refers to Sawyer Hogg's 3rd (1973) catalogue K96 refers to Kaluzny et al. (1996) K97a refers to Kaluzny et al. (1997a) K97b refers to Kaluzny et al. (1997b) vL refers to van Leeuwen et al. (2000) Wel refers to Weldrake et al. (2007) Nav refers to Navarrete et al. (2015) The data for V411 are from Navarrete et al. (2013,2015). All the data for V412-V450 are from Weldrake et al. (2007). Mean magnitudes have not been listed for these stars because the V magnitudes that they published were not mean values. Also the amplitudes have not been listed because the observations were not made on the standard V system; they are a combination of V and R. The data for V451-V454 and V460 are from Randall et al. (2011, 2016). The sdOV classification is based on the system devised by Kilkenny et al. (2013). The data for V455 and V456 are from Navarrete et al. (2015). The data for V457-459 are from Figuera Jaimes et al. (2016) The field status for V240 (Ogle #48), V247 (Ogle #57) and V257 (Ogle #67) was established by Rucinski (2000) who determined that the other EW variables discovered by Kaluzny et al. (1996, 1997a), i.e., the EW stars with numbers in the range V197-V260, are cluster members. Samus et al. (2009) have pointed out that V1, V2, V56, V65, V78, V129, V133, V168, V269, V283 are listed in the GCVS as NSV 06235 and V0825, V0833, V0813, V0814, V0826, V0594, V0832, V0791, V1045 Cen, respectively. Braga et al. (2016) published homogenous pulsation parameters for 187 candidate RR Lyrae variables. ====================================================================== Notes on individual stars: V19, V21 (Ogle #192, 97): The possible field status for these two stars was suggested by Clement & Rowe (2001) based on their anomalous Fourier parameters when compared with other variables with similar periods. However, Navarrete et a. (2015) concluded that both were cluster members. V28: According to van Leeuwen et al. (2000), the star indicated as V28 by Bailey (1902) is now known as V2 and Bailey's V2 is not variable. V42: Dickens et al. (1972) listed this star as a "radial velocity" member, but according to van Leeuwen, the proper motion does not indicate cluster membership. Navarrete (2014, private communication) pointed out that V42 is the same star as V395 announced by Kaluzny et al. (2004). V52: van Leeuwen et al. (2000) commented that this star might have an unresolved companion which would account for the fact that it is brighter and has a lower amplitude than other RR Lyrae variables with the same period. This was confirmed by Navarrete et al. (2015). V53, V162, V167: These three stars lie on the red giant branch of the CM diagram. Martin (1938) classified V53 and V162 as irregulars and found that V167 exhibited small variations of unknown character. However, Dickens et al. (1972) found that none of these stars exhibited significant variations in their observations. V167: The proper motion study of van Leeuwen et al. (2000) indicated that V167 was not a cluster member. Bellini et al. (2009) derived a 23% membership probability. Kaluzny et al. (2004) pointed out that V167 lies within an arcsec of the X-ray source XMM-25. V56: V56 is considered to be a cluster member based on proper motion studies by van Leeuwen et al. (2000) and by Bellini et al. (2009). An earlier radial velocity study by Liller & Tokarz (1981) indicated that V56 was not a cluster member. However, Navarrete et al. (2015) pointed out that V56 undergoes random period changes, and as a result, the light-curve phase derived by Liller & Tokarz (1981) for the time of their radial velocity measurement was incorrect. V65, V78: The field status for these two variables is based on a radial velocity study by Geyer & Vogt (1978). This was confirmed by the proper motion studies of van Leeuwen et al. (2000) and Bellini et al. (2009). V68: According to Navarrete et al. (2015), the classification of V68 is uncertain. It could be an RR Lyrae (RR1) or an anomalous Cepheid. V80: Navarrete et al. (2015) pointed out that this is the same star as #53 of Weldrake et al. (2007). The variabiity of V80 was first announced by Bailey (1902) who commented that it was difficult to measure because it was too distant