Palomar 5 / Abell 5 / (formerly Baade's cluster) / C1513+000 RA: 15:16:05.25 DEC: -00:06:41.8 (J2000) (Most recent updates: Membership probability flag - 2024; Remaining data - May 2016) ============================================================ 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 15:15:57.18 -00:06:53.3 m1 0.2932 17.71 0.42 B RR1 2 15:15:57.95 -00:11:23.4 m1 0.3325 17.81 0.40 B RR1 3 15:16:12.76 -00:10:03.3 m1 0.3300 17.70 0.50 B RR1 4 15:16:05.79 -00:11:12.7 m1 0.2864 17.69 0.48 B RR1 5 15:15:58.23 -00:05:47.4 m1 0.2524 17.70 0.30 B RR1 ===================================================================== Supplementary Notes and References Pal 5 is a sparsely populated cluster. According to Odenkirchen et al. (2003), tidal tails associated with Pal 5 can be traced over an arc of 10 degrees on the sky. The RA and dec in the above table are from Samus et al. (2009). The periods, magnitudes, amplitudes and variablity types in the above table are from Kinman & Rosino (1962 - Table 1). Vivas et al. (2004) derived periods that were significantly for V1, V3 and V4, but concluded that the periods of Kinman & Rosino (1962) were more reliable because their observartions were more extensive.. =================================================================== Discovery of the Variable Stars in Pal 5: V1-5 Rosino (1951) with x,y positions and ID chart. Rosino also identified 5 suspected variables s1-s5, but Kinman & Rosino (1962) did not find any evidence for variability in these stars. -------------------------------------------------------------------- Three additional RR Lyrae variables that might be associated with Pal 5 have been discovered in surveys by Vivas et al. (2004): QUEST #403 and #405 and by Wu et al. (2005): Wu #133. These variables all lie outside the tidal radius which is 7.58 arcmin according to the 2010 update of the Harris (1996) catalogue. However, they might be part of the tidal tail identified by Odenkirchen et al. (2003). =================================================================== References Harris, W. E. 1996, AJ, 112, 1487 Kinman, T. D. & Rosino, L. 1962, PASP, 74, 499 Odenkirchen, M., Grebel, E. K., Dehnen, W., Rix, H.-W., Yanny, B., Newberg, H. J., Rockosi, C. M. and 3 coauthors, 2003, AJ, 126, 2385 Prudil Z., Arellano Ferro, A. 2024, MNRAS, 534, 3654 Rosino, L. 1951, Mem. Soc. Ast. Ital., 22, 309 = Bologna Publ. V, No. 15 Samus, N. N., Kazarovets, E. V., Pastukhova, E. N., Tsvetkova, T. M., Durlevich, O. V. 2009, PASP, 121, 1378 Vivas, A. K., Zinn, R., Abad, C., Andrews, P., Bailyn, C., Baltay, C., Bongiovanni, A. and 28 coauthors, 2004, AJ, 127, 1158 Wu, C., Qiu, Y. L., Deng, J. S., Hu, J. Y., Zhao, Y. H. 2005, AJ, 130, 1640 =====================================================================