NGC 3201 / C1015-461 (Updated March 2019) RA: 10:17:36.82 -46:24:44.9 (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 10:17:42.82 -46:26:37.8 R0 0.6048 14.81 0.92 V RR0 AF 2 10:17:39.98 -46:26:37.9 R0 0.5326 14.80 1.07 V RR0 AF 3 10:17:54.47 -46:25:25.4 R0 0.5994 14.91 0.80 V RR0 4 10:17:52.01 -46:24:40.5 R0 0.6300 14.80 1.02 V RR0 5 10:17:41.28 -46:25:06.3 R0 0.5013 14.73 0.94 V RR0 AF 6 10:17:26.09 -46:27:02.3 R0 0.5253 14.74 0.90 V RR0 7 10:17:28.48 -46:27:48.6 R0 0.6303 14.69 0.67 V RR0 8 10:17:30.75 -46:26:19.3 R0 0.6286 14.74 0.73 V RR0 AF 9 10:17:32.28 -46:26:12.6 R0 0.5254 14.82 0.96 V RR0 AF 10 10:17:20.13 -46:20:50.1 R0 0.5352 14.84 0.88 V RR0 11 10:17:27.55 -46:22:55.6 R0 0.2991 14.79 0.58 V RR1 AF 12 10:17:29.03 -46:22:55.8 R0 0.4974 15.16 0.17 V RR0 AF 13 10:17:22.03 -46:23:11.2 R0 0.5748 14.85 0.88 V RR0 AF 14 10:17:22.42 -46:22:31.5 R0 0.5089 14.99 1.13 V RR0 AF 15 10:17:10.56 -46:27:32.6 R0 0.5347 14.62 1.12 V RR0 16 10:17:18.47 -46:28:36.5 R0 0.2634 14.62 0.63 V RR1 17 10:17:38.29 -46:25:07.2 R0 0.5658 14.76 0.92 V RR0 AF 18 10:17:39.4 -46:25:07 R0 0.5404 14.74 1.05 V RR0 AF 19 10:17:39.47 -46:19:30.8 R0 0.5250 14.73 0.92 V RR0 20 10:17:41.01 -46:20:03.4 R0 0.5291 14.68 1.07 V RR0 21 10:17:46.23 -46:22:29.4 R0 0.5668 14.83 0.73 V RR0 AF 22 10:17:27.64 -46:25:38.0 R0 0.6058 14.75 0.86 V RR0 AF 23 10:17:32.64 -46:25:31.1 R0 0.5868 14.80 0.77 V RR0 AF 24 10:17:04.91 -46:24:25.2 R0 0.5890 14.65 0.76 V RR0 25 10:17:46.15 -46:21:52.1 R0 0.5147 14.73 1.05 V RR0 AF 26 10:17:58.09 -46:27:01.8 R0 0.5690 14.91 0.92 V RR0 27 10:17:42.79 -46:30:01.0 R0 0.4843 14.76 1.21 V RR0 28 10:17:43.50 -46:25:30.4 R0 0.5795 14.87 0.86 V RR0 AF 29 10:17:12.91 -46:22:49.7 R0 0.5291 14.78 0.68 V RR0 30 10:17:09.91 -46:20:14.3 R0 0.5159 14.60 0.87 V RR0 31 10:17:54.55 -46:22:34.2 R0 0.5191 14.90 1.26 V RR0 32 10:17:55.78 -46:21:26.7 R0 0.5612 14.73 1.24 V RR0 33 10:17:41.81 -46:25:22.4 R0 ---- -- -- CST 34 10:18:05.48 -46:20:02.2 R0 0.4679 14.75 1.27 V RR0 P02 35 10:17:36.29 -46:22:43.2 R0 0.6155 14.75 0.63 V RR0 AF 36 10:17:27.01 -46:24:53.0 R0 0.4796 14.73 1.26 V RR0 AF 37 10:17:30.69 -46:25:55.7 R0 0.5751 14.74 1.05 V RR0 AF 38 10:17:31.42 -46:25:41.1 R0 0.5094 14.81 0.81 V RR0 AF 39 10:17:41.23 -46:23:49.7 R0 0.4829 14.81 1.20 V RR0 AF 40 10:17:28.00 -46:23:35.9 R0 0.6437 14.84 0.58 V RR0 AF 41 10:18:05.02 -46:24:14.8 R0 0.665 14.81 0.45 V RR0 P02 42 10:17:08.66 -46:21:28.1 R0 0.5382 14.61 1.22 V RR0 43 10:17:01.35 -46:24:25.8 R0 0.6761 14.65 0.50 V RR0 C84 44 10:17:40.08 -46:23:36.7 R0 0.6107 14.76 0.62 V RR0 AF 45 10:17:49.29 -46:25:14.6 R0 0.5381 14.91 1.09 V RR0 AF 46 10:16:59.09 -46:33:04.1 R0 0.5432 14.74 0.98 V RR0 C84 47 10:17:47.56 -46:20:41.7 R0 0.5212 14.65 0.89 V RR0 48 10:17:13.33 -46:24:28.8 R0 0.3413 14.68 0.65 V RR1 49 10:17:33.63 -46:22:13.4 R0 0.5810 14.72 1.04 V RR0 AF 50 10:17:36.1 -46:24:14 R0 0.5423 14.71 1.00 V RR0 AF 51 10:17:17.66 -46:25:06.3 R0 0.5186 14.72 1.16 V RR0 52 10:17:38.28 -46:37:58.2 R0 0.38 -- -- RR1 K71 53 10:16:13.05 -46:37:01.2 R0 0.5335 14.45 0.78 V RR0 W41;Note 54 10:18:41.66 -46:37:53.4 R0 0.5559 14.87 0.85 V RR0 C84 55 10:17:05.38 -46:12:00.2 R0 0.6041 14.57 0.55 V RR0 