from the comparision stars. The star was oustide the field of view in subsequent investigations of Omega Centauri by other authors, until it was recovered by Weldrake et al. (2007) and later by Navarrete et al. (2015). V84: The field status for V84 was determined from the proper motion study of van Leeuwen et al. (2000) who also noted that the characteristics of its light curve differ from those of other stars with a similar period. Nemec et al. (1994) classified V84 as a candidate anomalous Cepheid. V142: Braga et al. (2016) classified this star as a candidate radial double-mode pulsator, the first one to be identified in Omega Centauri. However, no light curve or secondary period was provided in their paper. They noted that the double-mode variables found by Olech & Moskalik (2009) are not F+FO pulsators. V151: The data for V151 are from Martin (1938) because the star was outside the field in subsequent studies - until Navarrete et al. (2015). Kaluzny et al. (2004) classified V151 as a fundamental mode pulsator (RR0), but the near-infrared observations of Navarrete et al. demonstrated that it pulsates in the first-overtone (RR1), confirming Martin's original classification. V168: The field status for V168 was based initially on a radial velocity study by Liller & Tokarz (1981). This was later confirmed in proper motion studies by van Leeuwen et al. (2000) and by Bellini et al. (2009). V169, V289, V357: These three variables, all of which are considered to be RR1 variables according to Kaluzny et al. (2004), were classified as eclipsing variables by Weldrake et al. (2007). They are Weldrake #42, #43 and #121 respectively. Since they all lie in the RR Lyrae instability strip in the CM diagram, Kaluzny's classification is assumed to be correct. This conclusion was endorsed by Ed Guinan (2013, private communication). V172 (= Weldrake #18) V172 was listed as RR Lyrae by Sawyer Hogg (1973), based on the discovery paper by Wilkens (1965), but no further information was provided. It was outside of the field of view in subsequent studies until ti was recovered by Weldrake et al. (2007), Navarrete et al. (2015) and Torrealba et al. (2015). The period, V magnitude, V amplitude and classification listed for V172 are from Torrealba et al. (2015). V175: The period, V magnitude, V amplitude and classification listed for V175 are from Fernandez-Trincado et al. (2015) who concluded that it is probably a foreground variable because it is more that 1 magnitude brighter than the horizontal branch of Omega Centauri. Also, with a distance of 66 arcminutes from the cluster centre, it is well outside the tidal radius which is 48 arcminutes according to the 2010 update of the Harris (1996) catalogue. V177 (= Weldrake #49) V177 was listed as RR Lyrae by Sawyer Hogg (1973), based on the discovery paper by Wilkens (1965), but no further information was provided. It was outside of the field of view in subsequent studies until Weldrake et al. (2007) and Navarrete et al. (2015). The data listed in the above table are from Navarrete et al. V182, V183: Shokin & Samus (1996) pointed out that the identification for these two stars was highly uncertain because they lie far from the region occupied by most of the variables and no identification chart was published by the discoverer. However, Navarrete et al. (2015) recovered V183 at the RA and dec published by Samus et al. (2009). V186: This star, numbered V184, by Fourcade et al. (1978) in their discovery paper is the same as RGO 320 discussed by Dickens et al. (1972). This was pointed out by Shokin & Samus (1996) and is evident from a comparison of Fourcade's ID chart with the chart published for star #320 by Woolley (1966 - see Plate IX). It was confirmed as a radial velocity cluster member (Feast 1973) and the data listed in the above table are from Dickens et al. (1972). V216, V224 (Ogle #22, 31): Kaluzny et al. (1996) showed that these two variables have similar properties, but their classification is uncertain. Initially, they postulated that they might be spotted variables. However, they later (Kaluzny et al. 2004) classified them as long period variables. Both stars have periods in the 20-40 day range and lie