NGC 6715 / C1851-305 / Messier 54 RA: 18:55:03.33 DEC: -30:28:47.5 (J2000) (Most recent updates: Membership probability flag - 2024; Remaining data - October 2017) ============================================================ Bytes Format Explanation 1-8 A8 Star ID 10-32 A11,1x,A11 Position 34-35 A2 Membership probability flag based on data published by Prudil & Arellano Ferro (2024) m1: prob >=0.85; m2: prob >=0.7 and <0.85; m3: prob >= 0.5 and <0.7; f: prob <0.5 u: no data available 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 Mem Period ampl C Type Notes/ RA Dec Flag Remarks ========================================================================= 1 18:55:09.75 -30:28:36.5 m1 1.3476 16.591 0.621 I CW 2 18:55:02.91 -30:27:15.6 m1 1.0945 16.762 0.590 I CW 3 18:55:02.20 -30:25:46.4 m1 0.5753 17.542 0.579 I RR0 4 18:54:58.91 -30:23:35.2 m1 0.4801 17.638 0.792 I RR0 5 18:54:53.23 -30:28:01.1 m1 0.5791 17.485 0.701 I RR0 6 18:55:19.38 -30:31:43.4 m1 0.5430 17.534 0.592 I RR0 7 18:55:07.46 -30:31:23.8 m1 0.5926 17.521 0.509 I RR0 8 18:55:31.21 -30:34:16.5 u 0.3527 16.698 0.645 I EW max 9 18:54:57.89 -30:39:20.9 u 0.5978 17.397 0.683 I RR0 f 10 18:55:12.02 -30:37:36.3 u 0.5878 17.551 0.413 I RR0 f?;Note 11 18:54:54.81 -30:46:55.6 u 0.4878 17.694 0.854 I RR0 f 12 18:54:46.07 -30:32:52.4 f 0.3227 16.200 0.277 I RR01 f;Note 13 18:54:45.07 -30:21:13.2 u 0.5787 17.562 0.523 I RR0 f?;Note 14 18:55:21.86 -30:25:14.4 m1 ---- -- -- RR Note 15 18:55:13.29 -30:29:46.6 m1 0.5869 17.549 0.529 I RR0 16 18:55:08.81 -30:43:53.3 u 0.4445 17.929 0.835 I RR0 f 17 18:55:56.90 -30:36:03.6 u 0.4658 17.760 0.633 I RR0 f 18 18:55:42.66 -30:22:27.0 u 0.3012 15.633 0.453 I EW max;f;Note 19 18:53:25.71 -30:31:45.2 u 0.4704 15.553 0.785 I RR0 f 20 18:55:11.50 -30:27:09.1 m1 ---- -- -- CST Note 21 18:55:09.41 -30:32:32.7 m1 ---- -- -- CST Note 22 18:55:02.47 -30:31:31.4 m1 ---- -- -- CST Note 23 18:55:30.73 -30:25:31.1 u 0.5177 17.596 0.765 I RR0 24 18:55:38.24 -30:27:51.2 u ---- -- -- CST Note 25 18:54:58.31 -30:27:34.4 m1 100. 13.405 0.511 I SR 26 18:55:17.76 -30:31:13.8 m1 ---- -- -- CST Note 27 18:55:19.39 -30:33:49.6 u ---- -- -- CST Note 28 18:55:08.65 -30:26:02.9 m1 0.5131 17.580 0.810 I RR0 29 18:54:53.44 -30:29:32.8 m1 0.5897 17.563 0.458 I RR0 30 18:55:03.48 -30:27:25.5 m1 0.5739 17.55 0.56 I RR0 S10 31 18:54:55.77 -30:29:54.5 m1 0.6466 17.470 0.304 I RR0 32 18:54:49.53 -30:27:44.2 m1 0.5213 17.544 0.819 I RR0 33 18:55:09.39 -30:30:26.2 m1 0.4911 17.625 0.791 I RR0 34 18:54:59.37 -30:31:19.1 m1 0.5034 17.623 0.611 I RR0 35 18:54:57.07 -30:27:54.2 m1 0.5267 17.561 0.744 I RR0 36 18:55:13.27 -30:27:49.6 m1 0.5990 17.493 0.430 I RR0 37 18:55:06.83 -30:29:26.7 m1 0.6275 17.505 0.317 I RR0 38 18:54:58.20 -30:28:11.0 m3 0.6111 17.340 0.311 I RR0 39 18:54:55.76 -30:29:51.2 m1 0.5996 17.545 0.435 I RR0 40 18:54:59.59 -30:30:36.8 m1 0.5864 17.502 0.476 I RR0 41 18:55:13.25 -30:27:55.7 m1 0.6177 17.433 0.643 I RR0 42 18:55:08.81 -30:27:46.6 m1 0.3264 17.665 0.315 I RR1 43 18:54:51.62 -30:27:57.3 m1 0.5900 17.522 0.547 I RR0 44 18:55:04.54 -30:30:05.3 f 0.6178 17.523 0.384 I RR0 45 18:55:12.88 -30:30:28.7 m1 0.4888 17.614 0.482 I RR0 46 18:55:00.74 -30:29:25.3 m3 0.6047 17.355 0.379 I RR0 47 18:55:01.04 -30:27:11.6 m1 0.5070 17.589 0.530 I RR0 48 18:55:23.17 -30:29:21.0 m1 0.6870 17.419 0.450 I RR0 49 18:54:56.28 -30:31:01.6 m1 0.3313 17.562 0.255 I RR1 50 18:55:11.32 -30:27:40.7 m1 0.5642 17.560 0.492 I RR0 51 18:55:19.90 -30:25:18.3 m1 0.6054 17.512 0.456 I RR0 52 18:55:10.64 -30:29:31.3 m1 0.6408 17.469 0.259 I RR0 53 18:54:58.94 -30:30:01.6 u ---- -- -- CST Note 54 18:54:53.84 -30:23:25.7 m1 0.5704 17.558 0.520 I RR0 55 18:55:15.41 -30:32:02.5 m1 0.4261 18.000 0.717 I RR0 f 56 18:54:38.15 -30:31:01.0 m1 0.3677 17.61 0.23 I RR1 S10 57 18:55:26.06 -30:29:04.2 m1 0.5466 17.561 0.664 I RR0 58 18:55:09.25 -30:24:25.2 m1 0.5487 17.593 0.633 I RR0 59 18:54:47.62 -30:33:04.6 m1 0.5994 17.546 0.463 I RR0 60 18:54:43.67 -30:32:52.6 m1 0.5696 17.608 0.520 I RR0 61 18:54:59.95 -30:27:01.3 m1 0.6039 17.508 0.515 I RR0 62 18:54:56.12 -30:27:14.3 m1 0.6136 17.526 0.377 I RR0 63 18:55:00.90 -30:30:58.4 m1 0.5901 17.539 0.496 I RR0 64 18:55:24.95 -30:36:48.0 u 34.0 14.133 0.421 I SR 65 18:55:21.70 -30:25:52.0 f 0.5748 16.91 0.48 I RR0 f;S10 66 18:55:20.81 -30:25:11.1 m1 ---- 13.04 -- I SR Note 67 18:55:03.38 -30:27:36.8 m1 0.5904 17.394 0.487 I RR0 68 18:54:13.19 -30:23:36.8 u 0.5415 17.494 0.669 I RR0 f 69 18:54:37.54 -30:24:18.6 u 0.6834 17.382 0.532 I RR0 70 18:55:14.70 -30:35:41.9 u 0.3973 15.113 0.658 I EB max 71 18:55:00.80 -30:27:02.2 m1 79.0 13.352 0.217 I SR 72 18:54:58.56 -30:26:19.8 f ---- -- -- CST Note 73 18:55:04.35 -30:27:43.4 m1 ---- -- -- CST Note 74 18:55:12.65 -30:30:59.9 m1 0.2889 17.657 0.341 I RR1 75 18:55:04.68 -30:27:25.6 m1 0.5846 -- -- RR0 Note 76 18:54:55.78 -30:29:09.9 f 0.7070 17.344 0.415 I RR0 77 18:54:55.09 -30:29:30.8 m1 0.5769 17.520 0.536 I RR0 78 18:55:09.20 -30:28:55.3 m1 0.4019 17.450 0.242 I RR1 79 18:55:06.05 -30:29:28.3 m1 ---- -- -- CST Note 80 18:55:07.73 -30:29:08.3 m1 0.6309 17.481 0.299 I RR0 Note 81 18:55:06.85 -30:28:33.0 m1 ---- -- -- CST Note 82 18:55:00.01 -30:29:31.2 m1 0.5872 17.407 0.438 I RR0 83 18:54:53.97 -30:33:24.7 m1 0.5783 17.558 0.455 I RR0 84 18:55:02.81 -30:29:35.9 m1 0.5997 17.364 0.669 I RR0 85 18:55:02.04 -30:30:16.3 m1 0.5204 17.490 0.529 I RR0 86 18:55:08.66 -30:29:31.4 m1 0.5837 17.504 0.511 I RR0 Note 87 18:55:11.35 -30:29:10.6 m1 0.5551 17.561 0.610 I RR0 88 18:54:51.55 -30:25:47.7 m1 0.4923 17.621 0.600 I RR0 89 18:54:55.91 -30:25:16.6 m1 0.5911 17.535 0.499 I RR0 90 18:55:07.95 -30:26:10.5 m1 0.6131 17.532 0.419 I RR0 91 18:55:26.96 -30:24:51.2 u ---- -- -- CST? Note 92 18:55:06.06 -30:28:38.4 f 0.4847 17.331 0.578 I RR0 f 93 18:55:01.94 -30:25:41.2 f 0.5581 16.757 0.358 I RR0 f 94 18:55:10.22 -30:24:38.5 m1 0.6559 17.511 0.188 I RR0 95 18:55:01.43 -30:29:59.0 f 0.5584 17.292 0.502 I RR0 96 18:55:25.10 -30:34:19.6 u 0.5611 17.538 0.621 I RR0 97 18:55:05.59 -30:27:59.5 m1 0.3367 17.596 0.259 I RR1 98 18:55:10.78 -30:29:12.7 m1 0.6244 17.496 0.342 I RR0 99 18:54:57.11 -30:25:44.2 f 0.3465 17.350 0.314 I EC f?;Note 100 18:55:02.16 -30:28:07.5 m1 ---- -- -- CST Note 101 18:54:43.56 -30:28:55.5 m1 61.0 13.843 