Table 1.
Age estimates, mean metallicity, distance to the Sun, and GES membership studies from the literature for the 20 clusters in our sample.
| Cluster | Age | [Fe/H] | Distance | References | References | References | GES membership |
|---|---|---|---|---|---|---|---|
| (Myr) | (dex) | (kpc) | ages | [Fe/H] | distance | studies | |
| ρ Oph | 1–3 | −0.08 ± 0.02 | 0.13 ± 0.01 | 1, 2 | 2 | 2 | 1, 2 (a), 3 |
| Cha I | 2 | −0.07 ± 0.04 | 0.16 ± 0.02 | 4, 5, 6 | 2, 5 | 4, 5, 7, 8 | 2, 4, 5, 7, 8 |
| γ Vel | 10–20 | −0.06 ± 0.02 | 0.35–0.40 | 2, 5, 7, 9, 11, 12, 26 | 2, 11 | 5, 7, 9, 12, 26 | 2, 5, 7, 9, 10, 11, 12, 13, 26 |
| NGC 2547 | 35–45 | −0.03 ± 0.06 | 0.36 ± 0.02 | 2, 5, 15, 16, 17, 26, 39 | 2 | 2, 5, 26 | 2, 5, 14, 15, 17, 22 |
| IC 2391 | 36 ± 2 (b) | −0.03 ± 0.02 | 0.16 ± 0.01 | 2, 15, 18, 19, 21, 23 | 2, 20, 21, 23 | 2, 19, 20, 21, 39 | 2, 14, 15, 22 |
| IC 2602 | 35 ± 1 (b) | −0.02 ± 0.02 | 0.15 ± 0.01 | 2, 15, 18, 21, 23 | 2, 21, 23 | 2, 21, 39 | 2, 14, 15, 22 |
| IC 4665 | 38 ± 3 (b) | 0.00 ± 0.02 | 0.36 ± 0.01 | 2, 15, 18, 21, 24, 25 | 2, 39 | 2, 24, 25 | 2, 14, 15, 22 |
| NGC 2516 | 251 ± 3 (b) | −0.06 ± 0.05 | 0.41 | 16, 18, 27, 28, 29 | 27, 28 | 29, 39 | 14, 15, 17, 27, 28 |
| NGC 6705 | 300 ± 50 | +0.16 ± 0.04 | 1.88 | 27, 28 | 27, 28, 48 | 30, 39 | 14, 27, 28, 31, 32 a, 33 |
| NGC 4815 | 570 ± 70 | +0.11 ± 0.01 | 2.40–2.90 | 27, 28, 34, 48 | 27, 28, 34, 48 | 34, 39 | 14, 27, 28, 31, 32, 33, 34 |
| NGC 6633 | 773 ± 10 (b) | −0.01 ± 0.11 | 0.39 | 16, 18, 27, 28, 48 | 16, 27, 28, 35 48 | 30, 35, 39 | 14, 15, 27, 28 |
| Trumpler 23 | 800 ± 100 | +0.21 ± 0.04 | 2.20 | 27, 28, 36, 48 | 27, 28, 36, 48 | 36, 39 | 27, 28, 36 |
| Berkeley 81 | 860 ± 100 | +0.22 ± 0.07 | 3.00 | 27, 28, 32, 37, 48 | 27, 28, 37, 48 | 37, 39 | 14, 27, 28, 32 |
| NGC 6005 | 973 ± 4 b | +0.19 ± 0.02 | 2.70 | 18, 27, 28, 48 | 27, 28, 48 | 30, 39 | 14, 27, 28 |
| NGC 6802 | 1000 ± 100 | +0.10 ± 0.02 | 1.80 | 27, 28, 38, 48 | 27, 28, 38, 48 | 39 | 14, 27, 28, 38 |
| Pismis 18 | 1200 ± 400 | +0.22 ± 0.04 | 2.20 | 27, 28, 40, 48 | 27, 28, 48 | 39, 40 | 27, 28, 41 |
| Trumpler 20 | 1500 ± 150 | +0.10 ± 0.05 | 3.00 | 27, 28, 42 | 27, 28 | 39, 42 | 14, 27, 28, 31, 32, 33, 42, 43 |
| Berkeley 44 | 1600 ± 300 | +0.27 ± 0.06 | 1.80–3.10 | 27, 28, 44, 48 | 27, 28, 48 | 39, 44 | 14, 27, 28 |
| M67 | 4000–4500 | −0.01 ± 0.04 | 0.90 | 16, 45, 46 | 16, 48, 49, 50 | 30, 39, 47 | ... |
| NGC 2243 | 4000 ± 120 | −0.38 ± 0.04 | 4.50 | 28, 48, 49, 51, 52 | 28, 48, 49, 51 | 31, 39, 51 | 14, 28 |
Notes. (a)GES studies that reference the clusters and/or study them without taking membership analysis primarily into account. (b)Updated cluster ages using Gaia data, as listed by Bossini et al. (2019).
References. For cluster ages, metallicities, distances, and membership studies. For the reference values shown here we chose the latest or most robust estimates for each cluster, while larger ranges taking into account more than one literature value are additionally cited in the individual notes of Appendix A: (1) Rigliaco et al. (2016); (2) Spina et al. (2017); (3) Cánovas et al. (2019); (4) Spina et al. (2014a); (5) Sacco et al. (2015); (6) López Martí et al. (2013); (7) Frasca et al. (2015); (8) Roccatagliata et al. (2018); (9) Jeffries et al. (2014); (10) Damiani et al. (2014); (11) Spina et al. (2014b); (12) Franciosini et al. (2018); (13) Prisinzano et al. (2016); (14) Cantat-Gaudin et al. (2018); (15) Randich et al. (2018); (16) Sestito & Randich (2005); (17) Jackson et al. (2016); (18) Bossini et al. (2019); (19) Platais et al. (2007); (20) De Silva et al. (2013); (21) Smiljanic et al. (2011); (22) Bravi et al. (2018); (23) Randich et al. (2001); (24) Martin & Montes (1997); (25) Jeffries et al. (2009); (26) Beccari et al. (2018); (27) Jacobson et al. (2016); (28) Magrini et al. (2017); (29) Jeffries et al. (2001); (30) Kharchenko et al. (2005); (31) Magrini et al. (2014); (32) Magrini et al. (2015); (33) Tautvaišienė et al. (2015); (34) Friel et al. (2014); (35) Jeffries et al. (2002); (36) Overbeek et al. (2017); (37) Donati et al. (2014a); (38) Tang et al. (2017); (39) Dias et al. (2002); (40) Piatti et al. (1998); (41) Hatzidimitriou et al. (2019); (42) Donati et al. (2014b); (43) Smiljanic et al. (2016); (44) Hayes & Friel (2014); (45) Pallavicini et al. (2005); (46) Richer et al. (1998); (47) Friel et al. (2010); (48) Magrini et al. (2018); (49) Heiter et al. (2014); (50) Overbeek et al. (2016); (51) Jacobson et al. (2011); (52) Friel & Janes (1993).
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