NGC 6388 / C1732-447
RA: 17:36:17.23 DEC: -44:44:07.8  (J2000)

(Most recent updates: 
Membership probability flag - 2024; Remaining data - January 2015)
============================================================
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        17:36:15.44 -44:44:15.2 m1 ----     --     --      M     LM
2        17:36:18.49 -44:44:19.2 f  ----     --     --      M     LM
3        17:36:15.04 -44:43:32.5 f  156.0     8.97  0.28  K M     Sl
4        17:35:58.94 -44:43:39.8 m1 253.0     8.47  0.80  K M     Sl;Note
5        17:36:23.43 -44:44:22.3 m1 ----     14.6   0.8   V L     LM
6        17:36:17.37 -44:45:46.0 m1 ----     15.35  0.7   V L     LM
7        17:36:08.13 -44:45:02.2 m1 ----     15.2   0.8   V L     LM
8        17:36:18.14 -44:43:24.5 f  ----     13.7   0.6   V L     LM
9        17:36:14.86 -44:43:12.2 m1 ----     15.75  0.3   V L     LM
10       17:36:20.97 -44:40:52.6 f  ----     14.45  0.5   V L     LM
11       17:36:16.37 -44:40:38.1 m1 ----     15.75  0.9   V L     LM
12       17:36:11.41 -44:44:07.9 m1 ----     14.6   0.6   V L     LM
13       17:36:56.51 -44:45:51.3 f  ----     17.1   --    B L     f?;HH
14       17:35:59.72 -44:49:24.2 f    2.16   16.179 1.30  V E     f?;Note
15       17:35:39.03 -44:39:36.3 f  ----     16.2   --    B E     f?;HH
16       17:35:52.22 -44:39:57.3 f    0.251  16.895 0.26  V RR1   Note
17       17:36:13.6  -44:44:33   f    0.611  16.525 0.85  V RR0
18       17:36:14.5  -44:43:21   f    2.89   15.616 0.77  V CW
19       17:36:21.12 -44:43:46.5 f  ----     --     --      CST   Note  
20       17:36:22.4  -44:43:28   f    0.467  16.787 0.36  V RR1
21       17:36:23.43 -44:41:49.7 m1   0.814  17.030 0.87  V RR0
22       17:36:23.7  -44:44:13   f    0.587  16.858 1.12  V RR0
23       17:36:00.12 -44:43:46.8 m1   0.338  16.893 0.48  V RR1
24       17:36:15.38 -44:36:28.8 f    0.322  16.8   0.6   B RR1   f?;HH
25       17:36:33.52 -44:45:48.0 f  ----     16.15  --    B L     HH
26       17:36:27.8  -44:45:14   m1   0.2390 17.403 0.38  V RR1   f?
27       17:36:22.80 -44:44:23.7 m1   0.365  16.953 0.46  V RR1   
28       17:36:19.4  -44:44:59   f    0.840  16.820 0.80  V RR0
29       17:36:15.32 -44:44:02.6 u    1.8652 14.63  0.77  I CWB   Sk
30       17:36:21.77 -44:44:17.0 m1   0.951  16.766 --    V RR0?  
31       17:36:28.67 -44:42:32.6 m1   0.341  17.031 0.52  V RR1   
32       17:36:13.57 -44:44:36.0 f    0.522  16.578 0.42  V RR1   
33       17:36:23.48 -44:42:44.5 m1   0.558  16.747 0.29  V RR1   
34       17:35:58.98 -44:44:53.5 m2   0.236  17.409 0.36  V RR1   f?
35       17:36:23.92 -44:40:39.7 m3   0.300  17.041 0.18  V RR1   
36       17:36:19.80 -44:43:51.6 m1   3.10   15.558 1.05  V CW
37       17:36:17.23 -44:44:31.6 f   10.0    14.707 --    V CW
38       17:36:16.47 -44:47:52.2 u    0.412  18.270 0.46  V EC    f?
39       17:36:27.16 -44:37:13.2 f    0.537  17.996 0.28  V EC    f?
40       17:36:23.67 -44:40:35.6 u    0.311  18.806 0.39  V EC    f?
41       17:36:55.12 -44:39:21.1 f    1.71   17.364 2.20  V E     f?     
42       17:36:40.36 -44:41:13.3 f    1.82   15.724 0.48  V E     f?
43       17:36:02.58 -44:43:45.3 m1   2.02   19.606 1.22  V E     f?
44       17:35:57.30 -44:44:40.5 f    0.080  18.082 0.50  V SX?   f?;DSct?
45       17:36:33.23 -44:39:23.8 u  ----     --     --      L
46       17:36:09.37 -44:44:43.5 m1 ----     --     --      L
47       17:36:43.71 -44:47:07.9 f  ----     --     --      L
48       17:36:19.79 -44:43:53.7 u    0.355  16.574 --    V RR1?  
49       17:36:18.11 -44:44:47.6 f    0.384  16.925 0.52  V RR1?  
50       17:36:15.13 -44:43:43.9 m1   0.364  16.898 0.54  V RR1?  
51       17:36:19.68 -44:44:34.4 f    0.397  16.604 0.34  V RR1?  
52       17:36:00.05 -44:47:22.5 u    0.387  16.686 0.23  V RR1?  
53       17:36:09.63 -44:43:30.8 m1   0.986  16.868 --    V RR0?  
54       17:35:58.00 -44:44:26.1 m2   0.366  19.447 0.67  V EC
55       17:36:18.53 -44:45:11.9 f    0.489  16.795 --    V RR1?  
56       17:36:15.08 -44:44:20.7 m1   0.552  16.825 --    V RR1?  
57       17:35:49.50 -44:40:52.5 u    0.278  19.116 0.80  V EC
58       17:36:14.58 -44:44:14.1 f    0.683  --     --    V RR0   Corw
