Terzan 5 / C1745-247 (Updated August 2019) RA: 17:48:04.80 DEC: -24:46:45 (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 17:48:03.80 -24:47:54.6 R0 245.0 14.3 1.5 I M Note 2 17:47:59.46 -24:47:17.6 R0 217.0 7.65 0.67 K M Note 3 17:48:05.14 -24:46:38.2 R0 0.6 -- 0.25 R RR0 4 17:48:05.06 -24:46:52.5 R0 0.291 -- 0.33 R E? 5 17:48:03.40 -24:46:42.0 R0 464.0 6.83 0.86 K M 6 17:48:09.25 -24:47:06.3 R0 269.0 7.50 0.61 K M 7 17:47:54.33 -24:49:54.6 R0 377.0 7.03 0.76 K M f? 8 17:48:07.18 -24:46:26.6 R0 261.0 7.44 0.80 K M 9 17:48:11.86 -24:50:17.1 R0 464.0 8.41 0.83 K M f 10 17:47:53.2 -24:44:34.0 R0 455.0 -- -- M f? 11 17:48:02.8 -24:47:47.5 R0 0.72 -- -- RR0 12 17:48:08.2 -24:45:42.1 R0 0.64 -- -- RR0 13 17:48:04.3 -24:47:37.7 R0 0.89 -- -- RR0 PSR A-Z; PSR aa-am PSR ======================================================================= Supplementary Notes Terzan 5 is a heavily reddened cluster in the galactic bulge. According to the 2010 update to the Harris (1996) catalogue, it has core, half-light and tidal radii of 10, 43 and 400 arcseconds respectively. Origlia et al. (2011) showed that Terzan 5 is a complex system that has two stellar populations with distinct iron abundances. Their result has been confirmed in subsequent studies which have also demonstrated that there is an age difference of several gigayears among the stars in Terzan 5. In a spectroscopic analysis of variable stars in the cluster, Origlia et al. (2019) showed that the population difference also occurs among the cluster's Mira variables. They discovered that one of the Miras is younger and more metal rich than the others. Most of the data in the above table are from the discovery papers by Spinrad et al. (1974), Edmonds et al. (2001), Sloan et al. (2010) and Origlia et al. (2019) respectively, unless indicated otherwise in the Notes on individual stars. Terzan 5 has more millisecond pulsars than any other globular cluster. ======================================================================== Notes on individual stars: V1: The RA and dec are from Samus et al. (2009). The remaining data are from Spinrad et al. (1974). V2: The RA and dec are from Samus et al. (2009). The remaining data are Sloan et al. (2010). V7, V10: The possible field status for these two variables is from Origlia et al. (2019), based on proper motions from the Gaia collaboration. Both are located more than 200 arcseconds from the the cluster centre where field contamination might be a factor. ======================================================================== Discovery of the variable stars in Terzan 5: V1-2 = V and V_S Spinrad et al. (1974) who labelled the stars on an ID chart The numbers V1 and V2 were assigned by Clement (1997) in the first electronic update of the Sawyer Hogg (1973) catalogue. V3-4 = V1 and V2 of Edmonds et al. (2001) who published RA, dec and finder charts The numbers V3 and V4 were assigned by Clement et al. (2001). V5-9 Sloan et al. (2010) who published RA and dec V10 = M6 This variable was announced by Origlia et al. (2019) who published its RA and dec. The number V10 has been assigned in this on-line catalogue. Origlia et al. noted that M6 was originally discovered by Matsunaga when he conducted an intensive search for Mira variables for his PhD thesis. They also claimed that M6 was V12 in the study by Sloan et al. (2010), but Sloan et al. did not list V12 in their paper. In their investigation, Origlia et al. also included the five previously known Mira variables which they numbered M1 to M5: M1=V2, M2=V6, M3=V8, M4=V5, M5=V7 V11-13 = RR1, RR2, RR3 Origlia et al. (2019) who published RA and dec Their search was carried out on 24 images obtained with the HST Wide Field Planetary Camera 2. They also recovered the previously known RR Lyrae variable, V3. The numbers V11-13 have been assigned in this on-line catalogue. ---------------------------------------------------------------------- PSR: According to Paulo Freire's website (August 2019), there are 38 millisecond pulsars in Terzan 5. (www.naic.edu/~pfreire/GCpsr.html) ======================================================================== References Clement, C. M. 1997, AAS Newsletter, 84, 15 Clement, C. M., Muzzin, A., Dufton, Q., Ponnampalam, T., Wang, J., Burford, J., Richardson, A., Rosebery, T. 2001, AJ, 122, 2587 Edmonds, P. D., Grindlay, J. E., Cohn, H., Lugger, P. 2001, ApJ, 547, 829 Harris, W. E. 1996, AJ, 112, 1487 Origlia, L., Mucciarelli, A., Fiorentino, G., Ferraro, F. R., Dalessandro, E., Lanzoni, B., Rich, R. M. and 3 coauthors, 2019, ApJ 871, 114 Origlia, L., Rich, R. M., Ferraro, F. R., Lanzoni, B., Bellazzini, M., Dalessandro, E., Mucciarelli, Valenti, E., & Beccari, G. 2011, ApJ 726, L20 Samus, N. N., Kazarovets, E. V., Pastukhova, E. N., Tsvetkova, T. M., Durlevich, O. V. 2009, PASP, 121, 1378 Sloan, G. C., Matsunaga, N., Matsuura, M., Zijlstra, A. A., Kraemer, K. E., Wood, P. R., Nieusma, J., Bernard-Salas, J., Devost, D., Houck, J. R. 2010, ApJ, 719, 1274 Spinrad, H., Smith, M. G., Harlan, E. 1974, ApJ, 192, 405 =======================================================================