Notes. ^(a)For γ Vel, NGC 2547 and NGC 2451 A and B, we used the selections listed in Table 1. ^(b)For these clusters, the final mean [Fe/H] values deviate more appreciably from the literature values. ^(c)We could not find any prior measurements from the literature for these clusters. ^(d)In the individual notes of Appendix A we also list the number of stars that we accepted as robust members despite deviating from these 3σ intervals. ^(e)Final selection only consists of two members, final fit is not possible.

References. Shown here are the most recent or robust estimates for each cluster, several studies are further cited in Appendix A: (1) Randich et al. (2018); (2) Spina et al. (2017); (3) Sacco et al. (2015); (4) Carrera et al. (2019); (5) Binks et al. (2022); (6) De Silva et al. (2013); (7) Dumont et al. (2021b); (8) Smiljanic et al. (2011); (9) Netopil & Paunzen (2013); (10) Kılıçoğlu et al. (2016); (11) Magrini et al. (2018); (12) Bossini et al. (2019); (13) Jacobson et al. (2016); (14) Casali et al. (2019); (15) Paunzen et al. (2010); (16) Fritzewski et al. (2019); (17) Heiter et al. (2014); (18) Friel et al. (2014); (19) Sestito & Randich (2005); (20) Rain et al. (2021); (21) Overbeek et al. (2017); (22) Tang et al. (2017); (23) Carraro et al. (2005); (24) Liu & Pang (2019).