NGC 6749 / Berkeley 42 / C1902+017 (Updated June 2016) RA: 19:05:15.3 DEC: +01:54:03 (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 19:05:20.0 +01:55:57 R0 4.481 12.34 0.44 K CW PSR:A-B -- -- ---- -- -- PSR ====================================================================== Supplementary Notes VI color-magnitude diagrams published by Kaisler et al. (1997) and by Rosino et al. (1997) show a blue HB. Rosino et al. concluded that this is a halo cluster located close to the Galactic plane. The surrounding field is rich in Mira variables (75 within 1 degree of the cluster centre), but they do not appear to be members. They are probably associated with the metal rich disc/bulge population. Skiff (2001) listed RA, dec and magnitudes for the variables, but agreed with Rosino that probably none of the Mira variables are related to the cluster. The data for the type II Cepheid V1 are from Matsunaga et al. (2006). ======================================================================= Discovery of the Variable Stars in NGC 6749 V1 Matsunaga et al. (2006) with RA and dec PSR: According to Paulo Freire's website, there are 2 millisecond pulsars in NGC 6749. (www.naic.edu/~pfreire/GCpsr.html) ========================================================================= References Kaisler, D., Harris, W. E., McLaughlin, D. E. 1997, PASP, 109, 920 Matsunaga, N., Fukushi, H., Nakada, Y., Tanabe, T., Feast, M. W., Menzies, J. W., Ita, Y. and 7 coauthors, 2006, MNRAS, 370, 1979 Rosino, L., Ortolani, S., Barbuy, B., Bica, E. 1997, MNRAS, 289, 745 Skiff, B. A. 2001, IBVS, 5187 =========================================================================