NGC 6093 / C1614-228 / Messier 80 (Updated July 2017) 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, 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 16:16:52.62 -22:57:16.1 R0 16.3042 13.365 -- V CW Note 2 16:17:04.22 -22:58:53.8 R0 ---- 13.31 -- V SR? Note 3 16:17:10.23 -22:57:38.0 R0 0.3457 16.144 0.418 V RR1 4 16:16:56.48 -22:57:34.2 R0 0.3864 16.164 0.430 V RR1 5 16:17:03.59 -22:59:40.4 R0 0.6642 16.180 0.931 V RR0 6 16:17:40.21 -22:53:35.8 R0 178.2010 10.46 3.75 V M f;max;Note 7 16:17:39.07 -22:56:40.4 R0 225.1432 9.94 5.2 V M f;max;Note 8 16:17:00.76 -22:58:17.1 R0 0.6618 16.070 1.097 V RR0 9 16:17:03.66 -22:57:58.7 R0 0.6641 16.833 0.927 V RR0 10 16:17:01.17 -22:58:34.6 R0 0.6140 -- -- RR0 Note 11 16:17:02.2 -22:58:37.9 R0 ---- 19.3 2.3 U UG? max;Note 12 16:16:59.8 -22:58:18.0 R0 ---- 19.0 3.3 U UG? max;Note 13 16:17:12.94 -22:58:49.3 R0 0.4974 -- -- V RR1 14 16:16:55.32 -22:57:30.9 R0 0.3164 16.180 0.134 V RR1 15 16:17:04.04 -22:58:40.2 R0 0.3479 -- -- RR1 16 16:17:04.61 -22:56:40.0 R0 0.3532 16.126 0.181 V RR1 multi P 17 16:17:02.88 -22:58:32.6 R0 0.4154 -- -- RR1 Note 18 16:16:58.60 -22:58:35.3 R0 0.4282 16.260 0.089 V RR1 19 16:17:02.11 -22:58:29.5 R0 0.5956 -- -- RR0 Note 20 16:17:03.26 -22:58:37.5 R0 0.7448 -- -- RR0 21 16:17:02.60 -22:58:06.9 R0 0.8143 15.967 0.494 V RR0 22 16:17:06.76 -22:58:29.4 R0 0.0458 18.170 0.298 V SXP 23 16:16:58.11 -22:57:44.1 R0 0.0459 18.838 0.112 V SXP 24 16:17:02.99 -22:59:21.1 R0 0.0494 18.259 0.099 V SXP Note 25 16:17:00.33 -22:56:20.9 R0 0.1394 21.821 0.340 V SXP? f?;Note 26 16:17:04.49 -22:59:17.9 R0 0.3190 19.280 0.147 V EW 27 16:17:04.02 -22:58:26.5 R0 0.4117 -- -- EW 28 16:17:01.89 -23:00:47.7 R0 2.14 19.306 0.166 V ? f? 29 16:17:06.22 -22:58:36.9 R0 2.421 17.870 0.115 V ? f 30 16:17:05.54 -22:57:42.6 R0 ---- 13.864 0.027 V SR? 31 16:17:05.24 -22:57:55.3 R0 ---- 13.520 0.037 V SR? 32 16:17:05.33 -22:58:41.5 R0 ---- 13.871 0.029 V SR? 33 16:17:02.16 -22:58:33.2 R0 0.0385 -- -- SXP Note 34 16:17:02.82 -22:58:33.8 R0 ---- 16.44 0.36 I ? Note 35 16:17:03.31 -22:58:33.2 R0 ---- 11.40 0.09 I L 36 16:17:03.15 -22:58:41.9 R0 ---- 11.50 0.12 I L 37 16:17:02.32 -22:58:30.5 R0 ---- 11.51 0.09 I L 38 16:17:03.26 -22:58:35.0 R0 ---- 11.70 0.04 I L 39 16:17:02.20 -22:58:34.5 R0 ---- 11.75 0.07 I L 40 16:17:03.04 -22:58:25.7 R0 ---- 12.36 0.13 I L Nova 16:17:02.82 -22:58:33.9 R0 ---- 6.8 -- V N max;TSco ==================================================================== Supplementary Notes The data for V1-33 are from Kopacki (2013) unless indicated otherwise in the notes on individual stars (e.g. V6, V7, V11, V12) The data for V34-40 are from Figuera Jaimes et al. (2016). For the Nova, the RA and dec are from Dieball et al. (2010). It is their X-ray source CX01. The maximum visual apparent magnitude was derived by Sawyer (1938 - see page 75), based on the estimates of 7.0 and 6.5 by Auwers and Luther respectively, on May 21, 1860. =================================================================== Notes on Individual Stars V1: Wehlau et al. (1984) pointed out that the y value that Sawyer Hogg listed for for V1 in her 2nd and 3rd catalogues (Sawyer 1955, 1973) was incorrect. It should be y = +79 arcsec (instead of +49). The period listed above is from Wehlau et al. (1990) and the mean V magnitude is from Kopacki (2013). Matsunaga