NGC 5272 / C1339+286 / Messier 3 (Updated 2009) 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 or P (for photographic). 61-65 A5 Type of variable (draft 2006 GCVS classifications) NV denotes not variable 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 13:42:11.13 +28:20:33.9 R0 0.5206 15.591 1.15 V RR0 2 13:42:12.72 +28:23:35.3 R0 ---- -- -- V NV Note 3 13:42:15.71 +28:21:41.6 R0 0.5582 15.545 1.22 V RR0 4n 13:42:08.19 +28:22:33.5 R0 0.5850 -- -- V RR0 4s 13:42:08.22 +28:22:33.2 R0 0.5931 -- -- V RR0 5 13:42:31.29 +28:22:20.9 R0 0.5057 15.592 0.88 V RR0 6 13:42:02.10 +28:23:41.7 R0 0.5143 15.686 1.20 V RR0 7 13:42:11.10 +28:24:10.4 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 Benko 9 13:41:49.51 +28:19:13.6 R0 0.5416 15.630 1.06 V RR0 10 13:42:23.10 +28:25:00.7 R0 0.5695 15.615 0.89 V RR0 11 13:41:59.99 +28:19:12.0 R0 0.5079 15.580 1.30 V RR0 12 13:42:11.26 +28:20:17.2 R0 0.3179 15.557 0.57 V RR1 13 13:42:09.59 +28:20:24.7 R0 0.4795 15.612 0.86 V RR01 Note 14 13:42:07.82 +28:20:01.3 R0 0.6359 15.506 1.08 V RR0 15 13:42:04.68 +28:18:08.7 R0 0.5301 15.597 1.11 V RR0 16 13:41:48.72 +28:21:08.3 R0 0.5115 15.676 1.15 V RR0 17 13:42:22.41 +28:15:22.8 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 13:42:38.11 +28:18:37.9 R0 0.6320 15.679 0.49 V RR0 20 13:42:36.83 +28:18:11.9 R0 0.4913 15.611 1.04 V RR0 21 13:42:37.78 +28:23:01.7 R0 0.5158 15.656 1.12 V RR0 22 13:42:25.92 +28:22:32.2 R0 0.4814 15.654 1.08 V RR0 23 13:42:02.85 +28:27:20.9 R0 0.5954 15.621 0.86 V RR0 24 13:42:00.32 +28:22:52.1 R0 0.6634 15.499 0.87 V RR0 25 13:42:02.09 +28:22:10.3 R0 0.4801 15.642 1.28 V RR0 26 13:41:58.05 +28:21:58.6 R0 0.5977 15.539 1.03 V RR0 27 13:42:03.18 +28:20:59.3 R0 0.5791 15.610 0.95 V RR0 28 13:42:09.63 +28:20:56.6 R0 0.4706 15.651 1.09 V RR0 29 13:42:06.59 +28:21:28.6 R0 0.4718 15.622 1.22 V RR0 Note 30 13:42:08.73 +28:23:40.1 R0 0.5121 15.571 1.24 V RR0 31 13:42:13.99 +28:23:47.6 R0 0.5807 15.527 1.25 V RR0 32 13:42:12.40 +28:23:42.5 R0 0.4954 15.558 1.23 V RR0 33 13:42:16.84 +28:21:13.5 R0 0.5252 15.614 1.25 V RR0 34 13:42:21.72 +28:25:32.7 R0 0.5591 15.638 1.05 V RR0 35 13:42:03.45 +28:18:03.6 R0 0.5305 15.570 1.37 V RR0 36 13:42:24.54 +28:22:07.6 R0 0.5456 15.618 1.17 V RR0 37 13:41:53.57 +28:25:25.8 R0 0.3266 15.637 0.51 V RR1 38 13:41:56.05 +28:24:49.2 R0 0.5580 15.628 1.08 V RR0 39 13:41:52.98 +28:24:42.6 R0 0.5871 15.674 0.89 V RR0 40 13:41:50.94 +28:24:33.2 R0 0.5515 15.680 1.02 V RR0 41 13:42:04.40 +28:23:35.9 R0 0.4859 15.728 0.87 V RR0 42 13:42:05.52 +28:23:22.6 R0 0.5901 15.476 1.36 V RR0 43 13:42:19.07 +28:23:07.1 R0 0.5405 15.651 1.29 V RR0 44 13:42:24.37 +28:24:22.2 R0 0.5064 15.620 0.75 V RR0 45 13:41:53.24 +28:20:31.5 R0 0.5369 15.649 1.17 V RR0 46 13:42:01.83 +28:21:50.7 R0 0.6134 15.668 0.64 V RR0 47 13:42:02.62 +28:21:29.0 R0 0.5409 15.666 0.85 V RR0 48 13:42:21.17 +28:21:00.4 R0 0.6278 15.494 0.66 V RR0 49 13:42:22.11 +28:21:02.8 R0 0.5482 15.677 0.95 V RR0 50 13:42:12.25 +28:18:48.0 R0 0.5128 15.595 1.20 V RR0 51 13:42:13.88 +28:18:56.1 R0 0.5840 15.621 0.86 V RR0 52 13:42:05.63 +28:25:13.5 R0 0.5162 15.705 1.01 V RR0 53 13:42:10.94 +28:24:44.9 R0 0.5049 15.638 1.20 V RR0 54 13:42:08.99 +28:24:28.6 R0 0.5063 15.691 0.74 V RR0 55 13:41:55.93 +28:28:05.8 R0 0.5298 15.666 1.08 V RR0 56 13:42:00.69 +28:28:39.9 R0 0.3296 15.614 0.50 V RR1 57 13:42:23.26 +28:22:42.4 R0 0.5122 15.676 1.15 V RR0 58 13:42:04.95 +28:23:28.1 R0 0.5171 15.509 1.28 V RR0 59 13:42:03.25 +28:18:53.4 R0 0.5888 15.646 0.79 V RR0 60 13:41:49.06 +28:17:25.7 R0 0.7077 15.520 0.75 V RR0 61 13:42:25.80 +28:28:45.8 R0 0.5209 15.641 1.03 V RR0 62 13:42:18.23 +28:29:39.3 R0 0.6524 15.620 0.58 V RR0 63 13:42:14.24 +28:28:24.2 R0 0.5704 15.661 0.79 V RR0 64 13:42:20.12 +28:28:12.6 R0 0.6055 15.664 0.75 V RR0 65 13:42:20.93 +28:28:10.1 R0 0.6683 15.496 0.97 V RR0 66 13:42:03.79 +28:24:43.0 R0 0.6202 15.607 0.80 V RR0 67 13:42:01.52 +28:24:44.5 R0 0.5683 15.657 1.17 V RR0 68 13:42:13.11 +28:25:37.2 R0 0.3560 15.642 0.86 V RR01 69 13:42:17.58 +28:25:03.4 R0 0.5666 15.673 0.99 V RR0 70 13:42:14.34 +28:25:14.6 R0 0.4864 15.350 0.40 V RR1 71 13:42:23.66 +28:22:40.5 R0 0.5491 15.659 0.80 V RR0 72 13:42:45.24 +28:22:41.5 R0 0.4561 15.679 1.30 V RR0 73 13:42:44.71 +28:23:45.9 R0 