NGC 5272 / C1339+286 / Messier 3 (Updated March 2019) RA: 13:42:11.62 DEC: +28:22:38.2 (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 13:42:11.12 +28:20:33.8 R0 0.5206 15.591 1.15 V RR0 2 13:42:12.71 +28:23:35.1 R0 ---- -- -- V CST Note 3 13:42:15.71 +28:21:41.8 R0 0.5582 15.545 1.22 V RR0 4n 13:42:08.19 +28:22:33.5 R0 0.5850 -- -- V RR0 Note 4s 13:42:08.22 +28:22:33.2 R0 0.5931 -- -- V RR0 Note 5 13:42:31.29 +28:22:20.7 R0 0.5057 15.592 0.88 V RR0 6 13:42:02.08 +28:23:41.6 R0 0.5143 15.686 1.20 V RR0 7 13:42:11.09 +28:24:10.2 R0 0.4974 15.688 1.28 V RR0 8 13:42:05.30 +28:22:18.8 R0 0.6367 15.634 0.65 V RR0 Ben06 9 13:41:49.51 +28:19:13.3 R0 0.5416 15.630 1.06 V RR0 10 13:42:23.10 +28:25:00.6 R0 0.5695 15.615 0.89 V RR0 11 13:41:59.98 +28:19:11.8 R0 0.5079 15.580 1.30 V RR0 12 13:42:11.26 +28:20:17.0 R0 0.3179 15.557 0.57 V RR1 13 13:42:09.58 +28:20:24.4 R0 0.3507 15.673 0.29 V RR012 J15 14 13:42:07.81 +28:20:01.1 R0 0.6359 15.506 1.08 V RR0 15 13:42:04.67 +28:18:08.5 R0 0.5301 15.597 1.11 V RR0 16 13:41:48.71 +28:21:08.0 R0 0.5115 15.676 1.15 V RR0 17 13:42:22.42 +28:15:22.7 R0 0.5762 15.620 1.11 V RR0 18 13:42:18.95 +28:17:47.3 R0 0.5165 15.673 1.18 V RR0 19 13:42:38.12 +28:18:37.8 R0 0.6320 15.679 0.49 V RR0 20 13:42:36.83 +28:18:11.8 R0 0.4913 15.611 1.04 V RR0 21 13:42:37.78 +28:23:01.4 R0 0.5158 15.656 1.12 V RR0 22 13:42:25.92 +28:22:32.1 R0 0.4814 15.654 1.08 V RR0 23 13:42:02.84 +28:27:20.9 R0 0.5954 15.621 0.86 V RR0 24 13:42:00.31 +28:22:51.9 R0 0.6634 15.499 0.87 V RR0 25 13:42:02.08 +28:22:10.1 R0 0.4801 15.642 1.28 V RR0 26 13:41:58.05 +28:21:58.3 R0 0.5977 15.539 1.03 V RR0 27 13:42:03.17 +28:20:58.9 R0 0.5791 15.610 0.95 V RR0 28 13:42:09.63 +28:20:56.5 R0 0.4706 15.651 1.09 V RR0 29 13:42:06.58 +28:21:28.4 R0 0.47 15.622 1.22 V RR0 Note 30 13:42:08.72 +28:23:39.9 R0 0.5121 15.571 1.24 V RR0 31 13:42:13.97 +28:23:47.4 R0 0.5807 15.527 1.25 V RR0 32 13:42:12.39 +28:23:42.3 R0 0.4954 15.558 1.23 V RR0 33 13:42:16.83 +28:21:13.3 R0 0.5252 15.614 1.25 V RR0 34 13:42:21.71 +28:25:32.5 R0 0.5591 15.638 1.05 V RR0 35 13:42:03.44 +28:18:03.4 R0 0.5305 15.570 1.37 V RR0 36 13:42:24.55 +28:22:07.4 R0 0.5456 15.618 1.17 V RR0 37 13:41:53.56 +28:25:25.6 R0 0.3266 15.637 0.51 V RR1 38 13:41:56.04 +28:24:49.1 R0 0.5580 15.628 1.08 V RR0 39 13:41:52.97 +28:24:42.4 R0 0.5871 15.674 0.89 V RR0 40 13:41:50.93 +28:24:33.1 R0 0.5515 15.680 1.02 V RR0 41 13:42:04.39 +28:23:35.8 R0 0.4859 15.728 0.87 V RR0 42 13:42:05.51 +28:23:22.3 R0 0.5901 15.476 1.36 V RR0 43 13:42:19.07 +28:23:07.0 R0 0.5405 15.651 1.29 V RR0 44 13:42:24.37 +28:24:22.0 R0 0.3681 15.646 0.19 V RR01 J15 45 13:41:53.23 +28:20:31.1 R0 0.5369 15.649 1.17 V RR0 46 13:42:01.82 +28:21:50.4 R0 0.6134 15.668 0.64 V RR0 47 13:42:02.58 +28:21:28.7 R0 0.5409 15.666 0.85 V RR0 48 13:42:21.16 +28:21:00.4 R0 0.6278 15.494 0.66 V RR0 49 13:42:22.11 +28:21:02.6 R0 0.5482 15.677 0.95 V RR0 50 13:42:12.24 +28:18:47.8 R0 0.5128 15.595 1.20 V RR0 51 13:42:13.87 +28:18:55.9 R0 0.5840 15.621 0.86 V RR0 52 13:42:05.62 +28:25:13.2 R0 0.5162 15.705 1.01 V RR0 53 13:42:10.94 +28:24:44.7 R0 0.5049 15.638 1.20 V RR0 54 13:42:08.98 +28:24:28.5 R0 0.5063 15.691 0.74 V RR0 55 13:41:55.91 +28:28:05.7 R0 0.5298 15.666 1.08 V RR0 56 13:42:00.67 +28:28:39.9 R0 0.3296 15.614 0.50 V RR1 57 13:42:23.25 +28:22:42.3 R0 0.5122 15.676 1.15 V RR0 58 13:42:04.95 +28:23:27.9 R0 0.5171 15.509 1.28 V RR0 59 13:42:03.25 +28:18:53.2 R0 0.5888 15.646 0.79 V RR0 60 13:41:49.05 +28:17:25.5 R0 0.7077 15.520 0.75 V RR0 61 13:42:25.78 +28:28:45.7 R0 0.5209 15.641 1.03 V RR0 62 13:42:18.22 +28:29:39.1 R0 0.6524 15.620 0.58 V RR0 63 13:42:14.21 +28:28:24.1 R0 0.5704 15.661 0.79 V RR0 64 13:42:20.11 +28:28:12.5 R0 0.6055 15.664 0.75 V RR0 65 13:42:20.92 +28:28:10.0 R0 0.6683 15.496 0.97 V RR0 66 13:42:03.77 +28:24:42.8 R0 0.6202 15.607 0.80 V RR0 67 13:42:01.51 +28:24:44.3 R0 0.5683 15.657 1.17 V RR0 68 13:42:13.09 +28:25:37.1 R0 0.3560 15.635 0.40 V RR01 J15 69 13:42:17.57 +28:25:03.3 R0 0.5666 15.673 0.99 V RR0 70 13:42:14.32 +28:25:14.4 R0 0.4864 15.350 0.40 V RR1 71 13:42:23.65 +28:22:40.5 R0 0.5491 15.659 0.80 V RR0 72 13:42:45.25 +28:22:41.3 R0 0.4561 15.679 1.30 V RR0 73 13:42:44.72 +28:23:45.7 R0 0.6736 15.623 0.29 V RR0 74 13:42:18.15 +28:25:13.1 R0 0.4922 15.653 1.30 V RR0 75 13:42:15.13 +28:25:21.4 R0 0.3141 15.626 0.54 V RR1 Note 76 13:42:10.41 +28:21:14.0 R0 0.5018 15.719 1.38 V RR0 77 13:42:04.29 +28:23:09.6 R0 0.4593 15.725 1.30 V RR0 78 13:42:15.06 +28:23:48.5 R0 0.6119 15.554 0.86 V RR0 79 13:42:14.69 +28:28:31.4 R0 0.4833 15.716 0.72 V RR0 Note 80 13:42:43.02 +28:27:27.8 R0 0.5384 15.646 0.61 V RR0 81 13:42:37.36 +28:28:34.3 R0 0.5291 15.656 1.10 V RR0 82 13:42:03.89 +28:12:40.5 R0 0.5245 15.601 1.21 V RR0 Note 83 13:41:38.00 +28:24:33.4 R0 0.5013 15.651 1.20 V RR0 84 13:42:16.31 +28:25:27.1 R0 0.5957 15.630 0.72 V RR0 85 13:42:34.65 +28:26:29.0 R0 0.3558 15.483 0.52 V RR1 86 13:42:50.39 +28:20:48.9 R0 0.2927 15.637 0.57 V RR1 87 13:42:19.84 +28:23:42.6 R0 0.3575 15.573 0.37 V RR01 J15 88 13:42:08.83 +28:21:32.2 R0 0.2987 15.714 0.58 V RR1 89 13:42:13.63 +28:20:51.5 R0 0.5485 15.579 1.13 V RR0 90 13:42:18.92 +28:19:34.2 R0 0.5170 15.639 1.17 V RR0 91 13:42:10.56 +28:13:31.9 R0 0.5294 15.616 1.24 V RR0 Note 92 13:42:09.38 +28:15:53.3 R0 0.5035 15.632 1.14 V RR0 93 13:41:47.40 +28:16:04.1 R0 0.6023 15.640 0.76 V RR0 94 13:41:34.54 +28:18:55.1 R0 0.5237 15.677 1.18 V RR0 95 13:41:59.74 +28:22:56.8 R0 103.73 14.03 0.74 P SR Note 96 13:41:59.12 +28:18:47.3 R0 0.4994 15.652 1.21 V RR0 Note 97 13:42:01.70 +28:19:24.6 R0 0.3349 15.651 0.45 V RR1 98 13:42:21.52 +28:22:38.8 R0 ---- 15.593 -- V CST 99 13:42:26.76 +28:21:48.0 R0 0.3611 15.644 0.39 V RR01 J15 100 13:42:16.75 +28:24:19.7 R0 0.6188 15.681 0.67 V RR0 101 13:42:14.98 +28:24:05.6 R0 0.6439 15.696 0.68 V RR0 102 13:42:15.88 +28:24:37.2 R0 ---- 15.674 -- V CST 103 13:42:15.90 +28:24:42.5 R0 ---- 15.930 -- V CST 104 13:42:09.49 +28:25:07.3 R0 0.5699 15.536 1.25 V RR0 105 13:42:09.85 +28:25:53.2 R0 0.2877 15.532 0.35 V RR1 106 13:42:07.79 +28:25:30.0 R0 0.5471 15.668 0.92 V RR0 107 13:42:05.62 +28:28:16.7 R0 0.3090 15.631 0.59 V RR1 108 13:41:54.77 +28:27:51.9 R0 0.5196 15.692 1.14 V RR0 109 13:42:04.72 +28:22:44.3 R0 0.5339 15.673 1.23 V RR0 110 13:42:03.93 +28:22:25.9R0 0.5355 15.626 1.15 V RR0 111 13:42:04.45 +28:23:03.7 R0 0.5102 15.713 1.14 V RR0 112 13:42:00.79 +28:10:42.7 R0 ---- -- -- CST Note 113 13:42:26.84 +28:11:12.9 R0 0.5130 15.665 1.143 V RR0 Note 114 13:42:12.20 +28:33:03.6 R0 0.5977 15.686 1.16 V RR0 115 13:42:45.11 +28:33:47.5 R0 0.5134 15.717 1.20 V RR0 Note 116 13:41:34.05 +28:30:25.0 R0 0.5148 15.685 1.43 V RR0 117 13:42:18.39 +28:14:54.0 R0 0.6005 15.591 1.00 V RR0 118 13:42:22.50 +28:17:50.6 R0 0.4994 -- 1.13 V RR0 119 13:42:30.67 +28:24:28.8 R0 0.5177 15.606 1.16 V RR0 120 13:41:48.99 +28:26:32.2 R0 0.6401 15.676 0.51 V RR0 121 13:42:08.16 +28:23:37.7 R0 0.5352 15.744 1.00 V RR0 122 13:42:09.00 +28:21:55.0 R0 0.5160 -- -- RR0 Note 123 13:41:52.29 +28:06:04.1 R0 0.5455 15.648 1.113 V RR0 Note 124 13:42:06.52 +28:19:20.6 R0 0.7524 15.536 0.37 V RR0 125 13:42:25.64 +28:20:30.1 R0 0.3498 15.656 0.42 V RR01 J15 126 13:42:10.35 +28:20:15.6 R0 0.3484 15.609 0.46 V RR1 127 13:42:18.56 +28:21:41.6 R0 ---- -- -- CST Note 128 13:42:20.12 +28:24:53.5 R0 0.2920 15.620 0.63 V RR1 129 13:42:08.21 +28:23:59.8 R0 0.4061 15.481 0.47 V RR1? 