NGC 6229 / C1645+476 (Updated July 2016) RA: 16:46:58.79 DEC: +47:31:39.9 (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 16:46:56.34 +47:29:53.3 R0 0.5857 17.936 1.16 V RR0 2 16:46:51.62 +47:31:43.5 R0 0.5552 18.07 1.01 V RR0 3 16:46:39.38 +47:32:19.3 R0 0.5753 18.13 0.89 V RR0 4 16:46:53.12 +47:31:24.3 R0 0.5662 18.09 0.86 V RR0 5 16:47:00.11 +47:32:23.0 R0 0.5336 18.160 1.05 V RR0 6 16:47:03.03 +47:32:20.7 R0 0.5593 18.08 0.85 V RR0 7 16:46:54.60 +47:30:48.8 R0 0.5070 18.02 1.15 V RR0 8 16:46:58.33 +47:30:56.9 R0 14.846 15.50 0.75 V CW 9 16:46:54.85 +47:32:17.0 R0 0.5428 17.95 0.86 V RR0 10 16:46:55.76 +47:32:51.4 R0 0.5547 18.101 1.00 V RR0 11 16:47:01.08 +47:31:14.1 R0 0.5632 18.119 0.92 V RR0 12 16:47:02.11 +47:31:15.4 R0 0.4908 17.91 1.16 V RR0 13 16:47:12.51 +47:32:41.0 R0 0.5473 18.106 0.93 V RR0 14 16:46:57.21 +47:30:48.1 R0 0.4659 17.840 1.04 V RR0 15 16:47:02.07 +47:32:06.7 R0 0.2714 18.12 0.52 V RR1 16 16:47:03.36 +47:31:15.0 R0 0.3228 17.98 0.49 V RR1 17 16:46:49.25 +47:30:23.4 R0 0.3251 17.91 0.46 V RR1 18 16:46:55.13 +47:32:11.0 R0 0.5790 18.066 0.79 V RR0 19 16:47:03.99 +47:30:54.9 R0 0.4760 18.130 1.29 V RR0 20 16:46:56.03 +47:31:02.8 R0 0.4660 18.17 1.30 V RR0 21 16:47:10.32 +47:30:38.0 R0 0.5644 18.063 0.98 V RR0 22 16:46:58.95 +47:31:28.1 R0 15.8373 15.28 0.88 V CW 23 16:46:56.72 +47:32:36.0 R0 0.3977 17.868 0.38 V RR1 24 16:46:57.45 +47:30:40.5 R0 0.3034 18.016 0.44 V RR1 25 16:46:57.9 +47:31:35 R0 ---- -- -- CST Sam 26 16:46:58.4 +47:31:50 R0 ---- -- -- CST Sam 27 16:46:59.85 +47:31:46.1 R0 ---- 16.83 0.49 V CW? Note 28 16:46:59.5 +47:31:29 R0 ---- -- -- CST Sam 29 16:47:00.39 +47:31:41.5 R0 0.6295 18.30 1.50 RR0 30 16:46:58.63 +47:31:23.3 R0 0.4987 18.7 0.70 RR0 31 16:46:59.30 +47:31:18.9 R0 0.5379 17.77 0.88 V RR0 32 16:46:58.34 +47:31:17.7 R0 0.6038 18.17 0.61 V RR0 33 16:46:58.24 +47:32:01.1 R0 0.5175 18.26 1.24 V RR0 34 16:47:01.43 +47:31:44.7 R0 0.5554 18.14 0.99 V RR0 35 16:47:01.53 +47:31:57.2 R0 0.6345 18.062 0.31 V RR0 36 16:46:56.51 +47:32:02.9 R0 0.2641 17.942 0.32 V RR1 37 16:46:58.87 +47:32:11.9 R0 0.5192 17.947 0.83 V RR0 38 16:46:57.09 +47:31:11.4 R0 0.5222 18.06 1.06 V RR0 39 16:47:03.05 +47:31:08.1 R0 0.3330 18.113 0.42 V RR1 40 16:47:02.37 +47:31:58.8 R0 0.5914 17.58 0.51 V RR0 41 16:47:02.78 +47:31:30.4 R0 0.6346 18.12 0.42 V RR0 42 16:47:01.30 +47:32:00.9 R0 0.6217 18.07 0.50 V RR0 43 16:46:56.99 +47:32:01.8 R0 0.5676 17.94 1.14 V RR0 44 16:47:00.57 +47:30:51.6 R0 0.3574 17.988 0.45 V RR1 45 16:46:59.18 +47:30:22.2 R0 0.6401 18.027 0.48 V RR0 46 16:46:53.97 +47:31:24.8 R0 0.6387 17.965 0.28 V RR0 47 16:47:03.40 +47:31:26.5 R0 0.3339 17.80 0.36 V RR1 48 16:47:01.46 +47:31:20.0 R0 0.3403 17.85 0.38 V RR1 49 16:46:54.75 +47:32:36.5 R0 0.6373 18.08 0.35 V RR0 50 16:46:56.78 +47:31:43.9 R0 0.4924 18.11 1.25 V RR0 51 16:46:57.21 +47:31:27.4 R0 0.5481 16.66 0.26 V RR0 52 16:46:57.98 +47:32:02.3 R0 0.4917 18.13 1.05 V RR0 53 16:46:58.62 +47:33:41.4 R0 0.6252 18.12 0.36 V RR0 54 16:46:59.20 +47:31:50.2 R0 0.5704 17.90 0.73 V RR0 55 16:46:59.48 +47:31:18.1 R0 0.5252 18.00 1.19 V RR0 56 16:46:59.70 +47:31:52.6 R0 0.6383 18.04 0.41 V RR0 57 16:47:00.25 +47:31:31.2 R0 0.5616 18.22 0.99 V RR0 58 16:47:00.34 +47:32:14.6 R0 0.6395 17.319 0.30 V RR0 blend? 59 16:46:34.04 +47:32:26.0 R0 0.3358 18.0 0.55 V RR1 60 16:46:55.27 +47:31:31.0 R0 0.2604 18.016 0.38 V RR1 61 16:46:56.59 +47:31:41.6 R0 0.3431 17.67 0.31 V RR1 62 16:46:59.52 +47:32:02.2 R0 0.2990 17.48 0.27 V RR1 63 16:47:00.41 +47:31:27.6 R0 0.3417 16.750 0.12 V RR1 Note;Blend 64 16:46:55.87 +47:31:59.9 R0 ---- 15.42 0.29 V SR 65 16:46:58.11 +47:31:20.5 R0 ---- 15.22 0.17 V SR 66 16:46:59.01 +47:31:58.0 R0 ---- 15.04 0.33 V SR 67 16:47:00.83 +47:31:41.3 R0 1.5155 17.12 1.35 V CW? AnonC? 68 16:46:52.57 +47:33:23.1 R0 0.0385 20.49 0.4 V SXPHE 69 16:47:01.85 +47:32:13.3 R0 0.2713 20.46 0.22 V ? 