0.6736 15.623 0.29 V RR0 74 13:42:18.15 +28:25:13.2 R0 0.4922 15.653 1.30 V RR0 75 13:42:15.14 +28:25:21.5 R0 0.3141 15.626 0.54 V RR1 76 13:42:10.42 +28:21:14.2 R0 0.5018 15.719 1.38 V RR0 77 13:42:04.30 +28:23:09.9 R0 0.4593 15.725 1.30 V RR0 78 13:42:15.06 +28:23:49.0 R0 0.6119 15.554 0.86 V RR0 79 13:42:14.72 +28:28:31.7 R0 0.3581 15.658 0.66 V RR01 80 13:42:43.03 +28:27:28.0 R0 0.5384 15.646 0.61 V RR0 81 13:42:37.37 +28:28:34.3 R0 0.5291 15.656 1.10 V RR0 82 13:42:03.90 +28:12:40.6 R0 0.5245 15.601 1.21 V RR0 Note 83 13:41:38.01 +28:24:33.7 R0 0.5013 15.651 1.20 V RR0 84 13:42:16.32 +28:25:27.3 R0 0.5957 15.630 0.72 V RR0 85 13:42:34.65 +28:26:29.2 R0 0.3558 15.483 0.52 V RR1 86 13:42:50.39 +28:20:49.2 R0 0.2927 15.637 0.57 V RR1 87 13:42:19.86 +28:23:42.7 R0 0.3575 15.578 0.71 V RR01 88 13:42:08.84 +28:21:32.4 R0 0.2987 15.714 0.58 V RR1 89 13:42:13.62 +28:20:51.7 R0 0.5485 15.579 1.13 V RR0 90 13:42:18.92 +28:19:34.3 R0 0.5170 15.639 1.17 V RR0 91 13:42:10.58 +28:13:32.1 R0 0.5294 15.616 1.24 V RR0 Note 92 13:42:09.39 +28:15:53.6 R0 0.5035 15.632 1.14 V RR0 93 13:41:47.41 +28:16:04.4 R0 0.6023 15.640 0.76 V RR0 94 13:41:34.55 +28:18:55.5 R0 0.5237 15.677 1.18 V RR0 95 13:41:59.77 +28:22:57.3 R0 103.73 14.03 0.74 P SR Note 96 13:41:59.13 +28:18:47.6 R0 0.4994 15.652 1.21 V RR0 Note 97 13:42:01.71 +28:19:24.9 R0 0.3349 15.651 0.45 V RR1 98 13:42:21.53 +28:22:39.3 R0 ---- 15.593 -- V NV 99 13:42:26.76 +28:21:48.1 R0 0.3609 15.602 0.77 V RR01 100 13:42:16.77 +28:24:20.0 R0 0.6188 15.681 0.67 V RR0 101 13:42:14.99 +28:24:05.9 R0 0.6439 15.696 0.68 V RR0 102 13:42:15.89 +28:24:37.4 R0 ---- 15.674 -- V NV 103 13:42:15.91 +28:24:42.7 R0 ---- 15.930 -- V NV 104 13:42:09.51 +28:25:07.5 R0 0.5699 15.536 1.25 V RR0 105 13:42:09.86 +28:25:53.4 R0 0.2877 15.532 0.35 V RR1 106 13:42:07.81 +28:25:30.1 R0 0.5471 15.668 0.92 V RR0 107 13:42:05.65 +28:28:16.8 R0 0.3090 15.631 0.59 V RR1 108 13:41:54.79 +28:27:52.1 R0 0.5196 15.692 1.14 V RR0 109 13:42:04.74 +28:22:44.5 R0 0.5339 15.673 1.23 V RR0 110 13:42:03.94 +28:22:26.3 R0 0.5355 15.626 1.15 V RR0 111 13:42:04.46 +28:23:03.9 R0 0.5102 15.713 1.14 V RR0 112 13:42:00.80 +28:10:42.7 R0 ---- -- -- NV Note 113 13:42:26.85 +28:11:12.7 R0 0.5130 15.57 1.35 P RR0 Note 114 13:42:12.22 +28:33:03.6 R0 0.5977 15.686 1.16 V RR0 115 13:42:45.11 +28:33:47.5 R0 0.5133 15.717 1.20 V RR0 Note 116 13:41:34.06 +28:30:25.1 R0 0.5148 15.685 1.43 V RR0 117 13:42:18.40 +28:14:54.0 R0 0.6005 15.591 1.00 V RR0 118 13:42:22.51 +28:17:50.6 R0 0.4994 -- 1.13 V RR0 119 13:42:30.67 +28:24:29.0 R0 0.5177 15.606 1.16 V RR0 120 13:41:49.00 +28:26:32.3 R0 0.6401 15.676 0.51 V RR0 121 13:42:08.17 +28:23:37.9 R0 0.5352 15.744 1.00 V RR0 122 13:42:09.05 +28:21:55.3 R0 0.5160 -- -- RR0 blend 123 13:41:52.26 +28:06:04.0 R0 0.5454 15.61 1.39 P RR0 Note 124 13:42:06.53 +28:19:20.9 R0 0.7524 15.536 0.37 V RR0 125 13:42:25.65 +28:20:30.1 R0 0.3498 15.611 0.47 V RR1 126 13:42:10.36 +28:20:15.9 R0 0.3484 15.609 0.46 V RR1 127 13:42:18.56 +28:21:41.6 R0 ---- -- -- NV Note 128 13:42:20.13 +28:24:53.7 R0 0.2920 15.620 0.63 V RR1 129 13:42:08.21 +28:23:59.6 R0 0.4061 15.481 0.47 V RR1? 130 13:42:11.78 +28:24:06.3 R0 0.5661 15.574 0.80 V RR0 131 13:42:05.91 +28:23:09.3 R0 0.2977 15.648 0.59 V RR1 132 13:42:07.44 +28:22:20.2 R0 0.3399 15.589 0.54 V RR1 133 13:42:07.02 +28:23:26.2 R0 0.5507 15.693 1.16 V RR0 134 13:42:09.79 +28:23:34.9 R0 0.6181 15.745 0.64 V RR0 135 13:42:09.45 +28:23:20.7 R0 0.5684 15.663 0.86 V RR0 136 13:42:09.57 +28:23:16.3 R0 0.6172 -- -- RR0 blend 137 13:42:15.48 +28:22:23.3 R0 0.5751 15.579 0.93 V RR0 138 13:41:51.54 +28:23:22.7 R0 53.28 14.25 0.15 P SR Note 139 13:42:14.12 +28:23:10.6 R0 0.5600 15.587 1.45 V RR0 Note 140 13:42:10.30 +28:24:31.2 R0 0.3331 15.477 0.45 V RR1 Note 141 13:40:18.15 +28:18:21.3 R0 0.2696 14.98 1.0 P EC f?;max;Note 142 13:42:09.27 +28:21:43.9 R0 0.5686 15.703 0.97 V RR0 143 13:42:08.91 +28:22:59.2 R0 0.5965 15.472 0.99 V RR0 144 13:42:15.61 +28:21:02.9 R0 0.5968 15.582 0.56 V RR0 145 13:42:13.62 +28:22:51.2 R0 0.5145 -- -- RR0 blend 146 13:42:18.50 +28:21:44.1 R0 0.5022 15.704 1.31 V RR0 Note 147 13:42:09.84 +28:23:29.6 R0 0.3465 15.753 0.42 V RR1 148 13:42:10.96 +28:23:20.2 R0 0.4673 -- -- RR0 blend 149 13:42:14.10 +28:23:35.4 