130 13:42:11.77 +28:24:06.2 R0 0.5661 15.574 0.80 V RR0 131 13:42:05.89 +28:23:09.0 R0 0.2977 15.648 0.59 V RR1 132 13:42:07.43 +28:22:19.9 R0 0.3399 15.589 0.54 V RR1 133 13:42:07.01 +28:23:26.0 R0 0.5507 15.693 1.16 V RR0 134 13:42:09.78 +28:23:34.7 R0 0.6181 15.745 0.64 V RR0 135 13:42:09.45 +28:23:20.9 R0 0.5684 15.663 0.86 V RR0 136 13:42:09.57 +28:23:15.8 R0 0.6172 -- -- RR0 blend 137 13:42:15.47 +28:22:23.2 R0 0.5751 15.579 0.93 V RR0 138 13:41:51.52 +28:23:22.5 R0 53.28 14.25 0.15 P SR Note 139 13:42:14.11 +28:23:10.4 R0 0.5600 15.587 1.45 V RR0 Note 140 13:42:10.28 +28:24:30.7 R0 0.3331 15.477 0.45 V RR1 Note 141 13:40:18.15 +28:18:21.6 R0 0.2696 14.98 1.0 P EC f?;max;Note 142 13:42:09.26 +28:21:43.6 R0 0.5686 15.703 0.97 V RR0 143 13:42:08.88 +28:22:59.0 R0 0.5965 15.472 0.99 V RR0 144 13:42:15.61 +28:21:02.7 R0 0.5968 15.582 0.56 V RR0 145 13:42:13.61 +28:22:51.0 R0 0.5145 -- -- RR0 blend 146 13:42:18.49 +28:21:43.9 R0 0.5022 15.704 1.31 V RR0 Note 147 13:42:09.83 +28:23:29.4 R0 0.3465 15.753 0.42 V RR1 148 13:42:10.95 +28:23:20.0 R0 0.4673 -- -- RR0 blend 149 13:42:14.09 +28:23:35.2 R0 0.5482 15.687 1.14 V RR0 150 13:42:16.68 +28:23:20.4 150 13:42:16.68 +28:23:20.4 R0 0.5239 15.651 1.15 V RR0 151 13:42:11.98 +28:22:00.9 R0 0.5168 15.685 1.33 V RR0 152 13:42:17.47 +28:23:33.6 R0 0.3261 15.496 0.50 V RR1 153 13:42:08.60 +28:23:43.6 R0 ---- -- -- V CST 154 13:42:11.65 +28:22:13.5 R0 15.2842 12.63 1.25 V CW Note 155 13:42:06.69 +28:21:27.4 R0 0.3317 15.484 0.50 V RR1 Note 156 13:42:09.98 +28:22:01.4 R0 0.5320 15.694 1.20 V RR0 157 13:42:10.18 +28:23:17.9 R0 0.5429 15.728 -- V RR0 Note 158 13:42:10.33 +28:22:02.5 R0 ---- -- -- CST Note 159 13:42:10.36 +28:22:58.4 R0 0.5339 15.380 -- V RR0 Be06 160 13:42:10.80 +28:21:58.9 R0 0.6573 15.695 1.14 V RR0 161 13:42:12.80 +28:21:44.8 R0 0.5265 15.693 -- V RR0 Ben06 162 13:42:13.59 +28:22:11.1 R0 ---- -- -- V CST Note 163 13:42:10.28 +28:22:10.6 R0 ---- -- -- V CST Note 164 13:42:13.08 +28:22:06.6 R0 ---- -- -- V CST Note 165 13:42:17.04 +28:23:02.8 R0 0.4836 15.585 1.18 V RR0 Note 166 13:42:04.16 +28:22:34.4 R0 0.3567 15.736 0.23 V RR01 J15 167 13:42:05.59 +28:22:05.5 R0 0.6440 15.629 0.48 V RR0 168 13:42:08.09 +28:22:49.9 R0 0.2759 15.617 0.4 V RR1 Note 169 13:42:09.28 +28:22:08.0 R0 ---- -- -- V CST 170 13:42:09.33 +28:23:15.2 R0 0.4323 15.291 0.45 V RR1 171 13:42:09.50 +28:22:59.2 R0 0.3033 15.581 0.70 V RR1 172 13:42:09.90 +28:23:08.5 R0 0.5423 15.742 1.20 V RR0 173 13:42:10.50 +28:23:21.5 R0 0.6070 -- -- RR0 blend 174 13:42:10.82 +28:22:08.5 R0 0.5913 15.985 0.80 V RR0 175 13:42:14.63 +28:23:09.0 R0 0.5697 15.665 0.98 V RR0 Ben06 176 13:42:14.97 +28:23:15.8 R0 0.5396 15.840 0.74 V RR0 177 13:42:16.28 +28:22:13.9 R0 0.3483 15.567 0.59 V RR1 178 13:42:17.47 +28:23:29.5 R0 0.2670 15.706 0.37 V RR1 179 13:42:14.39 +28:09:41.1 R0 ---- -- -- CST Note 180 13:42:10.08 +28:22:13.3 R0 0.6091 15.679 0.75 V RR0 Note 181 13:42:09.19 +28:22:28.8 R0 0.6638 15.528 0.55 V RR0 Ben06 182 13:42:10.11 +28:23:42.3 R0 ---- -- -- V CST Note 183 13:42:13.77 +28:22:49.4 R0 ---- -- -- V CST Note 184 13:42:09.57 +28:22:27.5 R0 0.5312 15.779 1.30 V RR0 185 13:42:10.31 +28:23:13.6 R0 ---- -- -- V CST Note 186 13:42:12.49 +28:21:39.5 R0 0.6634 15.538 0.55 V RR0 187 13:42:09.66 +28:22:51.2 R0 0.5863 15.709 0.9 V RR0 Ben06 188 13:42:09.49 +28:23:06.5 R0 0.2665 15.782 0.4 V RR1 Note 189 13:42:09.58 +28:22:21.6 R0 0.6129 -- -- RR0 blend 190 13:42:10.87 +28:23:11.0 R0 0.5228 15.726 1.30 V RR0 191 13:42:11.62 +28:23:05.6 R0 0.5192 15.702 1.1 V RR0 Ben06 192 13:42:11.30 +28:22:46.4 R0 0.4974 -- -- RR0 Note;blend 193 13:42:12.59 +28:22:35.4 R0 0.7479 15.490 1.20 V RR0 194 13:42:12.74 +28:22:29.8 R0 0.4892 15.628 1.1 V RR0 Ben06 195 13:42:10.48 +28:22:14.5 R0 0.6441 15.606 0.5 V RR0 Note 196 13:42:15.0 +28:22:44 R0 ---- -- -- CST Note 197 13:42:15.90 +28:22:51.8 R0 0.4999 15.704 1.38 V RR0 198 13:42:09.74 +28:22:57.5 R0 ---- -- -- CST Note 199 13:42:10.02 +28:22:53.7 R0 ---- -- -- CST Note 200 13:42:11.17 +28:23:03.8 R0 0.3610 15.561 -- V RR01 J15 201 13:42:11.77 +28:22:33.6 R0 0.5405 15.770 1.30 V RR0 202 13:41:42.83 +28:24:17.5 R0 0.7736 15.524 0.180 V RR0 203 13:42:09.44 +28:17:30.2 R0 0.2898 15.546 0.150 V RR1 204 13:42:38.71 +28:22:48.2 R0 ---- -- -- V CST? Note 205 13:40:47.63 +28:33:26.2 R0 0.6369 15.695 0.474 V RR0 Note 206 13:42:20.39 +27:53:51.6 R0 0.5093 15.65 0.91 V RR0 Note 207 13:42:14.19 +28:22:11.9 R0 0.3453 15.455 0.40 V RR1 208 13:42:11.70 +28:21:44.1 R0 0.3384 15.698 0.40 V RR1 Note;Ben06 209 13:42:06.36 +28:21:02.7 R0 0.3483 15.607 0.52 V RR1 Ben06 210 13:42:04.98 +28:22:32.1 R0 0.3529 -- -- V RR1 211 13:42:07.39 +28:22:49.0 R0 0.5582 -- -- RR0 blend 212 13:42:09.87 +28:22:04.2 R0 0.5422 15.803 1.30 V RR0 213 13:42:09.56 +28:22:12.4 R0 0.3000 15.533 0.50 V RR1 214 13:42:13.92 +28:22:48.5 R0 0.5395 -- -- V RR0 215 13:42:10.43 +28:22:41.3 R0 0.5287 15.617 1.20 V RR0 216 13:42:13.59 +28:22:31.2 R0 0.3465 15.833 0.60 V RR1 217 13:42:11.47 +28:22:15.4 R0 0.5284 -- -- V RR Note 218 13:42:13.61 +28:22:12.8 R0 0.5449 15.828 1.20 V RR0 Note 219 13:42:07.05 +28:22:57.5 R0 0.6136 15.700 0.70 V RR0 220 13:42:13.99 +28:22:26.3 R0 0.6001 15.710 0.8 V RR0 Ben06 221 13:42:10.21 +28:22:28.6 R0 0.3788 -- -- RR1 blend 222 13:42:18.75 +28:21:38.8 R0 0.5967 15.552 0.85 V RR0 Note 223 13:42:13.27 +28:22:36.3 R0 0.3292 15.576 0.5 V RR1 Ben06 224 13:42:09.81 +28:22:47.0 R0 ---- -- -- CST? Note 225 13:42:12.05 +28:26:26.5 R0 89.59 14.12 0.33 P SR Note 226 13:42:12.97 +28:22:23.8 R0 0.4884 -- -- RR0 blend 227 13:42:03.14 +28:21:40.3 R0 ---- 15.469 -- V CST 228 13:42:08.98 +28:23:18.6 R0 ---- 15.630 -- V CST 229 13:42:09.00 +28:21:56.5 R0 0.5161 -- -- RR0 blend;Note 230 13:42:30.93 +28:14:29.2 R0 ---- -- -- ? Note 231 13:42:20.93 +28:23:29.4 R0 ---- 16.000 -- V CST 232 13:42:20.51 +28:23:23.8 R0 ---- 15.582 -- V CST 233 13:42:13.84 +28:22:35.0 R0 ---- 15.935 -- V CST 234 13:42:13.08 +28:22:02.5 R0 0.5080 15.926 1.65 V RR0 f;Note 235 13:42:13.76 +28:23:19.4 R0 0.7598 15.467 0.60 V RR0 236 13:42:41.50 +28:19:08.1 R0 31.395 14.295 0.25 P SR Note 237 13:42:15.75 +28:18:16.8 R0 0.0420 18.02 0.232 V SXPHE Note 238 13:42:12.95 +28:19:41.7 R0 0.4983 17.25 0.1 V EC f;max;Note 239 13:42:09.87 +28:22:15.9 R0 0.5040 15.700 1.25 