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).
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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
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