NGC 3201 / C1015-461 (Updated January 2012) 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 or P (for photographic). 61-65 A5 Type of variable (draft 2006 GCVS classifications) NV denotes not variable 67-80 A19 Notes and Remarks (f denotes field star) "--" or "----" indicates no data available ========================================================================= ID Position Period ampl C Type Notes/ RA/X Dec/Y Units Remarks ========================================================================= 1 10:17:42.82 -46:26:37.8 R0 0.6049 14.81 0.92 V RR0 2 10:17:39.98 -46:26:37.9 R0 0.5327 14.80 1.07 V RR0 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 0.5016 14.73 0.94 V RR0 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 0.6287 14.74 0.73 V RR0 9 10:17:32.28 -46:26:12.6 R0 0.5255 14.82 0.96 V RR0 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 0.2990 14.79 0.58 V RR1 12 10:17:29.03 -46:22:55.8 R0 0.4956 15.16 0.17 V RR0 13 10:17:22.03 -46:23:11.2 R0 0.5752 14.85 0.88 V RR0 14 10:17:22.42 -46:22:31.5 R0 0.5093 14.99 1.13 V RR0 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 0.5656 14.76 0.92 V RR0 18 10:17:39.4 -46:25:07 R0 0.5397 14.74 1.05 V RR0 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 0.5666 14.83 0.73 V RR0 22 10:17:27.64 -46:25:38.0 R0 0.6060 14.75 0.86 V RR0 23 10:17:32.64 -46:25:31.1 R0 0.5868 14.80 0.77 V RR0 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 0.5148 14.73 1.05 V RR0 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 0.5800 14.87 0.86 V RR0 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 ---- -- -- NV 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 36 10:17:27.01 -46:24:53.0 R0 0.4842 14.73 1.26 V RR0 37 10:17:30.69 -46:25:55.7 R0 0.5757 14.74 1.05 V RR0 38 10:17:31.42 -46:25:41.1 R0 0.5091 14.81 0.81 V RR0 39 10:17:41.23 -46:23:49.7 R0 0.4832 14.81 1.20 V RR0 40 10:17:28.00 -46:23:35.9 R0 0.6438 14.84 0.58 V RR0 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 45 10:17:49.29 -46:25:14.6 R0 0.5375 14.91 1.09 V RR0 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 50 10:17:36.1 -46:24:14 R0 0.5422 14.71 1.00 V RR0 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 0.3800 -- -- RR1 K71 53 10:16:13.05 -46:37:01.2 R0 0.5335 -- -- RR0 W41 54 10:18:41.66 -46:37:53.4 R0 0.5559 14.87 0.85 RR0 C84 55 10:17:05.38 -46:12:00.2 R0 0.6070 -- -- RR0 K71 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 0.5400 -- -- RR0 K71 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 14.01 1.02 P E max;W41;f 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 ---- -- -- NV 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 0.3600 RR1 K71;P? 73 10:17:25.20 -46:23:15.2 R0 0.5200 14.76 1.24 V RR0 74 10:17:28.15 -46:24:06.4 R0 ---- -- -- NV 75 10:17:29.58 -46:22:20.4 R0 --- -- -- NV 76 10:17:31.29 -46:25:23.6 R0 0.5267 14.81 0.66 V RR0 77 10:17:36.13 -46:25:36.1 R0 0.5676 14.71 0.86 V RR0 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 0.5900 14.80 0.59 V RR0 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 ---- -- -- NV 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 ---- -- -- NV W41;K71 86 10:18:36.46 -46:29:58.4 R0 ---- -- -- NV W41;K71 87 10:19:15.15 -46:32:07.9 R0 0.6039 -- -- RR W41 88 10:18:00.49 -46:06:40.2 R0 0.5700 -- -- RR K71 89 10:19:53.58 -46:28:00.0 R0 0.3690 -- -- RR K71 90 10:17:34.95 -46:24:33.3 R0 0.6061 14.68 0.94 V RR0 91 10:15:11.31 -46:04:43.3 R0 0.3450 -- -- RR1? K71 92 10:17:22.7 -46:25:11 R0 0.5396 14.76 0.99 V RR0 93 10:20:51.15 -46:28:03.6 R0 0.48 -- -- RR K71 94 10:13:02.52 -45:53:44.2 R0 ---- -- -- NV K71 95 10:20:37.83 -45:41:39.9 R0 ---- -- -- NV K71 96 10:13:05.16 -46:32:03.0 R0 0.59 -- -- RR K71 97 10:17:11.64 -46:25:51.0 R0 ---- -- -- NV 98 10:17:25.14 -46:25:20.0 R0 0.3356 14.78 0.43 V RR1 L1405 99 10:17:25.80 -46:24:39.4 R0 ---- -- -- NV 100 10:17:36.14 -46:24:27.9 R0 0.5489 14.77 1.02 V RR0 L2710 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 SXPHE 103 10:17:32.10 -46:22:37.9 R0 0.0373 17.37 0.04 V SXPHE 104 10:17:36.60 -46:23:03.4 R0 0.0375 17.46 0.025 V SXPHE 105 10:17:42.60 -46:24:19.5 R0 0.0376 17.37 0.07 V SXPHE 106 10:17:36.00 -46:24:38.2 R0 0.0435 16.89 0.04 V SXPHE 107 10:17:42.50 -46:24:49.1 R0 0.0405 16.96 0.13 V SXPHE 108 10:17:40.20 -46:25:07.8 R0 0.0673 16.35 0.37 V SXPHE 109 10:17:36.00 -46:25:40.2 R0 0.0543 17.05 0.39 V SXPHE 110 10:17:48.10 -46:25:53.4 R0 0.0502 16.59 0.36 V SXPHE 111 10:17:50.90 -46:25:57.7 R0 0.0479 17.07 0.03 V SXPHE 112 10:17:20.10 -46:26:38.0 R0 0.0542 16.48 0.20 V SXPHE 113 10:17:25.86 -46:26:21.0 R0 26.0 11.809 0.024 V LB =LS2;Field? 