0.659 I SR 102 18:55:14.63 -30:33:12.4 m1 80.0 13.878 0.240 I SR 103 18:54:57.22 -30:28:54.3 m1 131.0 12.773 0.792 I SR 104 18:54:58.79 -30:25:35.2 m1 410.0 13.435 0.429 I SR 105 18:54:54.15 -30:28:09.9 m1 37.0 13.483 0.166 I SR 106 18:55:02.13 -30:33:09.4 m1 38.0 13.321 0.127 I SR 107 18:55:04.93 -30:28:49.4 m2 ---- -- -- CST Note 108 18:55:21.39 -30:25:20.3 m1 ---- 13.42 -- I SR? Note 109 18:55:13.47 -30:26:42.5 f 33.0 13.747 0.103 I SR 110 18:55:14.40 -30:28:13.1 m1 60.0 13.517 0.122 I SR 111 18:55:01.13 -30:28:27.1 m1 75.0 13.619 0.194 I SR 112 18:55:02.01 -30:28:35.0 m1 90.0 13.525 0.333 I SR Note 113 18:54:52.22 -30:29:13.0 m1 ---- 13.695 0.085 I SR 114 18:54:54.36 -30:33:43.0 m1 27.0 13.699 0.084 I SR 115 18:54:59.48 -30:28:19.5 m1 45.0 13.432 0.174 I SR 116 18:55:09.20 -30:25:34.4 m1 1.5422 19.02 0.82 I EA max 117 18:55:20.01 -30:25:44.2 f 0.3288 17.976 0.302 I EC max 118 18:55:23.31 -30:31:04.4 m1 0.6267 17.621 0.240 I RR0 119 18:55:18.47 -30:31:49.4 f 0.6354 15.075 0.270 I RR0 f 120 18:55:10.84 -30:27:47.6 m1 0.7362 17.355 0.309 I RR0 121 18:55:10.35 -30:27:48.6 u 0.7478 16.813 0.152 I RR0 f 122 18:55:09.80 -30:27:31.8 m1 0.6493 17.420 0.216 I RR0 123 18:55:03.13 -30:28:04.9 f 0.5138 17.359 0.527 I RR0 124 18:55:09.05 -30:29:44.2 m1 0.5829 17.465 0.498 I RR0 125 18:55:06.10 -30:27:49.0 m1 0.7335 17.327 0.310 I RR0 126 18:55:04.54 -30:27:42.4 m1 0.3517 17.518 0.244 I RR1 127 18:55:02.97 -30:27:52.3 m1 0.5921 17.395 0.351 I RR0 128 18:55:00.60 -30:28:35.3 u 0.6794 16.877 0.279 I RR0 blend? 129 18:54:55.20 -30:29:09.3 m2 0.6021 17.581 0.450 I RR0 130 18:55:00.16 -30:28:12.9 m1 0.6760 17.536 0.197 I RR0 131 18:54:55.12 -30:31:04.6 m1 0.6358 17.514 0.253 I RR0 132 18:55:01.10 -30:28:54.9 m1 0.6601 17.446 0.607 I RR0 133 18:55:00.39 -30:29:24.2 m3 0.3648 17.425 0.226 I RR1 134 18:55:08.73 -30:24:00.0 m1 0.9119 18.560 0.397 I EC max 135 18:54:35.59 -30:33:54.3 u 0.3189 16.945 0.084 I EC f? 136 18:54:48.93 -30:29:45.6 m1 0.6944 17.435 0.185 I RR0 137 18:55:06.09 -30:27:59.8 m1 0.7754 17.302 0.159 I RR0 138 18:55:05.99 -30:28:22.1 u 0.3116 17.614 0.329 I RR1 139 18:55:03.96 -30:29:24.7 m1 0.6068 17.498 0.499 I RR0 140 18:55:02.49 -30:30:00.3 m1 0.7482 17.308 0.282 I RR0 141 18:55:01.26 -30:29:19.2 m1 0.3344 17.496 0.202 I RR1 142 18:54:59.64 -30:28:51.0 m1 0.2979 17.313 0.249 I RR1 143 18:54:57.42 -30:29:43.3 m1 0.6678 17.451 0.129 I RR0 144 18:55:12.10 -30:30:04.5 m1 0.7207 18.673 0.419 I EC max 145 18:55:06.42 -30:28:26.6 m1 0.2617 17.436 0.100 I spot? 146 18:54:34.79 -30:34:30.1 u 0.0653 19.000 0.232 I SXPHE 147 18:55:04.81 -30:28:49.7 u 0.2762 17.003 0.141 I RR1 148 18:55:02.80 -30:29:26.6 m3 0.2670 17.362 0.081 I RR1 149 18:54:58.65 -30:29:57.2 u 0.0808 18.086 0.151 I SXPHE 150 18:54:33.58 -30:29:16.8 u 0.0615 19.753 0.424 I SXPHE 151 18:54:51.78 -30:28:32.1 m1 0.3434 17.631 0.260 I RR1 152 18:55:06.25 -30:28:45.2 f 0.3141 17.382 0.278 I RR1 153 18:55:00.68 -30:27:56.9 m1 ---- 14.148 0.075 I SR 154 18:55:00.93 -30:28:08.0 m1 35.0 13.561 0.113 I SR 155 18:55:00.08 -30:30:33.5 m1 ---- -- -- CST 156 18:54:57.74 -30:25:57.4 m1 65.0 13.643 0.094 I SR 157 18:55:21.50 -30:25:20.5 m1 ---- -- -- RR? S10;Note 158 18:54:58.30 -30:30:27.1 m1 0.6182 17.547 0.385 I RR0 159 18:55:03.58 -30:29:55.4 m1 0.7419 17.326 0.285 I RR0 160 18:55:03.92 -30:28:30.1 m2 0.6281 17.559 0.682 I RR0 Note 161 18:55:06.83 -30:28:46.7 f 0.5921 17.078 0.318 I RR0 162 18:55:03.75 -30:29:30.3 m1 0.6004 17.405 0.450 I RR0 163 18:55:05.04 -30:29:29.6 m2 0.5891 17.520 0.452 I RR0 164 18:55:01.71 -30:29:20.9 f 0.5142 17.651 0.708 I RR0 165 18:55:05.97 -30:29:14.9 m2 0.5977 17.467 0.394 I RR0 166 18:54:44.42 -30:24:28.7 m1 ---- -- -- CST 167 18:54:59.85 -30:23:56.0 f ---- -- -- CST 168 18:55:07.13 -30:29:05.0 f 0.5560 17.237 0.525 I RR0 169 18:55:04.68 -30:29:02.7 m1 ---- -- -- CST 170 18:55:24.73 -30:24:39.7 u ---- -- -- CST 171 18:55:04.26 -30:28:18.4 u 0.5716 17.537 0.497 I RR0 172 18:55:06.13 -30:29:00.8 m1 0.6058 17.777 0.507 I RR0 173 18:55:02.48 -30:29:00.2 m1 0.3603 17.69 0.30 I RR1 FJ16;Note 174 18:55:05.89 -30:29:29.9 f 0.2975 17.703 0.347 I RR1 175 18:55:04.89 -30:28:19.0 m1 ---- -- -- CST 176 18:55:06.84 -30:27:57.9 m1 0.5978 17.509 0.444 I RR0 177 18:55:01.14 -30:28:30.7 u 0.4881 17.523 0.516 I RR0 178 18:55:01.66 -30:28:32.4 u 0.6618 17.317 0.615 I RR0 179 18:55:01.22 -30:28:34.7 f 0.5710 17.707 0.794 I RR0 180 18:55:03.45 -30:29:14.9 m1 0.5313 17.244 0.403 I RR0 181 18:55:02.40 -30:28:34.3 m1 0.4667 17.60 0.87 I RR0 Note 182 18:55:01.61 -30:28:51.7 m1 0.6886 17.181 0.536 I RR0 183 18:55:04.84 -30:29:45.8 m1 0.2694 17.659 0.192 I RR1 184 18:55:01.42 -30:29:22.0 u 0.9592 17.071 0.389 I RR0 AC? 185 18:55:01.67 -30:28:26.5 u 0.3285 17.577 0.265 I RR1 186 18:54:59.85 -30:28:35.4 f 0.4724 17.322 0.282 I RR1 187 18:55:02.61 -30:29:08.8 m1 0.6221 17.383 0.793 I RR0 188 18:55:03.15 -30:29:19.7 m1 0.5639 17.533 0.568 I RR0 189 18:55:14.97 -30:33:14.0 f ---- -- -- CST 190 18:55:20.03 -30:26:46.1 m1 ---- 13.683 0.126 I SR 191 18:55:04.34 -30:29:08.8 m1 118.0 13.265 0.493 I SR 192 18:55:01.97 -30:29:02.9 m1 0.6004 17.63 0.60 I RR0 Note 193 18:55:05.29 -30:28:47.4 u 0.3090 17.230 0.241 I RR1 194 18:55:02.73 -30:29:14.2 f 0.5775 17.362 0.327 I RR0 195 18:55:07.94 -30:30:16.2 f ---- -- -- CST 196 18:55:08.02 -30:25:03.2 m1 ---- -- -- CST 197 18:55:27.01 -30:27:35.0 u ---- -- -- CST 198 18:55:17.99 -30:27:48.8 f ---- -- -- CST 199 18:55:07.30 -30:25:50.3 m1 ---- -- -- CST 200 18:55:01.42 -30:25:36.5 f ---- -- -- CST 201 18:55:02.70 -30:25:39.8 m1 ---- -- -- CST 202 18:55:03.00 -30:24:49.8 m1 ---- -- -- CST 203 18:55:14.54 -30:28:13.1 m1 ---- -- -- CST 204 18:54:56.47 -30:27:54.4 u ---- -- -- CST 205 18:55:05.91 -30:30:04.9 f ---- -- -- CST 206 18:55:00.64 -30:28:39.4 m1 ---- 13.468 0.070 I SR 207 18:54:54.46 -30:33:43.1 m1 ---- -- -- CST 208 18:54:48.82 -30:31:29.7 m1 ---- -- -- CST 209 18:54:49.70 -30:31:33.6 m1 ---- -- -- CST 210 18:55:09.64 -30:29:05.3 m1 ---- 13.807 0.064 SR 211 18:55:05.83 -30:28:23.2 m1 ---- -- -- CST 212 18:55:03.78 -30:29:03.5 m1 0.2021 17.59 0.79 I E FJ16 213 18:55:02.13 -30:28:39.6 m1 0.2861 17.95 0.64 I RR1 Note 214 18:55:02.96 -30:28:35.4 u 0.6239 17.404 0.282 I RR0 Note 215 18:55:02.70 -30:28:52.7 u 0.3072 17.599 0.282 I RR1 Note 216 18:55:04.01 -30:28:37.7 m1 0.3311 16.49 0.20 I RR1 FJ16 217 18:55:02.07 -30:29:03.4 m1 0.3315 17.492 0.232 I RR1 Note 218 18:55:03.56 -30:28:56.8 u 0.3485 16.92 0.20 I RR1 FJ16 219 18:55:03.23 -30:28:59.5 m2 0.3826 17.367 0.210 I RR1 Note 220 18:55:03.20 -30:28:38.5 f 0.6026 17.496 0.308 I RR0 Note 221 18:55:04.35 -30:28:51.2 m1 0.4596 17.39 0.71 I RR01 FJ16;Note 222 18:55:02.50 -30:28:46.4 m1 0.4657 17.70 0.70 I RR0? FJ16 223 18:55:02.43 -30:28:45.2 m1 0.4719 17.561 0.509 I RR0 Note 224 18:55:03.55 -30:28:45.1 m1 0.4823 16.16 0.27 I RR0? FJ16 225 18:55:03.86 -30:28:43.9 f 0.4830 17.28 0.35 I RR1? FJ16 226 18:55:03.95 -30:28:42.7 m3 0.4979 16.39 0.36 I RR0? FJ16 227 18:55:03.05 -30:28:35.8 f 0.5081 17.66 0.90 I RR0 FJ16 228 18:55:02.76 -30:28:50.9 u 0.5252 16.87 0.41 I RR0 FJ16 229 18:55:04.03 -30:28:58.2 u 0.5268 -- -- RR0 Note 230 18:55:03.64 -30:28:55.4 m2 1.1431 -- -- I CW Note 231 18:55:02.89 -30:28:58.3 f 0.5342 17.80 0.83 I RR0 Note 232 18:55:03.58 -30:28:47.6 u 0.5565 16.35 0.29 I RR0 FJ16 233 18:55:03.74 -30:28:40.2 f 0.5575 17.41 0.85 I RR0 Note 234 18:55:02.26 -30:28:37.1 f 0.5598 17.72 0.60 I RR0 Note 235 18:55:03.41 -30:29:05.8 f 0.5667 17.41 0.69 I RR0 FJ16 236 18:55:03.15 -30:28:34.9 f 0.5685 -- -- I RR0 Note 237 18:55:02.11 -30:28:44.4 f 0.5799 17.461 0.449 I RR0 Note 238 18:55:03.24 -30:28:42.9 u ---- 17.63 -- I RR? FJ16;Note 239 18:55:02.85 -30:29:06.9 m1 0.5962 17.506 0.501 I RR0 Note 240 18:55:02.73 -30:28:30.5 m1 0.5963 17.494 0.669 I RR0 Note 241 18:55:04.19 -30:28:39.2 m1 0.6026 17.389 0.389 I RR0 Note 242 18:55:02.76 -30:29:00.2 u 0.6048 17.538 0.514 I RR0 Note 243 18:55:02.59 -30:28:38.6 f 0.6102 -- -- I RR0 FJ16;blend 244 18:55:03.03 -30:29:01.2 m3 0.6152 -- -- I RR0 Note 245 18:55:02.85 -30:28:57.8 f 0.6268 17.68 0.47 I RR0 FJ16 246 18:55:02.62 -30:28:40.9 m1 0.6288 -- -- I RR0 Note 247 18:55:02.83 -30:28:43.5 u 0.6509 17.503 0.415 I RR0 Note 248 18:55:03.80 -30:28:54.4 m1 0.6690 17.05 0.46 I RR0 FJ16;blend? 249 18:55:03.23 -30:28:44.0 f 0.6737 -- -- I RR0 FJ16;blend 250 18:55:03.71 -30:29:00.4 m1 0.6806 17.919 0.762 I RR0 Note 251 18:55:02.88 -30:28:30.5 f 0.6893 17.571 0.771 I RR0 Note 252 18:55:03.79 -30:29:07.8 m1 0.7287 17.28 0.50 I RR0 Note 253 18:55:03.27 -30:28:28.7 u 0.7439 17.32 0.29 I RR0 Note 254 18:55:02.81 -30:28:49.7 f 0.7476 17.430 0.758 I RR0 Note 255 18:55:03.12 -30:28:38.0 m1 0.7601 17.151 0.183 I RR0 Note 256 18:55:03.73 -30:28:44.9 f 14.7877 15.292 1.284 I CW Note 257 18:55:03.00 -30:28:43.2 f 20.747 14.04 0.09 I SR FJ16 258 18:55:03.73 -30:28:48.3 f 37.980 13.16 0.04 I SR FJ16 259 18:55:04.22 -30:28:49.9 f 154.0 13.30 0.45 I SR FJ16 260 18:55:03.17 -30:28:54.4 f ---- 12.76 0.06 I L FJ16 261 18:55:03.40 -30:28:45.0 m1 ---- 13.78 0.07 I L FJ16 262 18:55:01.88 -30:28:43.8 m1 ---- 13.916 0.058 I L? Note 263 18:55:03.88 -30:28:59.3 m1 0.5851 17.439 0.465 I RR0 Note 264 18:55:03.75 -30:28:49.4 f ---- 13.87 0.08 I L FJ16 265 18:55:02.99 -30:28:52.0 f ---- 14.00 0.08 I L FJ16 266 18:55:03.46 -30:28:46.5 m1 ---- 14.04 0.08 I L FJ16 267 18:55:03.46 -30:28:45.1 m1 ---- 13.66 0.09 I L FJ16 268 18:55:03.00 -30:28:44.3 m1 ---- 13.79 0.09 I L FJ16 269 18:55:03.71 -30:28:43.1 f ---- 13.62 0.10 I L FJ16 270 18:55:02.60 -30:28:48.9 f ---- 13.550 0.095 I L? Note 271 18:55:04.00 -30:28:37.1 m1 ---- 13.737 0.104 I SR Note 272 18:55:03.07 -30:28:48.0 u ---- 14.25 0.05 I L FJ16 273 18:55:03.71 -30:28:35.3 m1 61.0 13.284 0.137 I SR Note 274 18:55:03.83 -30:29:03.9 m1 40.0 13.407 0.077 I SR Note 275 18:55:02.35 -30:28:43.4 m1 56.0 13.697 0.182 I SR Note 276 18:55:03.66 -30:28:50.5 m1 ---- 14.06 0.16 I L FJ16 277 18:55:03.31 -30:28:49.8 f ---- 13.71 0.19 I L FJ16 278 18:55:04.07 -30:28:49.8 f ---- 13.13 0.33 I L FJ16 279 18:55:04.05 -30:28:41.4 m3 ---- 13.352 0.256 I SR Note 280 18:55:03.69 -30:28:52.0 m1 136.0 13.25 0.46 I SR Note 281 18:55:03.32 -30:28:47.3 u ---- 16.71 0.45 I ? FJ16 282 18:55:03.01 -30:28:35.8 u ---- 17.52 0.74 I ? FJ16 283 18:55:03.75 -30:28:53.9 f ---- 16.97 0.76 I ? FJ16 284 18:55:03.37 -30:28:38.0 f ---- 17.343 0.269 I RR0 Note 285 18:55:02.69 -30:28:32.5 f 0.6335 17.244 0.245 I RR0 Note 286 18:55:03.54 -30:28:51.1 m3 473.0 15.04 -- I ? max;Note 287 18:55:03.37 -30:28:35.9 f 36.0 13.936 0.141 I SR Note 288 18:55:03.41 -30:28:52.8 m2 ---- -- -- I ? FJ16 289 18:55:02.90 -30:28:39.9 m1 0.4739 17.398 0.587 I RR0 Note 290 18:55:03.48 -30:29:06.2 f ---- 13.984 0.119 I L? Note 291 18:55:03.26 -30:28:41.1 m1 0.3381 17.209 0.171 I RR1 Note 292 18:54:58.75 -30:28:41.7 m1 0.2784 17.703 0.217 I RR1 293 18:55:03.70 -30:28:26.6 m1 0.6193 17.460 0.257 I RR0 294 18:55:03.06 -30:28:24.0 m1 0.3596 17.322 0.209 I RR1 295 18:55:02.89 -30:28:27.8 m3 0.6118 17.224 0.305 I RR0 296 18:54:31.64 -30:29:41.5 u 0.6423 17.507 0.275 I RR0 297 18:54:34.83 -30:30:41.8 u 50. 13.359 0.275 I SR 298 18:54:49.14 -30:25:51.5 f 0.8643 16.412 0.314 I spot 299 18:54:50.41 -30:32:49.7 f 0.2374 14.177 0.113 I spot 300 18:54:52.46 -30:25:38.5 m1 0.7699 18.277 0.262 I EW max 301 18:54:52.95 -30:29:53.5 m1 ---- 13.959 0.110 I ? 302 18:54:54.51 -30:24:53.1 m1 2.7959 18.599 1.635 I EB max 303 18:54:55.88 -30:32:43.4 m1 130. 14.514 0.043 I SR 304 18:54:58.80 -30:28:10.5 m3 0.7118 18.751 0.268 I EB max 305 18:55:00.07 -30:28:47.0 f 0.6570 18.457 0.447 I EW max 306 18:55:00.19 -30:28:36.2 m1 ---- 14.012 0.093 I ? 307 18:55:00.47 -30:28:16.7 m1 44.0 13.774 0.096 I SR 308 18:55:00.51 -30:28:48.4 m1 0.5720 17.652 0.494 I RR0 309 18:55:01.10 -30:28:33.8 f 30.0 13.599 0.080 I SR 310 18:55:01.70 -30:28:39.7 u 0.6168 17.009 0.228 I RR0 311 18:55:02.20 -30:28:42.5 m1 24.0 13.996 0.056 I SR 312 18:55:03.08 -30:28:28.4 f 0.7671 17.434 0.285 I ? 313 18:55:03.42 -30:29:13.4 m1 85.0 13.870 0.097 I SR 314 18:55:03.49 -30:28:35.7 m1 ---- 16.421 0.388 I L 315 18:55:03.49 -30:29:21.2 m1 ---- 16.547 1.054 I L 316 18:55:03.51 -30:30:35.9 m1 7.4788 17.901 0.281 I EB 317 18:55:03.56 -30:28:00.0 m1 ---- 13.670 0.054 I L 318 18:55:03.61 -30:28:53.6 f 125. 14.651 0.355 I SR 319 18:55:03.81 -30:28:34.1 m1 ---- 17.438 0.753 I L 320 18:55:03.83 -30:28:45.3 f 29.5829 13.709 0.052 I Ell max 321 18:55:03.84 -30:28:19.2 m1 0.3537 17.570 0.240 I RR01 Note 322 18:55:04.38 -30:28:50.0 m1 145. 15.304 0.423 I SR 323 18:55:04.81 -30:28:06.0 u 0.2782 17.444 0.070 I RR1 324 18:55:04.89 -30:28:18.9 m1 0.5894 17.431 0.430 I RR0 325 18:55:05.13 -30:28:42.5 m1 ---- 16.015 0.780 I ? 