NGC 6760 / C1908+009
RA: 19:11:12.01 DEC: +01:01:49.7  (J2000)

(Most recent updates: 
Membership probability flag - 2024; Remaining data - September 2015)
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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
=========================================================================
1        19:11:16.01 +01:00:58.6 m1 ----     16.35  1.3   P L?    Note
2        19:11:11.91 +01:00:16.4 m1 ----     16.95  0.5   P ?
3        19:11:14.31 +01:01:46.6 m1 251.0     7.69  0.72  K M
4        19:11:15.03 +01:02:36.8 m1 226.0     7.96  0.94  K M

PSR      -- -- --     -- -- --   u  ----     --     --            2 msPs
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Supplementary Notes 

NGC 6760 is a metal rich cluster in the Galactic bulge.  The 2010
update to the Harris (1996) catalogue lists [Fe/H] = -0.4. A VI
CM diagram by Heitsch & Richtler (1999) shows a prominent red HB and 
also demonstrates that the cluster is located in a rich field near the 
plane of the Galaxy.

For V1 and V2, the magnitudes are from the discovery paper by Sawyer
(1953) and the RA and dec are from Samus et al. (2009).

All the data for V3 and V4 are from Sloan et al. (2010).

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Notes on individual stars

V1:   Prosser (1988) commented that V1 could be a possible Mira because 
      it has a late type spectrum.  In Sawyer's (1953) study, V1 was
      the same brightness as the two Mira variables, V3 and V4, at 
      maximum light.  However, its light amplitude is smaller than that
      expected for a Mira. 

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Discovery of the variable stars in NGC 6760:

  V1-4
    Sawyer (1953) with x,y coordinates and an ID chart
    Prosser (1988) later published a more legible ID chart

  PSR:  According to Paulo Freire's website at the Max Planck 
        Institute in Bonn (July 2024 version), there are 
        2 millisecond pulsars in NGC 6760.
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References

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

Heitsch, F. & Richtler, T. 1999, A&A, 347, 455

Prosser, C. F. 1988, IBVS, 3268

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

Samus, N. N., Kazarovets, E. V., Pastukhova, E. N., Tsvetkova, T. M.,
Durlevich, O. V. 2009, PASP, 121, 1378

Sawyer, H. B. 1953, JRASC, 47, 229 

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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