K71;Note 56 10:18:00.72 -46:23:10.1 R0 0.5903 14.89 0.79 V RR0 P02 57 10:18:04.87 -46:25:54.6 R0 0.5934 14.83 0.71 V RR0 P02 58 10:18:10.57 -46:26:04.6 R0 0.6220 14.70 0.72 V RR0 P02 59 10:16:50.02 -46:25:49.7 R0 0.5177 14.66 1.08 V RR0 C84 60 10:16:15.51 -46:23:16.1 R0 0.5036 14.59 1.10 V RR0 C84 61 10:15:49.23 -46:21:39.8 R0 0.5455 14.41 0.82 V RR0 K71;Note 62 10:15:55.75 -46:27:55.3 R0 0.5698 -- -- RR0 W41 63 10:16:01.31 -46:23:51.9 R0 0.5681 -- -- RR0 W41 64 10:16:35.78 -46:10:31.2 R0 0.5224 14.64 0.93 RR0 C84 65 10:16:45.35 -46:11:30.9 R0 1.6600 14.03 0.77 B E f;max;Note 66 10:16:59.09 -46:19:48.2 R0 0.2840 -- -- RR2? K71 67 10:17:00.89 -46:26:35.2 R0 0.3279 14.69 0.39 V RR1 C84 68 10:17:10.57 -46:10:46.2 R0 71.8 11.99 0.87 V Lb max;Note 69 10:17:16.26 -46:08:10.7 R0 0.5123 14.74 1.10 V RR0 C84 70 10:17:15.93 -46:24:54.5 R0 ---- -- -- CST 71 10:17:19.36 -46:26:36.5 R0 0.6012 14.70 0.78 V RR0 72 10:17:22.26 -46:14:50.6 R0 ---- -- -- RR1 K71;P=0.36? 73 10:17:25.20 -46:23:15.2 R0 0.5195 14.76 1.24 V RR0 AF 74 10:17:28.15 -46:24:06.4 R0 ---- -- -- CST 75 10:17:29.58 -46:22:20.4 R0 --- -- -- CST 76 10:17:31.29 -46:25:23.6 R0 0.5267 14.81 0.66 V RR0 AF 77 10:17:36.13 -46:25:36.1 R0 0.5674 14.71 0.86 V RR0 AF 78 10:17:36.88 -46:27:03.9 R0 0.5139 14.85 1.00 V RR0 79 10:17:38.39 -46:26:23.9 R0 ---- 11.87 -- V L Note;P>30 80 10:17:43.07 -46:24:16.8 R0 0.5887 14.80 0.59 V RR0 AF 81 10:17:46.51 -46:27:17.3 R0 0.5198 14.83 1.13 V RR0 82 10:17:52.85 -46:27:31.2 R0 ---- -- -- CST 83 10:17:54.76 -46:21:54.4 R0 0.5452 14.78 1.23 V RR0 84 10:18:11.69 -46:13:06.6 R0 0.5137 14.80 0.94 V RR0 C84 85 10:18:31.85 -46:31:23.8 R0 ---- -- -- CST W41;K71 86 10:18:36.46 -46:29:58.4 R0 ---- -- -- CST W41;K71 87 10:19:15.15 -46:32:07.9 R0 0.6039 14.55 0.61 V RR0 W41;Note 88 10:18:00.49 -46:06:40.2 R0 0.5487 -- -- RR0 K71;Note 89 10:19:53.58 -46:28:00.0 R0 0.6098 14.53 0.53 RR0 K71;Note 90 10:17:34.95 -46:24:33.3 R0 0.6064 14.68 0.94 V RR0 AF 91 10:15:11.31 -46:04:43.3 R0 0.3471 14.51 0.45 V RR1 K71:Note 92 10:17:22.7 -46:25:11 R0 0.5395 14.76 0.99 V RR0 AF 93 10:20:51.15 -46:28:03.6 R0 0.4781 14.48 0.93 V RR0 K71;Note 94 10:13:02.52 -45:53:44.2 R0 210.0 13.2 3.9 V M f;Note 95 10:20:37.83 -45:41:39.9 R0 ---- -- -- CST K71 96 10:13:05.16 -46:32:03.0 R0 0.5942 14.53 0.63 RR0 K71;Note 97 10:17:11.64 -46:25:51.0 R0 ---- -- -- CST LS03 98 10:17:25.60 -46:25:18.6 R0 0.3363 14.78 0.43 V RR1 A;Note 99 10:17:25.80 -46:24:39.4 R0 ---- -- -- CST LS03 100 10:17:36.14 -46:24:27.9 R0 0.5485 14.77 1.02 V RR0 AF 101 10:17:59.04 -46:33:25.5 R0 0.3731 17.27 -- V EC max 102 10:17:43.50 -46:21:53.4 R0 0.0453 17.15 0.05 V SXP 103 10:17:32.10 -46:22:37.9 R0 0.0373 17.37 0.04 V SXP 104 10:17:36.60 -46:23:03.4 R0 0.0375 17.46 0.025 V SXP 105 10:17:42.60 -46:24:19.5 R0 0.0376 17.37 0.07 V SXP 106 10:17:36.00 -46:24:38.2 R0 0.0435 16.89 0.04 V SXP 107 10:17:42.50 -46:24:49.1 R0 0.0405 16.96 0.13 V SXP f?;Note 108 10:17:40.20 -46:25:07.8 R0 0.0673 16.35 0.37 V SXP 109 10:17:36.00 -46:25:40.2 R0 0.0543 17.05 0.39 V SXP 110 10:17:48.10 -46:25:53.4 R0 0.0502 16.59 0.36 V SXP 111 10:17:50.90 -46:25:57.7 R0 0.0479 17.07 0.03 V SXP 112 10:17:20.10 -46:26:38.0 R0 0.0542 