326 18:55:05.27 -30:29:24.6 m1 ---- 14.305 0.050 I ? 327 18:55:05.45 -30:28:45.3 m1 ---- 13.785 0.149 I L 328 18:55:05.91 -30:28:11.2 m1 ---- 13.354 0.048 I L 329 18:55:06.24 -30:28:43.2 m1 65.0 13.729 0.163 I SR 330 =V80;Note 331 18:55:09.74 -30:31:37.8 m1 0.97 17.395 0.123 I ? 332 18:54:34.98 -30:26:21.0 u 0.2664 17.407 0.201 I EW max 333 18:55:10.26 -30:33:40.6 m1 ---- 13.415 0.091 I L 334 18:55:13.18 -30:29:02.4 m1 ---- 14.719 0.049 I ? 335 18:55:13.59 -30:26:04.2 m1 ---- 13.618 0.092 I L 336 18:55:30.23 -30:32:09.2 u 0.5056 15.761 0.305 I Ell 337 18:55:15.27 -30:33:59.6 m1 1.0818 19.226 1.170 I EB max 338 18:55:23.78 -30:34:44.7 u 0.6387 17.330 0.216 I RR0 339 18:55:25.53 -30:26:12.8 m1 ---- 13.245 0.379 I L 340 18:55:27.07 -30:24:03.2 u ---- 13.949 0.068 I L 341 18:55:29.13 -30:33:09.4 u 0.89 16.838 0.111 I ? 342 18:55:29.58 -30:24:30.7 u ---- 14.400 0.036 I ? 343 18:55:30.46 -30:25:00.0 u 0.2502 19.279 0.927 I EW max 344 18:55:32.63 -30:25:26.2 u ---- 14.408 0.050 I ? 345 18:55:33.61 -30:26:12.9 u 0.2372 19.873 1.427 I EB 346 18:55:25.56 -30:26:15.1 u ---- -- -- ? 347 18:55:36.68 -30:30:28.4 u 0.4725 19.893 0.897 I ? 348 18:54:27.78 -30:25:50.7 u 0.5874 17.526 0.461 I RR0 Sos14 349 18:54:40.59 -30:24:29.8 u 0.2285 19.098 0.610 I EC max;Sos16 350 18:54:45.39 -30:30:13.3 f 2.9526 18.777 0.169 I E max;Sos16 351 18:54:58.71 -30:25:51.3 m1 1.3325 19.203 0.392 I E max;Sos16 352 18:55:03.34 -30:28:03.9 m1 0.8593 17.159 0.269 I E max;Sos16 ======================================================================= Supplementary Notes NGC 6715 (M54) is located in a Milky Way Galactic Bulge field. However, the cluster resides in the centre of the Sagittarius dwarf galaxy which is about three times more distant than the Galactic Bulge. The cluster and its surrounding field were observed in the OGLE IV Galactic Bulge survey. Results from this survey have been reported by Soszynski et al. (2014 - hereafter Sos14) for RR Lyrae variables and by Soszynski et al. (2016 - hereafter Sos16) for eclipsing binaries. The most comprehensive investigation of the variable stars in NGC 6715 was by Hamanowicz et al. (2016 - hereafter H16), based on the OGLE IV data. They announced 52 new variables, V296-V347 and also published data for most of the previously known variables. Among their new variables, H16 listed only variable stars located less than 7.5 arcmin from the cluster centre, the tidal radius that was published in the 1999 and 2003 updates to the Harris (1996) catalogue. A few additional OGLE IV variables have been included in this catalogue, variables with r<9.5 arcminutes, which is the tidal radius derived from the data published by Harris (2010.) The data in the above table are from H16 unless indicated otherwise in the Notes/Remarks column where S10 refers to Sollima et al. (2010). These stars were located in the gaps between CCDs in OGLE IV investigation. FJ16 refers to Figuera Jaimes et al. (2016), a study of the central region of the cluster. FJ16 discovered 80 new variables in the central region and the RA and dec listed for these variables are from their study. 45 of the FJ16 variables were also recovered by H16 and in these cases, the Notes on individual stars indicate the source for the entries in the table Sos14 refers to Soszynski et al. (2014), OGLE IV RR Lyrae data Sos16 refers to Soszynski et al. (2016), OGLE IV eclipsing data For variable stars in clusters located in Galactic bulge fields, it is challenging to establish cluster membership because field stars can often be found within the tidal radius. Without radial velocities or proper motions, the best approach is to consider the location in the CM diagram as well as distance from the cluster centre. ============================================ Notes on individual stars V10, V13: These two variables were considered to be field stars by H16 on the basis of their distances from the cluster centre: 9.0 and 8.5 arcminutes respectively, both outside their assumed tidal radius of 7.5 arcminutes. However, the tidal radius, derived from the data published by Harris (2010) is 9.47 arcminutes. Thus, since their mean magnitudes are appropriate for cluster membership, they might be cluster members. V12: This is a double mode RR Lyrae variable (RR01) with the first overtone mode dominant. The period and I amplitude of the fundamental mode are 0.4357 days and 0.068 mag. Thus the period ratio P1/P0 is 0.7405 and the amplitude ratio A1/A0 is 4.1. Rosino & Nobili (1958) concluded that this was probably a field star. However, H16 considered it to be a cluster member, probably based on the fact that, with r=5.5 arcmin, it is well inside the cluster tidal radius. However, since V12 is more than 1 magnitude brighter than the cluster RR Lyrae variables, it probably belongs to the rich field in which the cluster is located. V14: This star is a confirmed RR Lyrae variable, but there is some uncertainty concerning its period. Rosino & Nobili (1958) derived P=0.6892 days and published a good light curve. However, according to S10, this period was in clear disagreement with their observations and claimed that 0.4807214 was a better value. Unfortunately, they did not publish a light curve for V14 because they did not have calibrated photometry. No data are available from H16 because V14 was located in the gap between CCDs in the OGLE IV investigation and Layden & Sarajedini (2000) did not have enough observations to derive a period. The apparent magnitudes published by Rosino & Nobili and by Layden & Sarajedini are appropriate for cluster membership. V18: The data are from the OGLE investigation of Bulge eclipsing binary systems by Sos16 where the star is listed as OGLE-BLG-ECL-424738. Since r=10.6 arcmin from the cluster centre, this star probably belongs to the rich field around the cluster. H16 also published data for V18, based on OGLE IV observations, but their magnitudes and amplitudes were different from the ones listed by Sos16. V20, V22, V27, V53, V72: The non-variable status of these five stars was first noted by Layden & Sarajedini (2000) and later confirmed by both S10 and by H16. Rosino & Nobili (1958) had suggested