NGC 6333 / C1716-184 / Messier 9 (Updated July 2012) 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 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 17:19:18.31 -18:32:21.7 R0 0.5857 16.232 1.205 V RR0 2 17:19:14.9 -18:31:36 R0 0.6282 16.172 1.163 V RR0 3 17:19:26.39 -18:34:34.9 R0 0.6054 16.540 1.320 B RR0 Note 4 17:19:13.8 -18:31:40 R0 0.6713 16.084 0.943 V RR0 5 17:19:14.5 -18:31:12 R0 0.3788 16.230 0.455 V RR1 6 17:19:07.1 -18:31:19 R0 0.6078 16.199 1.007 V RR0 7 17:19:04.16 -18:32:24.5 R0 0.6285 16.520 1.157 V RR0 8 17:19:06.84 -18:32:42.7 R0 407.0 16.45 -- B SR Note 9 17:19:35.40 -18:34:17.4 R0 0.3230 16.520 0.560 B RR1 Note 10 17:19:14.7 -18:30:39 R0 0.3199 16.258 0.469 V RR1 11 17:19:11.72 -18:31:15.2 R0 0.7363 16.85 0.90 B RR0 Note 12 17:18:52.68 -18:33:20.3 R0 1.3402 16.620 1.160 B CW Note 13 17:19:30.23 -18:30:55.0 R0 0.4799 17.450 0.480 B RR0 f;Note 14 17:19:14.12 -18:31:20.1 R0 0.3269 16.209 0.431 V RR1 15 17:19:10.42 -18:29:59.5 R0 0.6418 16.220 1.065 V RR0 16 17:19:13.55 -18:30:42.9 R0 0.3855 16.154 0.465 V RR1 17 17:19:10.46 -18:31:21.8 R0 0.3176 16.222 0.413 V RR1 18 17:19:10.6 -18:30:42 R0 0.3423 16.532 0.550 V RR1 19 17:19:12.75 -18:30:38.9 R0 0.3665 16.336 0.519 V RR1 20 17:19:11.0 -18:31:02 R0 0.3147 16.044 0.350 V RR1 21 17:19:09.75 -18:32:30.2 R0 0.3602 16.817 0.202 V EW ======================================================================= Supplementary Notes According to Clement et al. (1984), some of the variables in M9 are subject to differential reddening. There is a heavy obscuring cloud to the southwest of the cluster. It can be detected on their published photograph and is even more marked on plates E and O of the Palomar Sky Survey. The RA and dec for all the variables are from Samus et al. (2009). The remaining data are from Clement & Shelton (1999) unless indicated otherwise in the notes on individual stars. ===================================================================== Notes on individual stars V3, V9, V12, V13: These variables were outside of the field of view in Clement & Shelton's (1996, 1999) investigations. The periods, B magnitudes and amplitudes are from the photographic study by Clement et al. (1984). V3, V12 and V13 appear in the Moscow GCVS as V1864, V1840 and V2208 Oph respectively. V7 (V1845 Oph) is also in the GCVS. 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, based on the star's colour, (B-V) = 1.5, and the fact that it did not vary during the 4-night observing run of Clement & Shelton (1996), with observations that spanned more than 7 hours on one night, it was classified as a long period variable. The B magnitude listed above is from Clement & Shelton (1996 - see page 620). It may not represent the mean. V11: The data are from Clement & Shelton (1996). V magnitudes for V11 were obtained by Clement & Shelton (1999), but there was a gap in observations near the phase of maximum light so it was not possible to derive reliable values for mean V magnitude and amplitude. V12: This type II Cepheid is considered to be a cluster member even though it appears to be too faint. With a distance of approximately 5 arcminutes from the cluster centre, it is well within the tidal radius (~ 8 arcminutes). Its faintness is attributed to the obscuring cloud that lies to the southwest of the cluster. V13: This star is considered to be a field star because it is much fainter than the other RR Lyrae variables (even though is not in the region affected by the obscuring cloud) and does not fit their period-amplitude relation. ====================================================================== 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 ========================================================================== References Clement, C. M., Ip, P., Robert, N. 1984, AJ, 89, 1707 Clement, C.M. & Shelton, I. 1996, AJ, 112, 618 Clement & Shelton, ApJ 118, 453 (1999) Samus, N. N., Kazarovets, E. V., Pastukhova, E. N., Tsvetkova, T. M., Durlevich, O. V. 2009, PASP, 121, 1378 Sawyer, H. B. 1951, Publ. DDO, 1, 24 Shapley, H. 1916, PASP, 28, 282 ===========================================================================