Table 1
Information about studied clusters.
| Cluster | α 2000 | δ 2000 | Age | ⟨vr⟩ | [Fe/H] | Radius | Starsa | Ref. | |
| hrs | deg | Gyr | km s-1 | dex | arcmin | ||||
|
|
|||||||||
| NGC 2158 | 06:07:25 | +24:05:48 | 1.0 | 24.9 ± 1.9 | −0.15 ± 0.14 | 8.0 | 35 | 1, 3, 4 | |
| NGC 2420 | 07:38:23 | +21:34:24 | 2.0 | 69 ± 5 | −0.39 ± 0.20 | 12.0 | 67 | 1, 3, 5 | |
| NGC 2682 | 08:51:18 | +11:48:00 | 2.6 | 36 ± 6 | 0.01 ± 0.07 | 21.0 | 46 | 1, 3, 6, 7 | |
| NGC 7789 | 23:57:24 | +56:42:30 | 1.4 | −58 ± 6 | −0.04 ± 0.05 | 28.84 | 11 | 1, 3, 6, 7, 8 | |
| Berkeley 29 | 06:53:18 | +16:55:00 | 1.1 | 24.7 ± 0.4 | −0.42 ± 0.07 | 7.5 | 9 | 1, 2, 3 | |
Notes.
This is the total number of stars used in our analysis for each cluster as a function of their spatial distribution, radial velocities, metallicities and position in the colour−magnitude diagram and with photometric magnitudes and a good available signal-to-noise ratio spectrum (see text for details).
Reference. (1) Dias et al. (2002); (2) Sestito et al. (2008); (3) Carrera & Pancino (2011); (4) Jacobson et al. (2011); (5) Chen et al. (2004); (6) Carrera et al. (2007); (7) Friel et al. (2002); (8) Wu et al. (2007).
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