Terzan 5 / C1745-247 RA: 17:48:04.80 DEC: -24:46:45 (J2000) (Most recent updates: Membership probability flag - 2024; Remaining data - September 2025) ============================================================ 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 17:48:03.80 -24:47:54.6 f 245.0 14.3 1.5 I M Note 2 17:47:59.46 -24:47:17.6 m1 217.0 7.65 0.67 K M Note 3 17:48:05.13 -24:46:38.6 f 0.5909 18.367 0.57 I RR0 Note 4 17:48:05.06 -24:46:52.5 f 0.291 -- 0.33 R E? 5 17:48:03.40 -24:46:42.0 f 464.0 6.83 0.86 K M 6 17:48:09.25 -24:47:06.3 m1 269.0 7.50 0.61 K M 7 17:47:54.33 -24:49:54.6 u 377.0 7.03 0.76 K M f? 8 17:48:07.18 -24:46:26.6 m3 261.0 7.44 0.80 K M 9 17:48:11.86 -24:50:17.1 u 464.0 8.41 0.83 K M f 10 17:47:53.2 -24:44:34.0 u 455.0 -- -- M f? 11 17:48:02.8 -24:47:47.5 f 0.72 -- -- RR0 12 17:48:08.2 -24:45:42.1 m1 0.64 -- -- RR0 13 17:48:04.3 -24:47:37.7 m1 0.89 -- -- RR0 14 17:48:04.39 -24:46:41.7 u 120.37 14.656 0.28 I SR 15 17:48:04.61 -24:46:42.9 u 77.70 14.879 0.26 I SR 16 17:48:03.85 -24:46:39.3 u 41.9 16.173 0.18 I SR 17 17:48:04.68 -24:46:42.7 u 55.16 15.275 0.14 I SR G1 17:48:05.38 -24:46:58.4 u 110.51 14.735 0.46 I SR G2 17:48:04.51 -24:46:44.3 u 154.08 14.759 0.36 I SR G3 17:48:05.06 -24:46:60.0 u 48.64 15.270 0.25 I SR G4 17:48:05.31 -24:46:51.0 u 265.96 15.452 0.24 I SR G5 17:48:05.34 -24:46:46.3 u 110.04 15.114 0.21 I SR G6 17:48:05.06 -24:46:48.4 u 44.83 14.966 0.13 I SR G7 17:48:04.38 -24:46:46.0 u 20.40 15.268 0.10 I SR G8 17:48:05.43 -24:47:02.8 u 28.85 15.575 0.10 I SR G9 17:48:04.79 -24:46:41.3 u 48.48 -- -- I SR G10 17:48:03.50 -24:47:03.5 u 0.3018 15.618 0.11 I EW? G11 17:48:03.58 -24:46:59.3 u ---- 17.220 0.14 I LPV G12 17:48:04.51 -24:46:55.5 u ---- 16.448 0.16 I LPV G13 17:48:05.79 -24:46:40.7 u ---- 16.931 0.07 I LPV G14 17:48:04.95 -24:46:37.0 u ---- 15.717 0.08 I LPV G15 17:48:03.95 -24:46:39.3 u ---- 15.113 0.17 I LPV G16 17:48:04.10 -24:46:42.7 u ---- 15.250 0.10 I LPV G17 17:48:03.85 -24:46:42.4 u ---- 15.424 0.08 I LPV G18 17:48:06.11 -24:46:49.6 u ---- 15.480 0.11 I LPV G19 17:48:04.05 -24:47:02.6 u ---- 15.492 0.16 I LPV G20 17:48:05.30 -24:46:42.1 u ---- 15.637 0.09 I LPV G21 17:48:05.85 -24:46:45.8 u ---- 15.658 0.08 I LPV G22 17:48:05.09 -24:46:43.6 u ---- 15.683 0.10 I LPV G23 17:48:05.51 -24:46:53.7 u ---- 15.734 0.16 I LPV G24 17:48:06.10 -24:46:54.5 u ---- 15.742 0.20 I LPV G25 17:48:03.72 -24:46:47.0 u ---- 15.779 0.16 I LPV G26 17:48:04.34 -24:46:26.9 u ---- 15.804 0.22 I LPV G27 17:48:04.32 -24:46:37.3 u ---- 15.808 0.08 I LPV G28 17:48:04.23 -24:46:57.3 u ---- 15.918 0.20 I LPV G29 17:48:04.75 -24:46:56.7 u ---- 16.574 0.24 I LPV G30 17:48:05.70 -24:46:29.0 u ---- 16.622 0.13 I LPV G31 17:48:04.00 -24:46:53.0 u ---- 16.840 0.17 I LPV G32 17:48:06.07 -24:46:37.3 u ---- 16.913 0.22 I LPV G33 17:48:06.03 -24:46:30.1 u ---- 17.271 0.43 I LPV G34 17:48:03.71 -24:46:27.4 u ---- 18.195 0.60 I LPV CX3 17:48:05.21 -24:46:47.6 u ---- -- -- LMXB? Note N1 17:48:04.91 -24:46:53.2 u ---- -- -- Note PSR -- -- -- -- -- -- u ---- -- -- 49 msPs ======================================================================= 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 