NGC 6093 / C1614-228 / Messier 80 (Updated March 2010) RA: 16:17:02.41 DEC: -22:58:33.9 (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 or P (for photographic). 61-65 A5 Type of variable (draft 2006 GCVS classifications) NV denotes not variable 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 16:16:52.60 -22:57:15.9 R0 16.3042 14.19 1.3 B CW Note 2 16:17:04.22 -22:58:53.8 R0 ---- 14.88 0.5 B SR? Note 3 16:17:10.23 -22:57:37.9 R0 0.3457 16.32 0.6 B RR1 4 16:16:56.46 -22:57:34.0 R0 0.3865 16.34 0.6 B RR1 5 16:17:03.60 -22:59:40.7 R0 0.6640 16.41 1.1 B RR0 6 16:17:40.21 -22:53:35.8 R0 176.5 14.05 4.7 B M f;SSco 7 16:17:39.07 -22:56:40.4 R0 224.5 14.65 5.7 B M f;RSco 8 16:17:00.8 -22:58:18 R0 0.6618 16.25 1.0 B RR0 9 16:17:03.70 -22:57:58.6 R0 0.6642 16.3 1.0 B RR0 10 16:17:01.2 -22:58:34 R0 0.6141 15.7 0.9 B RR0 11 16:17:02.2 -22:58:37.9 R0 ---- 19.3 2.2 U UG? max 12 16:16:59.8 -22:58:18.0 R0 ---- 19.0 3.3 U UG? max 13 16:17:12.94 -22:58:49.3 R0 0.4974 -- -- RR1 14 16:16:55.30 -22:57:30.7 R0 0.3167 -- -- RR1 15 16:17:04.01 -22:58:40.4 R0 0.3474 -- -- RR1 16 16:17:04.62 -22:56:40.3 R0 0.3540 -- -- RR1 17 16:17:02.87 -22:58:32.6 R0 0.4277 -- -- RR1 Note 18 16:16:58.59 -22:58:35.2 R0 0.5968 -- -- RR0 19 16:17:02.07 -22:58:29.2 R0 0.7432 -- -- RR0 Note 20 16:17:03.26 -22:58:38.0 R0 0.8146 -- -- RR0 21 16:17:02.59 -22:58:07.2 R0 0.4165 -- -- RR1 22 16:17:06.75 -22:58:29.2 R0 0.0458 -- -- SXPHE 23 16:16:58.10 -22:57:44.1 R0 0.0459 -- -- SXPHE 24 16:17:03.01 -22:59:21.3 R0 0.0494 -- -- SXPHE 25 16:17:00.34 -22:56:20.8 R0 ---- -- -- SXPHE 26 16:17:04.48 -22:59:18.4 R0 ---- -- -- EC 27 16:17:04.03 -22:58:26.6 R0 ---- -- -- EC 28 16:17:01.88 -23:00:47.8 R0 ---- -- -- L f? 29 16:17:06.21 -22:58:36.9 R0 ---- -- -- L f 30 16:17:05.55 -22:57:42.6 R0 ---- -- -- SR? 31 16:17:05.20 -22:57:55.5 R0 ---- -- -- SR? 32 16:17:05.33 -22:58:41.4 R0 ---- -- -- SR? 33 16:17:02.16 -22:58:33.2 R0 0.0382 -- -- SXPHE Nova 16:17:02.82 -22:58:33.9 R0 ---- 6.8 -- V N max;TSco ==================================================================== Supplementary Notes and References The periods, magnitudes, amplitudes and variability types for V1-V10 are from Wehlau et al. (1990, AJ 99, 1159) and the RA and dec are from Samus et al. (2009, PASP 121, 1378). The data for V11-12 are from the discovery paper by Shara et al. (2005, ApJ 634, 1272) The data for V13-V32 are from Kopacki (2010, private communication). He is currently preparing a paper on the variable stars in this cluster. In a preliminary report (Kopacki 2009, Stellar Pulsation: Challenges for Theory and Observation, 194), he announced new variables, but the numbering system in that paper differs from his revised numbers which are the ones we list in the above table. The RA and dec for V33 are from Kopacki (2010, private communication) and the period and classification are from Dieball et al. (2010, ApJ 710, 332). It is their star #2238. The RA and dec for the Nova are from Dieball et al. (2010, ApJ 710, 332). It is their X-ray source CX01. The maximum visual apparent magnitude was derived by Sawyer (1938, JRASC 32, 69 - see page 75), based on the estimates of 7.0 and 6.5 by Auwers and Luther respectively, on May 21, 1860. Another study of the M80 