et al. (2006) observed V1 in the JHK bands and confirmed Wehlau's period. In their paper, Matsunaga et al. listed incorrect values of RA and dec for V1. The values they listed were the RA and dec for V2. K magnitude observations of V1 were obtained with the Kepler space telescope. The results were reported by Plachy et al. (2016) who detected clear cycle-to-cycle variations in the light curve and period doubling in the pulsation. V2: The V magnitude listed for V2 in the above table is from the CM diagram (Fig 10) published by Kopacki (2013) which shows that the star is located at the RG tip. He derived the V magnitude by adding 0.61 to the value published by Alcaino et al. (1998) to match the photometric system of Stetson (2000). Kopacki did not detect any variability in V2 but pointed out this might have been due to the short length of his observing run. Wehlau et al. (1990) commented that V2 showed very little amplitude in either B or V and pointed out that the tentative period (24.9 days) published by Sawyer Hogg (1973) in her 3rd catalog was not confirmed in subsequent data. V6, V7: These two stars are S Sco and R Sco respectively. The RA and dec listed above are from Samus et al. (2009) and the remaining data are from the ASAS survey (Pojmanski 2002). The listed magnitudes are maximum V magnitudes. Both stars are considered to be field stars. V10: Figuera Jaimes et al. (2016) derived mean I = 14.25 mag for V10, which is a magnitude brighter than the values they derived for the three other RR Lyrae variables in their field: V17 (I=15.31), V19 (I=15.28), V20 (I=15.31). Since these stars are all located in the crowded central region of the cluster, it is assumed that they are all cluster members and that the anomalously bright magnitude for V10 is caused by an unresolved companion. Kopacki (2013) published V-filter light curves, expressed in flux units, for these four variables, but did not derive mean magnitudes. V11, V12: The data for V11-12 are from the discovery paper by Shara et al. (2005) V17, V19: These two stars were independently detected as variables by Thomson et al. (2010) who designated them as TDK1 (V19) and TDK3 (V17). Dieball et al (2010) designated them as #2324 and #2817. They were also observed by Figuera Jaimes et al. (2016) who derived mean I magnitudes of 15.31 and 15.28 respectively. V24: Kopacki (2013) found 2 periods for this star with period ratio f1/f2=0.98. He concluded that one of the modes is nonradial. Salinas et al. (2016) derived a mean r magnitude and amplitude 18.67 and 0.13 mag. V25: Kopacki (2013) tentatively classified this star as SX Phe, but pointed out that it could also be a W UMa or ellipsoidal binary system. If V25 in an SX Phe variable, it is probably not a cluster member since it is about 3 magnitudes fainter than the SX Phe variables, V22, V23 and V24. V33: The period and classification for V33 are from Thomson et al. (2010). It was their variable TDK#2. V34: Figuera Jaimes et al. (2016) detected a brightening in this star which is located at the position that Dieball et al. (2010) published for the Nova. It has not been determined whether or not this is associated with the Nova. ======================================================= Discovery of the variable stars in M80: V1-2 Bailey (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) with