V RR0 Note 240 13:42:09.45 +28:22:34.9 R0 0.2760 15.672 0.4 V RR1 Note 241 13:42:10.75 +28:22:37.6 R0 0.5962 -- -- V RR0 blend 242 13:42:13.20 +28:22:24.2 R0 0.5964 -- -- V RR0 blend 243 13:42:12.26 +28:22:15.5 R0 0.6346 15.629 0.6 V RR0 Ben06 244 13:42:09.61 +28:22:46.2 R0 0.5378 15.682 1.1 V RR0 Ben06 245 13:42:09.89 +28:22:59.7 R0 0.2840 15.622 0.5 V RR1 Ben06 246 13:42:12.75 +28:22:40.1 R0 0.3391 15.622 0.5 V RR1 Ben06 247 13:42:14.78 +28:22:15.5 R0 0.6054 15.670 0.7 V RR0 Ben06 248 13:42:09.66 +28:22:49.3 R0 0.5098 -- -- V RR0 blend 249 13:42:10.30 +28:22:47.9 R0 0.5330 15.640 1.1 V RR0 Note;Ben06 250n 13:42:10.48 +28:22:52.9 R0 0.57 -- -- V RR0 Note 250s 13:42:10.54 +28:22:52.1 R0 0.59 -- -- V RR0 Note 251 13:42:10.94 +28:22:33.6 R0 0.3542 -- -- V RR01 J15 252 13:42:10.99 +28:22:43.6 R0 0.3361 -- -- V RR01 J15 253 13:42:12.13 +28:22:32.4 R0 0.3326 15.493 0.5 V RR1 Ben06 254 13:42:12.41 +28:22:53.2 R0 0.6057 15.531 0.6 V RR0 Ben06 255 13:42:12.60 +28:22:43.6 R0 0.5727 15.581 0.8 V RR0 Ben06 256 13:42:13.09 +28:22:58.4 R0 0.3181 15.692 0.5 V RR1 Ben06 257 13:42:13.05 +28:22:28.0 R0 0.6020 15.705 0.9 V RR0 Ben06 258 13:42:14.30 +28:23:31.2 R0 0.7134 15.641 0.68 V RR0 259 13:42:14.56 +28:22:54.5 R0 0.3335 15.720 0.5 V RR1 Ben06 260 13:41:58.17 +28:15:51.9 R0 ---- -- -- CST? Note 261 13:42:10.08 +28:22:40.0 R0 0.4449 15.187 0.4 V RR1 Ben06 262 13:42:10.81 +28:22:37.1 R0 0.6551 -- -- RR0 Note 263 13:42:10.86 +28:22:24.0 R0 0.2169 17.043 0.35 V SXPHE Ben06 264 13:42:10.86 +28:22:29.5 R0 0.3565 15.465 0.5 V RR1 Ben06 265 13:42:11.70 +28:22:15.4 R0 ---- -- -- V RR Note 266 13:42:09.54 +28:22:43.9 R0 0.3425 15.508 0.45 V RR1 Ben06 267 13:42:09.77 +28:22:47.7 R0 ---- -- -- V SXPHE Note 268 13:42:11.70 +28:22:14.0 R0 ---- -- -- V RR Note 269 13:42:12.78 +28:22:32.7 R0 0.36 15.505 0.5 V RR1 Note;Ben06 270n 13:42:11.95 +28:23:32.7 R0 0.63 -- -- RR0 Note 270s 13:42:11.96 +28:23:31.9 R0 0.69 -- -- RR0 Note 271 13:42:12.18 +28:23:17.6 R0 0.6328 15.624 0.65 V RR0 Ben06 272 13:42:13.30 +28:19:50.9 R0 ---- -- -- SR? Note 273 13:42:06.73 +28:20:56.7 R0 46.43 -- -- SR? Note 274 13:42:12.12 +28:21:20.3 R0 ---- -- -- SR? Note;f? S1-11 ---- -- -- Note 286 13:41:51.55 +28:17:00.6 R0 ---- 17.406 0.171 V ? 287 13:41:41.00 +28:20:55.5 R0 ---- 16.964 0.060 V ? 288 13:42:17.39 +28:13:35.1 R0 0.0366 17.489 0.087 V SXPHE 289 13:42:12.17 +28:19:20.9 R0 0.0358 17.399 0.109 V SXPHE 290 13:42:21.30 +28:23:45.0 R0 0.2404 15.670 0.060 V RR01 291 13:42:18.07 +28:22:39.6 R0 0.0716 17.462 0.838 V SXPHE 292 13:42:11.18 +28:21:54.0 R0 0.2966 15.704 0.267 V RR1 293 13:42:20.59 +28:28:32.8 R0 0.0295 17.813 0.087 V SXPHE 294 13:42:13.69 +28:25:30.3 R0 0.0388 18.024 0.093 V SXPHE 295 13:41:58.56 +28:27:59.4 R0 0.0361 18.272 0.196 V SXPHE 296 13:41:42.98 +28:24:04.0 R0 0.4460 18.767 0.466 V EB 297 13:41:31.72 +28:24:10.9 R0 0.4020 15.844 0.046 V RR1 298 13:42:12.41 +28:22:34.4 R0 0.2510 15.534 0.2 V RR1 Note 299 13:41:18.85 +28:01:57 R0 0.2492 15.675 0.051 V RR1 300 13:42:08.21 +28:21:38.9 R0 252.85 -- -- L? CX1 13:42:09.77 +28:22:47.6 R0 ---- 18.05 -- V CV? Note CX6 13:42:13.90 +28:23:04.9 R0 ---- 21.32 -- V CV? Note CX9 13:42:11.73 +28:22:34.6 R0 ---- 18.31 -- V RS+E? Note CX14 13:42:13.90 +28:22:20.3 R0 ---- 15.51 -- V RS+E? Note =================================================================== Supplementary Notes The variable stars in M3 have been the subject of many investigations since the pioneering work of Bailey (1902, 1913) who showed that M3 is a variable-rich cluster. Since the late 1990s, M3 has been the subject of numerous CCD photometric investigations, e.g. Kaluzny et al. (1998), Corwin & Carney (2001 - hereafter CC01), Clementini et al. (2004), Hartman et al. (2005), Benko et al. (2006- hereafter Ben06), and Jurcsik et al. (2015, 2017 - hereafter J15, J17). Also, some of the M3 variables were observed by Guhathakurta et al. (1994 - hereafter Gu94) in an HST investigation of the core of M3 and by Drake et al. (2013a,b, 2014) in connection with the Catalina Sky Survey. In addition, Siegel et al. (2015) conducted a near-ultraviolet (NUV) survey of the variable stars in M3 using the UV optical telescope on board the Swift Gamma-ray burst mission. They identified 217 of the variable stars and variable star candidates listed in the 2009 version of our catalogue which included variables numbered up to V298. In 2000, a valuable paper by Bakos et al. (2000 - hereafter Bak00) presented variability types, astrometry and cross-identifications for all previously known or suspected variables in M3 and assigned numbers from V1 to V274, continuing the numbering system of Bailey (1902) and Sawyer Hogg (1973). ----------------- In the above table, the data sources for the variables numbered higher than V274 are from the discovery papers. ----------------- For V1 to V274, the sources are as follows: RA, dec: Samus et al. (2009) unless indicated otherwise in the notes on individual stars Variability types: Bak00, unless indicated otherwise in the notes on individual stars. J15 in the remarks column indicates that the data are from Jurcsik et al. (2015). Periods: Ben06 unless indicated otherwise in the notes. RR Lyrae magnitudes and amplitudes: CC01 or, if designated "Ben06" in the remarks column, they are from Ben06. Since Ben06 did not list amplitudes in their table, the amplitudes were estimated from their light curves. For stars with blended images in the data of both CC01 and Ben06, no magnitudes or amplitudes have been listed. These stars are designated "blend" in the remarks column. NOTE: For the multimode RR Lyrae variables: the periods, magnitudes, and classifications are from J15 and in each case, the period listed pertains to the first overtone mode. NOTE: The V magnitude system of Ben06, J15 and J17 is approximately 0.02 mag fainter on average than CC01's. ------------ Identification charts for most of the variables numbered up to V259 have been published by Kholopv (1977) or by Kadla & Gerashchenko (1982). For V1 to V225, they used the numbering system of Sawyer Hogg (1973). However, for V226 to V259 in the above table, they used their own numbers which are listed below in the "Discovery" section. An important catalog of 1571 M3 stars was published by von Zeipel (1908). It is available from the Harvard ADS. Many authors have cited the von Zeipel numbers. Sawyer (1955) listed vZ numbers for variables V1-204 in her second catalog and for V205-225 in her third catalog (1973). --------------------------------------------------------------==== Notes on individual stars V2: Shapley (1914) commented that V2 (star 9 in his Table II) is a close double and that it is almost certain that both components are variable. However, Bak00 found that neither component varied on the CCD images they obtained. We have therefore