that V72 might be an eclipsing variable that was not part of the cluster. V21, V26: Layden & Sarajedini (2000) found that the positions of these stars on Rosino & Nobili's finder charts did not match their published x,y coordinates which were later listed by Sawyer Hogg (1973) in her 3rd catalog. They checked several candidate variables in the regions in question and found no evidence for variability. Rosino & Nobili had already noted that V21 might not be variable. The non-variable status of both V21 and V26 was subsequently confirmed by S10 and by H16. V24: Rosino & Nobili (1958) concluded that V24 might not be variable and its non-variability was confirmed by H16. It was outside the field observed by Layden & Sarajedini (2000) and by S10. V66: The photometry for V66 is from Layden & Sarajedini (2000). No data are available from H16 because the star was located near the edge of the CCD in the OGLE IV investigation. Furthermore, its image was saturated. S10 confirmed its status as a long period variable, but did not publish any photometry. V73, V79, V81: Rosino & Nobili (1958) noted that it was difficult to estimate the magnitudes for these three stars, but nevertheless concluded that they were all variable. Layden & Sarajedini (2000) had difficulty locating them from the x,y coordinates that were published by Rosino & Nobili and later listed by Sawyer Hogg (1973) in her 3rd catalog. However, they checked several candidate stars in the regions in question and in each case they detected one candidate variable, but were unable to derive any acceptable periods. They marked the positions of each of these candidate variables on a finder chart. However, no variability was detected in any of these stars in the subsequent investigations of S10 and H16. Therefore they are classified as CST. V75: This variable was announced by Rosino & Nobili (1958) who derived a period: 0.5797 days, but did not publish a light curve. They commented that there was a lot of scatter, particularly at minimum light because its image was blended with that of a nearby star. Because of this image blending, Layden & Sarajedini (2000) could not confirm the variability of V75 and unfortunately it fell in a gap between the chips in the OGLE IV investigation. Consequently, it was not studied by H16. The period listed for this variable (0.5846 days) was derived by S10 who published a satisfactory light curve, but were unable to obtain reliable calibrated photometry. V80, V86, V330: There has been some confusion concerning the identification of these three variables. V80 is OGLE-BLG-RRLYR-37621 (P=0.6309 days) V86 is OGLE-BLG-RRLYR-37624 (P=0.5837 days) V330 is OGLE-BLG-RRLYR-37621 and therefore the same star as V80. V80 was announced by Rosino & Nobili (1958) with x,y coordinates (arcsec) and an ID chart. V86 was discovered by Layden & Sarajedini (2000) who published pixel positions, finder charts and periods for both V80 and V86. A close comparison of the pixel postions and periods that Layden & Sarajedini published for V80 and V86 with the OGLE IV data (Sos14) indicates that V80 = OGLE-BLG-RRLYR-37621 and V86 = OGLE-BLG-RRLYR-37624. However, both Sos14 and H16 indicated that V80 was OGLE-BLG-RRLYR-37624. This mis-identification arose because of an error by S10 who confused V80 with V86. The RA and dec they published for V80 were the coordinates of V86 and they did not publish a position for V86. Furthermore, the period they derived for their V80 (0.6394 days) was not the correct period for either star. The S10 data for V80 were listed in the 2010 and 2014 updates to this (Clement) electronic catalogue and that is why Sos14 and H16 both adopted their ID for V80. The RA and dec that were listed for V86 in the 2010, 2014 updates of this (Clement) catalogue were derived by Samus et al. (2009) and are in good agreement (less than 2 arcsec) with the coordinates listed by Sos14 and H16 for OGLE-BLG-RRLYR-37624. V91: Layden & Sarajedini (2000) classified this star as a detached binary and derived a period of 0.4098 days. However, H16 did not confirm its variability nor was it on the list of OGLE IV eclipsing binaries (Sos16). It might be a binary that was not observed in eclipse in the OGLE IV investigation. However, its position in the CM diagram indicates that it is probably not a cluster member. V99: This is OGLE-BLG-ECL-424691. There are significant differences between the magnitudes listed by Sos16 and H16 for this star, particularly in V. The values listed in the above table are from Sos16. The location of V99 in the CM diagram indicates that it is probably not a cluster member. V100: Layden & Sarajedini derived a period of 0.96473. However, they pointed out that their light curve had large scatter and poor phase coverage so that the period and photometry were uncertain. No variabiity was detected in subsequent studies by S10 or by H16. Therefore V100 is classified as CST. V107: Layden & Sarajedini (2000) listed this star as a probable long period variable, but noted that it was in a crowded field. H16 did not detect any variation. It is therefore classified as CST. V108: The photometry for V108 is from Layden & Sarajedini (2000). No data are available from H16 because the star was located in the gap between CCDs in the OGLE IV investigation. Furthermore, it was not studied by S10 because it was located near a bright (saturated) star on their CCD and its image had to be masked. The VI magnitudes published by Layden & Sarajedini indicate that V108 is located near the RG tip in the CM diagram published by H16 where the SR variables are located. V112: The data listed for this SR variable are from H16. They derived a period of 90 days based on approximately 150 observations made between March and November 2011. Figuera Jaimes et al. (2016) derived a slightly longer period (100 days) from observations made on 44 nights between May 2013 and September 2015. V157: This star was not observed in the OGLE IV investigation because it fell in the gap between the CCDs. The only available data for V157 are from the discovery paper by S10. They derived a period of 0.4556 days and classified it as an RR1 variable, but did not publish a light curve. This period is longer than any of the other RR1 