Terzan 2 / C1724-307 / HP 3/ ESO 454-29 (Updated September 2018) RA: 17:27:33.10 DEC: -30:48:08.4 (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 2 is a metal rich core-collapsed cluster in a crowded field in the Galactic bulge. VI photometry by Ortolani et al. (1997) illustrated that the cluster has a red HB in its CM diagram, but no information about blue stragglers can be discerned because of the contamination by field stars. The red HB has been confirmed by Valenti et al. (2010) based on infrared photometry and by Cohen et al. (2018) based on HST observations with F110W, F160W and F606W filters. Cohen et al. also noted that there is considerable differential reddening in the cluster. There is a low-mass X-ray binary associated with the X-ray source in Terzan 2. Its properties were discussed by Altamirano et al. (2008). No optical identification has been made because the object is near the cluster centre where the crowding is severe. ================================================================= References Altamirano, D., vander Klis, M., Mendez, M., Wijnands, R., Markwardt, C., Swank, J. 2008, ApJ, 687, 488 Cohen, R. E., Mauro, F., Alonso-Garcia, J., Hempel, M., Sarajedini, A., Ordonez, A. J., Geisler, D., Kalirai, J. S. 2018, AJ, 156, 41 Ortolani, S., Bica, E., Barbuy, B. 1997, A&A, 326, 614 Valenti, E., Ferraro, F. R., Origlia, L. 2010, MNRAS, 402, 1729 ==================================================================