Palomar 1 / C0325+799
RA: 03:33:20.04  DEC: +79:34:51.8  (J2000)

(Most recent updates: 
Membership probability flag - 2024; Remaining data - May 2011)
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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 

Variable searches of Pal 1 were carried out by Kinman & Rosino (1962)
and by Ortolani & Rosino (1985).
        
A VI color-magnitude diagram by Rosenberg et al. (1998a) does not 
indicate any obvious HB stars. Based on this and on the metal
abundance they derived, [Fe/H]=-0.6, (1998, AJ 115, 658), Rosenberg
et al. (1998b) concluded that Palomar 1 is a very young globular cluster. 

The young age (as much as 8 Gyr younger than 47 Tuc) was confirmed by
Sarajedini et al. (2007) who also said they could not rule out the 
possibility that Palomar 1 has been misclassified as a globular cluster. 
An analysis by Monaco et al. (2011)  indicated that the chemical
abundance is similar to that of Galactic open clusters. They proposed
that Pal 1 might be a globular cluster that experienced a peculiar 
chemical evolution or an open cluster ejected from the Galactic disk.
From a study of tidal tails, Niederste-Ostholt et al. (2010) suggested
that Pal 1 may have been accreted from a now disrupted dwarf galaxy
about 500 Myr ago.

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References

Kinman, T. D. & Rosino, L. 1962, PASP, 74, 499

Monaco, L., Saviane, I., Correnti, M., Bonaficio, P., Geisler, D. 2011,
A&A, 525, A124

Niederste-Ostholt, M., Belkurov, V., Evans, N. W., Koposov, S., Gieles,
M., Irwin, M. J. 2010, MNRAS, 408, L66

Ortolani, S. & Rosino, L. 1985,  Mem. S. A. I., 56, 113 

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

Rosenberg, A., Saviane, I., Piotto, G., Aparicio, A., Zaggia, S. R.
1998a, AJ, 115, 648

Rosenberg, A., Piotto, G., Saviane, I., Aparicio, A., Gratton, R.
1998b, AJ, 115, 658

Sarajedini, A., Bedin, L. R., Chaboyer, B., Dotter, A., Siegel, M.,
Anderson, J., Aparicio, A., KIng, I., Majewski, S., Marin-Franch, A.,
Piotto, G., Reid, I. N., Rosenberg, A. 2007, AJ, 133, 1658
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