CCD photometry of the open clusters NGC 2627, NGC 5617, Pismis 7, and Ruprecht 75

Details CCD photometry of the open clusters NGC 2627, NGC 5617, Pismis 7, and Ruprecht 75 CCD photometry of the open clusters NGC 2627, NGC 5617, Pismis 7, and Ruprecht 75

Jan 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005an....326....3a&link_type=abstract

Astronomische Nachrichten, Vol.326, Issue 1, p.3-18

Astronomy and Astrophysics

Astronomy

6

Open Clusters And Associations: General, Open Clusters And Associations: Individual (Ngc 2627, Ngc 5617, Pismis 7, Ruprecht 75)

Scientific paper

We present broad-band, optical CCD photometry of the galactic open clusters NGC 2627, NGC 5617, Pismis 7, and Ruprecht 75. By means of the comparison between the observed cluster sequences and the theoretical isochrones of Girardi et al. (2000, A&AS 141, 371), we derive the following parameters. For NGC 2627, E(B-V)=0.04-0.02+0.10, log (age)=9.25+0.10-0.05, and (m-M)_0 = 11.33±0.31; for NGC 5617, E(B-V)=0.54-0.08+0.09 , log (age)= 8.15-0.15+0.25, and (m-M)_0 = 11.53-0.43+0.36; for Pismis 7, E(B-V)= 0.69-0.16+0.18, log (age)= 8.70±0.10, and (m-M)_0 =13.46±0.56; and for Ruprecht 75, E(B-V)= 0.24-0.13+0.18, log (age)= 9.15± 0.05, and (m-M)_0 =13.16-0.57+0.60. The isochrones have been renormalized to the solar values (B-V)_&sun;=0.65 and M_V=4.84, along the lines established in Ahumada (2003, RMxAA 39, 41), and following, for instance, Twarog, Ashman & Anthony-Twarog (1997, AJ 114, 2556). Besides, a comparison is made between the isochrones by Girardi et al. (2000) and those, also renormalized, by Castellani, Degl'Innocenti & Marconi (1999, MNRAS 303, 265) in the range of ages and metallicities of interest. It is noted that discrepancies arise mainly for the amount of core overshooting incorporated into the models, which implies different ages for a given cluster.

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