variables and shorter than any of the RR0 variables. Thus the classification is uncertain. V160: The period that H16 derived for this star was independently confirmed by Figuera Jaimes et al. (2016). It is ~0.01 day greater than the period announced by S10 in their discovery paper. The H16 values are listed in the above table. V173: V173 was discovered by S10 and its variablity was confirmed by both FJ16 and H16. However, its variability was not announced by Sos14 when they reported their results for RR Lyrae variables in the OGLE IV Galactic bulge survey. FJ16 and H16 derived the same period (0.3603 days), which was a bit shorter than the one derived by S10 (0.3616 days) in their discovery paper. The H16 I magnitude was brighter and the amplitude smaller than the values pubished by FJ16, possibly because the star's image was unresolved in the OGLE IV data. Therefore the FJ16 magnitude and amplitude are listed in the above table. V181: V181 was discovered by S10 who derived a period of 0.5071515 days, which is close to half a day. They did not publish a light curve or any magnitudes. Their period was not confirmed in the subsequent studies and is unlikely to be correct. The period published by H16 (~0.467 days) is an alias of the period published by FJ16 (~0.877 days). In the above table, the H16 period and the FJ16 magnitude and amplitude have been adopted because they fit the period amplitude relation published by H16. V192: V192 was discovered by S10 who derived a period of ~0.399 days, but did not publish a light curve or any magnitudes. Its variablity was confirmed in subsequent investigations by Sos14, H16 and FJ16, but they did not confirm the S10 period. They all derived a period of 0.6004 days. The OGLE IV (Sos14 and H16) I magnitude was brighter and the amplitude smaller than the values published by FJ16, probably because the star's image was unresolved in the OGLE IV data. Therefore the FJ16 magnitude and amplitude are listed in the above table. V213: V213 was investigated by both FJ16 and H16 who derived the same period (0.2861 days). The H16 I magnitude was brighter and the amplitude smaller than the values pubished by FJ16, probably because the star's image was unresolved in the OGLE IV data. Therefore the FJ16 magnitude and amplitude are listed in the above table. V214: V214 was investigated by both FJ16 and H16, but they derived different periods. Since the light curve of FJ16 (P=0.3054) has a lot of scatter, the H16 period (0.6239 days), mean magnitude and amplitude have been adopted in the above table. Their values fit well on their period-amplitude relation. However, we note that the magnitudes labelled on their light curve for V214 do not correspond to the values they listed in their table. V215: Both FJ16 and H16 investigated V215 and their results are in good agreement. The H16 values for period, mean magnitude and amplitude are listed in the above table. V217: Both FJ16 and H16 investigated V217 and their results are in good agreement. The H16 values for period, mean magnitude and amplitude are listed in the above table. V219: Both FJ16 and H16 investigated V219 and their results are in good agreement. The H16 values for period, mean magnitude and amplitude are listed in the above table. V220: V220 was investigated by both FJ16 and H16, but they derived different periods. Since the light curve of FJ16 (P=0.3389) has a lot of scatter, the H16 period (0.6026 days), mean magnitude and amplitude have been adopted in the above table. Their phase coverage is more extensive and their values fit well on their period-amplitude relation. V221: FJ16 derived two periods for V221: 0.459608 (fundamental mode) and 0.343828 (first overtone). The period ratio is typical for a double mode RR Lyrae variable and therefore the star is classified as a double mode RR Lyrae. The data listed in the above table correspond to the fundamental mode. V221 was not investigated by H16. V223: Both FJ16 and H16 investigated V223 and their results are in good agreement. The H16 values for period, mean magnitude and amplitude are listed in the above table. V229: Although FJ16 discovered V229, the data they published were from the OGLE IV survey (Sos14 and H16). The magnitude and amplitude have not been listed above because the published values indicate that the star has an unresolved companion. FJ16 also pointed out McDonald et al. (2014) identified V229 as short period variable #SPVSgr18550405-3028580 in the VISTA survey of variables in the Sagittarius dwarf galaxy. V230: V230 was investigated by both FJ16 and H16, but they derived different periods and classifications. Since the light curve of FJ16 (P=0.5326) has a lot of scatter and the H16 phase coverage is more extensive, the H16 period (1.1431 days), has been adopted. The star is located in a crowded field near the cluster centre and the magnitudes published by both FJ16 and H16 (I=16.04 and 15.669) seem too bright and the amplitudes (0.29 and 0.127) seem too small for a star of this type so these quantities have not been listed in the above table. V231: V231 was investigated by both FJ16 and H16 who derived the same period (0.5342 days). The H16 I magnitude was brighter and the amplitude smaller than the values pubished by FJ16, probably because the star's image was unresolved in the OGLE IV data. Therefore the FJ16 magnitude and amplitude are listed in the above table. V233: V233 was investigated by both FJ16 and H16 who derived the same period (0.5575 days). The H16 I magnitude was brighter and the amplitude smaller than the values pubished by FJ16, probably because the star's image was unresolved in the OGLE IV data. Therefore the FJ16 magnitude and an amplitude (derived from their published light curve) are listed in the above table. V234: V234 was investigated by both FJ16 and H16 who derived the same period (0.5598 days). The H16 I magnitude was brighter and the amplitude smaller than the values pubished by FJ16, probably because the star's image was unresolved in the OGLE IV data. Therefore the FJ16 magnitude and amplitude are listed in the above table. V236: V236 was investigated by both FJ16 and H16 who derived the same period (0.5685 days). The star is located in a crowded field near