R0 0.5482 15.687 1.14 V RR0 150 13:42:16.69 +28:23:20.6 R0 0.5239 15.651 1.15 V RR0 151 13:42:11.99 +28:22:01.1 R0 0.5168 15.685 1.33 V RR0 152 13:42:17.47 +28:23:33.8 R0 0.3261 15.496 0.50 V RR1 153 13:42:08.61 +28:23:43.7 R0 ---- 13.574 -- V NV 154 13:42:11.66 +28:22:13.7 R0 15.290 12.63 1.25 V CW Note 155 13:42:06.70 +28:21:27.3 R0 0.3381 15.484 0.50 V RR1 Note 156 13:42:09.99 +28:22:01.6 R0 0.5320 15.694 1.20 V RR0 157 13:42:10.19 +28:23:18.1 R0 0.5429 15.728 -- V RR0 Note 158 13:42:10.34 +28:22:02.5 R0 ---- -- -- NV Note 159 13:42:10.36 +28:22:58.9 R0 0.5339 15.380 -- V RR0 Benko 160 13:42:10.81 +28:21:59.3 R0 0.6573 15.695 1.14 V RR0 161 13:42:12.81 +28:21:45.0 R0 0.5265 15.693 -- V RR0 Benko 162 13:42:13.60 +28:22:11.3 R0 ---- -- -- V NV Note 163 13:42:10.30 +28:22:10.8 R0 ---- -- -- V NV Note 164 13:42:13.09 +28:22:06.8 R0 ---- 13.818 -- V NV Note 165 13:42:17.05 +28:23:03.0 R0 0.4836 15.585 1.18 V RR0 Note 166 13:42:04.17 +28:22:34.7 R0 0.4850 15.700 0.90 V RR01 167 13:42:05.59 +28:22:05.8 R0 0.6440 15.629 0.48 V RR0 168 13:42:08.08 +28:22:49.7 R0 0.2759 15.617 0.4 V RR1 Note 169 13:42:09.28 +28:22:08.2 R0 ---- 14.864 -- V NV 170 13:42:09.34 +28:23:15.5 R0 0.4323 15.291 0.45 V RR1 171 13:42:09.51 +28:22:59.4 R0 0.3033 15.581 0.70 V RR1 172 13:42:09.91 +28:23:08.7 R0 0.5423 15.742 1.20 V RR0 173 13:42:10.51 +28:23:21.7 R0 0.6070 -- -- RR0 blend 174 13:42:10.83 +28:22:08.7 R0 0.5913 15.985 0.80 V RR0 175 13:42:14.64 +28:23:09.2 R0 0.5697 15.665 0.98 V RR0 Benko 176 13:42:14.98 +28:23:16.0 R0 0.5396 15.840 0.74 V RR0 177 13:42:16.27 +28:22:13.8 R0 0.3483 15.567 0.59 V RR1 178 13:42:17.48 +28:23:29.7 R0 0.2670 15.706 0.37 V RR1 179 13:42:14.39 +28:09:41.1 R0 ---- -- -- NV Note 180 13:42:10.09 +28:22:13.5 R0 0.6091 15.679 0.75 V RR0 Note 181 13:42:09.20 +28:22:29.0 R0 0.6638 15.528 0.55 V RR0 Benko 182 13:42:10.12 +28:23:42.5 R0 ---- 15.454 -- V NV Note 183 13:42:13.78 +28:22:49.6 R0 ---- -- -- V NV Note 184 13:42:09.58 +28:22:27.7 R0 0.5312 15.779 1.30 V RR0 185 13:42:10.32 +28:23:13.8 R0 ---- -- -- V NV Note 186 13:42:12.50 +28:21:39.7 R0 0.6634 15.538 0.55 V RR0 187 13:42:09.65 +28:22:51.8 R0 0.5863 15.709 0.9 V RR0 Benko 188 13:42:09.50 +28:23:06.7 R0 0.2665 15.782 0.4 V RR1 Note 189 13:42:09.59 +28:22:21.8 R0 0.6129 -- -- RR0 blend 190 13:42:10.88 +28:23:11.2 R0 0.5228 15.726 1.30 V RR0 191 13:42:11.63 +28:23:05.8 R0 0.5192 15.702 1.1 V RR0 Benko 192 13:42:11.31 +28:22:46.9 R0 0.4815 -- -- RR0 Note;blend 193 13:42:12.60 +28:22:35.6 R0 0.7479 15.490 1.20 V RR0 194 13:42:12.75 +28:22:30.0 R0 0.4892 15.628 1.1 V RR0 Benko 195 13:42:10.49 +28:22:14.7 R0 0.6441 15.606 0.5 V RR0 Note 196 13:42:15.05 +28:22:43.6 R0 ---- -- -- NV Note 197 13:42:15.91 +28:22:52.0 R0 0.4999 15.704 1.38 V RR0 198 13:42:09.75 +28:22:57.7 R0 0.2830 15.425 0.60 V RR1 Note 199 13:42:10.03 +28:22:53.9 R0 ---- 15.55 1.5 P RR? Note 200 13:42:11.18 +28:23:04.0 R0 0.3610 15.561 -- V RR01 Note;Benko 201 13:42:11.78 +28:22:33.8 R0 0.5405 15.770 1.30 V RR0 202 13:41:42.85 +28:24:17.8 R0 0.7736 15.524 0.180 V RR0 203 13:42:09.45 +28:17:30.4 R0 0.2898 15.546 0.150 V RR1 204 13:42:38.71 +28:22:48.2 R0 ---- 15.877 -- V NV Note 205 13:40:47.60 +28:33:25.9 R0 0.6369 15.8 0.8 P RR0 Note 206 13:42:20.31 +27:53:51.1 R0 0.5094 15.45 1.3 P RR0 Note 207 13:42:14.22 +28:22:11.5 R0 0.3453 15.455 0.40 V RR1 208 13:42:11.71 +28:21:44.3 R0 0.3384 15.475 0.40 V RR1 209 13:42:06.36 +28:21:02.8 R0 0.3483 15.607 0.52 V RR1 Benko 210 13:42:04.99 +28:22:32.4 R0 0.3529 -- -- V RR1 211 13:42:07.40 +28:22:49.2 R0 0.5582 -- -- RR0 blend 212 13:42:09.87 +28:22:04.2 R0 0.5422 15.803 1.30 V RR0 213 13:42:09.57 +28:22:12.6 R0 0.3000 15.533 0.50 V RR1 214 13:42:13.93 +28:22:48.7 R0 0.5395 -- -- V RR0 215 13:42:10.44 +28:22:41.5 R0 0.5287 15.617 1.20 V RR0 216 13:42:13.60 +28:22:31.4 R0 0.3465 15.833 0.60 V RR1 217 13:42:11.48 +28:22:15.6 R0 ---- -- -- V RR Note 218 13:42:13.62 +28:22:13.0 R0 0.5449 15.828 1.20 V RR0 219 13:42:07.06 +28:22:57.7 R0 0.6136 15.700 0.70 V RR0 220 13:42:14.00 +28:22:26.5 R0 0.6001 15.710 0.8 V RR0 Benko 221 13:42:10.22 +28:22:28.8 R0 0.3788 -- -- RR1 blend 222 13:42:18.76 +28:21:39.0 R0 0.5967 15.552 0.85 V RR0 Note 223 13:42:13.28 +28:22:36.5 R0 0.3292 15.576 0.5 V RR1 Benko 224 13:42:09.82 +28:22:47.2 