ESO 452-SC11 / C1636-283
RA: 16:39:25.45 DEC: -28:23:55.3 (J2000)

(Most recent updates: 
Membership probability flag - 2024; Remaining data - September 2018)
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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
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ID       Position               Mem   Period <mag>  ampl  C Type  Notes/
         RA          Dec        Flag                              Remarks
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No known variables.
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Supplementary Notes 

    Bica et al. (1999) published a VI color-magnitude diagram and 
    confirmed that this object is a poorly populated globular cluster 
    with evidence of depletion at the lower main sequence. Their HB
    had a red ccomponent along with some bluer stars. Subsequently, 
    Cornish et al. (2006) published a VI CMD and found the features were 
    consistent with the Bica et al. diagram. 
    A [g vs g-z] CM diagram published by Simpson et al. (2017) included 
    11  stars known to be cluster members; 8 of them were on the RGB or 
    AGB and the other 3 were red HB stars.

    The cluster is relatively metal rich according to spectroscopic 
    observations of red giants by Koch et al. (2017): [Fe/H]=-0.88  
    and by Simpson et al. (2017): [Fe/H] ~-0.8.
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References

Bica, E., Ortolani, S., Barbuy, B. 1999, A&A Supp., 136, 363

Cornish, A. S. M., Phelps, R. L., Briley, M. M., Friel, E. D. 2006,
AJ, 131, 2543

Koch, A., Hansen, C. J., Kunder, A. 2017, A&A, 604, A41

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

Simpson, J. D., De Silva, G., Martell, S. L., Navin, C. A., Zucker, D.
B. 2017, MNRAS, 472, 2856
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