NGC 6362 / C1726-670 (updated March 2019) RA: 17:31:54.99 DEC: -67:02:54.0 (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 17:31:54.72 -67:02:45.7 R0 0.5048 15.352 1.292 V RR0 2 17:31:50.23 -67:04:25.4 R0 0.4890 15.368 1.366 V RR0 3 17:31:40.91 -67:04:15.8 R0 0.4473 15.378 1.185 V RR01? Note 4 17:31:41.44 -67:04:13.5 R0 ---- -- -- CST Note 5 17:32:08.82 -67:02:59.4 R0 0.5214 15.348 1.177 V RR0 6 17:32:03.85 -66:59:51.8 R0 0.2627 15.312 0.47 V RR1 Note 7 17:31:58.52 -67:01:01.4 R0 0.5216 15.368 1.242 V RR0 8 17:31:10.05 -67:01:01.3 R0 0.3815 15.082 0.517 V RR1 9 17:31:19.49 -67:00:29.8 R0 ---- -- -- CST f;Note 10 17:32:26.13 -66:56:52.6 R0 0.2656 15.257 0.471 V RR1 Note 11 17:31:49.90 -67:01:57.8 R0 0.2888 15.255 0.502 V RR1 12 17:31:13.13 -67:04:30.9 R0 0.5330 15.227 1.308 V RR0 13 17:31:15.14 -67:04:47.6 R0 0.5800 15.258 1.251 V RR0 14 17:32:57.94 -67:02:12.8 R0 0.2462 15.374 0.344 V RR1 Note 15 17:32:03.47 -67:02:44.3 R0 0.2799 15.263 0.448 V RR1 f?;Note 16 17:31:58.10 -67:07:12.0 R0 0.5257 15.359 1.12 V RR0 17 17:32:29.46 -67:03:51.2 R0 0.3146 15.335 0.511 V RR1 18 17:32:13.59 -67:01:33.1 R0 0.5129 15.073 0.913 V RR0 19 17:32:15.96 -67:03:09.4 R0 0.5945 15.365 0.663 V RR0 20 17:32:02.64 -67:02:59.4 R0 0.6984 15.273 0.436 V RR0 21 17:32:22.59 -67:04:30.6 R0 0.2814 15.321 0.535 V RR1 22 17:32:26.74 -67:07:55.1 R0 0.2668 15.318 0.516 V RR1 Note 23 17:32:00.12 -67:03:07.5 R0 0.2751 15.359 0.571 V RR1 24 17:32:07.16 -67:03:20.3 R0 0.3293 15.195 0.489 V RR1 25 17:30:54.37 -67:06:18.5 R0 0.4558 15.45 1.23 V RR0 26 17:31:58.87 -67:03:22.2 R0 0.6022 15.351 0.610 V RR0 27 17:31:21.62 -66:56:27.7 R0 0.2781 15.253 0.520 V RR1 Note 28 17:31:59.16 -67:02:07.7 R0 0.3584 15.111 0.457 V RR1 29 17:31:52.49 -67:03:20.2 R0 0.6477 15.272 0.502 V RR0 30 17:31:39.59 -67:01:33.6 R0 0.6134 15.186 0.954 V RR0 31 17:31:49.20 -67:01:20.7 R0 0.6002 15.323 0.749 V RR0 32 17:32:01.83 -67:02:12.7 R0 0.4972 15.385 1.258 V RR0 Note 33 17:32:47.91 -66:56:36.2 R0 0.3064 15.319 0.398 V RR1 f;Note 34 17:31:52.81 -67:03:34.3 R0 0.4943 15.305 1.070 V RR01? Note 35 17:32:08.14 -67:03:03.0 R0 0.2908 15.318 0.462 V RR1 36 17:31:43.57 -67:02:16.8 R0 0.3101 15.173 0.393 V RR1 f?;Note 37 17:31:32.12 -67:02:03.4 R0 0.2546 15.319 0.403 V RR? Note 38 17:31:43.61 -67:02:58.5 R0 0.0666 17.02 0.63 V SXP0 39 17:32:08.46 -67:03:14.8 R0 0.3633 17.86 0.20 V EW max 40 17:32:04.08 -67:03:45.5 R0 5.2962 18.22 0.54 V EA max 41 17:31:35.37 -67:04:03.1 R0 17.8888 18.77 0.58 V EA max 42 17:31:09.01 -66:51:38.9 R0 2.7694 17.51 0.64 V EA f;max 43 17:34:03.34 -66:52:53.5 R0 0.285 16.02 0.44 V EW f;max;Note 44 17:33:25.96 -66:53:43.9 R0 0.9577 14.95 0.62 V RR0? f;Note 45 17:30:52.68 -66:58:58.8 R0 0.3407 16.92 0.33 V EW f;max;Note 46 17:32:24.95 -67:00:31.4 R0 0.0506 17.55 0.05 V SXP0 47 17:32:13.02 -67:02:37.9 R0 0.0522 17.35 0.05 V SXP0 48 17:31:59.82 -67:03:49.9 R0 0.0479 17.12 0.06 V SXP1 49 17:32:24.13 -67:04:00.4 R0 32.504 14.97 0.36 V EB max 50 17:34:09.50 -67:07:54.4 R0 ---- 18.44 0.35 V E? f;max;Note 51 17:34:15.66 -67:12:05.3 R0 ---- 16.87 0.17 V ? f;max;Note 52 17:33:10.70 -67:13:16.6 R0 0.399 15.36 0.46 V EW f;max;Note 53 17:33:09.74 -66:51:21.8 R0 0.2827 19.61 0.25 V EW f;max 54 17:32:54.02 -67:05:55.6 R0 0.4430 20.41 0.48 V EA max 55 17:32:54.08 -66:55:36.3 R0 6.4935 17.35 0.05 V EB f;max 56 17:32:52.77 -66:58:28.0 R0 0.5193 17.50 0.09 V EW f?;max;Note 57 17:32:46.11 -66:55:33.3 R0 0.8185 16.62 0.08 V spot? f;max 58 17:32:28.08 -67:08:43.5 R0 3.815 17.96 0.09 V spot? f;max 59 17:32:24.69 -67:06:41.3 R0 0.6601 17.48 0.03 V EW? max 60 17:32:14.01 -67:01:07.5 R0 6.0255 17.89 0.12 V spot f;max;Note 61 17:32:18.14 -67:03:39.3 R0 46.35 17.23 0.07 V spot max 62 17:32:05.83 -67:03:08.0 R0 16.7321 19.39 0.33 V EA max 63 17:32:03.47 -67:08:22.4 R0 1.8902 17.80 0.15 V EB f;max 64 17:31:58.24 -67:03:45.8 R0 0.0502 17.06 0.03 V SXP1 65 17:31:47.72 -67:03:53.3 R0 30.9723 18.39 0.43 V EA max 66 17:31:48.03 -67:01:58.0 R0 1.9742 19.13 0.20 V EA f?;max;Note 67 17:31:45.53 -67:04:26.1 R0 0.2508 19.55 0.52 V EW f;max 68 17:31:44.90 -67:03:20.9 R0 17.98 17.62 0.08 V spot max 69 17:31:43.72 -67:01:46.7 R0 2.0125 17.14 0.08 V spot f?;max;Note 70 17:31:38.90 -67:02:53.7 R0 0.3393 17.60 0.47 V EW f?;max;Note 71 17:31:36.58 -67:02:14.5 R0 11.9654 19.17 0.30 V EA max 72 17:31:28.97 -67:02:33.8 R0 0.0437 17.61 0.03 V SXP0 73 17:31:16.90 -67:03:36.4 R0 0.3389 20.86 0.82 V EB f;max 74 17:31:17.58 -66:59:57.4 R0 0.2611 18.82 0.17 V EW f;max 75 17:31:33.11 -67:01:46.6 R0 1.2290 18.40 0.10 V spot f 76 17:31:04.35 -67:03:24.0 R0 30.9635 17.04 0.09 V EA f;max 77 17:30:51.18 -66:55:28.6 R0 6.2746 18.41 0.52 V EA f;max ========================================================================== Supplementary Notes There have been a number of CCD investigations of the variable stars in NGC 6362: Mazur et al. (1999), Olech et al. (2001), Kaluzny et al. (2014), Smolec et al. (2017) and Arellano Ferro et al. (2018). In the above table, we have listed the data of Arellano Ferro et al. (2018) for the the RR Lyrae and SX Phe variables, unless indicated otherwise in the notes on individual stars. The data for the eclipsing binaries and other variables are mainly from Kaluzny et al. (2014). However, for some of the variables, (V42, V45, V49, V53, V54, V55, V56, V57, V58, V60, V63, V75, V76, V77) there were errors in their published RA and dec. For these stars, the RA and dec are from Arellano Ferro et al. (2018 - Table B1). V43, V44, V50, V51, V52 were analysed only by Mazur et al. (1999) because they were outside the field of view in the other studies. For these stars, the RA and dec are from Samus et al. (2009) and the remaining data are from Mazur et al., unless indicated otherwise in the notes on individual stars. Most of the information about membership status in the remarks column is from an investigation by Bustos Fierro & Calderon (2018) which was based on GaiaDR2 astrometry. They established membership status for all of the variables numbered 1 to 77 except V60. Stars designated 'f' or 'f?' in the remarks column are the ones they found to be field stars. They considered all of the other stars to be cluster members. Kaluzny et al. (2014) also listed the membership status for the stars in their investigation. Stars for which their results differed are designated 'f?' and are discussed in the notes on individual stars. =================================================================== Notes on individual stars V3, V34: Smolec et al. (2017) classified these two stars as anomalous RRd (double mode) variables. These stars differ from classical RRd variables because their period ratios (P1/P0) are smaller and the fundamental mode most often dominates the pulsation. Also, a long term modulation of pulsation of one or both radial modes, is often detected in anomalous RRd stars. V4, V9: The non-variable status of these variables was first noted by van Agt (1961) and confirmed by Clement et al. (1995). Mazur et al. (1999) concurred that V4 was probably constant, but V9 was outside of their field. The RA and dec listed for these stars is from Samus et al. (2009). V6, V10, V14, V22, V27, V33: For these variables, the periods listed were the ones derived by Smolec et al. (2017). The remaining data are from Arellano Ferro et al. (2018). V15, V36: According to the membership investigation of Bustos Fierro & Calderon (2018), both of these RR Lyrae