R0 ---- -- -- Note 225 13:42:12.06 +28:26:26.6 R0 89.59 14.12 0.33 P SR Note 226 13:42:12.98 +28:22:24.0 R0 0.4884 -- -- RR0 blend 227 13:42:03.15 +28:21:40.6 R0 ---- 15.469 -- V NV 228 13:42:08.97 +28:23:18.8 R0 ---- 15.630 -- V NV 229 13:42:09.01 +28:21:56.9 R0 0.4992 -- -- RR0 blend 230 13:42:30.93 +28:14:29.2 R0 ---- -- -- Note 231 13:42:20.93 +28:23:29.7 R0 ---- 16.000 -- V NV 232 13:42:20.51 +28:23:24.2 R0 ---- 15.582 -- V NV 233 13:42:13.82 +28:22:35.0 R0 ---- 15.935 -- V NV 234 13:42:13.09 +28:22:02.7 R0 0.5080 15.926 1.65 V RR0 f;Note 235 13:42:13.77 +28:23:19.6 R0 0.7598 15.467 0.60 V RR0 236 13:42:41.54 +28:19:08.0 R0 31.395 14.295 0.25 P SR Note 237 13:42:15.75 +28:18:17.2 R0 0.0420 18.02 0.232 V SXPHE Note 238 13:42:12.96 +28:19:41.9 R0 0.4983 17.25 0.1 V EC f;max;Note 239 13:42:09.87 +28:22:15.7 R0 0.5040 15.700 1.25 V RR0 Note 240 13:42:09.46 +28:22:35.1 R0 0.2760 15.672 0.4 V RR1 Note 241 13:42:10.76 +28:22:37.8 R0 0.5962 -- -- V RR0 blend 242 13:42:13.21 +28:22:24.4 R0 0.5964 -- -- V RR0 blend 243 13:42:12.27 +28:22:15.7 R0 0.6346 15.629 0.6 V RR0 Benko 244 13:42:09.62 +28:22:46.4 R0 0.5378 15.682 1.1 V RR0 Benko 245 13:42:09.90 +28:22:59.9 R0 0.2840 15.622 0.5 V RR1 Benko 246 13:42:12.76 +28:22:40.3 R0 0.3391 15.622 0.5 V RR1 Benko 247 13:42:14.79 +28:22:15.7 R0 0.6054 15.670 0.7 V RR0 Benko 248 13:42:09.67 +28:22:49.5 R0 0.5098 -- -- V RR0 blend 249 13:42:10.31 +28:22:48.1 R0 0.5330 15.640 1.1 V RR0 Benko 250n 13:42:10.48 +28:22:52.9 R0 0.5671 -- -- V RR0 Note 250s 13:42:10.54 +28:22:52.1 R0 0.5861 -- -- V RR0 Note 251 13:42:10.95 +28:22:33.8 R0 0.4705 15.596 -- V RR01 Note;Benko 252 13:42:11.00 +28:22:43.8 R0 0.3360 15.719 -- V RR01 Benko 253 13:42:12.14 +28:22:32.6 R0 0.3326 15.493 0.5 V RR1 Benko 254 13:42:12.42 +28:22:53.4 R0 0.6057 15.531 0.6 V RR0 Benko 255 13:42:12.61 +28:22:43.8 R0 0.5727 15.581 0.8 V RR0 Benko 256 13:42:13.10 +28:22:58.6 R0 0.3181 15.692 0.5 V RR1 Benko 257 13:42:13.06 +28:22:28.2 R0 0.6020 15.705 0.9 V RR0 Benko 258 13:42:14.31 +28:23:31.4 R0 0.7134 15.641 0.68 V RR0 259 13:42:14.57 +28:22:54.7 R0 0.3335 15.720 0.5 V RR1 Benko 260 13:41:58.18 +28:15:52.1 R0 ---- 14.287 -- P SR? Note 261 13:42:10.09 +28:22:40.2 R0 0.4449 15.187 0.4 V RR1 Benko 262 13:42:10.82 +28:22:37.3 R0 ---- NV? Note 263 13:42:10.87 +28:22:24.2 R0 0.2169 17.043 0.35 V SXPHE Benko 264 13:42:10.87 +28:22:29.7 R0 0.3565 15.465 0.5 V RR1 Benko 265 13:42:11.71 +28:22:15.6 R0 ---- -- -- V RR Note 266 13:42:09.55 +28:22:44.1 R0 0.3425 15.508 0.45 V RR1 Benko 267 13:42:09.78 +28:22:47.9 R0 ---- -- -- V SXPHE Note 268 13:42:11.71 +28:22:14.2 R0 ---- -- -- V RR Note 269 13:42:12.79 +28:22:32.9 R0 0.3593 15.505 0.5 V RR1 Benko 270n 13:42:11.95 +28:23:32.7 R0 0.6258 -- -- RR0 Note 270s 13:42:11.96 +28:23:31.9 R0 0.6902 -- -- RR0 Note 271 13:42:12.19 +28:23:17.8 R0 0.6328 15.624 0.65 V RR0 Benko 272 13:42:13.29 +28:19:50.4 R0 ---- -- -- SR? Note 273 13:42:06.73 +28:20:56.9 R0 46.43 -- -- SR? Note 274 13:42:12.10 +28:21:20.5 R0 ---- -- -- SR? Note 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 =================================================================== Supplementary Notes and References For V1 to V274: The RA and dec, as well as the variability types, listed in the above table are from Bakos et al. (2000, Acta Ast 50, 221), unless otherwise indicated in the notes on individual stars. The periods are from Benko et al. (2006, MNRAS 372, 1657) unless otherwise indicated in the notes on indvidual stars. RR Lyrae magnitudes and amplitudes are mainly from Corwin & Carney (2001, AJ 122, 3183) or from Benko et al. (2006), if designated "Benko" in the remarks column. Exceptions are explained in the notes on indiviual stars. Since Benko et al. (2006) did not list amplitudes in their table, the amplitudes were estimated from their light curves. Note that the V magnitude system of Benko could be 0.02 mag fainter on average than Corwin's. No magnitudes or amplitudes have been listed for stars that had blended images in the data of both Corwin & Carney and Benko et al. These stars are designated "blend" in the "Remarks" column. For V286 to V297: All of the information listed in the above table is from the discovery paper by Hartmann et al. (2005, AJ 129, 1596). Identification charts for most of the variables numbered up to V259 have been published by Kholopv (1977, Per. Zvez. 20, 419) or by Kadla & Gerashchenko (1982, Izvestia Glavnaia Obs Pulkovo No. 199, p86). However, the numbering system for V226 and up was assigned after these papers were published so these higher numbered stars were labelled by their designations according to Kholopov or Kadla. An important catalog of 1571 M3 stars was published by von Zeipel (1908, Annales of l'Observatoire de Paris Mem v25, F1-101). 