on the RG branch in the CM diagram, at a luminosity level lower than SR variables. V223 (Ogle #30): Kaluzny et al. (2004) noted that this star lies near the X-ray source XMM-29 and also that the proper motion study of van Leeuwen et al. (2001) indicates its probability of membership is in the 0-2% range. The study by Bellini et al. (2009) also indicates a low (0%) membershgip probability. Its position in the CM diagam is also consistent with non-membership in the cluster. V268: Naverrete et al. (2015) concluded that V268 is a cluster member based on its observed properties and the proper motion study by Bellini et al. (2009). van Leeuwen et al. (2000) claimed it had a membership probability of 0%, but Navarrete et al. provided evidence that the van Leeuwen result pertained to a different star. V269: This star is RGO 4789 (Woolley 1966) and Ogle #123 (Kaluzny et al. 1997b). It is considered to be a field star. It was one of 5 TiO variables discussed by Dickens et al. (1972) who noted that they needed to determine its radial velocity to establish its membership before discussing it further. In a later paper that included the TiO variables for which membership was established (Feast 1973), RGO 4789 was not included. The non-member status of V269 was confirmed in the proper motion study by van Leeuwen et al. (2000). V282 = Ogle #171 = Weldrake #84: This star was not in the field of view of Kaluzny et al. (2004). In their earlier study (Kaluzny et al. 1997b), they derived a period of 0.5005 days but were unable to assign a classification. Weldrake et al. (2007) derived a period of 0.664 days and showed that the star could be an eclipsing binary. The V mag and amplitude listed above are from the Kaluzny et al. (2004) catalogue and the period is from Weldrake et al. The proper motion study of van Leeuwen et al. indicated that V282 was not a cluster member. V284 = Ogle #173 = Weldrake #129: This star was not in the field of view of Kaluzny et al. (2004), but in their earlier study (Kaluzny et al 1997b), they derived a period of approximately 3.3 days and classified it as a spotted variable. Weldrake et al. (1997b) confirmed this period and also derived a colour index that is more red than expected for a cluster member at the V=18.5 level. It is therefore considered to be a field star. V367, V369, V375, V376, V377, V378, V383: Kaluzny et al. (2004) noted that all of these objects are associated with X-ray sources. The proper motion study of van Leeuwen et al. (2000) indicated that V367, V375, V378 were not cluster members but the other 4 stars were too faint to be included in their investigation. However, based on location in the CM diagram, Kaluzny et al. (2004) concluded that none of these stars are cluster members. The proper motion study by Bellini et al. (2009) supported this conclusion except in the case of V369 and V383 for whch they found membership probabilties greater than 90%. A subsequent spectroscopic study by Rozyczka et al. (2012) showed that V369 is not a cluster member. V349, V351 These two RR1 variables were discovered by Kaluzny et al. (2004) in the crowded central region. As a result, they could not obtain calibrated photometry. Navarrete et al. (2015) were not able to recover either of these variables in their investigation. V372, V384: These two stars are labelled f_CM because they are considered to be field stars based on their location on the CM diagram published by Kaluzny et al. (2004). The data in the above table are from Kaluzny et al. (2004). Weldrake et al. (2007) classified V384 (= Weldrake #104) as a long period variable. V378 = Weldrake #166: Kaluzny et al. (2004) noted that this star is an eclipsing binary with its light curve affected by chromospheric activity. V365, V368, V370, V381, V388, V403, V410: The field status for these variables is based on the proper motion study of Bellini et al. (2009). V395: Navarrete (2014, private communication) pointed out that V395 is V42. V406, V409 = Weldrake 39, 161: These stars were classified as possible Algol-like eclipsing binaries (EA) by Kaluzny et al. (2004), but they did not derive periods. The periods listed in the above table were determined by Weldrake et al. (2007). V433 = Weldrake 74: Navarrete et al. (2015) confirmed the variablity of this star. They derived P= 0.6681, similar to Weldrake's value, but could not determine its variability type. They also noted that the star was listed as a radial velocity non-member (#12_8_2515) by Da Costa & Coleman (2008). ====================================================================== Discovery of the variable stars in Omega Centauri: V1-132 Bailey (1902) with an ID chart (Plate I, Frontispiece) and x,y coordinates (Table VI, pages 133-135). By the time he published his paper, he considered V28, 31, 37 and 93 to be non-variable (see page 14) and this conclusion was later confirmed by Martin (1938) and by Kaluzny et al. (2004). V133-165 discovered by van Gent and Hertzsprung and announced by Martin (1938) with x,y coordinates (bottom of page 20, Table 5 on pages 22-27 or Table 6 on page 35) and ID charts (Plates I and II). V133 and V159 were outside the field of his ID charts and were later identified on ID charts by van Gent (1948). All of Bailey's variables (except V80) are labelled on Martin's charts. V166-167 Martin (1938) with ID charts (Plates I and II) and x,y coordinates (bottom of page 20). Martin assigned these numbers to his comparison stars 89b and p3, (see page 16 and 18 of his paper) V168 Kooreman (1942) with x,y coordinates V169 Belserene (1956) with x,y coordinates V170 = star G of Belserene (1959) who published x,y coordinates Eggen (1961a,b) detected its variability. The number V170 was assigned by Sawyer Hogg (1973) who also identified it as RGO #53 (Woolley 1966). Woolley established that it is a cluster member. However, it was not included in the studies of red variables in Omega Cen by Dickens et al. (1972). V171-180 = V1-10 of Wilkens (1965) who published ID charts and x,y, coordinates. The numbers V171-180 were assigned by Sawyer Hogg (1973). Wilkens (1965) listed 5 additional variables, V11-15, but according to Sawyer Hogg (1973), he later indicated (Letter, 1972) that these were suspected variables. V181-183 Wesselink (1969,1972 in private correspondence with Sawyer Hogg) The numbers V181-183 were assigned by Sawyer Hogg (1973) who also published Wsselink's x,y coordinates and periods. V184-185 Butler et al. (1978) with no ID By matching periods and approximate distance from the cluster centre, Clement & Rowe (2000) determined that V184=Ogle #191 and V185=Ogle #71 from the investigation of Kaluzny et al. (1997b). Kaluzny et al. published RA, dec and X,Y pixel positions. V186 =V184 of Fourcade et al. (1978) with ID chart and x,y coordinates The number V186 was assigned in our electronic catalogue (Clement et al. 2001) because Butler et al. (1978) had assigned the number 184 to a different star. Fourcade's variable is the same star as RG 320 that was discussed by Dickens et al. (1972) and confirmed as a cluster member by Feast (1973 - page 138). V187-193 = eclipsing binary candidates NJL #221, 216, 58, 1, 218, 5, 212 of Niss et al. (1978) who published x,y coordinates and an ID chart. The numbers 187-193 were assigned in our electronic catalogue (Clement et al. 2001). Niss et al. stated that NJL#5 was almost certainly eclipsing and that the other six were reasonably certain variables. A subsequent study by Kaluzny et al. (1996) confirmed the variability of NJL #5 (=Ogle #18), but did not list the other six as variables. In a later paper, Kaluzny et al. (2004) announced that none of the other six were variable. Margon & Cannon (1989) measured the radial velocity of NJL#5 and established its cluster membership. V194 = candidate variable NJL #220 of Niss et al. (1978) who published x,y coordinates and an ID chart. Its variability was later confirmed by Niss (1981). The number 194 was assigned in our electronic catalogue (Clement et al. 2001). V195 = star NJL #79 of Niss et al. (1978) who published x,y coordinates and an ID chart. Jorgensen (1982) detected its variability and the number V195 was assigned in our electronic catalogue (Clement et al. 2001). V196 = E39 of Jorgensen & Hansen (1984) with ID chart The number V196 was assigned in our electronic catalogue (Clement et al. 2001). V197-233 = Ogle #1-4, 6-17, 19-22, 24-40 of Kaluzny