the cluster centre and the magnitudes published by both FJ16 and H16 (I=16.53 and 15.526) seem too bright and the amplitudes (0.28 and 0.099) seem too small for a star of this type so these quantities have not been listed in the above table. V237: Both FJ16 and H16 investigated V237 and their results are in reasonable agreement. The H16 values for period, mean magnitude and amplitude are listed in the above table. V238: FJ16 derived a period for this star but the light curve has a great deal of scatter. Based on its mean magnitude the star is tentatively classified as an RR Lyrae variable. It was not investigated by H16. V239: Both FJ16 and H16 investigated V239 and their results are in reasonable agreement. The H16 values for period, mean magnitude and amplitude are listed in the above table. V240: V240 was investigated by Sos14, FJ16 and H16 who derived the same period (0.5963 days). However, the FJ16 and Sos14 mean I magnitudes were brighter and their amplitudes smaller than the values published by H16 probably due to the effects of crowding. Therefore the H16 magnitude and amplitude are listed in the above table. V241: Both FJ16 and H16 investigated V241 and their results are in reasonable agreement. The H16 values for period, mean magnitude and amplitude are listed in the above table. V242: Both FJ16 and H16 investigated V242 and derived the same period (0.6048 days). However, the FJ16 mean I magnitude was brighter and their amplitude smaller than the values published by H16 probably due to the effects of crowding. Therefore the H16 magnitude and amplitude are listed in the above table. V242 was not investigated by Sos14. V244: The period for V244 is from H16. Although FJ16 discovered V244, the data they published were from the OGLE IV survey (Sos14 and H16). The magnitude and amplitude have not been listed above because the published values indicate that the star has an unresolved companion. V246: The period for V246 is from H16. Although FJ16 discovered V246, the data they published were from the OGLE IV survey (Sos14 and H16). The magnitude and amplitude have not been listed above because the published values indicate that the star has an unresolved companion. V247: Both FJ16 and H16 investigated V247 and derived the same period (0.6509 days). However, the FJ16 mean I magnitude was brighter probably due to the effects of crowding. Therefore the H16 magnitude and amplitude are listed in the above table. V247 was not investigated by Sos14. V250: Both FJ16 and H16 investigated V247 and derived the same period (0.6806 days). The H16 values for magnitude and amplitude have been listed in the above table. V251: Both FJ16 and H16 investigated V251 and their results are in reasonable agreement. The H16 values for period, mean magnitude and amplitude are listed in the above table. V252: V252 was investigated by both FJ16 and H16 who derived the same period (0.7287 days). The H16 I magnitude was a bit brighter and the amplitude smaller than the values pubished by FJ16, probably because the star's image was unresolved in the OGLE IV data. Therefore the FJ16 magnitude and amplitude are listed in the above table. V253: V253 was investigated by both FJ16 and H16 who derived the same period (0.7439 days). The H16 I magnitude was brighter and the amplitude smaller than the values pubished by FJ16, probably because the star's image was unresolved in the OGLE IV data. Therefore the FJ16 magnitude and amplitude are listed in the above table. V254: Both FJ16 and H16 investigated V254 and their results are in reasonable agreement. The H16 values for period, mean magnitude and amplitude are listed in the above table. V255: V255 was investigated by both FJ16 and H16 who derived the same period (0.7601 days). However, the FJ16 mean I magnitude was brighter probably due to the effects of crowding. Therefore the H16 magnitude and amplitude are listed in the above table. V255 was not investigated by Sos14. V256: V256 was investigated by both FJ16 and H16 who derived the same period (14.8 days). However, the FJ16 mean I magnitude was brighter probably due to the effects of crowding. Therefore the H16 magnitude and amplitude are listed in the above table. V256 was not investigated by Sos14. V262: Both FJ16 and H16 investigated V262 and their results are in reasonable agreement. Neither group derived a period. The H16 values for mean magnitude and amplitude are listed in the above table. V263: Both FJ16 and H16 investigated V263, but obtained different results. H16 classified it as an RR Lyrae, while FJ16 concluded that it was a slow variable. However, the FJ16 light curve is consistent with the possibility of short term variation. The H16 values for period, mean magnitude and amplitude are listed in the above table. FJ16 pointed out that McDonald et al. (2014) identified V263 as short period variable #SPVSgr18550386-3028593 in the VISTA survey of variables in the Sagittarius dwarf galaxy. V270: Both FJ16 and H16 observed this slow variable and obtained similar results. The mean magnitude and amplitude of H16 have been listed in the above table. V271: Both FJ16 and H16 observed this slow variable and obtained similar results. The mean magnitude and amplitude of H16 have been listed in the above table. V273: Both FJ16 and H16 observed this slow variable and obtained similar results. The period, mean magnitude and amplitude of H16 have been listed in the above table. V274: Both FJ16 and H16 observed this slow variable and obtained similar results. The period, mean magnitude and amplitude of H16 have been listed in the above table. V275: Both FJ16 and H16 observed this slow variable and obtained similar results. The period, mean magnitude and amplitude of H16 have been listed in the above table. V279: Both FJ16 and H16 observed this slow variable and obtained similar results. The mean magnitude and amplitude of H16 have been listed in the above table. V280: Both FJ16 and H16 observed this slow variable and obtained similar results. In the above table, the period and classification of H16 and the mean magnitude and amplitude of FJ16 have been listed. V284, V285, V287, V289, V290 V291: All of these variables were dicovered by FJ16 but they were unable to classify