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, ApJ 40, 443) 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, Bakos et al. (2000, Acta Ast 50, 221) found that neither component varied on the CCD images they obtained. We have therefore classified V2 as non-variable. V13: The double-mode nature of V13, V200 and V251 was first recognized by Clementini et al. (2004, AJ 127, 938) V29: V29 and V155 were interchanged by Evstigneeva et al. (1994, Ast Let 20, 596) and by Corwin & Carney (2001, AJ 122, 3183) The period we list for V29 is from Benko and the mean magnitude and amplitude are the ones Corwin & Carney (2001) listed for V155. V82: Benko et al. (2006) did not list a period for V82, V91, V115 or V192. For these stars, we list the periods, as well as the mean magnitudes and amplitudes, published by Corwin & Carney (2001) V91: See V82. V95: The period, magnitude and amplitude listed for V95 and V225 are from Russev (1971, Per Zvez 18, 171). Rosino (1978, Vistas in Ast, 22, part 1, 39) classified V95, V138 and V225 as semi-regular variables. V96: For V96, V139, V168, V188 and V195, we list the magnitudes from Benko et al. (2006) and amplitudes from Corwin & Carney (2001). Corwin & Carney did not publish mean magnitudes for these stars. V112: Bailey (1913, HA 78, p. 67) 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 all of her catalogs. The star was not included in subsequent investigations by other authors. V113: The period, magnitude and amplitude listed for V113 and V123 are from Szeidl (1965, Budapest Mitt 58). According to Samus (2009, private communication), V113 is XX CVn in the GCVS. V115: Period, as well as the mean magnitude and amplitude, published by Corwin & Carney (2001). See V82. V123: Data from Szeidl. See V113. V127: Bailey (1913) was unable to derive a period for V127 because it had two close companions. Muller (1933, Berlin Babelsberg Veroff 11, 1) 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, Per Zvez 14, 275) found that the southwest component (his X34 = vZ 1198) was also variable. Sawyer Hogg (1973) designated X34 as V222 in her 3rd catalog. V138: Period, magnitude and amplitude from Olah and Russev (1979, IBVS 1656). In an earlier paper, Russev (1971, Per Zvez, 18, 171) derived a longer period. Rosino (1978, Vistas in Ast, 22, part 1, 39) classified V95, V138 and V225 as semi-regular variables. V139: Magnitudes from Benko et al. and amplitude from Corwin & Carney. See V96. V140: When this 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, Budapest Mitt. No. 63) who considered it to be a field star. However, a proper motion study by Tucholke et al. (1994, A&AS 104, 161) indicates thag it is a probable member. V146: According to Benko et al. (2006), V146 and V222 were interchanged by Corwin & Carney (2001, AJ 122, 3183) and by Clementini et al. (2004, AJ 127, 9380). The magnitude and amplitude that we list for V146 in the above table are the values listed by Corwin & Carney for V222. Kholopov (1977, Per Zvez 20, 419) pointed out that the observations that Greenstein published for V146 are really for V222. See also the comment for V127. V154: Period, magnitude, amplitude and variability type listed in the above table are from Kholopov (1972, Ast Tsirk 676, p7) V155: V29 and V155 were interchanged by Evstigneeva et al. (1994, Ast Let 20, 596) and by Corwin & Carney (2001, AJ 122, 3183) The period we list for V155 is from Benko and the mean magnitude and amplitude are the ones Corwin & Carney (2001) listed for V29. V157: Mean magnitude from Benko et al. (2006) because Corwin & Carney (2001) did not publish a value. Amplitude difficult to estimate because of Blazhko effect. V158: Greenstein (1935, AN 257, 