et al. (1996) with RA and dec and X,Y pixel positions The numbers V197-233 were assigned in our electronic catalogue (Clement 2001). V234-260 = Ogle #41, 43-49, 51, 53-70 of Kaluzny et al. (1997a) with RA and dec and X,Y pixel positions The numbers V234-260 were assigned in our electronic catalogue (Clement 2001). V261-291 = Ogle #81, 95-96, 108, 111, 115, 121-123, 131-132, 134, 139, 148-149, 152, 155-156, 161-162, 167, 171-173, 177, 186, 196, 202-203, 208-209 of Kaluzny et al. (1997b) with RA and dec and X,Y pixel positions The numbers V261-291 were assigned in our electronic catalogue (Clement 2001). V292-293 = #50259 and #55071 van Leeuwen et al. (2000) with RA and dec The numbers V292-293 were assigned in the 2002 update to the Clement (2001) on-line catalog and were adopted by Kaluzny et al. (2004) when they published their catalog. van Leeuwen et al. listed two other candidate red variables that were cluster members: #37110 (RA 13:26:34.12, dec -47:26:21.1) #39105 (RA 13:26:25.00, dec -47:27:06.3) which is star #201 in Woolley's (1966) study. V294-410 = NV294-410 with RA, dec and individual finder charts Kaluzny et al. (2004) V411 = V133 of Weldrake et al. (2007) who published RA and dec They stated that this star was the same as V144 of Kaluzny et al. (2004), but Navarrete et al. (2013) showed that Weldrake's #133 was a different star, not previously known to be variable. They assigned the number V411 and published an ID chart for both V144 and V411. V412-450 Weldrake et al. (2007) with RA and dec They introduced their own numbering system which was different from the one that is generally used for Omega Cen, i.e. the system started by Bailey (1902) and continued by Martin (1938) and subsequent investigators. The Weldrake (W) numbers are indicated in the ID column of the above table. Weldrake et al. announced 81 new variables, but only 43 are included here. Navarrete et al. (2015) pointed out that some of their "new" varables were previously known. W53 is V80, W144 is V272 and W145 might be V15. Also W115 is V264 and W135 is V266. Weldrake et al. had incorrectly listed these two variables as V48 and V356, respectively. Variables for which Weldrake et al. derived an amplitude less than 0.05 mag (W1, W4, W15, W58, W68, W69, W86, W93, W98, W125, W126, W130, W132, W187) have been excluded from the above table. In addition, variables which appear to be field stars based on their location in the CM diagram (e.g. W5, W6, etc.) and variables with 0% probability of membership (W31, W59), based on the proper motion study of Bellini et al. (2009) are also excluded. Future investigations might show that some of these stars are variables that belong to Omega Centauri. V451-454 = Randall's V1-4 with RA and dec Randall et al. (2011) published the coordinates and summarized the properties of these rapidly pulsating extreme horizontal branch (EHB) stars. Three of them had been announced in earlier papers by Randall and collaborators. Finding charts were later published by Randall et al. (2016). A fifth candidate was announced by Randall et al. (2013), but no position was published. V455-456 = NV455 and NV 456 of Naverrete et al. (2015) who published finder charts and RA and dec (epoch 2000). They also announced two other new RR Lyrae variables, NV457 and NV458, but their locations on the CM diagram indicate that they are too faint to be cluster members. V457-459 Figuera Jaimes et al. (2016) with RA, dec and a finder chart V460 = Randall's V5 (another EHB star) with finding chart and RA and dec by Randall et al. (2016) Randall et al. also detected an EHB variable with an apparent periodicity of approximately 0.03 days and speculated on possible explanations for its observed luminosity variation. --------------------------------------------------------------------- In a search for tidal tails around Omega Centarui, Fernandez-Trincado et al. (2015) have discussed the properties of 48 RR Lyrae variables (11 of which were previously known) in an area 50 square degrees around the cluster. Their newly discovered variables are all outside the tidal radius of the cluster and considered to be field stars.. --------------------------------------------------------------------- Cool