59       17:36:17.87 -44:43:54.8 f    0.5888 15.48  0.39  I RR0   Sk
60       17:36:17.17 -44:44:24.4 u    0.3734 16.19  0.31  I RR1   Sk
61       17:36:16.00 -44:44:12.7 u    0.6559 15.94  0.83  I RR0   Sk
62       17:36:16.40 -44:44:07.9 m1   0.7113 15.79  0.51  I RR0   Sk
63       17:36:17.94 -44:44:09.5 m3   2.038  14.64  0.73  I CWB   Sk
64       17:36:16.96 -44:44:16.7 u    0.6014 15.35  0.43  I RR0   Sk
65       17:36:16.66 -44:43:50.6 f    0.3960 16.19  0.36  I RR1   Sk
66       17:36:16.17 -44:44:17.0 u    0.3499 15.25  0.19  I RR1   Sk
67       17:36:04.77 -44:45:21.7 u    2.27   --     --    V CW    Corw
68       17:36:18.23 -44:43:39.1 m1   0.946  --     --    V RR0?  Corw
69       17:36:17.44 -44:44:18.5 f    3.539  14.55  0.47  I CWB   Sk
70       17:36:17.54 -44:43:59.5 f   12.38   13.28  0.24  I CWA   Sk
71       17:36:17.75 -44:44:04.2 f    0.854  13.96  0.05  I RR0   Sk
72       17:36:17.53 -44:44:16.2 f   18.01   13.08  0.82  I CWA   Sk
73       17:36:17.21 -44:44:14.7 f   26.1    12.74  1.11  I CWA   Sk
74       17:36:15.45 -44:44:23.4 f    0.3584 15.96  0.12  I RR1?  
75       17:36:17.01 -44:44:17.8 u    0.4039 16.07  0.22  I RR1  
76       17:36:16.48 -44:44:01.3 f    0.7574 15.98  0.67  I RR0  
77       17:36:17.40 -44:44:14.1 f    1.8643 14.30  0.44  I AC  
78       17:36:15.37 -44:43:54.1 f   24.0    12.80  0.04  I SR  
79       17:36:17.45 -44:44:07.3 f   27.07   12.46  0.05  I SR  
80       17:36:17.29 -44:44:18.5 f   30.28   12.86  0.20  I RV 
81       17:36:16.69 -44:44:23.0 f   33.78   12.58  0.08  I SR  
82       17:36:17.84 -44:43:56.9 f   40.47   12.89  0.06  I RV 
83       17:36:15.52 -44:44:26.4 m3  50.68   12.42  0.15  I SR  
84       17:36:15.89 -44:44:04.6 f   55.5    12.85  0.05  I SR  
85       17:36:16.96 -44:43:59.0 m2  56.8    13.03  0.07  I SR  
86       17:36:18.20 -44:44:00.4 f   57.0    12.75  0.08  I SR  
87       17:36:18.10 -44:44:16.7 m1  58.3    12.99  0.04  I SR  
88       17:36:16.09 -44:44:09.4 f   58.3    12.20  0.35  I SR  
89       17:36:16.93 -44:44:23.8 f   70.7    12.42  0.11  I SR  
90       17:36:16.78 -44:44:01.9 f   70.8    12.34  0.14  I SR  
91       17:36:17.29 -44:44:06.9 f  113.9    12.65  0.05  I SR  
92       17:36:15.31 -44:44:11.2 f  114.2    12.60  0.65  I SR  
93       17:36:17.55 -44:44:08.7 m1 157.0    11.97  0.43  I SR  
94       17:36:17.90 -44:44:21.6 m1 177.0    13.34  0.06  I SR  
95       17:36:15.41 -44:44:14.9 m1 180.0    11.91  1.06  I SR  
96       17:36:18.43 -44:44:19.1 f  ----     12.51  1.55  I L  
97       17:36:17.11 -44:43:57.9 f  ----     12.43  0.84  I L  
98       17:36:17.11 -44:44:00.4 f  ----     12.52  0.60  I L  
99       17:36:17.59 -44:44:08.0 m1 ----     12.37  0.35  I L  
100      17:36:17.21 -44:44:14.0 f  ----     12.53  0.34  I L  
101      17:36:17.73 -44:44:13.6 f  ----     12.58  0.26  I L  
102      17:36:15.97 -44:43:48.6 m1 ----     12.54  0.21  I L  
103      17:36:17.24 -44:44:08.8 f  ----     12.13  0.20  I L  
104      17:36:17.40 -44:44:08.4 f  ----     12.07  0.15  I L  
105      17:36:17.46 -44:44:13.5 f  ----     12.27  0.14  I L  
106      17:36:16.41 -44:44:10.9 f  ----     12.28  0.12  I L  
107      17:36:17.73 -44:44:22.1 f  ----     12.41  0.12  I L  
108      17:36:18.89 -44:44:04.2 f  ----     12.68  0.12  I L  
109      17:36:18.93 -44:44:14.1 m2 ----     12.63  0.09  I L  
110      17:36:18.04 -44:44:17.6 m1 ----     12.38  0.08  I L  
111      17:36:16.78 -44:44:07.0 f  ----     12.73  0.08  I L  
112      17:36:17.87 -44:44:03.2 f  ----     12.88  0.07  I L  
113      17:36:18.00 -44:43:52.7 f  ----     13.35  0.06  I L  
114      17:36:16.14 -44:44:04.6 m1 ----     12.71  0.05  I L  
115      17:36:17.17 -44:44:05.7 f  ----     12.11  0.04  I L  
116      17:36:18.92 -44:43:56.8 m1 ----     13.24  0.04  I L  
117      17:36:17.23 -44:44:04.4 m3 ----     12.83  0.04  I L  
118      17:36:17.15 -44:44:10.9 f  ----     12.95  0.04  I L  
119      17:36:18.09 -44:44:08.6 f  ----     12.53  0.05  I L? 
120      17:36:17.34 -44:43:53.9 f  ----     --     --      ?  
121      17:36:17.58 -44:43:50.6 f  ----     --     --      ?  
=========================================================================
Supplementary Notes 