x,y positions and an ID chart. V6-7 = 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) and V7 by Sawyer (1955) in the 2nd edition of her catalogue. V8-10 Wehlau et al. (1984) with x,y coordinates ID charts for V1-10 were later published by Wehlau et al. (1990). V11-V12 = DN1&DN2 Shara et al. (2005 ) with RA, dec and ID chart The numbers V11&V12 are assigned here. V13-V32 Kopacki (2013) with RA and dec In a preliminary report, Kopacki (2009) announced his new variables, but used a different numbering system. In the above table, we use the numbers he assigned in his 2013 paper. V33 = Dieball et al. (2010) #2238 = TDK #2 of Thomson et al. (2010) The number V33 was assigned by Kopacki (2013) Dieball et al. (2010) and Thomson et al. (2010) identified this star as a blue straggler and derived a period of approximately 55 minutes. They classified it as an SX Phe variable. V34-40 Figuera Jaimes et al. (2016) with RA, dec and ID chart Nova = T Sco The nova was discovered in 1860. An account of its discovery was given by Sawyer (1938) and also by Wehlau et al. (1990). The RA and dec listed above are from Dieball et al. (2010) ---------------------------------------------------- Additional candidate variables Heinke et al. (2003) 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) concur. Moni Bidin et al. (2009) identified a candidate EHB close binary in M80 (their star #16389). ====================================================================== References Alcaino, G., Liller, W., Alvarado, F., Kravtsov, V., Ipatov, A., Samus, N., Smirnov, O. 1998, AJ, 116, 2415 Bailey, S. I. 1902, Harv. Ann., 38 Dieball, A., Long, K. S., Knigge, C., Thomson, G. S., Zurek, D. R. 2010, ApJ, 710, 332 Figuera Jaimes, R., Bramich, D. M., Skottfelt, J., Kains, N., Jorgensen, U. G., Horne, K., Dominik, M. and 26 coauthors, 2016, A&A, 588, A128 Heinke, C. O., Grindlay, J. E., Edmonds, P. D., Lloyd, D. A., Murray, S. S., Cohn, H. N., Lugger, P. M. 2003, ApJ, 598, 516 Kopacki, G. 2009, in Stellar Pulsation: Challenges for Theory and Observation, ed. J. A. Guzik and P. A. Bradley, AIP Conf. Proc., 1170, 194 Kopacki, G. 2013, Ac. A., 63, 91 Matsunaga, N., Fukushi, H., Nakada, Y., Tanabe, T., Feast, M. W., Menzies, J. W., Ita, Y. and 7 coauthors, 2006, MNRAS, 370, 1979 Moni Bidin, C., Moehler, S., Piotto, G., Momany, Y., Recio-Blanco, A. 2009, A&A , 498, 737 Plachy, E., Molnar, L., Jurkovic, M. I., Smolec, R., Moskalik, P. A., Pal, A., Szabados, L., Szabo, R. 2016, MNRAS, 465, 173 Pojmanski, G. 2002, Ac. A., 52, 397 Salinas, R., Contreras Ramos, R., Strader, J., Hakala, P., Catelan, M., Peacock, M. B., Simunovic, M. 2016, AJ, 152, 55 Samus, N. N., Kazarovets, E. V., Pastukhova, E. N., Tsvetkova, T. M., Durlevich, O. V. 2009, PASP, 121, 1378 Sawyer, H. B. 1938, JRASC, 32, 69 Sawyer, H. B. 1942, Publ. DDO, 1, 241 (No.12) Sawyer, H. B. 1955, Publ. DDO, 2, No. 2 Sawyer Hogg, H. 1973, Publ. DDO, 3, No. 6 Shara, M. M., Hinkley, S., Zurek, D. R. 2005, ApJ, 634, 1272 Stetson, P. 2000, PASP, 99, 191 Thomson, G. S., Dieball, A., Knigge, C., Long, K. S., Zurek, D. R. 2010, MNRAS, 406, 1084 Wehlau, A., Butterworth, S., Sawyer Hogg, H. 1990, AJ, 99, 1159 Wehlau, A., Gannon, P., Rice, P., Sawyer Hogg, H. 1984, IBVS, 2586 ===================================================================