classified V2 as non-variable. V4n, V4s: In an investigation based on HST data, Gu94 showed that there were two RR Lyrae variables separated by about 0.5 arcseconds at this location and listed them as #9003 and #9004 (see their Table 3). Their data were not suitable for deriving periods, but they noted that #9004, the southern component had a period of at least 10 hours which is equivalent to 0.42 days. Bak00 designated the two stars as V4n and V4s respectively and published their delta RA and delta dec. The RA and dec listed above have been derived from their values. The HST data were not extensive enough to derive periods and the two components have never been resolved with ground based data. However, Chicherov (1997) derived periods for each component from a frequency analysis of about 900 photographs of M3 obtained with the AZT-2 telescope of the Sternberg Astronomical Institute over a period of more than 30 years. Ben06 listed these periods in their catalogue of variables in M3 (Table 3 of their paper). V29: V29 and V155 were interchanged by Evstigneeva et al. (1994) and by CC01. This was pointed out by Ben06. Therefore the magnitude and amplitude we list for V29 in the above table are the values that CC01 listed for V155. There is some uncertainty in the period of this star because it exhibits the Blazhko effect. CC01 derived P=0.47114 days while Ben06 derived P=0.4717879 days. V75: Drake et al. (2014) derived a shorter period, 0.2389 days for this star, but a 0.314 day period (a difference of one cycle per day) was derived in all other investigations. J15 showed that V75 was an f_0.61 variable. V79: This star has had an interesting pulsation history which was documented by J15. Throughout most of the 20th century V79 pulsated in the fundamental mode and exhibited the Blazhko effect. However, from 1992 to 2007, it was a double mode pulsator with the first overtone mode dominant most of the time. After 2007, it returned to fundamental mode pulsation and exhibited a strong Blazhko effect. V82: Ben06 did not list periods for V82, V91, V115 or V192. For V82, the period, mean magnitude and amplitude listed are the values published by CC01. V82 was also observed by Drake et al. (2013a) who derived a period that was in good agreement with the CC01 value. V91: Ben06 did not list periods for V82, V91, V115 or V192. For V91, the period (0.5294 days), mean magnitude and amplitude listed are the values published by CC01. Siegel et al. (2013) also observed V92 and derived a slightly longer period, 0.5302 days, but the quality of their light curve is not as good so the CC01 value has been adopted. The star exhibits the Blazhko effect. V95: The period (103.73 days), magnitude and amplitude are from Russev (1971). Rosino (1978) classified V95, as a semi-regular variable and Stromgren photometry published by Massari et al. (2016) indicates that the star is located near the red giant tip in the CM diagram. According to the proper motion study of Tucholke et al. (1994) the membership probability for V95 is 98%. V96: For V96, V139, V168, V188 and V195, the mean magnitudes are from Ben06 and amplitudes from CC01 because CC01 did not publish mean magnitudes for these stars. V112: Bailey (1913) commented that the range of variation was small for V112 so no effort was made to determine a period. Sawyer (1939) classified it as non-variable in all of her catalogs. Bak00 pubished a finder chart but did not list a variability type. V112 was not included in the investigations of variable stars by other authors. V113: V113, V123, V205, V206 were outside the field of the early CCD investigations of M3. The period, magnitude and amplitude listed for V113 are from J17. The period is the same as the value published by Szeidl (1965). Samus et al. (2009) noted that V113 is XX CVn in the GCVS. V113 is located at a distance of 11.9 arcminutes from the cluster centre, well within the tidal radius, 28.7 arcmin (Harris 2010) and according to the proper motion study of Tucholke et al. (1994) the membership probability for V113 is 98%. V115: Ben06 did not list periods for V82, V91, V115 or V192. For V115, the period is the mean value adopted by Jurcsik et al. (2012) in their investigation of period changes, and the mean magnitude and amplitude are from CC01. Both CC01 and Jurcsik et al. (2012) have noted that the period of V115 is decreasing. V115 was also observed by Drake et al. (2013a) who derived a period in good agreement with the other studies. V122: This star has a close companion and has a period close to half a day. As a result most investigators could not derive a period. The adopted period (0.4976 days) is from Jurcsik et al. (2017). Ben06 derived a slightly different period (0.5160 days) but their phase coverage was incomplete. V123: V113, V123, V205, V206 were outside the field of the early CCD investigations of M3. The period, magnitude and amplitude listed for V123 are from J17. The period is the same as the value published by Szeidl (1965) and by Drake et al. (2013a). V123 is located at a distance of 17.1 arcminutes from the cluster centre, well within the tidal radius, 28.7 arcmi andn according to the proper motion study of Tucholke et al. (1994) the membership probability for V123 is 98%. V127: Bailey (1913) was unable to derive a period for V127 because it had two close companions. Muller (1933) subsequently showed that the northern component, which he designated as V146, was the variable. Sawyer Hogg (1939) therefore classified V127 as non-variable in her first and subsequent catalogs. Later, Kholopov (1963) found that the southwest component (his X34 = vZ 1198) was also variable. Sawyer Hogg (1973) designated X34 as V222 in her 3rd catalog. In the 2003 update to the Clement catalogue, there was an error of about 100 arcseconds in the published dec for V127 and the incorrect value was adopted by Samus et al. (2009). The coordinates listed in the above table for V127 are derived from Bak00. V138: The period, magnitude and amplitude are from Olah and Russev (1979). Rosino (1978) classified V138 as a semi-regular variable and Stromgren photometry published by Massari et al. (2016) indicates that the star is located near the red giant tip in the CM diagram. Welty (1985) confirmed the variability of V138, but questioned Russev's amplitude because of inconsistencies between telescopes. According to the proper motion study of Tucholke et al. (1994) the membership probability for V138 is 98%. V139: Magnitudes are from Ben06 and amplitude from CC01. See V96. V140: When the M3 file was posted in 2009, V140 was incorrectly listed as an RR0 type. It should be RR1. Marcio Catelan (2011, private communication) pointed out the error. V141: V141=RV CVn in the GCVS. Period, magnitude, amplitude and classification