16.48 0.20 V SXP 113 10:17:25.86 -46:26:21.0 R0 26.0 11.809 0.024 V SR Note 114 10:17:31.59 -46:29:01.0 R0 ---- 11.892 0.044 V SR P>30 115 10:17:16.16 -46:25:32.7 R0 16.0 12.069 0.052 V SR 116 10:17:39.47 -46:25:32.3 R0 17.0 12.075 0.037 V SR 117 10:17:33.45 -46:24:34.6 R0 17.0 12.138 0.050 V SR 118 10:17:51.52 -46:22:09.7 R0 11.0 12.399 0.028 V SR 119 10:17:44.96 -46 25 13.3 R0 2.5516 16.049 0.202 V EA max;Note 120 10:17:38.30 -46:25:38.0 R0 0.0882 16.677 0.367 V SXP Note 121 10:17:36.58 -46:24:43.2 R0 0.0374 17.312 0.127 V SXP f?;Note 122 10:17:40.15 -46:25:12.7 R0 0.0673 18.107 0.053 V SXP f?;Note 123 10:17:48.12 -46:25:32.2 R0 0.0349 17.480 0.058 V SXP max 124 10:17:30.22 -46:26:09.1 R0 0.0401 17.245 0.022 V SXP max 125 10:18:07.43 -46:21:49.8 R0 0.0422 17.449 0.045 V SXP max 126 10:17:44.11 -46:20:58.4 R0 0.0399 17.405 0.052 V SXP f?;max;Note 127 10:17:40.68 -46:24:33.5 R0 0.0453 17.184 0.064 V SXP max 128 10:17:36.62 -46:23:55.1 R0 0.0345 17.410 0.052 V SXP max 129 10:17:35.73 -46:23:01.1 R0 0.0522 17.172 0.051 V SXP f?;max;Note 130 10:17:40.52 -46:25:17.7 R0 0.0473 16.357 0.021 V SXP max 131 10:17:15.36 -46:23:12.3 R0 0.0331 17.244 0.041 V SXP max 132 10:17:04.39 -46:19:54.7 R0 0.0476 16.551 0.103 V SXP max 133 10:17:44.70 -46:22:60.0 R0 0.2705 18.305 0.369 V EW max 134 10:17:44.08 -46:24:04.2 R0 0.2853 17.520 0.094 V EW? max;Ell? 135 10:17:39.12 -46:24:29.9 R0 0.2793 17.916 0.130 V EW? max;Ell? 136 10:17:24.64 -46:24:43.8 R0 0.7022 16.197 0.033 V EW? max;Ell? 137 10:17:43.14 -46:22:13.0 R0 7.4292 17.911 0.087 V EA max 138 10:17:28.33 -46:23:26.5 R0 9.1994 18.292 0.124 V EA max 139 10:17:22.58 -46:23:58.1 R0 8.7891 18.076 0.297 V EA max 140 10:17:15.32 -46:24:45.8 R0 ---- 18.499 0.411 V EA max 141 10:17:33.14 -46:25:07.4 R0 10.0037 17.154 0.149 V EA f?;max;Note 142 10:17:10.29 -46:22:38.5 R0 27.6930 17.257 0.108 V EA max 143 10:17:09.59 -46:28:03.7 R0 0.3807 20.565 0.324 V EA max 144 10:18:13.56 -46:19:42.5 R0 0.9382 14.626 0.025 V EB? max;Note 145 10:17:48.23 -46:29:05.0 R0 24.3462 18.133 0.110 V var? max;Note 146 10:17:30.48 -46:24:42.4 R0 13.7590 17.275 0.158 V Spot max;RG 147 10:17:21.25 -46:26:21.0 R0 1.9105 17.410 0.124 V Spot? max 148 10:18:10.19 -46:18:53.4 R0 0.4677 17.235 0.040 V var? max 149 10:18:01.79 -46:21:55.8 R0 0.0623 21.280 0.485 V EB? max 150 10:18:03.25 -46:23:39.2 R0 0.1864 15.225 0.016 V var? max 151 10:17:38.27 -46:19:49.2 R0 1.0335 14.275 0.021 V var? max 152 10:17:34.96 -46:19:37.7 R0 0.5168 14.692 0.018 V var? ma 153 10:17:39.66 -46:21:54.8 R0 0.8999 17.592 0.089 V ? max 154 10:17:27.35 -46:23:48.4 R0 0.1680 16.498 0.024 V ? max 155 10:17:25.15 -46:25:19.3 R0 0.2530 17.690 0.056 V EW? max 156 10:17:34.72 -46:26:30.0 R0 0.0413 17.084 0.029 V SXP? max 157 10:17:32.60 -46:26:45.5 R0 0.1746 15.651 0.016 V EW? max 158 10:17:21.78 -46:26:44.4 R0 0.1992 19.501 0.162 V EW? max 159 10:17:09.91 -46:23:09.3 R0 0.3872 17.392 0.028 V EW? max 160 10:17:46.98 -46:28:50.1 R0 ---- 17.695 0.170 V var? L? ======================================================================== Supplementary Notes The RA and dec for V1-101 are from Samus et al. (1999). They published ID charts in an earlier paper (Samus et al. 1996). Fourcade et al. (1966) also published charts, but Samus et al. (1996) pointed out that some of Fourcade's identifications were erroneous. Most of the elements for variables V1-100 are taken from Layden & Sarajedini (2003 = LS03) because their study was the most comprehensive. They also confirmed the "CST" classification that was previously reported by Wright (1941) and Kukarkin (1971a) for V33, V70, V74, V75 and V82. In addition they found that V97 and V99 were not variable. However, some variables were outside the LS03 field which was approximately 9.5 by 10 arcmin. In these cases, data from other sources are listed and this is indicated in the remarks column: P02 refers to a CCD investigation by Piersimoni et al. (2003). C84 refers to the photographic investigation by Cacciari (1984) W41 refers to stars for which Wright (1941) listed the only available data. These stars were all outside the field of the other studies of NGC 3201. Based on their mean magnitudes and the fact that they all lie within the 25.3 arcmin tidal radius derived from the 2010 update to the Harris catalogue, they appear to be cluster members. K71 refers to Kukarkin (1967,1971a,b). In 1967 and 1971a, he listed periods and in 1971b, he published the individual magnitudes. If no data were available from P02, the C84 data are listed and if C84 did not study the star, the W41 data are listed and failing that, K71. Kukarkin derived periods for variables announced by Wilkens (1965), that were outside the field of view in the other studies. He also investigated a few of the "outer" variables for which Wright (1941) was unable to derive periods. Some of the W41 and K71 variables have been included in the AAVSO VSX utility (Watson et al. 2006) and for these stars, the VSX data have been listed and this is discussed in the notes on individual stars. "AF" in the remarks column indicates that the period is from the study by Arellano Ferro et al. (2014). They derived their periods by combining their observations (made on 4 consecutive nights in March 2013) with those of LS03. Arellano Ferro's field of view was 5.1 by 5.1 arcminutes and included 34 of the 58 RRL stars observed by LS03. Their paper also includes an excellent finding chart that labels all of the variable stars in their field of view. The data for V101 (=V6 of von Braun & Mateo 2002), V102-112 (V1-11 of Mazur et al. 2003), V113-121 (LS03), V122-124 (Arellano Ferro et al. 2014) and V125-160 (Kaluzny et al 2016) are from the discovery papers unless indicated otherwise in the notes on individual stars. Information about membership status in the remarks column is from an investigation by Bustos Fierro & Calderon (2018). Their study was based on GaiaDR2 astrometry. They established membership status for all of the variables numbered 1 to 160 with the exception of V108, V119, V135, V149 and found that most variables were members or possible members. Stars designated 'f' or 'f?' in the remarks column are the ones they found to be field stars. ---------------- The effects of differential reddening across the face of NGC 3201 are substantial. This is illustrated in an extinction