variables is currently being carried out by G. C. Thomson, based on the data reported by Dieball et al. (2010, ApJ 710, 332). =================================================================== Notes on Individual Stars V1: Wehlau et al. (1984, IBVS 2586) pointed out that the y value that Sawyer Hogg listed for for V1 in her 2nd and 3rd catalogues was incorrect. It should have been +79 arcsec. V2: Wehlau et al. (1990, AJ 99, 1159) conclude that V2 belongs to the class of stars at the tip of the giant branch that show small variations in brightness. They also pointed out that the tentative period (24.9 days) published by Sawyer Hogg (1973) in her 3rd catalog was not confirmed in subsequent data. V17, V19: These two variables were independently detected as variables by Dieball et al. (2010, ApJ 710, 332). According to Kopacki (2010, private communication), Dieball #2324 = V17 and Dieball #2817 = V19. ======================================================= Discovery of the variable stars in M80: V1-2 Bailey, HA 38 (1902) with x,y position and ID chart (see Appendix page 237 for x,y tables and page 246 for description of plates). V3-6 Sawyer (1942, Publ David Dunlap Obs 1 No.12) with x,y positions and an ID chart. V6,V7 = S Sco, R Sco These are both Mira variables in the field and were discovered in 1853. The number V6 was assigned by Sawyer (1942, Publ DDO 1, No.12) and V7 by Sawyer (1955) in the 2nd edition of her catalogue. V8-10 Wehlau et al., IBVS 2586 (1984) with x,y coordinates ID charts for V1-10 were later published by Wehlau et al. (1990, AJ 99, 1159) V11&V12 = DN1&DN2 Shara et al. (2005, ApJ 634, 1272) with RA, dec and ID chart The numbers V11&V12 are assigned here. V13-V32 Kopacki (2010, private communication) In (2009, Stellar Pulsation: Challenges for Theory and Observation, p. 194) Kopacki announced new variables but the numbering system for the variables in that paper differs from his 2010 numbers that we list in the above table. Kopacki's (2009) V12-V19 correspond to V13-V20 in the revised system and his (2009) V20-V22 and V30 correspond to V22-V24 and V21 respectively in the revised system. V33 = Dieball #2238 The number V33 has been assigned by Kopacki (2010, private communication). Dieball et al. (2010, ApJ 710, 332) identified this star as a blue straggler and derived a period of approximately 55 minutes. They classified it as an SXPHE variable. These authors also identified two other variables, their #2324 and #2817 which were independently discovered by Kopacki and correspond to V17 and V19 in the above table. Nova = T Sco The nova was discovered in 1860. An account of its discovery was given by Sawyer (1938, JRASC 32, 69) and also by Wehlau et al. (1990, AJ 99, 1159) =========================================== Additional candidate variables Heinke et al. (2003,APJ 598, 516) identified 19 Chandra X-ray sources: CX1-CX19 in M80. They classified CX2 and CX6 as quiescent LMXBs and CX3, CX4, CX5 and CX15 as candidate cataclysmic variables. They also suggested that CX1 might be the X-ray counterpart of Nova 1860 and Dieball et al. (2010, ApJ 710, 332) concur. Moni Bidin et al. (2009, A&A 498, 737) identified a candidate EHB close binary in M80 (their star #16389).