are from Szeidl (1973) who considered it to be a field star. The proper motion study by Tucholke et al. (1994) listed a membership probability of 69%, indicating that it could be a cluster member. V146: According to Ben06, V146 and V222 were interchanged by CC01 and by Clementini et al. (2004). The magnitude and amplitude listed for V146 in the above table are the values listed by CC01 for V222. Kholopov (1977) pointed out that the observations that Greenstein (1935) published for V146 are really for V222. See also the comment for V127. V154: The period, listed above (15.2842 days) is from Ben06 and was confirmed by Siegel et al. (2015). The magnitude, amplitude and variability type are from Kholopov (1972) who derived P=15.290 days. Goranskij (1994) noted that V154 was #9024 in the Gu94 investigation. V155: V29 and V155 were interchanged by Evstigneeva et al. (1994) and by CC01. This was pointed out by Ben06. Therefore the period (0.331684 days), magnitude and amplitude we list for V155 are the values that CC01 listed for V29. Ben06 derived a slightly longer period (0.33805 days) but their light curve had more scatter. V157: The mean magnitude is from Ben06 because CC01 did not publish a value. No amplitude has been listed because it was difficult to estimate because of Blazhko effect. V158: Greenstein (1935) derived a period of 0.50809 which was listed by Sawyer Hogg in her catalogs. However, in her 2nd and 3rd catalogs, she indicated that the period was uncertain. Bak00 did not detect any variation. Therefore V158 is classified as constant. V162: Greenstein (1935) classified this star as non-variable. He noted that it was part of a triple system. However, Kholopov (1963) later found that one of the other stars in the triplet (vZ 950 = X28) was variable. Sawyer Hogg (1973) designated vZ 950 (X28) as V218 in her 3rd catalog. Ben06 derived a period of 0.5449 for V218. Later, Siegel et al. (2015) listed a period of 0.54484 for V162, but no period for V218. We therefore assume that Siegel's V162 is the same star as V218 in the above table. V163: Greenstein (1935) classified this star as non-variable and Sawyer (1939) classified it as non-variable in all three of her catalogs. However, Bak00 noted that the x,y position listed for V163 in Sawyer Hogg's catalogs was midway between V180 and a non-variable. According to Bak00, Kholopov (1977) labelled the non-variable as V163 so Bak00 accepted the non-variable as V163 to avoid confusion and labelled V180 as a variable. See also the comments for V180. V164: Greenstein (1935) noted that this star was badly blended and and that, if it was variable, its range was less than 0.35 mag. Ben06 classified it as non variable. CC01 derived a period, but in their subsequent paper (Clementini et al. 2004), they noted that the star they called V164 was actually V234. V165: Bak00 pointed out that there was an error in the sign of the "y" coordinate listed for this star in Sawyer Hogg's (1973) 3rd catalog, but it was correct in the 1939 and 1955 editions. The mean magnitude and amplitude we list for V165 were derived by Ben06 because CC01 did not publish an amplitude or mean magnitude for V165. V168: The mean magnitude is from Ben06 and the amplitude from CC01. See V96. V179: Greenstein (1935) commented that the star was difficult to measure and that if it was variable, it had a small range. Sawyer (1939) classified it as non-variable in all 3 of her catalogs. Bak00 were unable to locate the star unambiguously on POSS images. The RA and dec listed in the above table were calculated by Samus (2009, private communication). He derived a relation between x,y and RA, dec based on 39 M3 stars and used it to calculate the RA and dec for V179 from the published x,y coordinates. There is a 2MASS star in the same location. V180: V180 = vZ 676: Shapley (1914) stated that vZ 676 was composed of five distinct stars, of which the variable is the brightest and most centrally located. Greenstein (1935) could not measure it because of the crowding. Sawyer (1939) classified it as non-variable in all three of her catalogs. However, Kholopov (1977) and Bak00 found that there are two RR Lyrae variable stars close to (and equidistant from) the position listed for V180 in Sawyer Hogg's catalogs. The eastern component was chosen by them to be V180 and the western component, Kholopov's X13 was designated V239 by Bak00. See also the comments for V163. The period, magnitude, amplitude and classification listed for V180 in the above table are from Ben06. The amplitude was estimated from their published light curve. V182: Greenstein could not confirm the variability of this star. Sawyer (1939) classified it as non variable in all three of her catalogs and Bak00 and Ben06 confirmed its non-variable status. V183: Greenstein commented that V183 was blended with V145. Sawyer (1939) classified it as non-variable in all three of her catalogs. Bak00 confirmed its non-variable status. V185: Greenstein commented that this was a bright star with a small range. Bak00 did not detect any variation, nor did Clementini et al. (2004). CC01 and Ben06 did not study it. It is therefore classified as non-variable. V188: The magnitude is from Ben06 and amplitude from CC01. See V96. V192: Ben06 did not list periods for V82, V91, V115 or V192. The image of V192 is severely blended so it is not possible to derive a reliable mean magnitude or amplitude. CC01 derived a period, 0.48145 days, but noted that it was uncertain. Siegel et al. (2015) derived a slightly longer period, 0.4973590 day from the Swift NUV data. Since their light curve looks better than that of CC01, their period has been adopted. V195: The magnitude is from Ben06 and amplitude from CC01. See V96. V196: The variation of V196 was announced by Greenstein. He could not derive a period because it was a double star and difficult to measure. Bak00 found that both components are constant. V198: Bak00 did not confirm variation in this star based on one night of observations. CC01 derived a period from their observations and commented that the star appears to be slightly above the HB of the CMD. However, in a later paper, (Clementini et al. 2004), they stated that they had erroneously listed V245 as V198. V198 is therefore no longer considered to be variable. V199: This star is no longer considered to be variable. Its apparent variablity was due to blending. Near IR photometry (Valenti et al. 2004) and Stromgren photometry (Massari et al. 2016) both indicate that there are two stars near the published position of V199. One of them is located on the blue HB of the CM diagram and the other is on the giant branch near the red HB. V199 was listed as a possible variable by Greenstein (1935) who derived a period of 0.488, but noted that it