C2304+124 / Palomar 13
RA: 23:06:44.44  DEC: +12:46:19.2 (J2000)

(Most recent updates: 
Membership probability flag - 2024; Remaining data - March 2019)
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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        23:06:41.53 +12:46:58.9 m1   0.5382 17.886 0.80  V RR0
2        23:06:44.47 +12:46:16.1 m1   0.5971 17.819 0.79  V RR0
3        23:06:43.14 +12:46:47.8 m1   0.5782 17.766 0.83  V RR0
4        23:06:48.83 +12:41:22.3 u    0.5751 17.886 0.52  V RR0   
5        23:06:37.28 +12:49:27.5 u    7.26   17.029 0.4   V SR?
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Supplementary Notes 

The data are from Yepez et al. (2019) who concluded that all of these 
variables are cluster members, based on their proper motion and location 
in the CM diagram. 

In an analysis of the structure and dynamics of Pal 13, Bradford et al.
(2011) derived a tidal radius of 13.9 arcminutes, which is considerably
larger than previously assumed (Harris 2010). V1-5 are all well within 
Bradford's tidal radius.

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Discovery of the variable stars in Pal 13:

   V1-4
     Rosino (1957) with x,y positions and ID chart 

     An ID chart with the variables labelled was also published by 
     Rosino & Ortolani (1985) - see Fig. 9 and by Ortolani et al. 
     (1985) - see Fig. 1.

   V5
     Yepez et al. (2019) with RA, dec (2000) and an ID chart
     These authors discovered 3 additional variables which they 
     called Var 1, Var 2 and Var 3, but none  of them are considered
     to be cluster members and are therefore not listed in the above
     table. 
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Palomar 13 has a significant population of blue straggler stars.
However, none of them have been identified as variables in searches 
carried out by Siegel et al. (2001) and by Yepez et al. (2019)
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References

Bradford, J. D., Geha, M., Munoz, R. R., Santana, F. A., Simon, J. D.,
Cote, P., Stetson , P. B. and 2 co-authors, 2011, ApJ, 743, 167

Harris, W. E. 2010, arXiv:1012.3224

Ortolani, S., Rosino, L., Sandage, A.  1985, AJ, 90, 473

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

Rosino, L. 1957, Mem. SAI, 28, 293 = Asiago Cont. No. 85 

Rosino, L. & Ortolani, S. 1985, Mem. SAI, 56, 113 

Siegel, M. H., Majewski, S. R., Cudworth, K. M., Takmiya, M. 2001, AJ,
121, 935

Yepez, M. A., Arellano Ferro, A., Schoeder, K. P., Muneer, S., Giridhar,
S., Allen, C. 2019, New Ast. 71, 1
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