map published by von Braun & Mateo (2001) and was taken into account by Arellano Ferro et al. (2014) when they estimated the membership status of the SX Phe variables. Carretta et al. (2010) and Kravtsov et al. (2010) reported evidence for inhomogeneity in this cluster's stellar populations associated with radial distribution. ================================================================= Notes on individual stars V53 (1SWASPJ101613.07-463701.0): Watson et al. (2006) published a period, P=0.533469, in good agreement with Wright's (1941) earlier value. Watson et al. obtained their data from the Super WASP survey (Greer et al. 2017). Watson et al. also published maximum and minimum V magnitudes and the mean magnitude and amplitude listed above are based on their data. V55 (1SWASPJ101703.37-461159.9): Watson et al. (2006) published a period, P=0.60408, a bit lower than 0.6070, Kukarkin's (1971a) value. Watson et al. obtained their data from the Super WASP survey (Greer et al. 2017). Watson et al. also published maximum and minimum V magnitudes. The period, mean magnitude and amplitude listed above are based on their data. V61 (1SWASPJ101550.94-462115.7): Watson et al. (2006) published a period, P=0.545506, a bit higher than 0.54, Kukarkin's (1971a) value. Watson et al. obtained their data from the Super WASP survey (Greer et al. 2017). Watson et al. also published maximum and minimum V magnitudes. The period, mean magnitude and amplitude listed above are based on their data. V65 = KP Vel: The maximum magnitude and amplitude for this eclipsing binary are from Kukarkin (1971b). His data were not extensive enough to derive a period. The period was derived by W41 and was later confirmed by Chen et al. (2018) in the WISE catalogue of variable stars. The classification is from the GCVS and from Chen et al. V68 = NSV 4810 (ASAS 101711-4610.8): Wright (1941) noted that this star was probably a long period variable. It was not observed by LS03; it was outside their field. Samus et al. (2009) pointed out that V68 is the same star as NSV 4810 and ASAS 101711-4610.8 in the ASAS-3 catalogue (Pojmanski 2002). The period and magnitudes listed in the above table are from the ASAS-3 catalogue and the classification is from Samus et al. (2009). V79: Wright (1941) could not confirm the variability of this star, but both Piersimoni et al. (2002) and LS03 found that it was near the RGB tip, exhibited low level variability and could be a variable. V87 (1SWASPJ101912.42-463238.7): Watson et al. (2006) published a period, P=0.603924, in good agreement with Wright's (1941) earlier value. Watson et al. obtained their data from the Super WASP survey (Greer et al. 2017). Watson et al. also published maximum and minimum V magnitudes and the mean magnitude and amplitude listed above are based on their data. V88 (1SWASPJ101800.51-460640.2): Watson et al. (2006) published a period, P=0.54867882, somewhat lower than 0.57, Kukarkin's (1971) value. Watson et al. obtained their data from the Super WASP survey (Greer et al. 2017). Watson et al. listed maximum and minimum V magnitudes, but they were not on a standard system. The period listed above