Palomar 1 / C0325+799 (Updated May 2011) RA: 03:33:20.04 DEC: +79:34:51.8 (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 Variable searches of Pal 1 were carried out by Kinman & Rosino (1962) and by Ortolani & Rosino (1985). A VI color-magnitude diagram by Rosenberg et al. (1998a) does not indicate any obvious HB stars. Based on this and on the metal abundance they derived, [Fe/H]=-0.6, (1998, AJ 115, 658), Rosenberg et al. (1998b) concluded that Palomar 1 is a very young globular cluster. The young age (as much as 8 Gyr younger than 47 Tuc) was confirmed by Sarajedini et al. (2007) who also said they could not rule out the possibility that Palomar 1 has been misclassified as a globular cluster. An analysis by Monaco et al. (2011) indicated that the chemical abundance is similar to that of Galactic open clusters. They proposed that Pal 1 might be a globular cluster that experienced a peculiar chemical evolution or an open cluster ejected from the Galactic disk. From a study of tidal tails, Niederste-Ostholt et al. (2010) suggested that Pal 1 may have been accreted from a now disrupted dwarf galaxy about 500 Myr ago. ===================================================================== References Kinman, T. D. & Rosino, L. 1962, PASP, 74, 499 Monaco, L., Saviane, I., Correnti, M., Bonaficio, P., Geisler, D. 2011, A&A, 525, A124 Niederste-Ostholt, M., Belkurov, V., Evans, N. W., Koposov, S., Gieles, M., Irwin, M. J. 2010, MNRAS, 408, L66 Ortolani, S. & Rosino, L. 1985, Mem. S. A. I., 56, 113 Rosenberg, A., Saviane, I., Piotto, G., Aparicio, A., Zaggia, S. R. 1998a, AJ, 115, 648 Rosenberg, A., Piotto, G., Saviane, I., Aparicio, A., Gratton, R. 1998b, AJ, 115, 658 Sarajedini, A., Bedin, L. R., Chaboyer, B., Dotter, A., Siegel, M., Anderson, J., Aparicio, A., KIng, I., Majewski, S., Marin-Franch, A., Piotto, G., Reid, I. N., Rosenberg, A. 2007, AJ, 133, 1658 =====================================================================