NGC5897 / C1514-208 (Updated March 2014) RA: 15:17:24.50 DEC: -21:00:37.0 (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 15:17:16.62 -21:03:59.6 R0 0.7973 16.21 0.73 V RR0 2 15:17:20.24 -21:02:13.5 R0 0.4539 16.26 0.24 V RR1 3 15:17:21.46 -21:00:41.3 R0 0.4199 16.37 0.52 V RR1 4 15:17:29.31 -21:00:14.9 R0 0.8313 -- -- RR0 blended 5 15:17:14.76 -20:56:57.7 R0 ---- 13.36 0.2 V SR Note 6 15:17:25.46 -20:59:37.6 R0 0.8562 16.26 0.45 V RR0 7 15:17:26.45 -21:00:00.7 R0 0.3489 16.32 0.20 V RR2? RR1? 8 15:17:28.42 -20:58:33.3 R0 0.3418 16.34 0.15 V RR2? RR1? 9 15:17:20.42 -21:02:38.9 R0 0.0506 18.75 0.44 V SXPHE Note 10 15:17:19.75 -21:00:25.9 R0 0.4984 16.10 0.48 V RR1? AC? 11 15:17:25.69 -20:59:46.6 R0 0.4623 16.23 0.16 V RR1 12 15:17:29.19 -21:03:11.3 R0 0.3333 16.34 0.23 V RR2? RR1? 13 15:17:24.47 -20:59:12.4 R0 0.3491 16.27 0.14 V RR2? RR1? ===================================================================== Supplementary Notes The RA and dec are from Samus et al. (2009). The remaining data are from Clement & Rowe (2001) unless indicated otherwise in the notes on individual variables. The RR2 classifications for V7, V8, V12, and V13 were made by Clement & Rowe (2001). However, these are now called into question. These four stars are probably first overtone pulsators. They all have periods and amplitudes comparable to Omega Cen variables that were previously considered to be RR2 variables. However, after Kaluzny et al. (2004) derived (B-V) colours for the Omega Cen variables, it was clear that these Omega Cen stars were RR1 variables. ====================================================================== Notes on individual stars: V5: The mean magnitude is from Wehlau (1990) and the amplitude, which might be a lower limit, is from Eggen (1972 - see page 661). V9: The period, magnitude, amplitude and classification are from Wehlau et al. (1996) Various investigators (Sarajedini 1992, Ferraro et al. 1992, Testa et al. 2001) have shown that NGC 5897 has a well populated blue straggler sequence. Up to now, V9 is the only known BSS variable in NGC 5897, but there are probably others. ================================================================== Discovery of the variable stars in NGC 5897: V1-4 Sawyer (1953) with x,y coordinates and an ID chart V5-7 Sandage & Katem (1968) with ID chart; the x,y coordinates were published by Sawyer Hogg (1973) in her 3rd catalogue. Wehlau & Sawyer Hogg (1979) later pointed out that V7 was incorrectly identified by Sandage & Katem (1969). V7 is actually SK#161 not SK#119. Corrected x,y coordinates were published by Clement & Rowe (2001). V8 = Star 63 of Sandage & Katem (1968) who suggested that it may vary. Wehlau & Sawyer Hogg (1979) confirmed the variation and assigned the number V8 and x,y coordinates were derived by Clement & Rowe (2001). V9 Wehlau et al. (1996) with ID chart and x,y coordinates V10-13 Clement & Rowe (2001) with ID chart and x,y coordinates for all of the variables except V5 and V9. ---------------------------------------------------------- Lynch & Ransom (2011) conducted a search for pulsars, but did not find any in NGC 5897 =============================================================== References Clement, C. M. & Rowe, J. F. 2001, AJ, 122, 1464 Eggen, O. J. 1972, ApJ, 172, 639 Ferraro, F. R., Fusi Pecci, F., Buonanno, R. 1992, MNRAS, 256, 375 Kaluzny, J., Olech, A., Thompson, I. B., Pych, W., Krzeminski, W., Schwarzenberg-Czerny, A. 2004, A&A, 424, 1101 Lynch, R. S. & Ransom, S. M. 2011, ApJ, 730, L11 Samus, N. N., Kazarovets, E. V., Pastukhova, E. N., Tsvetkova, T. M., Durlevich, O. V. 2009, PASP, 121, 1378 Sandage, A. & Katem, B. 1968, ApJ 153, 569 Sarajedini, A. 1992, AJ, 104, 178 Sawyer, H. B. 1953, JRASC, 47, 229 Sawyer Hogg, H. 1973, Publ. DDO, 3, No. 6 Testa, V., Corsi, C. E., Andreuzzi, G., Iannicola, G., Marconi, G., Piersimoni, A. M., Buonanno, R. 2001, AJ, 121, 916 Wehlau, A. 1990, AJ, 99, 250 Wehlau, A., Rucinski, S. M., Shi, J., Fahlman, G. G., Thompson, I. 1996, IBVS, 4394 Wehlau, A. & Sawyer Hogg, H. 1979, IBVS, 1606 =====================================================================