NGC 6749 / Berkeley 42 / C1902+017
RA: 19:05:15.3   DEC: +01:54:03 (J2000)

(Most recent updates: 
Membership probability flag - 2024; Remaining data - June 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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1        19:05:20.0  +01:55:57   m1   4.481  12.34  0.44  K CW

PSR      -- -- --     -- -- --   u  ----     --     --            1 msP
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Supplementary Notes 

VI color-magnitude diagrams published by Kaisler et al. (1997) and by 
Rosino et al.  (1997)  show a blue HB.  Rosino et al. concluded that 
this is a  halo cluster located close to the Galactic plane. The 
surrounding field is rich in Mira variables (75 within 1 degree of the 
cluster centre), but they do not appear to be members. They are probably 
associated with the metal rich disc/bulge population.  Skiff (2001) 
listed RA, dec and magnitudes for the variables, but agreed with Rosino 
that probably none of theMira variables are related to the cluster.

The data for the type II Cepheid V1 are from Matsunaga et al. (2006).
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Discovery of the Variable Stars in NGC 6749

V1
  Matsunaga et al. (2006) with RA and dec 

PSR:  
  According to Paulo Freire's website at the Max Planck Institute in
  Bonn (July 2024 version), there is 1 millisecond pulsar in NGC 6749.
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References

Kaisler, D., Harris, W. E., McLaughlin, D. E.  1997, PASP, 109, 920 

Matsunaga, N., Fukushi, H., Nakada, Y., Tanabe, T., Feast, M. W.,
Menzies, J. W., Ita, Y. and 7 coauthors, 2006, MNRAS, 370, 1979

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

Rosino, L., Ortolani, S., Barbuy, B., Bica, E.  1997, MNRAS, 289, 745

Skiff, B. A. 2001, IBVS, 5187 

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