variables are field stars. However, with distances of 0.8 and 1.4 arcminutes from the cluster centre, both stars are well with the half-light radius, 2.05 arcminutes, listed by Harris (2010). In addition, their locations on the CM diagram are appropriate for cluster membership. V32: Clement et al. (1995) classified this star as non-variable, but Mazur et al. (1999) showed that it was an RR0 variable. They concluded that Clement et al. must have measured the wrong star. Later studies by Olech et al. (2001), by Smolec et al. (2017) and by Arellano Ferro et al. (2018) confirmed the variability of V32. V37: This star has two close and large amplitude periodicities (0.2550394, 0.2509836 days) which are both intrinsic to the star, but the shapes of the light curves for both periods differ from the shape typical for RR1 variables. Therefore Smolec et al. (2017) considered its RR Lyrae classification to be tentative. Arellano Ferro et al. (2018) pointed out that V37 has a close neighbour that might also be variable and that a firm conlusion regarding the nature of this star can only be made with images in which the two stars are resolved. According to Zloczewski et al. (2012) and Bustos Fierro & Calderon (2018), V37 is a cluster member. V43: Based on the distance modulus, Mazur et al. (1999) concluded that V43 lies in the cluster foreground. The non-membership status was confirmed by Rucinski (2000) and by Bustos Fierro & Calderon (2018). V44 (ASASSN-VJ173325.84-665344.7): Mazur et al. (1999) did not have enough observations to derive a period for V44. However, it was included in the ASAS-SN survey (Jayasinghe et al. 2018) and Watson et al. (2006) published a period and maximum and minimum V magnitudes based on data from the survey. The mean magnitude and amplitude listed above were derived from Watson et al. (2006). They classified the star as RR0. However, given that its period is almost one day, it could also be a short period type II Cepheid. According to the membership investigation of Bustos Fierro & Calderon (2018), V44 is a field star. V45: The non-membership status of V45 was confirmed by Rucinski (2000). V50: Mazur et al. noted that this star is located near the turn-off point in the CMD and is probably a W UMa-type contact system. They were unable to determine a period. According to the membership investigation of Bustos Fierro & Calderon (2018), V50 is a field star. V51: Mazur et al. were unable to classifiy this variable. They noted that it varied on a time scale of hours and that the variations might be caused by eclipses or by the ellipsoidal effect. It is located near the red giant branch, about 1.5 mag below the HB. According to the membership investigation of Bustos Fierro & Calderon (2018), V51 is a field star. V52: Based on the distance modulus, Mazur et al. (1999) concluded that V52 lies in the cluster foreground. The non-membership status was confirmed by Rucinski (2000) and by Bustos Fierro & Calderon (2018). V56: Kaluzny et al. (2014) classified V56 as a non-member, but according to Bustos Fierro & Calderon (2018), it is a cluster member. V60: The membership status is from Kaluzny et al. (2014). V66: Kaluzny et al. (2014) classified V56 as a member, but according to Bustos Fierro & Calderon (2018), it is not a cluster member. V69: Kaluzny et al. (2014) classified V69 as a non-member, but according to Bustos Fierro & Calderon (2018), it is a cluster member. V70: Kaluzny et al. (2014) classified V70 as a non-member, but according to Bustos Fierro & Calderon (2018), it is a cluster member. =================================================================== Discovery of the variable stars in NGC 6362: V1-15 Woods (1919) with