301) 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. Bakos et al. (2000, Acta Ast 50, 221) did not detect any variation. V162: Greenstein (1935, AN 257, 301) classified this star as non-variable. He noted that it was part of a triple system. Later Kholopov (1963, Per Zvez 14, 275) found that one of the other stars in the triplet (vZ 950 = X28) was variable. Sawyer Hogg (1973) designated vZ 950 as V218 in her 3rd catalog. V163: Greenstein (1935, AN 257, 301) classified this star as non-variable. Bakos et al (2000) noted that the x,y position listed in Sawyer Hogg's catalogs was midway between V180 and a non-variable. According to Bakos, Kholopov (1977, Per Zvez 20) labelled the non-variable as V163. Bakos therefore accepted the non-variable as V163 to avoid confusion. 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 les than 0.35 mag. Benko et al (2006) classified it as non variable. Corwin & Carney derived a period, but according to Clementini et al. (2004, AJ 127, 938), the star that they studied was V234, not V164. V165: Bakos et al. 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 Benko et al. because Corwin & Carney did not publish an amplitude or mean magnitude for it. V168: Magnitudes from Benko et al. and amplitude from Corwin & Carney. See V96. V179: Greenstein (1935, AN 257, 301) 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. Bakos et al. (2000) 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. The RA and dec listed in the 2001 on-line update to the catalog were incorrect. V180: V180 = vZ 676: Shapley (1914, ApJ 40, 443) stated that vZ676 was composed of five distinct stars, of which the variable is the brightest and most centrally located. Greenstein (1935, AN 257, 301) could not measure it because of the crowding. Sawyer (1939) classified it as non-variable in all three of her catalogs. However, Kholopov (1977, Per Zvez 20, 313) and Bakos et al. (2000, Acta Ast 50, 221) 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 Bakos et al. The period, magnitude, amplitude and classification we list in the above table are from Bakos et al. (2005). We estimated the amplitude 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 Bakos et al. (2000) and Benko et al. (2006) confirmed its non-varable status. V183: Greenstein commented that V183 was blended with V145. Sawyer (1939) classified it as non-variable in all three of her catalogs. Bakos et al. (2000) confirmed its non-variable status. V185: Greenstein commented that this was a bright star with a small range. Bakos et al. (2000) did not detect any variation. Corwin & Carney (2001) and Benko et al (2006) did not study it. V188: Magnitudes from Benko et al. and amplitude from Corwin & Carney. See V96. V192: Period from Corwin & Carney. See V82. V195: Magnitudes from Benko et al. and amplitude from Corwin & Carney. See V96. V196: The variation of V196 was announced by Greenstein. He could not derive a period because it was a double and difficult to measure. Bakos et al. (2000) found that both components are constant. V198: Bakos et al. did not confirm variation in this star based on one night of observations. However, Corwin & Carney derived a period from their observations and commented that the star appears to be slightly above the HB of the CMD. V199: The magnitude and amplitude listed above are from Greenstein's (1935, Astr Nach 257, 301) paper. He derived a period of 0.488, but noted that it was doubtful. Corwin & Carney derived 0.40891, but indicated that it was uncertain. They did not publish a light curve or list a mean magnitude. V200: The period, magnitude and variability type are from Benko et al. (2006). The double-mode nature of V200 was first recognized by Clementini et al. (2004, AJ 127, 938). 