47 Tucanae / NGC 104/ C0021-723 (Updated January 2017) RA: 00:24:05.67 DEC: -72:04:52.6 (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 00:24:12.65 -72:06:39.9 R0 221.0 13.15 5.0 V M 2 00:24:18.57 -72:07:59.0 R0 203.0 -- 3.4 V M 3 00:25:15.96 -72:03:54.8 R0 192.0 12.63 4.7 V M 4 00:24:00.53 -72:07:26.9 R0 165.0 12.34 2.3 V M? 5 00:25:03.63 -72:09:31.7 R0 50.0 11.80 0.4 V SR Note 6 00:24:25.68 -72:06:30.0 R0 48.0 11.74 1.0 V SR 7 00:25:20.53 -72:06:40.1 R0 52.0 11.83 0.4 V SR 8 00:24:08.59 -72:03:54.9 R0 155.0 12.01 1.7 V M? 9 00:23:40.53 -72:06:00.0 R0 0.7369 13.672 1.07 V RR0 Note 10 00:24:22.46 -71:53:28.6 R0 ---- 13.35 0.50 P L? Note 11 00:25:09.07 -72:02:16.2 R0 ---- 12.03 0.80 L Note 12 00:28:33.85 -72:10:08.8 R0 0.3714 13.90 0.47 V RR1 f;Note 13 00:22:58.37 -72:06:56.1 R0 40.0 12.36 0.7 V L +long 14 00:24:06.84 -72:03:38.0 R0 ---- -- -- ? Note 15 00:25:43.91 -72:06:50.9 R0 38.0 11.9 0.3 V L Note;Fox 16 00:25:23.18 -72:11:05.3 R0 41.0 11.65 0.2 V L =LW21 17 00:23:55.66 -71:57:28.6 R0 60.0 11.9 0.1 L Note;Fox 18 00:25:09.19 -72:02:39.7 R0 83.0 11.67 0.5 V L Note 19 00:24:14.75 -72:04:44.5 R0 83.0 11.46 0.8 V L f?;Note 20 00:24:14.47 -72:05:09.2 R0 ---- 12.30 0.8 V L P=232? 21 00:23:50.38 -72:05:50.5 R0 ---- 12.41 0.7 V L P=76?+long 22 00:24:10.02 -72:02:38.2 R0 62.0 11.80 0.25 V L 23 00:24:29.53 -72:09:07.8 R0 52.0 11.77 0.4 V L +long 24 00:23:47.61 -72:02:49.8 R0 ---- -- -- CST Note 25 00:23:58.94 -72:02:34.6 R0 44.0 11.96 0.2 V L 26 00:24:07.86 -72:04:31.7 R0 ---- -- -- CST Note 27 00:24:15.14 -72:04:36.5 R0 69.0 12.11 0.75 V L +long 28 00:22:35.81 -72:11:11.2 R0 40.0 11.92 0.4 L Note;Fox 29 00:24:06.37 -72:04:37.0 R0 0.0636 15.98 0.177 U SXPHE 30 00:24:09.07 -72:05:04.9 R0 0.1019 15.78 0.135 U SXPHE 31 00:24:06.53 -72:04:50.0 R0 0.0558 16.13 0.091 U SXPHE 32 00:24:07.82 -72:04:58.1 R0 0.3301 17.523 0.38 V EW PC1V4;W267 33 00:24:10.03 -72:04:51.6 R0 0.2907 16.654 0.034 V EW Note;W257 34 00:24:05.58 -72:04:53.7 R0 0.558 15.91 0.085 U EW? max 35 00:24:05.24 -72:04:51.1 R0 0.4188 18.857 0.30 V EB PC1V7 36 00:24:03.45 -72:05:04.6 R0 0.5305 18.383 0.24 V EB PC1V8;W47 37 00:24:03.26 -72:04:26.7 R0 1.50 17.93 0.419 U EB max 38 00:24:07.94 -72:05:01.6 R0 0.4309 16.761 0.22 V EB PC1V10;W266 39 00:24:04.95 -72:04:55.1 R0 1.108 17.391 0.234 V E/CV Note;W36 40 00:24:06.45 -72:04:45.2 R0 ---- 15.62 1.10 I ? Note;PC1V12 41 00:24:01.38 -72:04:47.7 R0 0.97 17.91 1.65 U EA? max 42 00:22:00.87 -72:02:04.3 R0 0.2737 17.96 0.38 V EW max 43 00:25:00.29 -72:00:02.4 R0 0.3135 17.78 0.44 V EW max 44 00:25:32.21 -72:01:51.4 R0 0.2346 19.47 0.53 V EW max 45 00:26:10.47 -72:11:08.2 R0 0.3788 16.49 0.28 V EW max 46 00:26:08.85 -72:07:01.7 R0 1.1504 15.90 0.40 V E max 47 00:25:15.93 -71:56:06.6 R0 0.2506 18.46 0.34 V EW max 48 00:24:43.95 -71:47:38.3 R0 4.3158 19.93 0.72 V EA max;f 49 00:23:15.75 -72:18:54.0 R0 0.3837 16.16 0.22 V EW max 50 00:22:47.46 -72:13:17.1 R0 0.2789 15.459 0.424 V EW f;Note 51 00:24:58.16 -72:22:11.4 R0 0.3226 17.33 0.33 V EW max 52 00:25:11.14 -72:12:14.6 R0 0.3514 16.34 0.22 V E max 53 00:26:43.03 -72:15:20.7 R0 0.4462 16.77 0.35 V E max 54 00:24:06.01 -72:04:53.4 R0 0.0468 16.59 0.020 U SXPHE 55 00:24:08.08 -72:05:14.0 R0 0.0332 15.71 0.028 U SXPHE 56 00:24:05.69 -72:05:15.6 R0 0.0356 16.03 0.022 U SXPHE Par-V1 00:24:04.29 -72:04:57.7 R0 0.146 19.88 -- V E/CV? Note;W42 Par-V2 00:24:06.02 -72:04:55.9 R0 ---- 20.44 -- V CV Note;W30 Sha-V3 00:24:06.40 -72:04:43.0 R0 0.160 23.11 -- V E/CV? Note;W27 PC1-V17 00:24:09.25 -72:05:04.5 R0 1.128 18.994 0.26 V EA W12 PC1-V18 00:24:07.08 -72:05:04.1 R0 0.2956 17.596 0.04 V EW W273 PC1-V19 00:24:04.05 -72:05:01.2 R0 0.4145 20.137 0.30 V E W41 PC1-V20 00:24:06.38 -72:04:49.3 R0 0.2114 22.805 0.35 V EW PC1-V21 00:24:05.31 -72:04:56.2 R0 0.3916 21.143 -- V E W287? PC1-V22 00:24:04.76 -72:04:56.0 R0 2.50 17.839 0.024 V BY PC1-V23 00:24:06.06 -72:04:52.7 R0 4.36 16.985 0.060 V BY W75 PC1-V24 00:24:06.94 -72:04:57.4 R0 2.43 17.363 0.048 V BY W73 PC1-V25 00:24:06.55 -72:04:55.9 R0 1.03 20.849 0.044 V BY PC1-V26 00:24:06.47 -72:04:46.0 R0 2.43 17.653 0.010 V BY PC1-V27 00:24:08.48 -72:05:00.4 R0 4.03 18.121 0.018 V BY PC1-V28 00:24:04.61 -72:04:59.5 R0 1.16 20.135 0.072 V BY PC1-V29 00:24:07.87 -72:05:13.2 R0 0.528 21.136 0.076 V BY W18 PC1-V30 00:24:03.85 -72:05:12.3 R0 0.798 19.279 0.030 V BY W299 PC1-V31 00:24:06.88 -72:04:48.8 R0 4.35 19.334 0.048 V BY PC1-V32 00:24:05.40 -72:04:52.3 R0 1.64 18.858 0.016 V BY W286 PC1-V33 00:24:06.65 -72:04:44.4 R0 1.74 19.075 0.022 V BY PC1-V34 00:24:06.90 -72:04:52.7 R0 1.38 20.382 0.034 V BY W274 PC1-V35 00:24:06.72 -72:04:42.0 R0 4.86 17.695 0.008 V BY PC1-V36 00:24:06.22 -72:04:52.2 R0 0.7958 17.69 0.025 V Ell Note PC1-V37 00:24:04.25 -72:04:56.9 R0 4.86 19.283 0.020 V BY PC1-V38 00:24:05.90 -72:04:57.1 R0 6.89 19.285 0.014 V BY PC1-V39 00:24:04.97 -72:05:00.6 R0 4.73 18.435 0.010 V BY PC1-V40 00:24:05.63 -72:04:53.5 R0 4.47 18.569 0.010 V BY PC1-V41 00:24:08.47 -72:05:07.4 R0 5.02 17.625 0.004 V BY W14 PC1-V42 00:24:01.71 -72:05:01.6 R0 0.521 21.170 0.030 V BY W304 PC1-V43 00:24:06.57 -72:04:44.1 R0 5.16 18.933 0.006 V BY PC1-V46 00:24:05.78 -72:04:49.1 R0 0.2656 17.785 -- V CST Note PC1-V47 =Par-V1 PC1-V48 00:24:10.17 -72:04:59.8 R0 6.71 17.386 0.010 V E W72;Note PC1-V49 00:24:08.40 -72:05:11.3 R0 7.51 12.152 -- V SR? PC1-V50 00:24:10.51 -72:05:02.3 R0 7.20 12.108 -- V SR? PC1-V52 00:24:05.97 -72:04:46.0 R0 ---- 18.514 -- V CST? Note PC1-V53 =Par-V2 WF2-V01 00:24:05.89 -72:04:24.8 R0 10.15 20.553 0.14 V EA WF2-V02 00:24:04.84 -72:04:04.3 R0 3.97 22.137 0.40 V EA W289 WF2-V03 00:24:15.43 -72:04:41.2 R0 1.340 16.194 0.17 V EA W92 WF2-V04 00:24:09.57 -72:03:47.6 R0 0.2234 19.250 0.24 V EW W258 WF2-V05 00:24:10.66 -72:03:52.6 R0 0.2021 20.184 0.28 V EW WF2-V06 00:24:06.07 -72:04:16.8 R0 0.3747 20.001 0.34 V E W280 WF2-V07 -- -- ---- -- -- =V33 WF2-V08 00:24:15.12 -72:03:36.6 R0 0.4003 21.43 0.04 V E E2003 WF2-V09 00:24:16.72 -72:04:27.1 R0 0.2410 20.137 0.13 V E W1;Note WF2-V10 00:24:15.57 -72:04:33.3 R0 9.18 17.487 0.018 V BY WF2-V11 00:24:13.78 -72:04:02.8 R0 0.843 20.025 0.148 V BY W242 WF2-V12 00:24:13.25 -72:04:47.2 R0 1.18 19.437 0.122 V BY W244 WF2-V13 00:24:13.29 -72:04:36.2 R0 5.93 18.066 0.010 V BY WF2-V14 00:24:08.14 -72:04:26.2 R0 4.14 17.986 0.008 V BY WF2-V15 00:24:10.81 -72:04:43.9 R0 1.29 18.192 0.014 V BY W251 WF2-V16 00:24:14.96 -72:03:32.0 R0 1.74 21.491 0.074 V BY WF2-V17 00:24:06.20 -72:04:30.2 R0 0.633 17.338 0.006 V BY W76 WF2-V18 00:24:12.38 -72:04:22.2 R0 3.06 18.312 0.028 V BY W69 WF2-V19 00:24:07.05 -72:04:14.3 R0 1.56 21.188 0.066 V BY WF2-V20 00:24:04.51 -72:03:56.5 R0 2.58 20.886 0.098 V BY WF2-V21 00:24:09.77 -72:04:26.2 R0 1.50 20.800 0.046 V BY W256 WF2-V22 00:24:06.89 -72:04:20.2 R0 0.549 20.713 0.108 V BY W275 WF2-V23 00:24:12.28 -72:04:11.6 R0 7.20 18.894 0.016 V BY WF2-V24 00:24:15.10 -72:04:23.0 R0 6.39 17.966 0.012 V BY WF2-V25 00:24:04.87 -72:04:24.9 R0 6.62 17.712 0.008 V BY WF2-V26 00:24:22.44 -72:04:05.3 R0 5.70 20.312 0.014 V BY WF2-V27 00:24:05.70 -72:04:18.7 R0 2.47 18.024 0.006 V BY WF2-V28 00:24:14.59 -72:04:05.4 R0 6.39 19.265 0.008 V BY WF2-V29 00:24:11.12 -72:04:40.1 R0 3.76 17.547 0.004 V BY WF2-V30 00:24:14.84 -72:03:44.8 R0 2.359 21.36 0.03 V E E2003 WF2-V31 00:24:14.91 -72:04:43.5 R0 5.34 17.576 0.146 V E W3;Note WF2-V32 00:24:13.54 -72:03:34.5 R0 9.2 17.141 0.022 V E Note;W243 WF2-V33 00:24:03.48 -72:04:18.0 R0 6.36 12.341 -- V SR? WF2-V34 00:24:08.18 -72:04:35.8 R0 5.50 12.266 -- V SR? WF2-V35 00:24:14.40 -72:04:27.3 R0 5.70 12.238 -- V SR? WF2-V36 00:24:01.62 -72:04:04.3 R0 2.85 12.789 -- V SR? WF2-V37 00:24:13.00 -72:03:55.6 R0 6.50 12.245 -- V SR? WF2-V38 00:24:14.51 -72:04:44.3 R0 9.0 11.214 -- V SR? WF2-V39 00:24:12.57 -72:03:38.4 R0 6.1 12.432 -- V SR? WF2-V40 00:24:01.62 -72:04:09.2 R0 9.0 12.011 -- V SR? WF2-V41 00:24:07.53 -72:04:23.2 R0 6.6 12.195 -- V SR? WF2-V42 00:24:11.38 -72:03:25.2 R0 ---- 11.868 -- V SR? P>10 WF2-V43 00:24:10.35 -72:04:40.8 R0 5.9 12.558 -- V SR? WF2-V44 00:24:17.00 -72:04:30.1 R0 ---- 12.175 0.02 V SR? P>10 WF2-V45 00:24:06.50 -72:04:25.9 R0 5.0 12.264 -- V SR? WF2-V46 00:24:13.52 -72:04:28.4 R0 3.5 12.648 -- V SR? WF2-V47 00:24:08.21 -72:04:27.2 R0 ---- 17.750 0.15 V E WF2-V48 00:24:15.63 -72:04:36.3 R0 ---- 21.677 -- V CST? Note WF3-V01 00:24:19.17 -72:04:31.3 R0 0.4174 19.985 0.52 V EA W182 WF3-V02 00:24:30.43 -72:04:46.8 R0 2.31 21.297 0.09 V EA W211 WF3-V03 00:24:15.02 -72:04:56.6 R0 0.3311 17.532 0.56 V EW W238 WF3-V04 00:24:18.36 -72:04:55.2 R0 0.2516 18.852 0.53 V EW W228 WF3-V05 00:24:24.93 -72:05:07.2 R0 0.3450 17.040 0.07 V EW W163 WF3-V06 00:24:25.46 -72:04:38.2 R0 0.2318 22.90 0.01 V E E2003 WF3-V07 00:24:14.29 -72:04:54.7 R0 0.316 19.63 0.01 V E E2003 WF3-V08 00:24:15.73 -72:04:51.7 R0 0.2108 20.832 -- V E W66 WF3-V09 00:24:11.97 -72:05:00.1 R0 0.3311 19.022 -- V E WF3-V10 00:24:13.32 -72:05:06.9 R0 0.3325 17.120 -- V Ell? WF3-V11 00:24:14.44 -72:05:05.3 R0 7.20 17.468 0.006 V BY WF3-V12 00:24:16.48 -72:04:47.0 R0 1.78 17.479 0.012 V BY W233 WF3-V13 00:24:22.85 -72:05:31.8 R0 1.99 17.582 0.006 V BY WF3-V14 00:24:21.02 -72:05:02.8 R0 5.16 19.669 0.056 V BY W222 WF3-V15 00:24:24.37 -72:05:00.3 R0 0.437 20.294 0.046 V BY W216 WF3-V16 00:24:14.79 -72:05:03.0 R0 2.50 19.257 0.020 V BY W239 WF3-V17 00:24:21.77 -72:04:25.5 R0 7.89 19.875 0.022 V BY WF3-V18 00:24:26.83 -72:05:25.7 R0 5.70 19.728 0.016 V BY WF3-V19 00:24:28.68 -72:05:00.6 R0 1.88 22.996 0.082 V BY WF3-V20 00:24:19.81 -72:05:25.5 R0 7.57 21.514 0.026 V BY WF3-V21 00:24:18.58 -72:05:04.4 R0 4.03 21.420 0.030 V BY WF3-V22 00:24:15.07 -72:04:49.7 R0 0.893 20.764 0.020 V BY W237 WF3-V23 00:24:16.03 -72:04:59.3 R0 9.75 17.501 0.002 V BY WF3-V24 00:24:24.55 -72:04:53.9 R0 7.89 22.160 0.040 V BY WF3-V25 00:24:28.59 -72:04:42.5 R0 6.1 12.132 0.02 V SR? WF3-V26 -- -- ---- -- -- =LW16 WF3-V27 00:24:19.05 -72:05:19.0 R0 7.5 11.962 -- V SR? WF4-V01 00:24:04.71 -72:06:08.6 R0 8.87 19.276 0.44 V EA WF4-V02 00:24:11.87 -72:05:07.7 R0 4.19 20.384 1.15 V EA W93 WF4-V03 00:24:18.47 -72:06:02.9 R0 0.5875 19.147 0.18 V EA W137 WF4-V04 00:24:08.30 -72:05:35.0 R0 4.92 17.129 0.17 V EA W262 WF4-V05 00:24:14.62 -72:05:40.4 R0 0.259 18.67 0.08 V E E2003 WF4-V06 00:24:10.26 -72:05:06.5 R0 6.13 17.120 0.062 V BY W9 WF4-V07 00:24:12.29 -72:05:21.8 R0 1.44 19.894 0.052 V BY W246 WF4-V08 00:24:07.28 -72:06:19.9 R0 2.04 20.670 0.026 V BY W271 WF4-V09 00:24:07.40 -72:05:53.7 R0 1.37 20.743 0.038 V BY WF4-V10 00:24:06.38 -72:05:42.0 R0 2.62 19.767 0.014 V BY W278 WF4-V11 00:24:14.97 -72:05:29.0 R0 8.72 20.604 0.032 V BY WF4-V12 00:24:04.50 -72:05:37.3 R0 6.13 17.624 0.008 V BY WF4-V13 00:24:13.05 -72:06:04.1 R0 9.18 20.911 0.026 V BY WF4-V14 00:24:09.51 -72:06:00.8 R0 4.35 18.180 0.008 V BY WF4-V15 00:24:08.10 -72:06:21.5 R0 0.903 21.813 0.056 V BY WF4-V16 00:24:04.60 -72:06:06.0 R0 ---- 24.070 -- V CST? Note WF4-V17 00:24:11.55 -72:06:31.7 R0 4.86 17.567 0.006 V E Note WF4-V18 00:24:11.74 -72:05:12.4 R0 5.90 17.277 0.040 V E Note;W248 WF4-V19 00:24:07.55 -72:05:20.1 R0 5.9 14.465 0.02 V L? Note WF4-V20 00:24:10.98 -72:05:08.8 R0 ---- 15.219 0.02 V L? Note;P>10 WF4-V21 00:24:09.98 -72:05:34.0 R0 7.0 12.383 -- V SR? WF4-V22 00:24:20.01 -72:05:51.8 R0 5.0 12.477 -- V SR? WF4-V23 00:24:06.60 -72:06:15.5 R0 3.9 12.530 -- V SR? WF4-V24 00:24:11.03 -72:05:35.6 R0 9.0 12.741 -- V SR? WF4-V25 00:24:20.23 -72:05:58.5 R0 ---- 12.387 -- V SR? P>10 WF4-V26 00:24:14.50 -72:05:59.2 R0 ---- 17.694 -- V ? Note W2_opt 00:24:15.63 -72:04:36.3 R0 0.262 21.50 0.55 V E/CV? Note W8_opt 00:24:10.50 -72:04:25.6 R0 0.1193 21.72 0.5 V E/CV? Note W11_opt 00:24:09.83 -72:03:59.7 R0 0.432 20.91 0.008 V E MSP;Note W15_opt 00:24:08.19 -72:05:00.2 R0 0.1764 22.47 0.75 V E/CV? Note W21_opt 00:24:07.50 -72:05:27.2 R0 0.0723 20.89 0.58 V E/CV? Note W22_opt 00:24:07.50 -72:05:24.3 R0 2.4494 18.08 -- V E W23_opt 00:24:07.53 -72:04:41.5 R0 0.2574 18.08 -- V E W25_opt 00:24:06.86 -72:05:45.7 R0 ---- 21.32 -- V CV? W26_opt 00:24:06.57 -72:05:12.3 R0 0.3939 22.29 -- V E W29_opt 00:24:06.07 -72:04:49.0 R0 0.1329 22.3 1.9 V E MSP;Note W33_opt 00:24:05.14 -72:04:21.5 R0 ---- 21.40 --- V CV? W34_opt 00:24:05.21 -72:04:46.6 R0 0.0677 22.75 0.7 V E MSP?;CV? W36_opt =V39/AKO9 W38_opt 00:24:04.64 -72:04:46.0 R0 1.866 17.2l -- V E W43_opt 00:24:04.20 -72:04:43.6 R0 ---- 17.10 -- V E W44_opt 00:24:03.41 -72:04:58.9 R0 ---- 23.20 -- V CV? W45_opt 00:24:03.52 -72:04:22.9 R0 0.1561 21.91 -- V E/CV? Note W49_opt 00:24:03.07 -72:04:47.5 R0 ---- -- -- V CV? V>22.02 W51_opt 00:24:02.79 -72:04:49.3 R0 ---- -- -- V CV? V>21.69 W53_opt 00:24:02.48 -72:05:11.5 R0 ---- -- -- V CV? V>21.68 W56_opt 00:24:02.06 -72:05:42.3 R0 ---- 23.32 -- V CV? W58_opt 00:24:00.90 -72:04:53.4 R0 ---- 21.90 -- V qLMXB Note W59_opt 00:24:00.34 -72:05:54.2 R0 0.2430 20.08 -- V E W64_opt 00:23:57.62 -72:05:02.1 R0 ---- 21.48 -- V E W68_opt 00:24:13.24 -72:05:23.4 R0 1.118 18.16 -- V W70_opt 00:24:11.63 -72:04:22.2 R0 ---- 23.30 -- V CV? W71_opt 00:24:10.38 -72:05:17.2 R0 0.0988 20.88 0.19 V E/CV? E2003 W82_opt 00:24:01.37 -72:04:42.0 R0 ---- -- -- V CV? V>21.47 W85_opt 00:23:59.34 -72:04:38.7 R0 ---- 19.48 -- V CV? W94_opt 00:24:11.52 -72:05:14.5 R0 0.2726 21.67 -- V E W120_opt 00:24:10.81 -72:06:19.9 R0 0.110 22.74 0.1 V E/CV? Note W121_opt 00:24:04.91 -72:06:04.3 R0 0.1578 21.78 -- V E W122_opt 00:24:03.78 -72:06:21.9 R0 ---- 20.71 -- V CV? W167_opt 00:24:09.97 -72:04:01.5 R0 0.3721 16.62 -- V E W184_opt 00:24:10.31 -72:05:29.1 R0 0.7722 19.70 -- V E A19 00:24:21.80 -72:04:13 R0 60.0 12.18 0.7 V L LW1 00:23:22.30 -72:05:40 R0 39.0 11.83 0.2 V L LW2 00:23:29.20 -72:06:20 R0 60.0 11.90 0.3 V L +long LW3 00:23:47.40 -72:06:53 R0 107.0 11.92 0.35 V L LW4 00:23:51.30 -72:03:49 R0 32.0 11.80 0.2 V L +long LW5 00:23:53.20 -72:04:16 R0 40.0 11.74 0.25 V L LW6 00:23:54.70 -72:03:39 R0 41.0 11.85 0.1 V L LW7 00:23:56.90 -72:05:33 R0 42.0 11.66 0.3 V L LW8 00:23:57.70 -72:05:30 R0 ---- 11.82 0.3 V L P=27?+long LW9 00:23:58.20 -72:05:49 R0 74.0 12.34 1.1 V L LW10 00:24:02.60 -72:05:07 R0 ---- 12.22 1.2 V L P=110? LW11 00:24:03.20 -72:04:51 R0 ---- 11.95 0.1 V L P=36? LW12 00:24:04.00 -72:05:10 R0 61.0 11.96 0.6 V L altP=116 LW13 00:24:07.9 -72:04:32 R0 ---- 12.56 0.3 V L Note;P=65? LW14 00:24:09.4 -72:04:49 R0 50.0 11.71 1.1 V L Note LW15 00:24:11.20 -72:05:09 R0 46.0 11.76 0.3 V L +long LW16 00:24:13.60 -72:04:52 R0 29.0 11.88 0.15 V L +long LW17 00:24:16.30 -72:01:31 R0 41.0 11.81 0.1 V L LW18 00:24:20.50 -72:04:50 R0 65.0 11.91 0.3 V L +long LW19 00:24:23.20 -72:04:23 R0 40.0 11.85 0.15 V L +long LW20 00:24:52.10 -71:56:11 R0 49.0 11.85 0.3 V L LW21 -- -- ---- -- -- =V16 LW22 00:25:30.10 -72:04:32 R0 63.0 12.06 0.8 V L +long Wel9 00:25:34.10 -72:09:58.2 R0 ---- 16.13 0.1 V L? Note;P>20 Wel15 00:25:06.18 -72:10:23.5 R0 ---- 15.36 0.39 V L? Note;P>30 Wel16 00:24:31.77 -72:09:29.5 R0 3.4629 16.72 0.18 V L? Note Wel21 00:29:09.42 -71:51:26.4 R0 0.2812 18.88 0.75 V E Wel25 00:27:56.58 -71:57:26.7 R0 5.8524 16.72 0.97 V L? Note Wel28 00:26:02.92 -72:03:02.9 R0 4.159 15.00 0.13 V L? Note Wel31 00:24:42.54 -71:59:23.9 R0 10.21 16.23 0.18 V L? Note Wel69 00:22:52.95 -72:03:40.7 R0 29.5398 16.799 0.616 V EA max;Note Wel78 00:28:21.06 -71:43:40.7 R0 ---- 19.31 0.2 V E Wel93 00:21:07.60 -72:08:55.8 R0 ---- 19.71 0.2 V E Wel96 00:22:40.87 -72:09:22.5 R0 8.235 16.56 0.07 V L? KalW1 00:24:10.23 -72:04:01.5 R0 0.3612 15.607 0.163 V EW max KalW2 00:23:39.68 -72:01:40.4 R0 0.2829 17.565 0.317 V EW max KalW4 00:23:05.00 -72:05:22.5 R0 0.3530 15.838 0.163 V EW max KalW5 00:23:59.29 -72:06:48.6 R0 0.2804 17.143 0.225 V EW max KalW7 00:23:49.34 -72:13:08.1 R0 3.8826 19.091 0.384 V EA max KalW8 00:22:47.96 -71:56:49.1 R0 12.7823 14.150 0.032 V RSCVn max KalW12 00:22:55.55 -72:05:15.2 R0 3.7320 17.462 0.411 V EA max KalW14 00:22:36.78 -72:07:11.9 R0 0.0460 14.679 0.037 V SX max KalE1 00:27:00.02 -71:55:09.0 R0 0.3475 17.025 0.485 V EW max;Wel26 KalE8 00:26:02.73 -71:58:21.9 R0 6.3715 14.141 0.152 V RSCVn max KalE19 00:25:38.37 -72:14:08.6 R0 ---- 14.344 0.194 V L max KalE23 00:24:49.31 -71:56:19.9 R0 0.2417 18.551 0.337 V EW max;Wel34 KalE25 00:24:42.54 -72:06:21.6 R0 3.3359 17.849 0.143 V ? max KalE31 00:24:13.55 -71:58:02.5 R0 20.4363 16.564 0.457 V RSCVn max KalE32 00:24:37.52 -72:03:53.1 R0 ---- 17.109 0.362 V EA max KalE33 00:24:18.73 -72:04:54.9 R0 0.2515 16.391 0.107 V Ell? max KalE34 00:24:25.84 -72:07:03.5 R0 9.8738 15.495 0.294 V L? max;Note KalE35 00:24:23.46 -72:08:29.6 R0 0.3004 18.021 0.345 V EW max;Wel17 KalE36 00:24:23.22 -72:07:22.7 R0 0.2799 18.053 0.641 V EW max KalE39 00:24:25.32 -72:13:38.4 R0 0.9875 18.792 0.507 V EA max EM1 00:24:03.07 -72:04:55.0 R0 20.28 10.26 0.05 I SR EM2 00:24:06.27 -72:04:45.4 R0 31.50 9.98 0.08 I SR EM3 00:24:08.31 -72:04:50.7 R0 33.41 10.07 0.05 I SR EM4 00:24:07.20 -72:04:46.5 R0 68.07 13.89 0.14 I SR EM5 00:24:05.09 -72:04:54.4 R0 ---- 10.34 0.06 I L EM6 00:24:02.73 -72:05:02.8 R0 ---- 10.60 0.07 I L EM7 00:24:07.89 -72:05:02.0 R0 ---- -- -- ? PSR (26) -- -- ---- -- -- PSR Note ==================================================================== Supplementary Notes The data for the stars listed in the above table are based mainly on the following sources. Exceptions are indicated in the Notes on individual stars. V1-28: The RA and dec are from Samus et al. (2009). For the stars classified as M, SR or L, the periods, mean magnitudes and classifications are from Lebzelter et al. (2005) or from Lebzelter & Wood (2005) and the V amplitudes were derived from their published light curves, unless indicated otherwise in the notes on individual stars. "Fox" in the remarks column indicates the the period is from Fox (1982). "+long" in the remarks column indicates that a longer period is superimposed on the published period. The source for the remaining stars (classified as RR, CST or ?) are indicated in the Notes on individual stars. V29-41 (= Edmonds et al. V1-13): The RA and dec are from Samus et al. (2009) The periods and magnitudes are from Edmonds et al. (1996) unless indicated otherwise in the notes on individual stars. A few of these stars (V32=PC1-V04, V35=PC1-V07, V36=PC1-V08, V38=PC1-V10, V39=PC1-V11, and V40=PC1-V12) were later investigated by Albrow et al. (2001). For these stars, the period, mean magnitude and amplitude are from Albrow et al. (2001) or from the sources indicated in Notes on individual stars. The RA values derived by Albrow et al. (2001) for these stars have a systematic shift relative to the values of Samus et al. (2009) which were based on Geffert et al. (1997). The Samus/Geffert values are larger on average by 0.29 sec than those derived by Albrow et al. This is equivalent to about 1.3 arcseconds. V42-53: The RA and dec are from Samus et al. (2009). The periods and magnitudes are from Kaluzny et al. (1998) unless indicated otherwise in the notes on individual stars. V54-56: The RA and dec are from Samus et al. (2009). The remaining data are from the discovery paper by Gilliland et al. (1998) ------------ The variables following V56 have been assigned numbers that have been designated according to their discovery papers. "Par" and "Sha" refer to variables announced by Paresce et al. (1992, 1994) and by Shara et al. (1996). These stars are discussed further in the notes on individual stars. "PC1, WF2, WF3, WF4" designate the variables discovered by Albrow et al. (2001) when they used the HST to search for Jupiter-sized planetary transits. The "W" numbers in the remarks column refer to the Chandra X-ray sources for which the variable star is the optical counterpart according to Edmonds et al. (2003a) or Heinke et al. (2005). The W numbers were assigned to Chandra X-ray sources in 47 Tuc by Grindlay et al. (2001) and authors of subsequent studies followed their numbering system. The data for these variables are from the discovery paper of Albrow et al. (2001) unless indicated otherwise in the Notes/Remarks column. E2003 in the Remarks column indicates that the data are from Edmonds et al. (2003a,b). "W#_opt" refers to variables discovered by Edmonds et al. (2001, 2002, 2003a,b) when they used the HST images of Albrow et al. (2001) to search for optical counterparts to Chandra X-ray sources. The data for these stars are from the discovery papers by Edmonds and collaborators. "LW" refers to long period variables discovered by Lebzelter & Wood (2005). The data for A19 and the LW stars are from Lebzelter & Wood (2005) or from Lebzelter et al. (2005). "+long" in the remarks column for LW variables indicates that a longer period is superimposed on the published period. "Wel" refers to variables discovered by Weldrake et al. (2004) in their search for planetary transits. All the data are from their discovery paper unless indicated otherwise in the notes on individual stars. "KalW" and "KalE" refer to the west and east fields observed by Kaluzny et al. (2013) in their search for eclipsing binaries. All the data are from their discovery paper unless indicated otherwise in the Notes on individual stars. "EM" refers to the variables discovered by Figuera Jaimes et al. (2016) based on their observations made with an electron-multiplying (EM) CCD. All the data are from their discovery paper unless indicated otherwise in the Notes on individual stars. ---------------------------------- Cataclysmic variables A number of variables have been classified as candidate CVs in investigations of 47 Tuc. This was based on their location in the CM diagram, their spectroscopic properties and the fact that they are optical counterparts of X-ray sources. Two of these stars (V39 and Par-V2) are confirmed CVs because they have exhibited eruptions on more than one occasion (see the Notes below). In the above table, the remaining CV candidates are designated "CV?" or "E/CV?" if a binary period has been derived. Michael Shara and his collaborators (2017, private communiction) have continued to monitor 47 Tuc with HST observations (~50 times since 1996) and plan to report their latest results in 2017. -------------------------------------------- According to the 2010 update to the Harris (1996) catalogue, 47 Tucanae has a tidal radius of approximately 42 arcminutes. However, 47 Tuc is located close to the SMC in the sky and as a result, at distances greater than 20 arcminutes from the cluster centre, there is significant contamination from the SMC and the Milky Way. This is illustrated in a paper by Cioni et al. (2016 -see Fig.3). Variables that are clearly known to be field stars are designated "f" in the above table. However, for some stars, the membership status may be ambiguous. =================================================================== Notes on individual stars V5: The period and V magnitude for V5 are from Lebzelter & Wood (2005). No amplitude is available from their study because Lebzelter et al. (2005) did not have sufficient usable data to plot a light curve. V5 was located on a bad area of their CCD. The V amplitude for V5 is from Lloyd Evans (1974) and is in good agreement with the value published by Arp et al. (1963). V9: The period, magnitude and amplitude are from Carney et al. (1993) who established that the RR Lyrae star V9 is a cluster member, based on radial velocity measurements. This result was later confirmed by Storm et al. (1994) who made more extensive observations. V10: The photographic magnitude and amplitude listed for V10 are the values reported by McKibben-Nail (1951). Payne-Gaposchkin & Gaposchkin (1966) later classified the star as an irregular variable, based on the original data. V10 was labelled on a chart by Fourcade et al. (1966) and in the SMC Atlas (Hodge & Wright 1977 - see chart 20B) but it has not been analysed