114 10:17:31.59 -46:29:01.0 R0 ---- 11.892 0.044 V SR =LS4;P>30 115 10:17:16.16 -46:25:32.7 R0 16.0 12.069 0.052 V SR =LS5 116 10:17:39.47 -46:25:32.3 R0 17.0 12.075 0.037 V SR =LS6 117 10:17:33.45 -46:24:34.6 R0 17.0 12.138 0.050 V SR =LS7 118 10:17:51.52 -46:22:09.7 R0 11.0 12.399 0.028 V SR =12 ======================================================================== Supplementary Notes The RA and dec for V1-101 are from Samus et al. (1999). In an earlier paper (Samus et al. 1996), ID charts were published. 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 V1-100 are taken from Layden & Sarajedini (2003) because their study was the most comprehensive. (They also confirmed the "NV" classification that was previously reported by Wright (1941) and Kukarkin (1971) for V33, V70, V74, V75 and V82.) However, some variables were outside the Layden & Sarajedini 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. 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. The data for V101 (=V6 of von Braun & Mateo 2002) and V102-112 (V1-11 of Mazur et al. 2003) are from the discovery papers. The periods, magnitudes and V amplitudes for V113-118 are from Layden & Sarajedini (2003) and their RA and dec were derived by Layden (2012 - private communication) based on 2MASS identifications. The classifications were assigned in this catalogue after consulation with Samus (2012- private communication). 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 V68: Wright (1941) pointed out that this star was probably a long period variable. It was outside Layden & Sarajedini's (2003) field. Samus et al. (2009) pointed out that V68 is the same stars as NSV 4810 and ASAS 101711-4610.8 in the ASAS-3 catalogue (Pojmanski 2002) at http://www.astrouw.edu.pl/asas 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 Layden & Sarajedini (2003) found that it was near the RGB tip, exhibited low level variability and could be a 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 also listed 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. V88-96 = Nr. 1-9 Wilkens (1965) with x,y coordinates to a precision of 0.1 arcmin and ID charts: V3, 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. 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). 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 Layden and Sarajedini (2003) 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 (L&S) published an incorrect version of Table 2 in their paper. V113-118 = LS 2, 4, 5, 6, 7, 12 Layden & Sarajedini (2009) with X,Y pixel numbers The RA and dec for these stars were derived by Layden (2012- private communication). Layden also established that the IDs listed for the RGB variables in Table 7 corresponded to the numbers listed in Table 2. Layden & Sarajedini (2003) 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. They also noted the possibility that #2 could be a field variable, presumably because of its red color - but the color is not extreme. ------------------ Pietrukowicz et al. (2008) searched for dwarf novae in NGC 3201 and found none. Their search was based on 751 V exposures obtained on 751 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 Bailey, S. I. 1922, Harvard Circ., 234, 1 Cacciari, C. 1984, AJ, 89, 231; erratum 1984, AJ 89, 1082 Carretta, E., Bragaglia, A., D'Orazi, V., Lucatello, S., Gratton. R. G. 2010, A&A, 519, 71 Clement, C. M., Muzzin, A., Dufton, Q., Ponnampalam, T., Wang, J., Burford, J., Richardson, A., Rosebery, T. 2001, AJ, 122, 2587 Dowse, M. 1940, Harvard Bull., 913, 17 Fourcade, C. R., Laborde, J. R., Albarracin, J. 1966, Atlas y Catalogue de Estrellas Variables en Cumulos Globulares al sur de -29 degrees, Cordoba Kravtsov, V., Alcaino, G., Marconi, G., Alvarado, F. 2010, A&A, 512, L6 Kukarkin, B. V., 1967, Astron Tsirk, 426, 4 Kukarkin, B. V., 1971a, Astron Tsirk, 637, 4 Kukarkin, B. V., 1971b, Per. Zvez., 17, 610 Layden, A. C. & Sarajedini, A. 2003, AJ, 125, 208 Lee, S.-W. 1977, A&A Supp., 28, 409 Mazur, B., Krzeminski, W., Thompson, I. B. 2003, MNRAS, 340, 1205 Piersimoni, A. M., Bono, G., Ripepi, V. 2002, AJ, 124, 1528 Pietrukowicz, P., Kaluzny, J., Schwarzenberg-Czerny, A., Thompson, I. B., Pych, W., Krzeminski, W., Mazur, B. 2008, MNRAS, 388, 1111 Pojmanski, G. 2002, Acta Ast, 52, 397 Samus, N. N., Kravtsov, V. V., Pavlov, M. V., Strel'nikov, V. V., Shokin, Yu. A., Alcaino, G., Liller, W., Alvarado, F. 1996, Ast. Let. 22, 239 Samus, N. N., Kazarovets, E. V., Pastukhova, E. N., Tsvetkova, T. M., Durlevich, O. V. 2009, PASP, 121, 1378 von Braun, K. & Mateo, M. 2002, AJ, 123, 279 Webb, N. A., Wheatley, P. J., Barret, D. 2006, A&A, 445, 155 Wilkens, H. 1965, Sonneberg Mitt. Veranderliche Sterne, 3, 75 Woods, I. E. 1919, Harvard Circ., 216, 1 Wright, F. W. 1941, Harvard Bull. 915, 2 ==================================================================