x,y coordinates According to Shapley (1930), Woods discovered 17 variables in NGC 6362, but it appears that 2 were unpublished and there is no further information about them. In her 3rd catalogue, Sawyer Hogg (1973) mentioned a field variable announced by Shapley (1922) V16-31 van Agt (1961) with x,y coordinates and an ID chart for all of V1-31 (except V4 and V9). van Agt also made small revisions to some of the x,y coordinates derived by Woods (1919) V32 Fourcade et al. (1966) with x,y coordinates and ID chart for V1-32 V33 = VH 11 van Hoof (1961) with x,y coordinates and an ID chart The number V33 was assigned by Sawyer Hogg (1973) in her 3rd catalogue. van Hoof announced the discovery of seven other variables, but these were all independently discovered by van Agt (1961) so Sawyer Hogg adopted van Agt's numbering system for her catalogue. However, all of the epochs, periods and magnitudes listed for the NGC 6362 variables in her 3rd catalogue were from van Hoof's paper. V34-52 Mazur et al. (1999) with RA, dec and individual finder charts They also discovered a hot subdwarf with V=19.1, V-I=-0.24, B-V=-0.28 at RA=17:31:46.3, dec=-67:05:03 (2000) which Zloczewski et al. (2012) found to be a probable cluster member based on its proper motion. V53-77 Kaluzny et al. (2014) with individual finding charts and RA, dec For some of these new variables (V53, V54, V55, V56, V57, V58, V60, V63, V75, V76, V77), their published RA and dec were incorrect. After consultation with Rozyczka (private communication), Arellano Ferro et al. (2018 - Table B1) published the correct values and these are listed in the above table. ------------------- Pietrukowicz et al. (2008) searched for dwarf novae in NGC 6362 and found none. Their search was based on observations made on 104 nights, spanning 7 years, from 1999 to 2005. =============================================================== References Arellano Ferro, A., Ahumada, J. A., Bustos Fierro, I., Calderon, J. H., Morrell, N. I. 2018, Ast. Nach., 339, 183 Bustos Fierro, I. H. & Calderon, J. H. 2018, private communication, paper presented at Astronomia Dinamica en Latinoamerica VIII, held in Tarija, Bolivia, October 2018 Clement, C., Dickens, R., Bingham, E. 1995, AJ, 110, 2195 Fourcade, C. R., Laborde, J. R., Albarracin, J. 1966, Atlas y Catalogue de Estrellas Variables en Cumulos Globulares al sur de -29 degrees, Cordoba Harris, W. E. 2010, arXiv:1012.3224 Jayasinghe, T., Kochanek, C. S., Stanek, K. Z., Shappee, B. J., Holoien, T. W.-S., Thompson, T. A., Prieto, J. L. and 7 coauthors, 2018, MNRAS, 477, 3145 (The All-Sky Automated Survey for Supernovae: ASAS-SN) Kaluzny, J., Thompson, I. B., Rozyczka, M., Pych, W., Narloch, W. 2014, Ac. A., 64, 309 Mazur, B., Kaluzny, J., Krzeminski, W. 1999, MNRAS, 306, 727 Olech, A., Kaluzny, J., Thompson, I. B., Pych, W., Krzeminski, W., Scwarzenberg-Czerny, A. 2001, MNRAS, 321, 421 Pietrukowicz, P., Kaluzny, J., Schwarzenberg-Czerny, A., Thompson, I. B., Pych, W., Krzeminski, W., Mazur, B. 2008, MNRAS, 388, 1111 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 Shapley, H. 1922, Harvard Bull., 177 Shapley, H. 1930, in Star Clusters, Harvard Observatory Monographs No. 2, (New York: McGraw Hill), pp 45-46 Smolec, R., Moskalik, P., Kaluzny, J., Pych, W., Rozyczka, M., Thompson, I. B. 2017, MNRAS, 467, 2349 van Agt, S. L. Th. J. 1961, BAN 15, 329 Van Hoof, A. 1961, Louvain Pub., 14, 131 Watson, C. L., Henden, A. A., Price, A. 2006, Soc. for Ast. Sci. Symp., 25, 47 Woods, I. E. 1919, Harvard Circ., 217 Zloczewski, K., Kaluzny, J.,Rozyczka, M., Krzeminski, W., Mazur, B. 2012, Ac. A., 62, 357 ======================================================================