in any subsequent investigations. V11, V18: These two variable stars are separated by about 23 arcsec in declination and are both close to the published x,y position for HV 813. It is now accepted that the position of V11 coincides with Wildey's (1961) star #12 and that V18, star L168 of Lloyd Evans & Menzies (1973), was a more recently discovered variable. Lloyd Evans (1974) gave some background information about this in a note to Table II in his paper. The data for these stars are from Lebzelter & Wood (2005). For V11, Lebzelter & Wood (2005) listed a period of 160 days, but noted that the current periodicity is uncertain. V12: The period, magnitude and amplitude are from Feast et al. (1960). Its non-membership status was established by Carney et al. (1993), based on radial velocity measurements. The star is listed in the GCVS as CO Tuc. V14: This variable, which was announced by Fourcade et al. (1966), has not been included in any subsequent study. V15, V17, V28: These variables were not listed by Lebzelter & Wood (2005). Their periods were derived by Fox (1982). The V magnitudes and amplitudes for V15 (Wildey #300) and V28 (LR5) are from Lloyd Evans (1974). The V magnitude for V17 (Wildey #81) is from Eggen (1972) and the amplitude is from Lloyd Evans & Menzies (1973). V16 = LW21 These two variables appear to be the same star according to the RA and dec listed by Lebzelter & Wood (2005) and both have irregular light curves that indicate an approximate periodicity of around 40 days. The reason their light curves differ is because the data for V16 were obtained at CTIO between August 2003 and January 2004, while the LW21 data were obtained at Mount Stromlo from August 2002 until the telescope was destroyed by fire in early 2003. V19: Lebzelter & Wood (2005) noted that this might be a star in the Galactic halo because it is brighter and bluer than the other long period variables. Another possibility is that it has a bright blue neighbour that was not resolved in their images. V24, V26: V24=A8 and V26=A13 were listed as red variables by Lloyd Evans & Menzies (1973). However, Lloyd Evans (1974) did not detect any significant variations in A8 (V24) and pointed out that A13 (V26) was severely crowded. Variability was not detected in either of these stars in subsequent studies (e.g. Fox 1982 or Lebzelter & Wood (2005). Therefore they are no longer considered to be variables. V33 = V5 of Edmonds et al. (1996) = WF2-V07 of Albrow et al. (2001): This variable was discovered by Edmonds et al. (1996) and the number V33 was assigned Clement et al. (2001). Since it is the same star as WF2-V07, the period, magnitude and amplitude listed above are the values listed by Albrow et al. (2001) for WF2-V07. Heinke et al. (2005) determined that this is the optical counterpart of Chandra X-ray source W257. V39 = V11 of Edmonds et al. (1996) = PC1-V11 of Albrow et al. (2001) = AKO9 of Knigge et al. (2002) = W36_opt of Edmonds et al. (2003a,b) The number V39 was assigned by Clement et al. (2001). The RA and dec are from Samus et al. (2009), based on the astrometry of Geffert et al. (1997). Albrow et al. (2001) derived a lower RA (00:24:04.65). The period, mean V magnitude and amplitude in the above table are from Albrow et al. (2001). A slightly longer period, 1.1091 days, was derived by Knigge et al. (2003). Knigge et al. (2008) presented evidence for a dwarf nova eruption in July 2002 and pointed out that eruptions had been observed previously in the 1980s and 1990s. Therefore they classified the star as a confirmed CV. V40 = V12 of Edmonds et al. (1996) = PC1-V12 of Albrow et al. (2001) The number V40 was assigned by Clement et al. (2001). V40 is a blue straggler. Edmonds et al. (1996) had difficulty classifying it and suggested that it might be a low amplitude SX Phe variable in a binary system. The image was saturated in the V band. Albrow et al. (2001) found that its variability amplitude seemed to grow and then decline during the time they observed. Figuera Jaimes et al. (2016) observed this star. They were unable to derive a period, but their light curve indicated several possible eclipses. The data listed above are from Figuera Jaimes et al. (2016). V50 = Wel 95 = OGLE 245 = W18 (of Kaluzny et al. 2013): Liu et al. (2013) analysed the light curves of this star and conluded that it is a foreground object and not part of the cluster. Rucinski (2000) reached the same conclusion. The period, maximum V magnitude and amplitude listed above are from Kaluzny et al. (2013). Par-V1 = PC1-V47: The mean V magnitude is from Edmonds et al. (2003a) who noted that the star exhibited sigmificant non-periodic variability. The period and classification are from Knigge et al. (2008) based on the study by Edmonds et al. (2003b). The RA and dec for Par-V1 are from Geffert et al. (1997). Par-V2 = PC1-V53: This star is a known CV because dwarf nova eruptions were observed by Paresce & De Marchi (1994) and by Shara et al. (1996). Evidence for additional outbursts in 1999 and in 2005 was presented by Knigge et al. (2008). The V magnitude listed in the above table is from Edmonds et al. (2003a). Sha-V3 The RA and dec are the values listed by Grindlay et al. (2001) for the X-ray source W27 for which they assumed that Sha-V3 is the optical counterpart. The V magnitude and period are from Edmonds et al. (2003a), who also published values for the RA and dec in their Tables 3 and Table 4. However, the RA they listed in Table 4 was 0.25 seconds greater that the Table 3 value (a difference that is equivalent to 1.15 arcseconds). Their Table 4 RA is closer to Grindlay's value (a difference of only 0.23 arcseconds). PC1-V36: The period and mean magnitude are from Edmonds et al. (2003a) and the classification is from Knigge et al. (2008) who noted that the star's proper motion indicates that it is a cluster member. PC1-V46, W29_opt: A careful examination