Table 3.
Fit parameters and metallicity membership for the sample clusters.
| Cluster (a) | [Fe/H] (b) | 2σ clipping |
2σ membership | Final fit of member list |
||
|---|---|---|---|---|---|---|
| (dex) | ⟨[Fe/H]⟩ (dex) | σ (dex) | intervals | ⟨[Fe/H]⟩ (dex) | σ (dex) | |
| ρ Oph | −0.08 ± 0.02 | −0.16 | 0.10 | [−0.36, +0.04] | −0.19 (c) | 0.09 |
| Cha I | −0.07 ± 0.04 | −0.09 | 0.13 | [−0.35, +0.17] | −0.18 (c) | 0.08 |
| IC 2391 | −0.03 ± 0.02 | −0.09 | 0.09 | [−0.27, +0.09] | −0.11 | 0.09 |
| IC 2602 | −0.02 ± 0.02 | −0.06 | 0.11 | [−0.28, +0.16] | −0.09 | 0.11 |
| IC 4665 | 0.00 ± 0.02 | −0.08 | 0.12 | [−0.32, +0.16] | −0.04 | 0.10 |
| NGC 2516 | −0.06 ± 0.05 | −0.01 | 0.09 | [−0.19, +0.17] | −0.02 | 0.09 |
| NGC 6705 | +0.16 ± 0.04 | +0.10 | 0.12 | [−0.14, +0.34] | +0.10 | 0.10 |
| NGC 4815 | +0.11 ± 0.01 | +0.05 | 0.17 | [−0.29, +0.39] | +0.01 | 0.13 |
| NGC 6633 | −0.01 ± 0.11 | −0.02 | 0.17 | [−0.36, +0.32] | −0.01 | 0.17 |
| Trumpler 23 | +0.21 ± 0.04 | +0.13 | 0.10 | [−0.07, +0.33] | +0.14 | 0.04 |
| Berkeley 81 | +0.22 ± 0.07 | +0.16 | 0.13 | [−0.10, +0.42] | +0.20 | 0.06 |
| NGC 6005 | +0.19 ± 0.02 | +0.08 | 0.14 | [−0.20, +0.36] | +0.13 | 0.06 |
| NGC 6802 | +0.10 ± 0.02 | −0.01 | 0.11 | [−0.23, +0.21] | +0.00 | 0.11 |
| Pismis 18 | +0.22 ± 0.04 | +0.05 | 0.13 | [−0.21, +0.31] | +0.05 (c) | 0.09 |
| Trumpler 20 | +0.10 ± 0.05 | +0.07 | 0.18 | [−0.29, +0.43] | +0.10 | 0.09 |
| Berkeley 44 | +0.27 ± 0.06 | +0.13 | 0.13 | [−0.17, +0.43] | +0.17 | 0.07 |
| M67 | −0.01 ± 0.04 | −0.03 | 0.06 | [−0.09, +0.03] | −0.02 | 0.03 |
| NGC 2243 | −0.38 ± 0.04 | −0.60 | 0.12 | [−0.84, −0.36] | −0.49 | 0.14 |
Notes. (a)Regarding the cluster γ Vel, we directly used the selections obtained by Jeffries et al. (2014), Damiani et al. (2014), Spina et al. (2014b), Frasca et al. (2015), and Prisinzano et al. (2016). Similarly, we use those done by Sacco et al. (2015), Cantat-Gaudin et al. (2018), and Randich et al. (2018) for the cluster NGC 2547. (b)See references on cluster [Fe/H] metallicities in Table 1. (c)In the cases of these clusters, the final mean [Fe/H] values obtained deviate appreciably from the literature values, potentially as a result of the lower resolution of the GIRAFFE spectra.
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