NGC 6171 / C1629-129 / Messier 107 (Updated March 2015) RA: 16:32:31.86 DEC: -13:03:13.6 (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 16:32:24.61 -13:12:01.3 R0 332.0 15.500 3.0 P M f;Note 2 16:32:42.46 -13:09:45.9 R0 0.5710 15.637 0.783 V RR0 Dkns 3 16:32:16.71 -13:06:23.6 R0 0.5663 15.430 0.524 V RR0 Dkns 4 16:32:25.28 -13:05:55.4 R0 0.2821 15.535 0.463 V RR1 5 16:32:47.90 -13:05:57.3 R0 0.7024 15.522 0.460 V RR0 Dkns 6 16:32:31.32 -13:04:25.6 R0 0.2603 15.654 0.521 V RR1 7 16:32:35.00 -13:04:18.9 R0 0.4975 15.789 0.868 V RR0 8 16:32:32.82 -13:03:59.9 R0 0.5599 15.607 1.090 V RR0 9 16:32:30.18 -13:03:37.9 R0 0.3206 15.640 0.467 V RR1 10 16:32:28.08 -13:03:10.3 R0 0.4155 15.773 1.142 V RR0 11 16:32:32.60 -13:02:44.9 R0 0.5928 15.553 0.620 V RR0 Dkns 12 16:32:35.98 -13:02:16.6 R0 0.4729 15.718 0.735 V RR0 13 16:32:30.10 -13:02:06.1 R0 0.4668 15.767 1.272 V RR0 Dkns 14 16:32:33.13 -13:01:55.5 R0 0.4816 15.704 1.284 V RR0 15 16:32:33.20 -13:01:17.6 R0 0.2886 15.615 0.451 V RR1 16 16:32:27.33 -13:01:25.0 R0 0.5228 15.676 0.733 V RR0 Dkns 17 16:32:25.16 -13:02:07.2 R0 0.5612 15.614 1.063 V RR0 18 16:32:37.13 -12:59:41.9 R0 0.5644 15.746 0.852 V RR0 19 16:32:47.79 -13:00:32.7 R0 0.2788 15.755 0.478 V RR1 20 16:32:34.08 -13:02:26.8 R0 0.5781 15.750 0.806 V RR0 21 16:32:37.61 -13:05:42.5 R0 0.2583 16.606 0.460 V RR1 f;Note 22 16:30:59.32 -13:06:33.1 R0 0.5024 16.62 1.20 V RR0 f;Note 23 16:32:13.96 -13:03:01.5 R0 0.3233 15.616 0.402 V RR1 24 16:32:31.98 -13:03:09.7 R0 0.5240 15.807 1.001 V RR0 25 16:32:31.41 -13:02:59.1 R0 ---- 12.9 0.4 V Lb: Note 26 16:32:32.66 -13:03:00.4 R0 0.0526 17.72 0.092 V SXPhe Note ===================================================================== Supplementary Notes and Periods, magnitudes and variability types are from Clement & Shelton (1997) unless designated "Dkns" in the remarks column (see V2, V3, V5, V11, V13, V16). For these stars, this information is from Dickens (1970). The RA and dec are from Samus et al. (2009) unless indicated otherwise in the Notes on individual stars. Cudworth et al. (1992) derived membership probabilities for some of the RR Lyrae variables in NGC 6171 from a proper motion study. ============== Notes on individual stars V1: V1 = V720 Oph in the GCVS Period, magnitude and classification by Coutts & Sawyer Hogg, (1971). A radial velocty spectrum by Feast (private communication to Sawyer Hogg) demonstrated that V1 is not a cluster member. NB: The star Dickens (1970) listed as V1 is V23 in the above table. V21: The "f" status for V21 was assigned by Dickens (1970) and confirmed by the proper motion study of Cudworth et al. (1992). V22: V22 = NSV 07824 in the GCVS = SSS_J163059.3-130633 Oosterhoff (1938) did not list any magnitudes for V22, but he commented that it was fainter than the other variables. It was located near the edge of his plates and not in the field of the finder chart he published. Sawyer Hogg (1973) classified it as a probable field star because it is outside the tidal radius which is 18.98 according to the 2010 version of the Harris (1996) cataogue. Torrealba et al. (2015) identified V22 as SSS_J163059.3-130633 in the southern Catalina surveys and the period, magnitude, amplitude and classification in the above table are from their catalogue. It is considerably fainter than the other RR Lyrae variables in the cluster thus comfirming Sawyer Hogg's conclusion that it is a field star. V25: Magnitude and amplitude from Lloyd Evans & Menzies (1977). They classified V25 as a red variable, but we have classified it as Lb because the GCVS does not use the term, red variable. V26: The data for V26 are from the discovery paper by McCombs et al. (2012). However, the amplitude they listed appeared to be the half amplitude (0.046 mag) so that value was doubled in the above table. =============================================================== Discovery of the variable stars in NGC 6171: V1-24 Oosterhoff (1938) with x,y positions and ID chart V25 Lloyd Evans & Menzies (1973) V25 is star 217 in the insert to Fig 1 of Sandage & Katem (1964) V26: McCombs et al. (2012) with RA dec and an ID chart ======================================================================= References Clement, C. M. & Shelton, I. 1997, AJ, 113, 1711 Coutts, C. M. & Sawyer Hogg, H. 1971, Publ. DDO, 3, No. 2 Cudworth, K. M., Smetanka, J. J., Majewski, S. R. 1992, AJ, 103, 1252 Dickens, R. J. 1970, ApJ Supp., 22, 249 Harris, W. E. 1996, AJ, 112, 1487 Lloyd Evans, T. & Menzies, J. W. 1973, in IAU Colloq. No. 21, Variable Stars in Globular Clusters and in Related Systems, 151 Lloyd Evans, T. & Menzies, J. W. 1977, MNRAS, 178, 163 McCombs, T. A., Reinhart, E. D., Darragh, A. N., Johnson, E. W., Murphy, B. W. 2012, JSARA, 7, 51 Oosterhoff, P. Th. 1938, BAN, 8, 273 Samus, N. N., Kazarovets, E. V., Pastukhova, E. N., Tsvetkova, T. M., Durlevich, O. V. 2009, PASP, 121, 1378 Sandage, A. & Katem, B. 1964, ApJ, 139, 1088 Samus, N. N., Kazarovets, E. V., Pastukhova, E. N., Tsvetkova, T. M., Durlevich, O. V. 2009, PASP, 121, 1378 Sawyer Hogg, H. 1973, Publ. DDO, 3, No. 6 Torrealba, G., Catelan, M., Drake, A. J., Djorgovski, S. G., McNaught, R. H., Belokurov, V., Koposov, S. and 4 coauthors, 2015, MNRAS, 446, 2251 =======================================================================