of the HST direct images by Edmonds et al. (2002a) showed that PC1-V46 (V=17.79 mag) was not the true variable. The variable is a faint nearby star with V~22.3 mag which they named W29_opt because they concluded that it is the optical counterpart for the Chandra X-ray source W29. They also concluded that this system is associated with the MSP 47 Tuc W because of the agreement between period and phase for the two systems. PC1-V52, WF4-V16: Edmonds et al. (2003a) noted that these two "variables" were possible artifacts. Their apparent variabiity was due to a diffraction spike (V52) or bad pixel (V16). PC1-V48 (W72), WF2-V31 (W3), WF2-V32, WF4-V17, WF4-V18: Albrow et al. (2001) classified these stars as red stragglers (RS). They postulated that they form a distinct class with properties explained by mass transfer, rapid rotation and enhanced activity. Three of these stars (PC1-V48, WF2-V31, WF4-V18) are associated with Chandra X-ray sources (W3, W72, W248 respectively). WF2-V09: This star is W1_opt (Edmonds et al. 2003a,b). The period and V amplitude are from the light curve published by Edmonds et al. (2003b) and the mean V magnitude was published by Edmonds et al. (2003a). WF2-V48, WF4-V26: Albrow listed these as miscellaneous variables and noted that they could be candidate CVs. However, subsequent studies (e.g. by Edmonds and collaborators) have not confirmed this. Furthermore, Albrow et al. noted that WF2-V48 lies on or close to a diffraction spike from a nearby bright star. W2_opt, W120_opt: The period and V amplitude are from Fig. 7 of Edmonds et al. (2003b). The remaining data are from Edmonds et al. (2003a). W8_opt, W15_opt: The V amplitude is from Fig. 2 pf Edmonds et al. (2003b). The remaining data are from Edmonds et al. (2003a).` W11_opt = U_opt of Edmonds et al. (2001). The data listed above are from their paper. W21_opt: The period and V amplitude are from Fig. 3 of Edmonds et al. (2003b). The remaining data are from Edmonds et al. (2003a). W45_opt: The period is the orbital period based on Fig. 5 of Edmonds et al. (2003b) and the V magnitude is from Edmonds et al. (2003a). W58_opt: Edmonds et al. (2003a) pointed out that this variable is the optical counterpart of X5 (=W58) which was classified as a qLMXB by Edmonds et al. (2002b). LW13, LW14 Lebzelter & Wood (2005) indicated that there was some uncertainty in the RA and dec they published for these two variables. Wel9, Wel15, Wel16, Wel25, Wel28, Wel31, Wel96, WF4-V19, WF4-V20, KalE34: Wel9, Wel15, Wel28, Wel31 are OGLEC 222, 219, 229 and 220 respectively, variable K subgiants that Kaluzny et al. (1998) suggested might be cluster members. Weldrake et al. (2004) concluded that three additional variables: Wel16, Wel25 and Wel96 might belong to the same category. In addition, WF4-V19 and WF4-V20 of Albrow et al. (2001) and KalE34 = star E34 of Kaluzny et al. (2013) appear to be variables of the same type. Wel69: The period, V magnitude, V amplitude and classification are from Kaluzny et al. (2013). Thompson et al. (2010) carried out an extensive analysis of Wel69, based on photometric and spectroscopic observations and concluded that this binary system is a cluster member. PSR: According to Paulo Freire's website, there are 26 millisecond pulsars in 47 Tucanae. Two of these have been identified as optical variables: J0024-7203U (W11_opt) and J0024-7204W (W29_opt). ==================================================================== Discovery of the Variable Stars in 47 Tucanae: V1-8 Bailey (1902) with x,y positions (see Table XXIV, p 237) and an ID chart (Plate 252.19) V9-12 = HV 810, HV 811, HV 813, HV 814 McKibben-Nail (1951) with x,y positions The numbers V9-12 were assigned by Sawyer (1955) in her 2nd catalogue. These variables had been discovered earlier by Levitt (1908) in a study of the SMC. There was also a suspected variable HV 812, but McKibben-Nail (1951) considered its variability to be doubtful. Consequently, Sawyer (1955) did not list it in her catalogue. No ID charts were published at the time of discovery. In subsequent studies of 47 Tuc, plates showing these variables were published. V9: An ID chart was published by Feast & Thackeray (1960). V10 = HV 811: This star was labelled in the SMC Atlas (Hodge & Wright 1977 - see chart 20B) V11 = HV 813: This star was labelled as W12 by Lloyd Evans & Menzies (1973) because, in their Table II, they noted that V11 (HV 813) is star #12 labelled by Wildey (1961) V12 = HV 814: HV 814 was labelled in the SMC Atlas (Hodge & Wright 1977 - see chart 20B). It was also labelled as star #7317 by Lee (1977 - see section 4.2 and the southeast segment of Figure 1 in his paper. V9, V10 and V11 were also labelled on an ID chart by Fourcade et al. (1966). V13-14 Fourcade et al. (1966) with x,y coordinates and an ID charts They noted that Wilkens had discovered V13. V15 = Star #300 labelled on an ID chart by Wildey (1961) Arp et al. (1963) demonstrated that Wildey's star #300 was probably variable and Eggen (1972) confirmed it. The number V15 was assigned by Sawyer Hogg (1973). V16 = Star #18 labelled on Plate I of Feast & Thackeray (1960) According to Sawyer Hogg (1973), the variablility of this star was announced by Brooke in a 1969 Doctoral Thesis at the Australian Nat'l Univ (1969). Lloyd Evans & Menzies (1973) pointed out that Brooke's variable is #18 of Feast & Thackeray (1960). Lloyd Evans (1974) labelled it as R18 on Plate II in his paper. The number V16 was assigned by Sawyer Hogg (1973). V17 = Star #81 labelled on an ID chart by Wildey (1961) Eggen (1972) showed that this star was variable. The number V17 was assigned by Sawyer Hogg (1973). V18-28 are red variables announced by Lloyd Evans & Menzies (1973) who labelled most of them on a plate they published. In addition, all but one of these variables were later labelled on a plate by Lloyd Evans (1974) V18 = L168 labelled as V11 in 1973 