NGC 6333 / C1716-184 / Messier 9
RA: 17:19:11.26  DEC: -18:30:57.4  (J2000)

(Most recent updates: 
Membership probability flag - 2024; Remaining data - October 2013)
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Bytes  Format      Explanation
1-8      A8        Star ID
10-32  A11,1x,A11  Position
34-35    A2        Membership probability flag based on data published
                   by Prudil & Arellano Ferro (2024)
                    m1: prob >=0.85;  m2: prob >=0.7 and <0.85;
                    m3: prob >= 0.5 and <0.7; f: prob <0.5
                    u:  no data available
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               Mem   Period <mag>  ampl  C Type  Notes/
         RA          Dec        Flag                              Remarks
=========================================================================
1        17:19:18.32 -18:32:21.6 m1   0.5857 16.276 1.155 V RR0
2        17:19:14.77 -18:31:36.2 m1   0.6282 16.209 1.110 V RR0
3        17:19:26.41 -18:34:34.8 f    0.6052 16.364 --    V RR0   amp>1.0
4        17:19:13.62 -18:31:39.6 m1   0.6713 16.168 1.017 V RR0
5        17:19:14.36 -18:31:12.5 m1   0.3788 16.256 0.449 V RR1
6        17:19:07.02 -18:31:20.9 f    0.6068 16.351 1.000 V RR0
7        17:19:04.18 -18:32:24.4 m1   0.6285 16.566 1.120 V RR0
8        17:19:06.84 -18:32:42.8 f  407.0    14.87  --    V SR    f?;Note
9        17:19:35.41 -18:34:17.1 m1   0.3230 16.261 --    V RR1   amp>0.38
10       17:19:14.53 -18:30:39.7 m1   0.3198 16.285 0.449 V RR1
11       17:19:11.73 -18:31:14.8 f    0.7424 16.065 0.704 V RR0   Note
12       17:18:52.69 -18:33:20.3 m1   1.3403 15.671 0.92  V AnCep
13       17:19:30.29 -18:30:54.6 f    0.4799 17.681 1.183 V RR0   f
14       17:19:14.14 -18:31:20.3 f    0.3271 16.253 0.443 V RR1
15       17:19:10.52 -18:29:59.2 f    0.6418 16.239 0.971 V RR0
16       17:19:13.52 -18:30:43.0 f    0.3847 16.073 0.336 V RR1
17       17:19:10.48 -18:31:20.4 f    0.3176 16.243 0.375 V RR1
18       17:19:10.61 -18:30:41.9 m1   0.3413 16.187 0.39  V RR1
19       17:19:12.76 -18:30:38.2 m2   0.3668 16.264 0.47  V RR1?  Note
20       17:19:11.09 -18:31:02.7 f    0.3142 16.340 0.423 V RR1
21       17:19:09.85 -18:32:34.5 f    0.7205 16.818 0.30  V EW
22       17:19:03.12 -18:35:31.1 m1   0.3508 16.483 0.510 V RR1
23       17:19:21.15 -18:30:10.2 m1   0.3047 16.513 0.311 V RR1
24       17:19:13.04 -18:27:39.4 f    0.3668 17.381 0.45  V EW
25       17:19:25.94 -18:27:43.9 f  ----     17.111 1.642 V E     max
26       17:19:13.84 -18:29:37.4 m2 ----     17.380 --    V ?     Note
27       17:18:56.40 -18:32:47.4 f  ----     17.069 --    V ?     Note
28       17:19:11.68 -18:31:04.5 m1 ----     13.216 --    V L     amp>0.2
29       17:19:02.68 -18:32:53.6 f  ----     13.591 --    V L     amp>0.2
30       17:19:11.83 -18:31:27.9 m2 ----     13.342 --    V L     amp>0.1
31       17:19:12.65 -18:31:01.7 m1 ----     13.190 --    V L     amp>0.1
32       17:19:37.10 -18:35:40.1 f    0.3446 15.961 0.19  V EW
33       17:18:46.97 -18:25:29.5 f    0.5760 17.920 0.517 V RR0   f
34       17:18:45.62 -18:28:52.0 f  ----     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  

Prudil Z., Arellano Ferro, A. 2024, MNRAS, 534, 3654

Sawyer, H. B. 1951, Publ. DDO, 1, 24 

Shapley, H. 1916, PASP, 28, 282 
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