NGC 6333 / C1716-184 / Messier 9 (Updated October 2013) RA: 17:19:11.26 DEC: -18:30:57.4 (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 17:19:18.32 -18:32:21.6 R0 0.5857 16.276 1.155 V RR0 2 17:19:14.77 -18:31:36.2 R0 0.6282 16.209 1.110 V RR0 3 17:19:26.41 -18:34:34.8 R0 0.6052 16.364 -- V RR0 amp>1.0 4 17:19:13.62 -18:31:39.6 R0 0.6713 16.168 1.017 V RR0 5 17:19:14.36 -18:31:12.5 R0 0.3788 16.256 0.449 V RR1 6 17:19:07.02 -18:31:20.9 R0 0.6068 16.351 1.000 V RR0 7 17:19:04.18 -18:32:24.4 R0 0.6285 16.566 1.120 V RR0 8 17:19:06.84 -18:32:42.8 R0 407.0 14.87 -- V SR f?;Note 9 17:19:35.41 -18:34:17.1 R0 0.3230 16.261 -- V RR1 amp>0.38 10 17:19:14.53 -18:30:39.7 R0 0.3198 16.285 0.449 V RR1 11 17:19:11.73 -18:31:14.8 R0 0.7424 16.065 0.704 V RR0 Note 12 17:18:52.69 -18:33:20.3 R0 1.3403 15.671 0.92 V AnCep 13 17:19:30.29 -18:30:54.6 R0 0.4799 17.681 1.183 V RR0 f 14 17:19:14.14 -18:31:20.3 R0 0.3271 16.253 0.443 V RR1 15 17:19:10.52 -18:29:59.2 R0 0.6418 16.239 0.971 V RR0 16 17:19:13.52 -18:30:43.0 R0 0.3847 16.073 0.336 V RR1 17 17:19:10.48 -18:31:20.4 R0 0.3176 16.243 0.375 V RR1 18 17:19:10.61 -18:30:41.9 R0 0.3413 16.187 0.39 V RR1 19 17:19:12.76 -18:30:38.2 R0 0.3668 16.264 0.47 V RR1? Note 20 17:19:11.09 -18:31:02.7 R0 0.3142 16.340 0.423 V RR1 21 17:19:09.85 -18:32:34.5 R0 0.7205 16.818 0.30 V EW 22 17:19:03.12 -18:35:31.1 R0 0.3508 16.483 0.510 V RR1 23 17:19:21.15 -18:30:10.2 R0 0.3047 16.513 0.311 V RR1 24 17:19:13.04 -18:27:39.4 R0 0.3668 17.381 0.45 V EW 25 17:19:25.94 -18:27:43.9 R0 ---- 17.111 1.642 V E max 26 17:19:13.84 -18:29:37.4 R0 ---- 17.380 -- V ? Note 27 17:18:56.40 -18:32:47.4 R0 ---- 17.069 -- V ? Note 28 17:19:11.68 -18:31:04.5 R0 ---- 13.216 -- V L amp>0.2 29 17:19:02.68 -18:32:53.6 R0 ---- 13.591 -- V L amp>0.2 30 17:19:11.83 -18:31:27.9 R0 ---- 13.342 -- V L amp>0.1 31 17:19:12.65 -18:31:01.7 R0 ---- 13.190 -- V L amp>0.1 32 17:19:37.10 -18:35:40.1 R0 0.3446 15.961 0.19 V EW 33 17:18:46.97 -18:25:29.5 R0 0.5760 17.920 0.517 V RR0 f 34 17:18:45.62 -18:28:52.0 R0 ---- 15.045 -- V L amp>0.1 ======================================================================= Supplementary Notes The most comprehensive study of the variables in M9 is a paper by Arellano Ferro et al. (2013). All of the material in the above table is from their study unless indicated otherwise in the notes. A serious problem in deriving the magnitudes and colours of the stars in M9 is that the cluster is subject to differential reddening. There is a heavy obscuring cloud to the southwest of the cluster. This can be detected on the photograph published by Clement et al. (1984) and is even more marked on the E and O plates of the Palomar Sky Survey. Arellano et al. (2013) used a reddening map by Alonso-Garcia et al. (2012) to correct for this effect. V3, V7, V12 and V13 appear in the Moscow GCVS as V1864, V1845, V1840 and V2208 Oph respectively. ===================================================================== Notes on individual stars V8: The period was derived by Clement et al. (1984) based on Sawyer's (1951) data. A period of 1.00027 days also fit the observations. However, in a later study, Clement & Shelton (1996) ruled out the one day period because the star did not vary during their 4-night observing run, even with observations that spanned more than 7 hours on one of the nights. It was therefore classified as a long period variable. Arellano Ferro et al. (2013) did not have enough observations to derive a period, but observed two minima that were separated by about 400 days. They concluded that V8 is not a cluster member, based on its extreme red colour compared with the other long period variables. V19: Arellano Ferro et al. (2013) noted that this star is a possible double mode RR Lyrae variable with the first overtone as the dominant mode. It appears that the fundamental mode oscillations are strong at some epochs and weak or non-existent at others, i.e. sometimes it is a double-mode pulsator and sometimes it is not. This conclusion is based on the fact that their secondary light curve, the plot of the residuals with the fundamental period, has a great deal of scatter. V26, V27: Arellano Ferro et al. (2013) found that these two stars vary on a long time scale, but their classification is uncertain. On the CM diagram, they are both located on the subgiant branch and not near the RG tip where one usually expects to observe longer period variables. Their properties are similar to the Omega Cen variables OGLE #22 and 31 (Kaluzny et al. 1996), later listed as V216 and V224 by Kaluzny et al. (2004). Kaluzny et al. derived periods in the 20-40 day range for these two stars. In their 1996 paper, they classified them as spotted variables and in 2004, they listed them as "LT". ====================================================================== Discovery of the variable stars in NGC 6333: V1 Shapley (1916) with delta RA and delta dec The number V1 was assigned by Sawyer (1951) who included it in her ID chart and derived its x,y coordinates. V2-13 Sawyer (1951) with x,y coordinates and an ID chart V14-21 Clement & Shelton (1996) with x,y coordinates and an ID chart V22-34 Arellano Ferro et al. (2013) with RA, dec and ID charts These authors published RA, dec and ID charts for all of the variables. ========================================================================== References Alonso-Garcia, J., Mateo, M., Sen, B., Banerjee, M., Catelan, M., Minniti, D., von Braun, K. 2012, AJ, 143, 70 Arellano Ferro, A., Bramich, D. M., Figuera Jaimes, R., Giridhar, S., Kains, N., Kuppuswamy, K., Jorgensen, U. G., and 33 coauthors, 2013, MNRAS, 434, 1220 Clement, C. M., Ip, P., Robert, N. 1984, AJ, 89, 1707 Clement, C.M. & Shelton, I. 1996, AJ, 112, 618 Kaluzny, J., Kubiak, M., Szymanski, A., Udalski, A., Krzeminski, W., Mateo, M. 1996, A&AS, 120, 139 Kaluzny, J., Olech, A., Thompson, I. B., Pych, W., Krzeminski, W., Schwarzenberg-Czerny, A. 2004, A&A, 424, 1101 Sawyer, H. B. 1951, Publ. DDO, 1, 24 Shapley, H. 1916, PASP, 28, 282 ===========================================================================