and L168 in 1974 (Plate II) V19 = R10 identified in 1973 and 1974 (Plate I) V20 = A1 identified in 1973 and 1974 (Plate I) V21 = A2 identified in 1973 and 1974 (Plate I) V22 = A4 identified in 1973 and 1974 (Plate I) V23 = A6 identified in 1974 (Plate II), but not in 1973 V24 = A8 identified in 1973, but not in 1974 V25 = A9 identified in 1973 and 1974 (Plate II) V26 = A13 identified in 1973 and 1974 (Plate I) V27 = A18 identified in 1973 and 1974 (Plate I) V28 = LR5 identified in 1974 (Plate II), but not in 1973 V29-41 = V1-13 Edmonds et al. (1996) who published x,y (arcsec) positions and an ID chart The numbers V29-41 were assigned in this electronic catalogue. Samus et al. (2009) later derived RA and dec (Epoch 2000) Albrow et al. (2001) referred to these stars as PC1-V01 to V13 and published new data for six of them. For these 6 stars, the RA values derived by Albrow et al. have a systematic shift relative to the values of Samus et al. (2009) which were based on Geffert et al. (1997). The Samus values are larger on average by 0.29 sec than those derived by Albrow et al. This is equivalent to about 1.3 arcseconds. V42-53 = OGLEC 214 (Wel61), 221 (Wel 32), 225 (Wel100), 227 (Wel6), OGLEC 228 (Wel7), 238 (Wel30), 240 (Wel85), 244 (Wel56), OGLEC 245 (Wel95), 249 (Wel51), 250 (Wel14), 253 (Wel12) Kaluzny et al. (1998) with 1950 RA and dec and X,Y coordinates in pixels. In their study, they detected 42 new variables, but these 13 were the ones they considered to be cluster members. V42 (OGLEC 214) was announced in an earlier study by Kaluzny et al. (1997) where it was listed as V6. A finder chart was published in the 1997 paper. The numbers V42-53 were assigned in this electronic catalogue and the 2000 RA and dec were later derived by Samus et al. (2009) These 12 variables were all detected later by Weldrake et al. (2004) and the "Wel" numbers listed above refer to their numbering system. Kaluzny et al. (1998) also listed properties for 6 variable K giant stars that might be cluster members: OGLEC 219, OGLEC 220, 222, 229, 231, 237. Variability was detected in four of these stars by Weldrake et al. (2004) and they are now listed as variables Wel9 (222), Wel15 (219), Wel28 (229) and Wel31 (220) in the above table. V54-56 = V14-16 of Gilliland et al. (1998) who published delta RA and delta dec in arcseconds. The numbers V54-56 were assigned in this electronic catalogue. Samus et al. (2009) later derived RA and dec (Epoch 2000) Albrow et al. (2001) referred to thse stars as PC1-V14 to V16 Par-V1 (= PC1-V47) Par-V1 is a variable star that Paresce et al. (1992) discovered close to Einstein X-ray source X0021.8-7221. In a later paper (Paresce et al. 1994), they referred to it as V1. Its RA and dec were published by Geffert et al. (1997). In a subsequent study, Albrow et al. (2001) announced the variable as PC1-V47 and derived an RA that was 0.31 seconds lower than Geffert's value. Edmonds et al. (2003a) subsequently published an ID chart. Par-V2 (= PC1-V53) Par-V2 is V2 of Paresce & De Marchi (1994) and they identified the variable on a series of three HST images. Its RA and dec were published by Geffert et al. (1997) In a later study, Albrow et al. (2001) announced the variable as PC1-V53 and derived an RA that was 0.30 seconds lower than Geffert's value. Edmonds et al. (2003a) subsequently published an ID chart. NOTE: There are discrepancies in the values of the RA derived for the "Paresce" variables by different authors. For Paresce-V1 (W42, PC1-47) and V2 (W30, PC1-V53)) the RA values of Geffert et al. (1997), Grindlay et al. (2001), and Heinke et al. (2005) are approximately 0.3 seconds larger than those published by Albrow et al. (2001) and Edmonds et al. (2003a). This corresponds to approximately 1.4 arcseconds. Sha-V3 Shara et al. (1996) with an HST "difference image" showing its position relative to Par-V2 (Fig 3c). Grindlay et al. (2001) identified the star as the optical counterpart to Chandra X-ray source W27 and Edmonds et al. (2003b) published a finding chart (see Figure 9 of their paper). PC and WF variables Albrow et al. (2001) with RA and dec PC1, WF2, WF3, and WF4 in the numbering system refer to the 4 different HST CCD fields. Many of these variables are optical counterparts to Chandra X-ray sources. Cross-reference lists were published by Edmonds et al. (2003a) and by Heinke et al. (2005). W11_opt = U_opt of Edmonds et al. (2001) who published a finding chart, derived RA, dec and demonstrated that this is the white dwarf companion to the MSP 47 Tuc U. The number W11_opt was assigned in this catalogue. W29_opt Edmonds et al. (2002a) with a finding chart, RA and dec They demonstrated that this is the optical companion to the MSP 47 Tuc W. W34_opt Edmonds et al. (2002a) with RA, dec They concluded that this object might be associated with an unknown MSP. Other W#_opt variables Edmonds et al. (2003a) with RA, dec (see Tables 3 and 4) Some of the stars were listed in Table 3, some in Table 4 and some in both Tables. The Table 3 values are listed if available. In cases, where stars were listed in both tables, there are systematic shifts in RA and dec in the sense that the Table 4 RA values are ~0.3 seconds further east (which corresponds to ~1 arcsecond) and 0.33 arcseconds further south. ID charts were published for some of the variables: W15_opt, W21_opt, W25_opt, W26_opt, W34_opt, W44_opt, W45_opt by Edmonds et al. (2003a) and W44_opt, W51_opt, W53_opt, W56_opt, W120_opt, W122_opt by Edmonds et al. (2003b). These variables were detected in the HST data of Albrow et al. (2001), but were not reported in Albrow's 2001 paper. A19 Lloyd Evans (1974) who identified it on plate II of his paper The RA and dec were later published by Lebzelter & Wood (2005) LW1-22 Lebzelter & Wood (2005) who published RA and dec. Wel9, Wel15, Wel16, Wel21, Wel25, Wel28, Wel31, Wel61, Wel69, Wel78, Wel93, Wel96: