IC 1276 / Palomar 7 / formerly Abell 7 /C1808-072 RA: 18:10:44.20 DEC: -07:12:27.4 (J2000) (Most recent updates: Membership probability flag - 2024; Remaining data - May 2014) ============================================================ Bytes Format Explanation 1-8 A8 Star ID 10-32 A11,1x,A11 Position 34-35 A2 Membership probability flag based on data published by Prudil & Arellano Ferro (2024) m1: prob >=0.85; m2: prob >=0.7 and <0.85; m3: prob >= 0.5 and <0.7; f: prob <0.5 u: no data available 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 Mem Period ampl C Type Notes/ RA Dec Flag Remarks ========================================================================= 1 18:10:51.55 -07:10:54.5 m1 222.0 21.1 1.8 B M Sloan 2 18:10:44.5 -07:12:31 m1 0.548 19.45 1.1 B RR0 3 18:10:50.79 -07:13:49.1 m1 300.0 19.9 4.2 B M Sloan 4 18:10:48.37 -07:10:33.0 m1 ---- 19.15 0.7 B SR 5 18:10:31.02 -07:08:57.1 m1 ---- 19.2 0.8 B SR ====================================================================== Supplementary Notes The RA and dec are from Samus et al. (2009). The periods and classifications for V1 and V3, the two Mira variables, are from Sloan et al. (2010) who published K band light curves. The B magnitudes and amplitudes for these stars are from Kinman & Rosino (1962). The periods, magnitudes, amplitudes and variability types for V2, V4 and V5 are from Kinman & Rosino (1962). They assumed that all of the variables were cluster members. Their magnitudes were appropriate for cluster membership and were located well inside the tidal radius which is 21.6 arcmin according to the 2010 update to the Harris (1996) catalogue. Barbuy et al. (1998) published a BV colour-magnitude diagram that showed a prominent red HB, characteristic of a metal rich population. Cote (1999) later derived [Fe/H] = -0.75 from the equivalent widths of iron lines in 5 RG stars considered to be cluster members on the basis of their radial velocities. ================================================================== Discovery of the Variable Stars in Pal 7: V1 Sawyer Hogg (1959) with ID chart The cluster was referred to as IC 1276 in her paper. V2-5 Kinman & Rosino (1962) with x,y positions and ID chart for V1-5 The cluster was referred to as Abell 7 = IC 1276 in their paper. ================================================================== References Barbuy, B., Ortolani, S., Bica, E. 1998, A&AS, 132, 333 Cote, P. 1999, AJ, 118, 406 Harris, W. E. 1996, AJ, 112, 1487 Kinman, T. D., Rosino, L. 1962, PASP, 74, 499 Prudil Z., Arellano Ferro, A. 2024, MNRAS, 534, 3654 Samus, N. N., Kazarovets, E. V., Pastukhova, E. N., Tsvetkova, T. M., Durlevich, O. V. 2009, PASP, 121, 1378 Sawyer Hogg, H. 1959, JRASC, 53, 97 Sloan, G. C., Matsunaga, N., Matsuura, M., Zijlstra, A. A., Kraemer, K. E., Wood, P. R., Nieusma, J., Bernard-Salas, J., Devost, D., Houck, J. R. 2010, ApJ, 719, 1274 ==================================================================