70 16:46:54.22 +47:33:37.2 R0 ---- 15.18 0.36 V SR 71 16:46:58.58 +47:31:36.9 R0 ---- 15.22 0.39 V SR 72 16:47:02.81 +47:30:21.2 R0 ---- 15.35 0.12 V SR Note 73 16:47:00.85 +47:31:43.4 R0 ---- 16.62 -- V CW? Note ====================================================================== Supplementary Notes The data in the above table are all from Arellano Ferro et al. (2015) - except for the stars classified as "CST". For these stars, "Sam" in the remarks column indicates that the RA and dec are from Samus et al. (2009). ====================================================================== Notes on individual stars V27, V73: Arellano Ferro et al. (2015) found that these two variables were located in the region of the CMD where type II Cepheids are located but they were unable to derive satisfactory periods. A period of 1.13827 days derived by Borissova et al. (2001) for V27 did not fit their data. V63: This RR1 variable is brighter and redder than the other RR Lyrae variables in the cluster. Also, its amplitude is low for its period. These facts indicate that the image of V63 is blended with that of a brighter star on the red giant branch. For example, if the red giant has V=17.15, then the actual mean magnitude and amplitude of V63 would be V ~ 18.1 and Vamp ~ 0.4 in good agreement with the other RR1 variables in the cluster. V58 is another RR Lyrae variable that appears to be affected by blending. V72: According to Ochsenbein (2016, private communication), this is star IV-12 of Searle & Zinn (1978). Carney et al. (1991) suggested that it appeared to be variable. They listed its x,y pixel coordinates in section 2.4 of their paper. ======================================================================= Discovery of the variable stars in NGC 6229: V1-21 Baade (1945) with x,y coordinates and an ID chart V8 had been previously announced by Davis (1917) with delta RA and delta dec values listed V22 Sawyer (1953) with x,y coordinates V23-24 = suspected RR Lyrae variables: star #88 and #155 of Carney et al. (1991) who listed x,y pixel coordinates for locating the stars on their published chart The numbers V23, 24 were assigned by Borissova et al. (2001) who published x,y coordinates and identified them on an ID chart. Carney et al. (1991) listed two other possible RR Lyrae candidates (their #104 and #134), but Borissova et al. (2001) did not detect any variability in these stars. V25-36 = stars #1-12 Spassova & Borissova (1996) with x,y coordinates and an ID chart The x,y coordinates they listed for three of the stars: #3, 4 and 5 are incorrect. They do not correspond to the positions on their chart which are the positions adopted by Borissova et al. (2001) in their subsequent, definitive study of the variables in NGC 6229. Samus et al. (2009) based their RA and dec on the chart published by Borissova et al. (2001). Borissova et al. (1997) also listed the Spassova & Borissova (1996) x,y coordinates for these candidate variables, but the x,y coordinates were interchanged in the 1996 paper, so they are incorrect. V37-48 Borissova et al. (2001) with x,y coordinates and an ID chart. These authors labelled all the variables V1-48 (except V3 which was outside their field of view) on their finding chart. V49-73 Arellano Ferro et al. (2015) with RA, dec and finding charts ---------------------------------------------------------------------------- A possible long period variable Carney et al. (1991) noted that two stars near the RG tip in the CMD: their #4 and star IV-12 of Searle and Zinn (1978) might be long period variables (see section 2.4 on page 1701 and section 3.2 on page 1713 of Carney's paper.) Arellano Ferro et al. (2015) observed star #4, and did not detect any variability. Star IV-12 is their V72. ============================================================================ References Arellano Ferro, A., Mancera Pina, P. E., Bramich, D. M., Giridhar, S., Ahumada, J. A., Kains, N., Kuppuswamy, K. 2015, MNRAS, 452, 727 Baade, W. 1945, ApJ, 102, 17 Borissova, J., Catelan, M., Spassova, N., Sweigart, A. V. 1997, AJ, 113, 692 Borissova, J., Catelan, M., Valchev, T. 2001, MNRAS, 324, 77 Carney, B. W., Fullton, L. K., Trammell, S. R. 1991, AJ 101, 1699 Davis, H. 1917, PASP, 29, 260 Sawyer, H. B. 1953, JRASC, 47, 229 Searle, L. & Zinn, R. 1978, ApJ, 225, 357 Spassova, N. & Borissova, J. 1996, IBVS, 4296 ========================================================================