Table 1.
Member counts, average metallicity, galactic radius, and age for clusters in our selection.
| Cluster | [Fe/H] | RGC [kpc] | log(Age/yr) | Members | Frequency |
|---|---|---|---|---|---|
| Berkeley 17 | −0.17 ± 0.03 | 10.62 | 10 ± 0.14 | 8 | 1 |
| NGC 1817 | −0.18 ± 0.03 | 9.46 | 9.09 ± 0.02 | 8 | 1 |
| NGC 6705 | 0.12 ± 0.02 | 6.23 | 8.47 ± 0.09 | 8 | 1 |
| Trumpler 5 | −0.46 ± 0.02 | 10.42 | 9.54 ± 0.02 | 8 | 1 |
| Melotte 22 | −0.05 ± 0.12 | 8.12 | 8.12 ± 0.11 | 9 | 1.1 |
| ASCC 16 ( * ) | −0.13 ± 0.09 | 8.33 | 7.09 ± 0.06 | 11 | 1.4 |
| NGC 2243 | −0.49 ± 0.03 | 9.96 | 9.54 ± 0.04 | 11 | 1.4 |
| Collinder 69 ( * ) | −0.12 ± 0.06 | 8.56 | 6.95 ± 0.05 | 12 | 1.5 |
| IC 348 ( * ) | −0.11 ± 0.12 | 8.27 | 6.78 ± 0.07 | 13 | 1.6 |
| ESO 211 03 | −0.19 ± 0.02 | 8.99 | 8.89 ± 0.04 | 14 | 1.8 |
| ASCC 19 ( * ) | −0.12 ± 0.12 | 8.33 | 7.14 ± 0.03 | 15 | 1.9 |
| IC 166 | −0.11 ± 0.03 | 10.69 | 9.01 ± 0.03 | 16 | 2.0 |
| Ruprecht 147 | 0.09 ± 0.06 | 7.73 | 9.45 ± 0.02 | 18 | 2.3 |
| NGC 2420 | −0.20 ± 0.03 | 9.86 | 9.35 ± 0.02 | 20 | 2.6 |
| NGC 1245 | −0.12 ± 0.03 | 10.27 | 9.08 ± 0.02 | 21 | 2.7 |
| NGC 2204 | −0.30 ± 0.03 | 10.46 | 9.32 ± 0.03 | 21 | 2.7 |
| Trumpler 20 | 0.09 ± 0.02 | 6.95 | 9.18 ± 0.02 | 21 | 2.7 |
| Kharchenko 1 | −0.04 ± 0.04 | 8.81 | 8.76 ± 0.09 | 24 | 3.1 |
| Berkeley 18 | −0.38 ± 0.03 | 11.98 | 9.61 ± 0.07 | 26 | 3.3 |
| BH 56 ( * ) | −0.09 ± 0.10 | 8.13 | 7.16 ± 0.08 | 28 | 3.6 |
| NGC 6819 | 0.03 ± 0.03 | 7.69 | 9.42 ± 0.03 | 37 | 4.8 |
| NGC 752 | −0.07 ± 0.05 | 8.29 | 9.18 ± 0.03 | 37 | 4.8 |
| NGC 188 | 0.06 ± 0.03 | 8.91 | 9.79 ± 0.04 | 42 | 5.4 |
| NGC 2158 | −0.25 ± 0.03 | 11.22 | 9.22 ± 0.12 | 53 | 6.8 |
| NGC 6791 | 0.29 ± 0.04 | 7.54 | 9.86 ± 0.04 | 65 | 8.4 |
| NGC 7789 | −0.03 ± 0.06 | 8.89 | 9.21 ± 0.01 | 68 | 8.8 |
| NGC 2682 | −0.00 ± 0.03 | 8.56 | 9.58 ± 0.03 | 161 | 20.8 |
Notes. The metallicity and its relative uncertainty are computed as a weighted average and weighted standard deviation of the metallicities of the individual members, respectively, where the weights are inversely proportional to the square of the uncertainties. Frequency indicates the percentage of stars in a particular cluster compared to the total data size. RGC indicates the distance from the galactic center, as obtained using parallaxes from Gaia Collaboration (2018). Ages taken from Dias et al. (2021). Ages for Berkeley 18 and NGC 2158 from Netopil et al. (2016). ( * )Clusters flagged as non high-quality (Donor et al. 2018).
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