he data for V1-17 in the above table are from the discovery papers by Spinrad et al. (1974), Edmonds et al. (2001), Sloan et al. (2010), Origlia et al. (2019), and Figuera Jaimes et al. (2024), respectively, unless indicated otherwise in the Notes on individual stars. The data for G1-34 are from Figuera Jaimes et al. (2024). For their study, they observed a field of about 38 by 40 arcseconds in the centre of the cluster. No membership flags are listed for these stars in the above table because they were not included in the investigation by Prudil & Arellano Ferro (2024). However, since they are so close to the cluster centre, they are probably all members. 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). V3: This RR Lyrae variable was recovered in the study by Figuera Jaimes et al. (2024) and the data listed in the above table are from their investigation. 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. Neither star had data for Prudil & Arellano Ferro (2024) investigation. CX3: This is an X-ray source that has been classified as a low-mass X-ray binary (LMXB). In their paper, Figuera Jaimes et al. (2024) provided background information about previous observations of this object. Also, in their own I-band observations, they recorded an increase, followed by a decrease in brightness of the source between May 1 and June 9, 2015. N1: Figuera Jaimes et al. (2024) detected an outburst in their observations of this object on June 4, 2015. A literature survey indicated that the object might be associated with millisecond pulsar J1748-2446N. In their paper, they give a summary of radio and X-ray investigations of the object. ======================================================================== 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. V14-17 Figuera Jaimes et al. (2024) who published RA and dec (2000) and labelled them on an ID chart G1-34 These stars were all flagged as variables in the Gaia DR3 survey (Eyer et al. 2023). Their variability was confirmed by Figuera Jaimes et al. (2024) who assigned the numbers G1-34 and listed their Gaia source IDs. They also published RA and dec (2000) and labelled them on their ID chart. CX3, N1: See Notes on individual stars ---------------------------------------------------------------------- PSR: According to Paulo Freire's website at the Max Planck Institute in Bonn (July 2024 version), there are 49 millisecond pulsars in Terzan 5. ================================================================== 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 Eyer,L., Audard, M., Holl, B., Rimoldini, L., Carnerero, M. I., Clementini. G., De Ridder, J. and 54 co-authors, 2023, A&A, 674, A13 Figuera Jaimes, R., Catelan, M., Horne, K., Skottfelt, J., Snodgrass, C., Dominik, M., Jorgensen, U. G. and 16 co-authors, 2024, A&A, 689, A108 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 co-authors, 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 Prudil Z., Arellano Ferro, A. 2024, MNRAS, 534, 3654 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 =======================================================================