NGC 6388 is a massive Galactic bulge cluster with [Fe/H]= -0.55
according to the 2010 version of the Harris (1996) catalogue.  Pritzl et
al. (2002) discovered that it had a significant number of RR Lyrae
variables with relatively long periods, an unexpected result for such a 
metal rich cluster.  NGC 6388 shares these properties with NGC 6441.
Bellini et al. (2013) have examined the CM diagrams for both clusters
and provided evidence that both clusters host at least two stellar
populations.

The RA and dec in the above table are from the following sources:
  V1-26 and V28 from Samus et al. (2009).  
  V70-121 and the variables indicated by "Sk" in the remarks column 
     from Skottfelt et al. (2015).

For the remaining variables, the RA and dec were derived from the Delta RA 
and Delta dec coordinates published by Pritzl et al. (2002) or by Corwin 
et al.  (2006).  For these calculations, it was assumed that the position 
of the cluster centre was RA=17:36:17.15 and dec=-44:44:06.9.  These 
coordinates for the cluster centre yielded RA and dec in agreement with
the values that Samus et al. derived for V1-26 and matched with the
2MASS catalogue. 

The remaining data for V1-73 in the above table are from Pritzl et al.  
(2002) unless designated LM, Sl, HH, Corw or Sk in the remarks column:
in which case they are from 
       LM    Lloyd Evans & Menzies (1977), 
       Sl    Sloan et al.  (2010), 
       HH    Hazen & Hesser (1986), 
       Corw  Corwin et al. (2006) or 
       SK    Skottfelt et al.  (2015). 
Most of the "HH" variables are considered to be field variables because 
they are outside the tidal radius which is 6.75 arcmin according to the 
2010 version of the Harris (1996) catalogue.

All the data for V74-V121 are from the discovery paper by Skottfelt et
al. (2015).

==========================================================================
Notes on individual stars

V4:  Samus et al. (2009) pointed out that V4 is MU Sco in the GCVS and
     HV 6570.  Its variability was announced by Shapley & Swope (1940). 

