Table 3
NGC 6087: previous and current determinations of color excess, distance, and age.
| Reference | E(B − V ) |  |
d | Age |
|---|---|---|---|---|
| [mag] | [mag] | [pc] | [Myr] | |
| Trumpler (1930)sp | ⋯ | ⋯ | 870 | ⋯ |
| Fernie (1961)ph | 0.22 | 9.4 | 750 | 10−20 |
| Landolt (1963)ph | 0.20 | 9.8 ± 0.1 | ⋯ | ⋯ |
| Breger (1966)ph | 0.20 ± 0.01 | 9.7 | ⋯ | ⋯ |
| Graham (1967)ph | ⋯ | 9.9 | 950 | ⋯ |
| Lindoff (1968)sc | ⋯ | ⋯ | 930 | ~41 |
| Becker & Fenkart (1971)ph | 0.13 | 9.96 | 820 | ⋯ |
| Tosi (1979)* | ⋯ | ⋯ | ⋯ | 55 ± 5; 55 ± 9.6;146 ± 11 |
| Schmidt (1980)ph | 0.17 ± 0.01** | 9.60 ± 0.09 | ⋯ | ⋯ |
| Janes & Adler (1982)ph | 0.21 | 10.23 | ⋯ | ~40 |
| Turner (1986)ph | ⋯ | 9.78 ± 0.13 | 902 ± 10 | ⋯ |
| Sagar (1987)ph,sp | 0.18 ± 0.05 | 9.8 | ⋯ | 20 |
| Meynet et al. (1993)i | ⋯ | ⋯ | ⋯ | ~71 |
| Sagar & Cannon (1997)ph | 0.22 | ⋯ | 1000 ± 100 | 65 |
| Robichon et al. (1999)h | ⋯ | ⋯ | 769 | ⋯ |
| Rastorguev et al. (1999)h | ⋯ | ⋯ | 820 | ⋯ |
| Baumgardt et al. (2000)h | ⋯ | ⋯ | 819.67 | ⋯ |
| Loktin & Beshenov (2001)h | ⋯ | 9.375 | ⋯ | ~95 |
| Kharchenko et al. (2005)h | ⋯ | ⋯ | 901 | ~85 |
| Piskunov et al. (2007)h | 0.18 | ⋯ | ⋯ | ⋯ |
| An et al. (2007)ph | 0.132 ± 0.007 | 9.708 ± 0.048 | ⋯ | ⋯ |
| This work | 0.35 ± 0.03 | 9.00 ± 0.19 | 629 ± 54 | ~55 |
Notes. (h) Results based on HIPPARCOS data. (i) Results based on the isochrone fitting method. (ph)Results based on photometric data. (sc)Results based on synthetic clusters. (sp)Results based on spectroscopic data. (*)The age of the cluster was derived by three different methods: isochrone fitting, position of the turn-off point, and period of Cepheid stars (55 Myr, 146 Myr, and 55 Myr, respectively). The author argued that the most accurate method is the isochrone fitting followed by the Cepheid periods. (**) The color excess E(B − V ) was calculated in this work, using the E(b − y) value given by Schmidt (1980) and the relation E(b − y) = 0.74 E(B − V ).
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