was doubtful. CC01 also derived a period but indicated that it was uncertain and they did not publish a light curve or list a mean magnitude. Furthermore, they did not include it in their subsequent study (Cacciari et al. 2005). V199 was not detected in the ultraviolet investigation of M3 variables by Siegel et al. (2015) and it was outside the HST field investigated by Gu94. V204: This star was incorrectly listed as von Zeipel 390 (instead of 1390) in Sawyer's (1955) 2nd catalog. As a result, its x,y was incorrect in her 2nd and 3rd catalogs. The RA and dec listed above were derived from the position listed by Bak00 who pointed out the error. According to CC01 and Ben06, V204 is non-variable. However, Yao (2007) claims that it is a red HB star with a period of 0.74785 and V amplitude 0.04. V205: V113, V123, V205, V206 were outside the field of the early CCD investigations of M3. V205 is WY CVn in the GCVS (Evstigneeva et al. 1994) The period, magnitude and amplitude listed above for V205 are from J17. The period is the same as the earlier value derived by Kukarkin (1960) and by Drake et al. (2013a). V205 is located at a distance of 21.4 arcminutes from the cluster centre, within the tidal radius, 28.7 arcmin. It was not included in the proper motion study of Tucholke et al. (1994), but its mean magnitude is appropriate for cluster membership. V206: V113, V123, V205, V206 were outside the field of the early CCD investigations of M3. V206 is WZ CVn in the GCVS (Evstigneeva et al. 1994). The period, magnitude and amplitude listed for V206 are from Drake et al. (2013a) and the period is in good agreement with the earlier value derived by Kukarkin (1960). V206 is located at a distance of 28.9 arcminutes from the cluster centre, close to the tidal radius, 28.7 arcmin. However, according to the proper motion study of Tucholke et al. (1994) the membership probability for V206 is 97% and its mean magnitude is appropriate for cluster membership. V208: The period derived by Ben06 and J15 (0.3384 days) has been adopted. Siegel et al. (2015) derived a slightly longer period (0.3696 days) from the Swift NUV data, but it appears this was due to an error in cycle count; the number of cycles elapsed in 4 days differs by one. A similar difference was found in the period they derived for V249. V217: From their HST observations, Gu94 classified this star (Gu9023) as an RR Lyrae, but did not have enough observations to derive a period. Because of its location near the cluster centre, other investigators had difficulty observing the star. However, in their NUV investigation of the M3 variables, Siegel et al. (2015) were able to derive a period, 0.5283713 days, which is listed in the above table. V218: See note for V162. V222: According to Ben06, V146 and V222 were interchanged by CC01 and by Clementini et al. (2004). The magnitude and amplitude that listed for V222 in the above table are the values listed by CC01 for V146. See the comment for V146. V224: Bak00 confirmed that this star was variable, but also commented that its image merges with that of a nearby star. It was not investigated further in their subsequent paper (Ben06) and Clementini et al. (2004) were unable to obtain any data. Therefore its variablility status is questionable. V224 was outside the field of the Gu94 HST investigation. V225: The period, magnitude and amplitude are from Russev (1971). Rosino (1978) classified V225 as a semi-regular variable and Stromgren photometry published by Massari et al. (2016) indicates that the star is located near the red giant tip in the CM diagram. Welty (1985) confirmed the variability of V225, but questioned Russev's amplitude because of inconsistencies between telescopes. According to the proper motion study of Tucholke et al. (1994) the membership probability for V225 is 97%. V229: The image is blended and the period is uncertain. The light curve plotted by Ben06, with P= 0.4992 days looks good, but there is a large phase gap on the descending branch. Siegel et al. (2015) derived a shorter period (0.4976 days) from NUV data, but their light curve has more scatter. J17 derived a longer period, 0.51606 days, but did not publish a light curve. However, the J17 period has been adopted because it is assumed that they had better phase converage than Ben06. V230: This was Kholopov's (1977) X41. It was not labelled on his ID chart because it was too far from the cluster centre and it was not studied by CC01 or by Ben06. Also Clementini et al. (2004) were unable to obtain data. Siegel et al. (2015) listed a period of 20.29 days for V230, based on Swift NUV data, but did not publish a light curve or provide further discussion. Their investigation dealt mainly with RR Lyrae variables. V234: CC01 classified V234 as non-variable, but in their subsequent paper (Clementini et al. 2004), they noted that the star they called V164 was V234. According to CC01, this star is an RR Lyrae that might be more distant than the cluster so it has been classified as a field star. V236 (vZ 1397): The period (31.395 days), magnitude and amplitude in the above table are from Olah (1979) based on 195 Budapest observations obtained between 1938 and 1962. A period of 215.8 days also fit the data. The star was also discussed by Welty (1985) who derived periods of 32.2 and 60.2 from Yerkes observations obtained between 1978 and 1983. Welty preferred the 60 day period. Stromgren photometry published by Massari et al. (2016) for V236 indicates that it is located near the red giant tip in the CM diagram and the star has therefore been classified as SR. According to the proper motion study of Tucholke et al. (1994) the membership probability for V236 is 97%. V237, V238, V239: Ben06 pointed out that the dec values for V238 and V239 were incorrectly listed in the 2001 on-line version of this catalog. Meanwhile, Hartman et al. (2005) pointed out that the coordinates of V237 and V238 were switched in the discovery paper (Kaluzny) and that this error had propagated through to the catalog of Bak00. The coordinates listed for V237, V238, V239 have all been revised accordingly in the above table. The RA and dec for V237 and V238 are the values published by Samus et al. (2009) for V238 and V237 respectively. The RA and dec for V239 are the values listed by Ben06. V237: The period, magnitude, amplitude and classification are from Hartman et al. (2005). V238: Period, magnitude, amplitude and classification from the discovery paper by Kaluzny et al. (1998) The non-membership status for V238 is from Rucinski (2000). V240: The mean magnitude is from CC01, but since these authors did not publish an amplitude, the amplitude was estimated from the light curve published by Ben06. V249: The period derived by Ben06 and J17 (0.5330 days) has been