et al. (2013) reported optical counterparts for approximately 40 Chandra X-ray sources that are probably associated with the cluster. These include 27 CV candidates, 3 BY Draconis stars, 1 qLMXB and 7 possible magnetically active binaries. ===================================================================== References Bailey, S. I. 1902, Harv. Ann., 38 Bellini, A., Piotto, G., Bedin, L. R., Anderson, J., Platais, I., Momany, Y., Moretti, A., and 2 coauthors, 2009, A&A,493, 959 Belserene, E. P., 1956, Rutherford Contrib. (Columbia Univ.), 33, 1 Braga, V. F., Stetson, P. B., Bono, G., Dall'Ora, M., Ferraro, I., Fiorentino, G., Freyhammer, L. M. and 27 coauthors, 2016, AJ, 152, 170 Butler, D., Dickens, R. J., Epps, E. 1978, ApJ, 225, 148 Clement, C. M. & Rowe, J. 2000, AJ, 120, 2579 Cool, A. M., Haggard, D., Arias, T., Brochmann, M., Dorfman, J., Gafford, A., White, V., Anderson, J. 2013, ApJ, 763, 126 Da Costa, G. S. & Coleman, M. G. 2008, AJ, 136, 506 Dickens, R. J., Feast, M. W., Lloyd Evans, T. 1972, MNRAS, 159, 337 Eggen, O. J. 1961a, Royal Obs. Bull., 27, E61 Eggen, O. J. 1961b, Royal Obs. Bull., 29, E73 Feast, M. W. 1965, Obs, 85, 16 Feast, M. W. 1973, IAU Colloq. No. 21, Variable Stars in Globular Clusters and in Related Systems, 131 Fernandez-Trincado, J. G., Vivas, A. K., Mateu, C. E., Zinn, R., Robin, A. C., Valenzuela, O., Moreno, E., Pichardo, B. 2015, A&A, 574, A15 Figuera Jaimes, R., Bramich, D. M., Skottfelt, J., Kains, N., Jorgensen, U. G., Horne, K., Dominik, M. and 26 coauthors, 2016, A&A, 588, A128 Fourcade, C. R., Laborde, J. R., Yurquina, E. 1978, IBVS, 1380 Geyer, E. H. & Szeidl, B. 1970, A&A, 4, 40 Geyer, E. H. & Vogt, N. 1978, A&A, 67, 297 Jorgensen, H. E. 1982, A&A, 108, 99 Jorgensen, H. E. & Hansen, L. 1984, A&A, 133, 165 Kaluzny, J., Kubiak, M., Szymanski, M., Udalski, A., Krzeminski, W., Mateo, M. 1996, A&AS, 120, 139 Kaluzny, J., Kubiak, M., Szymanski, M., Udalski, A., Krzeminski, W., Mateo, M., Stanek, K. 1997a, A&AS, 122, 471 Kaluzny, J., Kubiak, M., Szymanski, M., Udalski, A., Krzeminski, W., Mateo, M. 1997b, A&AS, 125, 343 Kaluzny, J., Olech, A., Thompson, I. B., Pych, W., Krzeminski, W., Schwarzenberg-Czerny, A. 2004, A&A, 424, 1101 Kilkenny, D., Fontaine, G., Green, E. M., Schuh, S. 2010, IBVS, 5927 Liller, M. H. & Tokarz, S. P. 1981, AJ, 86, 1204 Kooreman, C. J. 1942, BAN, 9, 271 Margon, B. & Cannon, R. 1989, Obs., 109, 82 Martin, W. Chr. 1938, Leiden Ann., 17, pt. 2 Navarrete, C., Catelan, M., Contreras Ramos, R., Alsonso-Garcia, J., Dekany, I., Gran, F. 2013, IBVS, 6078 Navarrete, C., Contreras Ramos, R., Catelan, M., Clement, C. M., Gran, F., Alsonso-Garcia, J., Angeloni, R., Hempel, M., Dekany, I., Minniti, D. 2015, A&A, 557, A99 Nemec, J. M., Nemec, A. F. L., Lutz, T. E. 1994, AJ, 108, 222 Niss, B. 1981, A&A, 98, 415 Niss, B., Jorgensen, H. E., Lausten, S. 1978, A&AS, 32, 387 Olech, A., Moskalik, P. 2009, A&A, 494, L17 Randall, S. K., Calamida, A., Fontaine, G., Bono, G., Brassard, P. 2011, ApJ, 737, L27 Randall, S. K., Calamida, A., Fontaine, G., Green, E. M., Monelli, M., Alonso, M. L., Catelan, M., and 3 coauthors, 2013, EPJWC, 43, 04006 Randall, S. K., Calamida, A., Fontaine, G., Monelli, M., Bono, G., Alonso, M. L., Van Grootel, V., and 6 coauthors, 2016, A&A, 589, A1 Rozyczka, M., Kaluzny, J., Pietrukowicz, P., Pych, W., Catelan, M., Contreras, C. 2012, A&A, 537, 89 Rucinski, S. M. 2000, AJ, 120, 319 Samus, N. N., Kazarovets, E. V., Pastukhova, E. N., Tsvetkova, T. M., Durlevich, O. V. 2009, PASP, 121, 1378 Sawyer Hogg, H. 1973, Publ. DDO, 3, No. 6 Shokin, Yu. A. & Samus, N. N. 1996, Ast. Let., 22, 532 Torrealba, G., Catelan, M., Drake, A. J., Djorgovski, S. G., McNaught, R. H., Belokurov, V., Koposov, S. and 4 coauthors, 2015, MNRAS, 446, 2251 van Gent, H. 1948, BAN, 10, 377 (paper prepared by Oosterhoff after the death of van Gent) van Leeuwen, F., Le Poole, R. S., Reijns, R. A., Freeman, K. C., de Zeeuw, P. T. 2000, A&A, 360, 472 Weldrake, D. T. F., Sackett, P. D., Bridges, T. J. 2007, AJ, 133, 1447 Woolley, R. v. d. R. 1966, Roy. Obs. Ann. 2 Wilkens, H. 1965, Mitt. Verand. Sterne Sonneberg, 3, 72 ====================================================================