is Watson's value. V89 (ASASSN-VJ101953.63-462759.8): Watson et al. (2006) published a period, P=0.609779 which is an alias of 0.369, Kukarkin's (1971a) value. Watson et al. obtained their data from the ASAS-SN survey (Jayasinghe et al. 2018). The 0.6098 day period was also listed in the WISE catalogue of variables stars (Chen et al. 2018). Watson et al. published maximum and minimum V magnitudes. The period, mean magnitude and amplitude listed above are based on their data. V91 (ASASSN-VJ101511.31-460663.3): Watson et al. (2006) published a period, P=0.347116, a bit higher than 0.345, Kukarkin's (1971a) value. Watson et al. obtained their data from the ASAS-SN survey (Jayasinghe et al. 2018). Watson et al. published maximum and minimum V magnitudes. The period, mean magnitude and amplitude listed above are based on their data. V93 (1SWASPJ102052.70-462708.6): Watson et al. (2006) published a period, P=0.478104, in good agreement with 0.48, Kukarkin's (1971a) value. Watson et al. obtained their data from the Super WASP survey (Greer et al. 2017). Watson et al. published maximum and minimum V magnitudes. The period, mean magnitude and amplitude listed above are based on their data. V94 (ASASJ101302-4553.7): This star was classified as CST by Kukarkin (1971a). However, more recent observations have demonstrated that it is a field Mira variable. V94 is ASAS J101302-4553.7 (Pojmanski 2002). Watson et al. (2006) listed a period of 210 days, based on the ASAS catalogue. They also listed maximum and minimum V magnitudes. The period, mean magnitude and amplitude listed above are based on their data. The long term variability of this variable was also confirmed by Drake et al. (2017). The proper motion study of Bustos Fierro & Calderon (2018) confirmed that V94 is not a cluster member. V96 (ASASSN-VJ101305.15-463203.3): Watson et al. (2006) published a period, P=0.594184), in good agreement with 0.59, Kukarkin's (1971a) value. Watson et al. obtained their data from the ASAS-SN survey (Jayasinghe et al. 2018). Watson et al. published maximum and minimum V magnitudes. The period, mean magnitude and amplitude listed above are based on their data. V98: The position previously listed in this catalogue, also published by Samus et al. (2009) and by Arellano Ferro et al. (2014) was off by about 5 arcseconds. The error was pointed out by Bustos Fierro & Calderon (2018) whose corrected values for RA and dec are listed in the above table. V107: This SX Phe variable was observed by both Mazur et al. (2003) and Arellano Ferro et al. (2014) and appeared to be a cluster member, based on its apparent brightness. However, according to the membership study of Bustos Fierro & Calderon (2018), based on GaiaDR2 photometry, V107 is not a cluster member. V113: LS03 indicated (in their Table 7) that this variable (their #2) might be a field star. However, according to the membership study of Bustos Fierro & Calderon (2018), based on GaiaDR2 photometry, V113 is a cluster member. It is located near the red giant tip in the CM diagram published by LS03. V119: The data are from Kaluzny et al. (2016) V120-121: The data are from Arellano Ferro et