any of them. Since they were also observed by H16, the H16 data are listed in the above table. V286: V286 was discovered by FJ16. They could not derive a mean magnitude or amplitude because the star disappeared below their detection limit at minimum light. Therefore they published the magnitude at maximum light (I=15.04) instead. H16 derived a period (473 days), but it appears that the star's image was blended in their data. According to Bramich (2017, private communication), I > 18.3 mag at minimum light. Thus the I amplitude is greater than 3.25 mag. The period and large amplitude of V286 are characteristic of a Mira variable. If it is a Mira variable, it seems too faint to be a cluster member. V321: This is a double mode RR Lyrae variable (RR01) with the first overtone mode dominant. The I magnitude, period and amplitude in the above table are the values Sos14 listed for the first overtone. The period and I amplitude of the fundamental mode are 0.4767 days and 0.080 mag. Thus the period ratio P1/P0 is 0.7420 and the amplitude ratio A1/A0 is 3. ================================================================= Discovery of the variable stars in M54: V1-28 Rosino (1952) with x,y (arcsec) coordinates and ID charts V29-82 Rosino & Nobili (1958) with x,y (arcsec) coordinates and ID charts. Also all the variables from V1-28 (with the exception of V11, 16 and 19) were labelled on the charts. V83-117 Layden & Sarajedini (2000) with X,Y (pixel) coordinates. They also published small finder charts (field 20 by 20 arcsec) for each of the variables they studied. These authors also announced three candidate variables which they numbered SV1-3. Their study was based on VI photometry. V118-211 S10 with RA and dec. They published magnitudes, amplitudes and colours based on BVI photometry for the variables in their investigation. V212-291 Figuera Jaimes et al. (2016) with RA, dec and an ID chart V292-295 = VC16, VC22, VC24, VC38 of Montiel & Mighell (2010) with RA and dec The numbers V292-295 were assigned by H16. V296-347 H16 with RA, dec and finder charts Their investigation was based on data from the OGLE IV survey and their tables and charts are available from the OGLE FTP Site: ftp://ftp.astrouw.edu.pl/ogle/ogle4/OCVS/M54/ Among their new variables, H16 list only variables that are located less than 7.5 arcmin from the cluster centre, the tidal radius that was published in the 1999 and 2003 updates to the Harris (1996) catalogue. V348 = OGLE-BLG-RRLYR-37496 from the Ogle IV investigation of RR Lyrae variables in the Galactic Bulge by Sos14. The number V348 has been assigned in this catalogue. Data and chart for V348 are available from the OGLE FTP Site: ftp://ftp.astrouw.edu.pl/ogle/ogle4/OCVS/blg/rrlyr With r=8.2 arcmin, V348 is inside the tidal radius, 9.7 arcmin, derived from the core concentration and radius publihed by Harris (2010). #37496 was independently announced by Cseresnjes et al. (2000) as vs11f53. Another RR Lyrae variable, OGLE-BLG-RRLYR-37506, with r=9.0 arcmin is located within the tidal radius, but its magnitudes are too bright for cluster membership. V349 = OGLE-BLG-ECL-424672 (r=7.5') V350 = OGLE-BLG-ECL-424680 (r=4.1') V351 = OGLE-BLG-ECL-424692 (r=3.1') V352 = OGLE-BLG-ECL-424696 (r=0.7') from the Ogle IV investigation of eclipsing binary stars in the Galactic Bulge by Sos16. Data and charts are available from the OGLE FTP Site: ftp://ftp.astrouw.edu.pl/ogle/ogle4/OCVS/blg/ecl The numbers V349-352 have been assigned in this catalogue. Two other eclipsing stars within the tidal radius, OGLE-BLG-ECL-000216 (r=9.5') and OGLE-BLG-ECL-424733 (r=7.9') appear to be field stars based on their positions in the CMD ----------------------------------- Montiel & Mighell (2010) announced 50 RR Lyrae candidates based on an analysis of archival HST WFPC2 data. They assigned numbers VC1 to VC50 to their candidates. The HST observations were obtained over an interval of a few hours on one day and were not sufficient for period determination. However, a comparison with the known RR Lyrae variables indicates that 40 of their candidates have been confirmed as RR Lyrae variables in other investigations: VC1=V241, VC2=V127, VC4=V220, VC5=V255, VC7=V234, VC8=V221, VC9=V216, VC10= V223, VC11=V162, VC12=V163, VC13=V95, VC14=V164, VC15=V142, VC16=V292, VC17=V129, VC18=V179, VC20=V224, VC22=V293, VC23=V250, VC24=V294, VC25=V215, VC26=V245, VC27=V291, VC28=V181, VC30=V233, VC31=V237, VC32=V284, VC33=V285, VC34=V160, VC35=V212, VC36=V236, VC37=V225, VC38=V295, VC39=V214, VC40=V213, VC41=V232, VC44=V46, VC45=V148, VC46=V192, VC47=V76. The declinations listed in the above table are on average 1 arcsec south of the decs listed by Montiel & Mighell and the RAs are approximately 0.02 seconds (of time) east. =============================================================== References Cseresnjes, P., Alard, C., Guibert, J. 2000, A&A, 357, 871 Figuera Jaimes, R., Bramich, D. M., Kains, N., Skottfelt, J., Jorgensen, U. G., Horne, K., Dominik, M. and 34 coauthors, 2016, A&A, 592, A120 Hamanowicz, A., Pietrukowicz, P., Udalski, A., Mroz, P., Soszynski, I., Szymanski, M. K., Skowron, J. and 5 coauthors, 2016, Acta A., 66, 197 (H16) Harris, W. E. 1996, AJ, 112, 1487 Harris, W. E. 2010, arXiv:1012.3224 Layden, A. C. & Sarajedini, A. 2000, AJ, 119, 1760 McDonald, I., Zijlstra, A. A., Sloan, G. C., Keris, E., Lagadec, E., Minniti, D. 2014, MNRAS, 439, 2618 Montiel, E. J. & Mighell, K. J. 2010, AJ, 140, 1500 Prudil Z., Arellano Ferro, A. 2024, MNRAS, 534, 3654 Rosino, L. 1952, Mem. S.A.I., 23, 49 = Bologna Publ., V, No. 18 Rosino, L. & Nobili, F. 1958, Mem. S.A.I., 29, 413 (No.4) = 1959, Univ. of Padova Asiago-Contr. 97 Samus, N. N., Kazarovets, E. V., Pastukhova, E. N., Tsvetkova, T. M., Durlevich, O. V. 2009, PASP, 121, 1378 Sollima, A., Cacciari, C., Bellazzini, M., Colucci, S. 2010, MNRAS, 406, 329 (S10) Soszynski, I., Pawlak, M., Pietukowicz, P., Udalski, A., Szymanski, M. K., Wyrzykowski, L., Ulaczyk, K. and 6 coauthors, 2016, Ac. A., 66, 405 (Sos16) Soszynski, I., Udalski, A., Szymanski, M. K., Pietukowicz, P. , Mroz, P., Skowron, J., Kozlowski, S. and 6 coauthors, 2014, Ac. A., 64, 177 (Sos14) =========================================================================