Weldrake et al. (2004) with RA, dec and individual finder charts. These authors carrried out a comprehensive search for stellar variability in 47 Tucanae as part of a search for transiting "hot Jupiters" in 47 Tucanae. They detected 100 variables, 69 of which were new discoveries. Based on positions on a V-(V-I) plot, they concluded that most of the variables belong to the SMC. The variables listed here are are the ones that are probably associated with 47 Tuc. In addition, Weldrake et al. recovered the 12 binary systems, V42-V53, that were announced earlier by Kaluzny et al. (1998). (See announcement of V42-53 above.) The membership status of three additional variables, Wel26, Wel17 and Wel34, was not clear, but in a subsequent investigation by Kaluzny et al. (2013), it appears that they may belong to the cluster. They are listed in the above table as KalE1, KalE35 and KalE23 respectively. KalW1, 2, 4, 5, 7, 8, 12, 14 and KalE1, 8, 19, 23, 25, 31, 32, 33, 34, 35, 36, 39: Kaluzny et al. (2013) with RA and dec for all of the variables and individual finder charts for all except KalE1, E8, E23 and E35 which had been identified previously by Kaluzny et al. (1998) or by Weldrake et al. (2004). Table 1 of Kaluzny et al. (2013) lists the IDs for the variables from previous investigations. EM1-7 Figuera Jaimes et al. (2016) with RA, dec and an ID chart -------------------------------------------------------------------- PSR: According to Paulo Freire's website, there are 26 millisecond pulsars in 47 Tuc. (www.naic.edu/~pfreire/GCpsr.html) ----------------------------------------------------------------------- Edmonds, P. D. & Gilliland, R. L. 1996, ApJ, 464, L157 reported the discovery of variability among K giants in 47 Tuc, mostly with periods in the 2-4 day range and V amplitudes in the range 5-15 nmag. ======================================================== References Albrow, M. D., Gilliland, R. L., Brown, T. M., Edmonds, P. D., Guhathakurta, P., Sarajedini, A. 2001, ApJ, 559, 1060 Guhathakurta, P., Sarajedini, A. 2001, ApJ, 559, 1060 Arp, H., Brueckel, F., Lourens, J. v. B. 1963, ApJ, 228 Bailey, S. I. 1902, Harv. Ann. 38 Carney, B. W., Storm, J., Williams, C. 1993, PASP, 105, 294 Cioni, M.-R. L., Bekki, K., Girardi, L., de Grijs, R., Irwin, M. J., Ivanov, V. D., Marconi, M. and 4 coauthors, 2016, A&A, 586, A77 Edmonds, P. D., Gilliland, R. L., Camilo, F., Heinke, C. O., Grindlay, J. E. 2002a, ApJ, 579, 741 Edmonds, P. D., Gilliland, R. L., Guhathakurta, P., Petro, L. D., Saha, A., Shara, M. M. 1996, ApJ, 468, 241 Edmonds, P. D., Gilliland, R. L., Heinke, C O., Grindlay, J. E., Camilo, F. 2001, ApJ, 557, L57 Edmonds, P. D., Gilliland, R. L., Heinke, C O., Grindlay, J. E. 2003a, ApJ, 596, 1177 Edmonds, P. D., Gilliland, R. L., Heinke, C O., Grindlay, J. E. 2003b, ApJ, 596, 1197 Edmonds, P. D., Heinke, C. O., Grindlay, J. E., Gilliland, R. L. 2002b, ApJ, 564, L17 Eggen, O. J. 1972, ApJ, 172, 639 Feast, M. W., Thackeray, A. D. 1960, MNRAS, 120, 463 Feast, M. W., Thackeray, A. D., Wesselink, A. J. 1960, MNRAS, 120, 64 Figuera Jaimes, R., Bramich, D. M., Skottfelt, J., Kains, N., Jorgensen, U. G., Horne, K., Dominik, M. and 26 coauthors, 2016, A&A, 588, A128 Fourcade, C. R., Laborde, J. R., Albarracin, J. 1966, Atlas y Catalogue de Estrellas Variables en Cumulos Globulares al sur de -29 degrees, Cordoba Fox, M. W. 1982, MNRAS, 199, 715 Geffert, M., Auriere, M., Koch-Miramond, L. 1997, A&A, 327, 137 Gilliland , R. L., Bono, G., Edmonds, P. D., Caputo, F., Cassisi, S., Petro, L. D., Saha, A., Shara, M. M. 1998, ApJ, 507, 818 Grindlay, J. E., Heinke, C., Edmonds, P. D., Murray, S. S. 2001, Sci., 292, 2290 Harris, W. E. 1996, AJ, 112, 1487 Heinke, C. O., Grindlay, J. E., Edmonds, P. D., Cohn, H. N., Lugger, P. M., Camilo, F., Bognadov, S., Freire, P. C. 2005, ApJ, 625, 796 Hodge, P. W. & Wright, F. W. 1977, The Small Magellanic Cloud, University of Washington Press Kaluzny, J., Krzeminski, W., Mazur, B., Wysocka, A., Stepien, K. 1997, Ac. A., 47, 249 Kaluzny, J., Kubiak, M., Szymanski, M., Udalski, A., Krzeminski, W., Mateo, M., Stanek, K. Z. 1998, A&AS, 128, 19 Kaluzny, J., Rozyczka, M., Pych, W., Krzeminski, W., Zloczewski, K., Narloch, W., Thompson, I. B. 2013, Ac. A., 63, 309 Knigge, C., Dieball, A., Maiz Apellaniz, J., Long, K. S., Zurek, D. R., Shara, M. M. 2008, ApJ, 683, 1006 Knigge, C., Shara, M. M., Zurek, D. R., Long, K. S., Gilliland, R. L. 2002, in Stellar Collisions, Mergers, and their Consequences, ASP Conf., 263, 137 Knigge, C., Zurek, D. R., Shara, M. M., Long, K. S., Gilliland, R. L. 2003, ApJ, 599, 1320 Leavitt, H. S. 1908, Harv. Ann., 60, 87 Lebzelter, T., Wood, P. R., Hinkle, K. H., Joyce, R. R., Fekel, F. C. 2005, A&A, 432, 207 Lebzelter, T. & Wood, P. R. 2005, A&A, 441, 1117 Liu, L., Qian, S.-B., Fernandez Lajus, E. 2014, New Ast., 26, 116 Lloyd Evans, T. 1974, MNRAS, 167, 393 Lloyd Evans, T. & Menzies, J. W. 1973, in IAU Colloq. No. 21, Variable Stars in Globular Clusters and in Related Systems, 151 McKibben-Nail, V. 1951, Harv. Bull., 920, 15 Paresce, F., De Marchi, G., Ferraro, F. 1992, Nature, 360, 46 Paresce, F., De Marchi, G. 1994, ApJ, 427, L33 Payne-Gaposchkin, C. & Gaposchkin, S. 1966, Smithsonian Contr., 9, 1 Rucinski, S. M. 2000, AJ, 120, 319 Samus, N. N., Kazarovets, E. V., Pastukhova, E. N., Tsvetkova, T. M., Durlevich, O. V. 2009, PASP, 121, 1378 Sawyer, H. B. 1955, Publ. DDO, 2, No. 2 Sawyer Hogg, H. 1973, Publ. DDO, 3, No. 6 Shara, M. M., Bergeron, L. E., Gilliland, R. L., Saha, A., Petro, L. 1996, ApJ, 471, 804 Storm, J., Nordstrom, B., Carney, B. W., Andersen, J. 1994, A&A, 291, 121 Thompson, I. B., Kaluzny, J., Rucinski, S. M., Krzeminski, W., Pych, W., Dotter, A., Burley, G. S. 2010, AJ, 139, 329 Weldrake, D. T. F., Sackett, P. D., Bridges, T. J., Freeman, K. C. 2004, AJ, 128, 736 Wildey, R. L. 1961, ApJ, 133, 430 =========================================================