V14, V16:
     There is a difference of 6 arcsec between the y coordinates
     derived by Hazen & Hesser (1986) and by Pritzl et al. (2002) for 
     these two stars.  However, it appears that they indicate the same stars
     on their ID charts.  The RA and dec in the above table were derived
     by Samus et al. (2009) who matched both stars with 2MASS sources.

V19: It appears unlikely that this star is variable because Corwin et
     al. (2006) did not detect any variability when they applied image
     subtraction to their observations.  Furthermore, when Hazen & Hesser 
     (1986) "discovered" its variability, they noted  that it was part of 
     a close pair and indicated that the star varied on a time scale of 
     less than 2 days. Variability on such a short time scale should have 
     been detected by Pritzl et al. (2002) or by Corwin et al. (2006). 
==========================================================================
Discovery of the variable stars in NGC 6388:

   V1-9 = 
      V1-4, V6-8, V10-11 of Lloyd Evans & Menzies (1973)
      who labelled them on an ID chart.  The numbering system
      V1-9 was assigned by Sawyer Hogg (1973) in her 3rd catalogue.
 
   V10-12
      Lloyd Evans & Menzies (1977) with an ID chart for V1-12

   V13-26
      Hazen & Hesser (1986) with x,y coordinates and an ID chart for
      V3-V26. (V1 and V2 were too close to the centre on their
      photographs.)  Hazen & Hesser also discovered 4 field variables
      that they numbered F1-4.

   V27-29
      Silbermann et al. (1994) with x,y coordinates and ID charts
      They also announced 4 suspected variables, three of which, S1-3,
      were later confirmed by Pritzl et al. (2002) and numbered V32, V49 
      and V53.  Pritzl et al. were unable to find any variation in S4,
      but noted that crowding might have been an issue.  However, no
      variation was detected by Corwin et al. when they applied the image
      subtraction technique to the observations.

   V30-57
       Pritzl et al. (2002) with x,y in pixels and arcsec, and ID charts

   V58-69 
      Corwin et al. (2006) with x,y coordinates in arcsec
      These authors also published data for six "suspected" variables 
      which they numbered SV1-SV6.

   V70-73 = SV1, SV2, SV4, SV5 of Corwin et al. (2006)
      The numbers V70-73 were assigned by Skottfelt et al. (2015) 
      who confirmed their variability, derived RA and dec and published
      a finding chart.
     
   V74-121
      Skottfelt et al. (2015) with RA, dec and a finding chart.
-------------------------------------------------------------------------
Dalessandro et al. (2008) identified a substantial population of BS
stars from HST observations, but they did not search for variability in 
their data.
==================================================================
References

Bellini, A., Piotto, G., Milone, A. P., King, I. R., Renzini, A.,
Cassisi, S., Anderson, J. and 3 coauthors, 2013, ApJ, 765, 32

Corwin, T. M., Sumerel, A. N., Pritzl, B., Smith., H. A., Catelan, M.,
Sweigart, A. V., Stetson, P. B. 2006, AJ 132, 1014 

Dalessandro, E., Lanzoni, B., Ferrarro, F. R., Rood, R. T., Milone, A.,
Piotto, G., Valenti, E. 2008, ApJ, 677, 1069

Harris, W. E. 1996, AJ, 112, 1487

Hazen, M. L. & Hesser, B. H. 1986, AJ, 92, 1094 

Lloyd Evans, T. & Menzies, J. W. 1973,  IAU Colloq, 21, Variable Stars
in Globular Clusters and in Related Systems, 151 

Lloyd Evans, T. & Menzies, J. W. 1977, MNRAS, 178, 163 

Pritzl, B. J., Smith, H. A., Catelan, M., Sweigart, A. V. 2002, 
AJ, 124, 949 

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

Sawyer Hogg, H. 1973,  Publ. DDO, 3, No.  6

Shapley, H. & Swope, H. H. 1940, Harv. Ann., 90, 177

Silbermann, N. A., Smith, H. A., Bolte, M., Hazen, M. L. 1994, AJ, 107,
1764

Skottfelt, J., Bramich, D. M., Figuera Jaimes, R., Jorgensen, U. G.,
Kains, N., Arellano Ferro, A., Alsubai, K. A. and 27 coauthors, 2015, 
A&A, 573, A103

Sloan, G. C., Matsunaga, N., Matsuura, M., Zijlstra, A. A., Kraemer, K.
E., Wood, P. R., Nieusma, J., Bernard-Salas, J., Devost, D., Houck, J. R. 
2010, ApJ, 719, 1274
=====================================================================