adopted. Siegel et al. (2015) derived a longer period (0.6149 days) from the Swift NUV data, but it appears this was due to an error in cycle count; the number of cycles elapsed in 4 days differs by one. A similar difference was found in the period they derived for V208. V250n, V250s: Ben06 discovered that the image of V250 consisted of two close companions, both RR0 variables. They derived a period for each star, 0.5671499 for 250n and 0.5861391 for 250s. However, separate light curves were not plotted and no magnitudes were published. J17 listed 0.5744 for 250a and 0.5924 for 250b, based on image subtraction method photometry. Because of these differences, only two digits are listed for the periods. The RA and dec are from Ben06. V260: This star (vZ 297) is among the brightest stars on the giant branch and Walker (1955) suggested that it might be variable. It was later designated as V260 by Bak00, but the variation was not confirmed in the photographic investigations of Olah (1979) and Welty (1985). However, since these studies were based on photographic data, the possibility of light variations with amplitude less than 0.15 mag are not ruled out. The variability status of V260 is uncertain. According to the proper motion study of Tucholke et al. (1994) the membership probability for V260 is 98%. V262: Gu94 classified this star (Gu 552) as an RR Lyrae variable from their HST data. Consequently, Bak00 designated it as V262, but found no trace of variation detectable on their light curve. The star was not included in the subsequent investigations of Clementini et al. (2004) or Ben06 because it was close to V241 and could only be resolved on HST images. It was classified as "CST?" in earlier versions of this catalogue. However, J17 derived a period (0.65508 days) from their image subtraction photometry data so V262 is now classified as RR0. V265, V267, V268: V265=Gu 1489, V267=Gu 9016, V268=Gu 9025: These stars all have close companions. The variability types were assigned by Gu94, based on HST data, but they did not derive precise periods for any of them. Clementini et al. (2004) commented that V265 and V268 were RR Lyrae variables blended with V154. V269: The period is uncertain due to blending. Ben06 derived a period of 0.3592861 days, but their light curve has more scatter than for the other variables. Siegel et al. (2015) derived 0.3557017 days from NUV observations, but their light curve has a very small amplitude due to the blending. J15 could not derive a period. V270n,s: Ben06 discovered that the image of V270 consisted of two close companions, both RR0 variables. They derived a period for each star, 0.625819 days for V270n and 0.690195 for V270s, but the light curves showed a lot of scatter because of the blending. They did not derive individual magnitudes for each star. These stars were labelled as V270 b,a respectively by J17 who listed periods of 0.62585 and 0.69018 respectively, derived from image subtraction method photometry. The RA and dec listed in the above table are from Ben06. V272, V273, V274: Light curves based on the image subtraction method were published by Bak00. Ben06 noted that they varied on "long" time scales. Stromgren photometry published by Massari et al. (2016) for these three stars indicates that they all lie near the red giant tip in the CM diagram. Therefore they have all been classified as SR. According to the proper motion study of Tucholke et al (1991), the membership probabilities for these three stars are 98%, 64% and 0% respectively. S1-S11: Strader et al. (2002) announced the discovery of 11 new suspected variables (S1-11). They derived periods ranging from 7 to 32 hours for 9 of the stars, but the observations of Ben06 did not confirm any of these discoveries. (See final sentence in section 3.2 of their paper.) When Hartmann et al. (2005) set up their numbering system for V286 to V297, they left a gap from V275 to V285 to accommodate these 11 variables. However, we have not assigned numbers to them because of Ben06's result. V298: This star is N2 in the paper by Ben06 and all of the information listed for it is from their paper. CX1, CX6, CX9, CX14 The data and classifications for the optical counterparts to these four Chandra X-ray sources are from Zhao et al. (2019). All of them are considered to be proper motion members of M3. ================================================================== Discovery of the Variable Stars in M3: V1-137 and star b Bailey (1902) with ID chart (Fig 1) and x,y coordinates (pages 238-239) Bailey (1913) with ID chart (Fig 1) and von Zeipel numbers (page 10) V138 = Bailey's star b (see Bailey 1913, pages 8-9) The number 138 was assigned by Larink (1922) V139-141 Larink (1922) with x,y positions; V141 is RV CVn. The variability of V141 was previously announced by Larink (1921), but it was identified only by RA and dec in the earlier paper. V142-183 Muller (1933) with x,y coordinates V184-199 Greenstein (1935) with x,y coordinates V200-201 = star numbers 12 and 14 from Table I of Shapley (1914). The numbers V200 and 201 were assigned by Sawyer (1939) in her 1st catalog. She also derived their x,y coordinates on the system of Bailey. V202 = von Zeipel #190 Schwarzschild (1940) announced that this star was variable and Sawyer (1955) designated it as V202 in her 2nd catalog V203-204 = star C and star I-I-42 in the ID chart of Sandage (1953) Roberts & Sandage (1955) announced the variability of these two stars and Sawyer (1955) designated them as V203 and 204 in her 2nd catalog. She also listed their von Zeipel numbers and derived x,y coordinates. She incorrectly listed V204 as vZ 390, instead of 1390. As a result, the x,y coordinates she listed for V204 were incorrect. Bak00 listed the correct position for this star. V205-206 = SVS (Soviet Variable Star) 1264 and 1276 Kurochkin (1959, 1960) These studies announced new variable stars in the vicinity of M3; SVS 1264 and 1276 were the only ones inside the tidal radius. Kukarkin (1960) later identified them as von Zeipel 89 and 1221 respectively and Sawyer Hogg (1973) designated them as V205 and 206 in her 3rd catalog. V207-224 = X3, X4, X6 X8, X9, X11, X12, X15, X16, X19, X27, X28, X29, X31, X32, X34, X37, X38 Kholopov (1963) with x,y coordinates, ID chart and von Zeipel numbers if available. The numbers V207-224 were assigned by Sawyer Hogg (1973) in her 3rd catalog. V225 = von Zeipel 837 Russev (1971) with von Zeipel number. He also indicated that vZ 238 was variable. Sawyer Hogg (1973) designated vZ 837 as V225 in her 3rd catalog, but she did not include vZ 238 which had a smaller amplitude. V226 = SVS 2041 Kholopov (1974) with x,y coordinates and ID chart In a later paper, Kholopov (1977) listed it as X39. We designated this as V226 in our first on-line