NGC 6355 / C1720-263
RA: 17:23:58.59  DEC: -26:21:12.3 (J2000)

(Most recent updates: 
Membership probability flag - 2024; Remaining data - April 2016)
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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        17:23:54.04 -26:22:04.0 m2   0.5945 15.895 0.616 I RR0
2        17:23:56.14 -26:20:45.6 f    0.3517 16.149 0.255 I RR1
3        17:23:57.39 -26:20:53.1 m1   0.8641 15.845 0.286 I RR0
4        17:24:02.75 -26:21:01.3 m1   0.7106 15.814 0.509 I RR0
5        17:24:06.10 -26:21:20.8 m1   0.6402 15.965 0.696 I RR0
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Supplementary Notes 

NGC 6355 is embedded in a crowded field in the Galactic bulge.
Chen & Chen (2007) used the 2MASS Point Source Catalogue to study shapes
of clusters and concluded that NGC 6355 is suffering from strong tidal 
distortion.

According to the 2010 version of the Harris (1996) catalogue, NGC 6355
is a core collapsed cluster with [Fe/H] = -1.37. 

Soszynski et al. (2014) listed a radius of 2.1 arcminutes for NGC 6355
and the variable stars are all well within that boundary.  

BVI photometry was published by Ortolani et al. (2003). Their CM diagram 
shows a prominent blue HB.
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Discovery of the variable stars in NGC 6355

  V1-5 = OGLE-BLG-RRLYR-17494, OGLE-BLG-RRLYR-17497, 
         OGLE-BLG-RRLYR-17501,  OGLE-BLG-RRLYR-17508,  
         OGLE-BLG-RRLYR-17516  
       from the OGLE IV survey (Soszynski et al. 2014) with RA and dec

       These variables have magnitudes and colours appropriate for
       cluster membership according to the CM diagram published by
       Ortolani et al. (2003).
===============================================================
References

Chen, C. W. & Chen, W. P. 2007, in Island Universes, Structure and
Evolution of Disk Galaxies, ed. R. S. De Jong (Springer), 287

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

Ortolani, S., Bica, E., Barbuy, B. 2003, A&A, 402, 565 

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

Soszynski, I., Udalski, A., Szymanski, M. K., Pietrukowicz, P., Mroz,
P., Skowron, J., Kozlowski, S. and 6 coauthors,  2014, Ac. A. 64, 177

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