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. According to Corwin & Carney (2001) and Benko et al. (2006), this star is non-variable. However, Yao (2007, Chinese A&A 7, 771) claims that it is a red HB star with a period of 0.74785 and V amplitude 0.04) V205, 206: Evstigneeva et al. (1994, Ast Let 20, 596) pointed out that V205 and 206 are WY CVn and VZ CVn in the GCVS. The periods and magnitudes we list for these two stars are from Kukarkin (1960, Ast Tsirk 216, 29). V217: Guhathakurta et al. (1994) classified this star (Gu9023) as an RR Lyrae. V222: According to Benko et al. (2006), V146 and V222 were interchanged by Corwin & Carney (2001, AJ 122, 3183) and by Clementini et al. (2004, AJ 127, 9380). The magnitude and amplitude that we list for V222 in the above table are the values listed by Corwin & Carney for V146. See the comment for V146. V224: Bakos et al. (2000) confirmed that this star was variable, but also commented that it is merging with a nearby star. It was not investigated further in their subsequent paper (Benko et al. 2006). V225: The period, magnitude and amplitude listed for V95 and V225 are from Russev (1971, Per Zvez 18, 171). Rosino (1978, Vistas in Ast, 22, part 1, 39) classified V95, V138 and V225 as semi-regular variables. V230: This was Kholopov's (1977) X41. It was not labelled on his ID chart because it was too far from the cluster centre. It was not studied by Corwin & Carney (2001) or by Benko et al. (2006). V234: According to Corwin & Carney (2001), this star is an RR Lyrae that might be more distant than the cluster so we have classified it as a field star. In their investigation, they called the star V164, but Clementini et al. (2004, AJ 127, 938) later pointed out that it was V234. V236 (vZ 1397): Period, magnitude and amplitude in the above table are from Olah (1979, Budapest Mitt. 73) 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, AJ 90, 2555) who derived periods of 32.2 and 60.2 from Yerkes observations obtained between 1978 and 1983. He preferred the 60 day period. We classify the star as SR. V237, V238, V239: Benko et al. (2006) pointed out that the dec for V238 and V239 were incorrectly listed in the 2001 on-line version of the catalog. Meanwhile, Hartman et al. (2005, AJ 129, 1596) pointed out that the coordinates of V237 and V238 were switched in the discovery paper (Kaluzny et al. 1998, MNRAS 296, 347) and that this error had propagated through to the catalog of Bakos et al. (2000, Acta Ast 50, 221). The coordinates listed for V237, V238, V239 have all been revised accordingly in the above table. V237: Period , magnitude, amplitude and classification 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, AJ 120, 319). V240: Mean magnitude from Corwin & Carney (2001) and amplitude estimated from the light curve published by Benko et al. (2006) V250n, V250s: Benko et al. (2006) discovered that the image of V250 consisted of two close companions, both RR0 variables. They derived a period for each star, but it was not possible to derive individual magnitudes or amplitudes. V251: The double-mode nature of V251 was first recognized by Clementini et al. (2004, AJ 127, 938). V260: This star (vZ 297) is among the brightest stars on the giant branch and Walker (1955 AJ 60, 197) suggested that it might be variable. However, the variation was not confirmed by Olah (1979, Budapest Mitt 73) or by Welty (1985, AJ 90, 2555). The mean magnitude we list in the above table is from Olah's paper. We classify it as SR? because its colour and magnitude are comparable to the SR variables in M3: V95, V138, V225 and V236. V262: Guhathakurta et al. (1994, AJ 108, 1786) classified this star (Gu 552) as an RR Lyrae variable, but Bakos et al. (2000) found no trace of variation, hence the "NV?" designation. V265, V267, V268: V265=Gu 1489, V267=Gu 9016, V268=Gu 9025: These stars all have close companions. The variability types were assigned by Guhathakurta et al. (1994, AJ 108, 1786) but they did not derive precise periods for any of them. V270n, V270s: Benko et al. (2006) discovered that the image of V270 consisted of two close companions, both RR0 variables. They derived a period for each star, but it was not possible to derive individual magnitudes or amplitudes. V272, V273, V274: Light curves based on the image subtraction method were published by Bakos et al. (2000). Benko et al. (2006) published a period for V273. We have classified them all as SR because Benko et al. indicated that they varied on "long" time scales. S1-S11: Strader et al. (2002, MNRAS 335, 621) 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 Benko et al. (2006, MNRAS 372, 1657) did not confirm any of these discoveries. 