al. (2014) who assumed that both were cluster members. However, according to the membership study of Bustos Fierro & Calderon (2018), based on GaiaDR2 photometry, V121 is a not cluster member. V122: Arellano Ferro et al. (2014) concluded that this SX Phe variable was probably a background object because it was much too faint for its period. However, according to the membership study of Bustos Fierro & Calderon (2018), based on GaiaDR2 photometry, V122 is a cluster member. V126, V129, V141: Kaluzny et al. (2016) classified all of these variables as cluster members, based on proper motion. However, according to the membership study of Bustos Fierro & Calderon (2018), based on GaiaDR2 astrometry, none of them are cluster members. V144: Kaluzny et al. (2016) noted that the variable status of this star needs additional confirmation. V145: Kaluzny et al. (2016) noted that since this star is a blend, it might not be variable. ============================================================== Discovery of the variable stars in NGC 3201: V1-56 Woods (1919) with x,y coordinates V57-61 Bailey (1922) with x,y coordinates V62-86 = HV 10328-10352 Dowse (1940) with x,y coordinates and the corresponding HV numbers V87 Wright (1941) with x, y coordinates and a corrected y value for V80 ID charts for V1-87 were later published by Fourcade et al. (1966). However, in her 3rd catalogue, Sawyer Hogg (1973) reported that Kukarkin had informed her that the Fourcade et al. identifications for V6, V11, V45, V52, V57, V68 and V81 were all erroneous. Later, Samus et al. (1996) found that V39 and V50 were also erroneously labelled. Arellano Ferro et al. (2014) published an ID chart for all of the variables that were in their field. V88-96 = Nr. 1-9 Wilkens (1965) with x,y coordinates to a precision of 0.1 arcmin and finder charts: Nrs. 3, 5 & 10 appear on one chart and the other charts are individual. The numbers V88 to 96 were assigned by Sawyer Hogg (1973) who noted that Wilkens' Nr. 10=V39. Kukarkin (1971a) noted that V94 and 95 (Wilkens #7 and 8) were not variable. However, V94 is now known to be a Mira variable in the field around the cluster. V97-100 = Lee 1103, 1405, 2403, 2710 Lee (1977) with ID charts. The numbers V97-100 were assigned in the electronic update to the Sawyer Hogg catalogs (Clement et al. 2001). Lee's ID chart also includes many of the other RR Lyrae variables which are labelled according to his Table 2 numbering system. V101 = V6 of von Braun & Mateo (2002) with ID chart and RA and dec. These authors discovered a total of 14 short period variables in the field of NGC 3201, but their V6 was the only one they considered to be a cluster member. The number V101 was assigned in the electronic update to the Sawyer Hogg catalogs (Clement et al. 2001). According to Kaluzny et al. (2016), proper motion data confirm that von Braun & Mateo's V2 and V4 are not cluster members. V102-112 = Mazur V1-11 Mazur et al. (2003) with RA, dec and finder charts Their paper lists multiple frequencies for some of the stars and they pointed out that some of these may be non-radial modes. For each star, the period listed in the above table is the inverse