Terzan 4 / C1727-315
RA: 17:30:39.00  DEC: -31:35:43.9  (J2000)  This needs to be checked

(Most recent updates: 
Membership probability flag - 2024; Remaining data - July 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
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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

Terzan 4 is a heavily reddened cluster in a rich field in the Galactic 
bulge.  Valenti et al. (2010) published a near infra-red CM diagram 
(K, J-K) which is heavily contaminated by stars in the surrounding metal 
rich field population. When looking at stars within 40 arcsec of the 
cluster centre, they detected a blue HB.
They used their data to derive a photometric [Fe/H] = -1.58, in good
agreement with the [Fe/H]=-1.6 published by Stephans & Frogel (2004) and
by Origlia & Rich (2004) from studies based on high-resolution IR 
spectroscopy.

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References

Origlia, L., Rich, R. M.  2004, AJ, 127, 3422

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

Stephans, A. W., Frogel, J. A. 2004, AJ, 127, 925

Valenti, E., Ferraro, F. R., Origlia, L. 2010, MNRAS, 402, 1729
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