NGC 6760 / C1908+009 (Updated September 2015) RA: 19:11:12.01 DEC: +01:01:49.7 (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 19:11:16.01 +01:00:58.6 R0 ---- 16.35 1.3 P L? Note 2 19:11:11.91 +01:00:16.4 R0 ---- 16.95 0.5 P ? 3 19:11:14.31 +01:01:46.6 R0 251.0 7.69 0.72 K M 4 19:11:15.03 +01:02:36.8 R0 226.0 7.96 0.94 K M PSR:A-B ---- -- -- PSR ====================================================================== Supplementary Notes NGC 6760 is a metal rich cluster in the Galactic bulge. The 2010 update to the Harris (1996) catalogue lists [Fe/H] = -0.4. A VI CM diagram by Heitsch & Richtler (1999) shows a prominent red HB and also demonstrates that the cluster is located in a rich field near the plane of the Galaxy. For V1 and V2, the magnitudes are from the discovery paper by Sawyer (1953) and the RA and dec are from Samus et al. (2009). All the data for V3 and V4 are from Sloan et al. (2010). =================================================================== Notes on individual stars V1: Prosser (1988) commented that V1 could be a possible Mira because it has a late type spectrum. In Sawyer's (1953) study, V1 was the same brightness as the two Mira variables, V3 and V4, at maximum light. However, its light amplitude is smaller than that expected for a Mira. ======================================================================= Discovery of the variable stars in NGC 6760: V1-4 Sawyer (1953) with x,y coordinates and an ID chart Prosser (1988) later published a more legible ID chart -------------------------------------------------------------------- PSR: According to Paulo Freire's website, there are 2 millisecond pulsars in NGC 6760. (www.naic.edu/~pfreire/GCpsr.html) ========================================================================= References Harris, W. E. 1996, AJ, 112, 1487 Heitsch, F. & Richtler, T. 1999, A&A, 347, 455 Prosser, C. F. 1988, IBVS, 3268 Samus, N. N., Kazarovets, E. V., Pastukhova, E. N., Tsvetkova, T. M., Durlevich, O. V. 2009, PASP, 121, 1378 Sawyer, H. B. 1953, JRASC, 47, 229 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 =========================================================================