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 Benko's result. V298: This star is N2 in the paper by Benko et al. (2006) and all of the information listed for it is from their paper. ================================================================== Discovery of the Variable Stars in M3: V1-137 and star b Bailey HA 38 (1902) with ID chart (Fig 1) and x,y coordinates (pages 238-239) Bailey HA 78 (1913) with ID chart (Fig 1) and von Zeipel numbers (page 10) V138 = Bailey's star b (see HA 78, pages 8-9) The number 138 was assigned by Larink (1922, Ast. Abh. of Hamburg Sternwarte in Bergedorf v2, no. 6) V139-141 Larink, (1922, Hamburg Ast. Abh. 2 No. 6) with x,y positions; V141 is RV CVn. The variability of V141 was previously announced by Larink (1921, AN 214, 71), but it was identified only by RA and dec in the earlier paper. V142-183 Muller (1933, Berlin Babelsberg Veroff 11, 1) with x,y coordinates V184-199 Greenstein (1935, AN 257, 301) with x,y coordinates V200-201 = star numbers 12 and 14 from Table I of Shapley (1914, ApJ 40, 443). 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 HC 437 (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, AJ 58, 61) Roberts & Sandage (1955, AJ 60, 185) 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. Bakos et al. (2000, Acta Ast 50, 221) listed the correct position for this star. V205-206 = SVS (Soviet Variable Star) 1264 and 1276 Kurochkin (1959, Ast Tsirk 205, 14 and 1960, Per Zvez 13, 84) 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, Ast Tsirk 216, 29) 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, Per Zvez 14, 275) 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, Per Zvez 18, 171) 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, AC 848, 8 (1974) with x,y coordinates and ID chart In a later paper, Kholopov (1977, Per Zvez 20, 313) listed it as X39. We desgnated this as V226 in our first on-line update to the catalog. V227-235 = X7, X10, X40, X41, X42, X43, X44, X47, X49 Kholopov (1977, Per Zvez 20, 313) 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 Sawyer Hogg catalog. V236 = von Zeipel 1397 This star (vZ 1397) is among the brightest stars on the giant branch and Walker (1955 AJ 60, 197) suggested that it might be variable. Olah (1973, Budapest Mitt. 73) confirmed the variation. vZ 1397 was designated as V236 in the first on-line update to the Sawyer Hogg catalog. V237-238 Kaluzny et al. (1998, MNRAS 296, 347) with x,y coordinates and ID charts. According to Hartman et al. (2005, AJ 129, 1596), the coordinates of V237 and V238 were switched in the discovery paper and this error propagated through to the compilation by Bakos (2000, Acta Ast 50, 221). 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, Per Zvez 14, 275) with x,y coordinates, ID chart and von Zeipel numbers if available. The numbers V239-248 were assigned by Bakos et al. (2000, Acta Ast 50, 221) 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 variables. V249-259 = KG1, KG2, KG3, KG4, KG7, KG8, KG9, KG11, KG12, KG14, KG15 Kadla & Gerashchenko (1980, Ast. Tsirk 1123) 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 (1982, Pulkovo Glavnaia Astron Izvestia 199, 86), 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. These KG stars were designated as V249-259 by Bakos et al. (2000, Acta Ast 50, 221) They 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 AJ 60, 197) suggested that it might be variable. However, the variation was not confirmed by Olah (1973, Budapest Mitt. 73) vZ 297 was designated as V260 by Bakos et al. (2000). V261-268 = Gu32, Gu552, Gu576, Gu586, Gu1489, Gu9012, Gu9016, Gu9025 Guhathakurta et al. (1994, AJ 108, 1786). These stars were designated as V261-268 by Bakos et al. (2000) V269-274 = B1-6 Bakos et al. (2000) S1-S11: Strader et al. (2002, MNRAS 335, 621) However, Benko et al. (2006, MNRAS 372, 1657) were unable to confirm these discoveries. V286-297 = New Variables 286-297 Hartman et al. (2005, AJ 129, 1596) 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 Benko et al. to be variable. V298 = N2 Benko et al. (2006, MNRAS 372, 1657) These authors also made independent discoveries of V291 (their N1) and V292 (their N3) =========================================================