Terzan 7 C1914-347 (Updated July 2016) RA: 19:17:43.92 DEC: -34:39:27.8 (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 ========================================================================= No known variables. ======================================================================= Supplementary Notes Terzan 7 is probably a member of the Sagittarius dwarf galaxy. A BV CM diagram by Buonanno et al. (1995) shows a steep red giant branch and a compact red HB, characteristics of a metal-rich cluster. A VI CM diagram by Held et al. (2002) shows a well populated blue straggler sequence. Sbordone et al. (2005) derived [Fe/H] = -0.6 from high resolution UVES-VLT spectra of 5 giant stars. In the 2010 update to his catalogue, Harris (1996) adopted [Fe/H]= -0.32. ======================================================================= References Buonanno, R., Corsi, C. E., Pulone, L., Fusi Pecci, F., Richer, H. B., Fahlman, G. G. 1995, AJ, 109, 663 Harris, W. E. 1996, AJ, 112, 1487 Held, E. V., Rosenberg, A., Saviane, I., Momany, Y. 2002, in IAU Symposium 207, ed. Geisler, Grebel & Minniti, San Francisco: ASP, p.165 Sbordone, L., Bonifaco, P., Marconi, G., Buonanno, R., Zaggia, S. 2005, A&A, 437, 905 =======================================================================