update to the catalog (Clement 1997). V227-235 = X7, X10, X40, X41, X42, X43, X44, X47, X49 Kholopov (1977) with ID chart (for all except X41), x,y coordinates, von Zeipel and/or SVS number. These were designated as V227-235 in the first on-line update to the catalog (Clement 1997). V236 = von Zeipel 1397 This star (vZ 1397) is among the brightest stars on the giant branch and Walker (1955) suggested that it might be variable. Olah (1979) confirmed the variation. vZ 1397 was designated as V236 in the first on-line update to the catalog (Clement 1997). V237-238 Kaluzny et al. (1998) with x,y coordinates and ID charts. According to Hartman et al. (2005), the coordinates of V237 and V238 were switched in the discovery paper and this error propagated through to the compilation by Bak00. The coordinates listed for these two stars in the above table have been revised accordingly. V239-248 = X13, X14, X17, X20, X22, X23, X25, X30, X35, X36 Kholopov (1963) with x,y coordinates, ID chart and von Zeipel numbers if available. The numbers V239-248 were assigned by Bak00. Sawyer Hogg (1973) was aware of Kholopov's paper because it was the discovery paper for her V207-224, but apparently she did not consider these other stars to be M3 variables. V249-259 = KG1, KG2, KG3, KG4, KG7, KG8, KG9, KG11, KG12, KG14, KG15 Kadla & Gerashchenko (1980) listed 17 suspected variable stars, 1 to 17 with x,y coordinates (on a different system from Bailey), Delta B and von Zeipel number if available. In a later paper (Kadla & Gerashchenko 1982), they listed only KG 1-15 as new variables and published ID charts for these stars as well as for V1-225 and Kholopov's (1963, 1977) variables. Eleven of these KG stars were designated as V249-259 by Bak00. Bak00 did not consider KG5, KG6 or KG13 to be variable and they concluded that KG10 was the same star as V194. V260 = von Zeipel 297 This star (vZ 297) is among the brightest stars on the giant branch and Walker (1955) suggested that it might be variable. vZ 297 was later designated as V260 by Bak00. However, the variation of this star has not yet been confirmed. V261-268 = Gu32, Gu552, Gu576, Gu586, Gu1489, Gu9012, Gu9016, Gu9025 These were announced as variables by Gu94 who published delta RA and delta dec values. They were designated as V261-268 by Bak00 who published ID charts and delta RA and delta dec  measured with respect to  RA=13:42:11.2 and dec=+28:22:32 (J2000). V269-274 Bak00 with ID charts and delta RA and delta dec measured with respect to RA=13:42:11.2 and dec=+28:22:32 (J2000). S1-S11: Strader et al. (2002) Ben06 were unable to confirm these discoveries and no data have been listed for them in the above table. V286-297 = NV286-297 Hartman et al. (2005) with RA and dec The gap in the numbering system between V274 and V286 occurs because of the 11 Strader et al. suspected variables which were not considered by Ben06 to be variable. V298 = N2 Ben06 These authors also made independent discoveries of V291 (their N1) and V292 (their N3) V299 = NV Jurcsik et al. (2017) with RA and dec V300 Siegel et al. (2015) with RA and dec CX1 This Chandra X-ray source in M3 is the same as 1E 1339.8+2837 which was first detected by the Einstein observatory. Using HST observations in U, V and I, Edmonds et al. (2004) detected variability in their plausible candidate for the optical counterpart of this source. They published a finder chart and RA, dec (2000). The variability was later confirmed by Zhao et al. (2019). CX6, CX9, CX14 These are Chandra X-ray sources in M3 announced by Zhao et al. (2019). They detected 16 X-ray sources within the half-light radius (2.3') and found plausible optical/UV counterparts for 10 of them. UV and optical variability was detected in these three sources. They published finding charts and RA, dec (2000) for all 10 of their optical/UV counterparts. ------------------------------------------------------ Previously known RR Lyrae variables recovered in the Catalina survey by Drake et al. (2013a,2013b,2014) Drake et al. (2013a) Catalina ID V Per (d) Vamp ID CSSJ134047.6+283326 15.69 0.6369032 0.47 V205 CSSJ134134.0+283025 15.71 0.5148095 1.10 V116 CSSJ134134.5+281856 15.62 0.5236852 0.96 V94 CSSJ134137.9+282434 15.72 0.5012926 0.89 V83 CSSJ134147.4+281605 15.47 0.6023073 0.61 V93 CSSJ134148.9+282632 15.53 0.6401389 0.37 V120 CSSJ134149.5+281914 15.47 0.5415572 0.80 V9 CSSJ134152.3+280602 15.69 0.5454910 0.92 V123 CSSJ134152.9+282442 15.53 0.5871094 0.59 V39 CSSJ134153.0+282030 15.38 0.5368978 0.53 V45 CSSJ134154.7+282752 15.61 0.5196060 0.91 V108 CSSJ134159.9+281912 15.63 0.5078999 1.11 V11 CSSJ134201.4+282444 15.03 0.5683071 0.60 V67 CSSJ134202.0+282210 15.69 0.4800641 1.57 V25 CSSJ134202.8+282721 15.21 0.5953799 0.46 V23 CSSJ134203.8+282443 15.06 0.6202254 0.46 V66 CSSJ134203.8+281241 15.67 0.5245456 0.93 V82? CSSJ134203.9+281239 15.70 0.5245415 0.96 V82? CSSJ134209.3+281553 15.66 0.5035447 0.84 V92 CSSJ134212.1+283304 15.66 0.5977218 0.77 V114 CSSJ134218.3+281454 15.61 0.6005285 0.86 V117 CSSJ134220.0+282812 15.76 0.6054515 0.65 V64 CSSJ134220.4+275350 15.65 0.5093377 0.91 V206 CSSJ134220.8+282810 15.44 0.6683344 0.93 V65 CSSJ134221.8+282530 14.87 0.5591099 0.36 V34 CSSJ134221.9+282103 15.13 0.5482318 0.69 V49 CSSJ134222.3+281523 15.59 0.5761617 0.60 V17 CSSJ134223.0+282501 15.09 0.5695082 0.46 V10 CSSJ134224.4+282207 15.41 0.5455972 1.31 V36 CSSJ134225.7+282846 15.70 0.5208700 0.93 V61 CSSJ134236.8+281812 15.52 0.4912573 0.79 V20 CSSJ134238.0+281838 15.62 0.6319630 0.39 V19 CSSJ134243.0+282727 15.63 0.5384629 0.92 V80 CSSJ134244.6+282345 15.59 0.6734891 0.20 V73 CSSJ134245.1+283347 15.66 0.5133518 0.96 V115 CSSJ134245.2+282241 15.57 0.4560852 0.96 V72 ------------------------------------ - Drake et al. (2013b) Catalina ID V Per (d) Vamp ID CSSJ134150.8+282433 15.48 0.551526 0.92 V40 CSSJ134203.3+281803 15.51 0.530560 0.74 V35 CSSJ134204.6+281806 15.04 0.530067 0.72 V15 CSSJ134218.1+282938 15.38 0.652410 0.53 V62 ------------------------------------- Drake et al. (2014) Catalina ID V Per (d) Vamp ID CSSJ134153.5+282526 15.59 0.3266358 0.43 V37 CSSJ134200.6+282840 15.53 0.3296010 0.41 V56 CSSJ134201.7+281925 15.29 0.3349270 0.31 V97 CSSJ134202.1+282343 15.64 0.5143280 1.23 V6 CSSJ134203.1+281853 15.32 0.5888109 0.66 V59 CSSJ134205.6+282816 15.51 0.3090350 0.53 V107 CSSJ134210.8+282444 15.10 0.5048850 0.63 V53 CSSJ134214.6+282831 15.62 0.4832990 0.91 V79 CSSJ134215.0+282521 15.82 0.2388550 0.56 V75 P should be 0.3141 CSSJ134218.9+281933 15.31 0.5170315 0.72 V90 CSSJ134234.6+282629 15.48 0.3558230 0.50 V85 CSSJ134250.2+282048 15.34 0.2926590 0.38 V86 ================================================================== References Bailey, S. I. 1902, Harv. Ann., 38 Bailey, S. I. 1913, Harv. 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