of the first frequency listed by Mazur et al. (their Table 3). Three of these variables (Mazur V7, 8, 9) were independently discovered by LS03 and are listed as #651, #1019, #752 in their Table 8. There are a number of transcription errors in the L&S paper. Consequently, the stars listed as #651, #1019, #752 in Table 8 are #652, #1020, #753 in their Table 2. A similar problem has occurred with their numbering system for some of the RR Lyrae variables. Layden (2011 - private communication) has indicated that this problem might have occurred because they (LS03) published an incorrect version of Table 2 in their paper. V113-118 = #2, 4, 5, 6, 7, 12 LS03 with X,Y pixel numbers The RA and dec for these stars were derived by Layden (2012, private communication), based on 2MASS identifications. Layden also established that the IDs listed for all of the RGB variables in Table 7 corresponded to the numbers listed in Table 2. The classifications for V113-V118 in the above table were assigned after consulation with Samus (2012, private communication). LS03 detected low level brightness variations in most of the brighter red giants and plotted light curves. (See their Fig. 7 and Table 7). For this catalogue, stars #2, 4, 5, 6, 7, 12 have been selected as the best candidate variables, on the basis of their V amplitudes (A_V>0.02) and their DAOPHOT variability criteria (Lambda>3). L&S star #3 (=V79) is also considered to be variable. L&S star #32 is variable, but L&S considered it to be a field star. With (V-I)= 3.235, it lies about 2 magnitudes redward of the cluster CMD. V119-121 = #565*, 776, 941 LS03 with X,Y pixel numbers *The star listed as #565 in their Table 2 is #564 in Table 8. The RA and dec for these stars were derived by Layden (2012, private communication). V122-124 Arellano Ferro et al. (2014) with RA, dec and an ID chart All of the variables, V1-121, that are included in their field are also labelled on their ID chart. V125-160 Kaluzny et al. (2016) with RA, dec and individual finder charts All of these stars are considered to be cluster members based on proper motion studies. Kaluzny announced an additional 21 variables which they numbered VN1-VN21. None of these were confirmed to be cluster members ------------------ Pietrukowicz et al. (2008) searched for dwarf novae in NGC 3201 and found none. Their search was based on 751 V exposures obtained on 22 nights during the years 2001-2005. They also checked at the location of 4 X-ray sources that were indicated as possible CVs by Webb et al. (2006) and found no brightness variations. ========================================================================== References Arellano Ferro, A., Ahumada, J. A., Calderon, J. H., Kains, N. 2014, Rev. Mex. A&A, 50, 307 (AF) Bailey, S. I. 1922, Harvard Circ., 234, 1 Bustos Fierro, I. H. & Calderon, J. H. 2018, private communication, from a paper presented at Astronomia Dinamica en Latinoamerica VIII, held in Tarija, Bolivia, October 2018 Cacciari, C. 1984, AJ, 89, 231; erratum 1984, AJ 89, 1082 (C84) Carretta, E., Bragaglia, A., D'Orazi, V., Lucatello, S., Gratton. R. 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