Table 2
Mean iron metallicity and standard deviation (σ) for the 34 clusters.
| Clusters | [Fe/H] (dex) | σ (dex) | N | [Fe/H]lit (dex) | Reference |
|---|---|---|---|---|---|
| IC2714 | −0.06 | 0.02 | 8 | 0.02 ± 0.06 | (1) |
| IC4651 | −0.01 | 0.04 | 11 | 0.12 ± 0.04 | (1) |
| IC4756 | −0.12 | 0.03 | 13 | 0.02 ± 0.04 | (1) |
| NGC1662 | −0.09 | 0.00 | 2 | −0.07 | (2) |
| NGC2204 | −0.28 | 0.06 | 2 | −0.23 ± 0.04 | (7) |
| NGC2251 | −0.01 | 0.01 | 3 | −0.09 | (1) |
| NGC2287 | −0.14 | 0.02 | 4 | −0.11 ± 0.01 | (1) |
| NGC2345 | −0.22 | 0.02 | 4 | −0.28 ± 0.07 | (3) |
| NGC2354 | −0.17 | 0.04 | 6 | −0.14± 0.02 | (2) |
| NGC2355 | −0.15 | 1 | −0.05 ± 0.08 | (1) | |
| NGC2360 | −0.13 | 0.02 | 8 | −0.03 ± 0.06 | (1) |
| NGC2423 | −0.03 | 0.06 | 4 | 0.08 ± 0.05 | (1) |
| NGC2447 | −0.13 | 0.03 | 3 | 0.00 | (4) |
| NGC2477 | 0.08 | 0.06 | 36 | 0.07 ± 0.03 | (1) |
| NGC2506 | −0.29 | 0.08 | 3 | −0.23 ± 0.05 | (1) |
| NGC2539 | −0.04 | 0.02 | 9 | −0.01 ± 0.004 | (2) |
| NGC2567 | −0.09 | 0.02 | 2 | −0.04± 0.08 | (1) |
| NGC2682 | −0.10 | 0.02 | 3 | 0.00 | (4) |
| NGC2925 | −0.01 | 0.01 | 2 | 0.00 | (4) |
| NGC2972 | 0.04 | 0.01 | 2 | −0.09 | (4) |
| NGC3114 | −0.10 | 0.19 | 8 | 0.05 ± 0.06 | (1) |
| NGC3532 | −0.08 | 0.03 | 7 | −0.03 ± 0.01 | (2) |
| NGC3680 | −0.15 | 0.02 | 5 | −0.01 ± 0.06 | (1) |
| NGC3960 | −0.09 | 1 | −0.04 ± 0.10 | (1) | |
| NGC4349 | −0.11 | 0.01 | 2 | −0.07 ± 0.06 | (1) |
| NGC5822 | −0.10 | 0.04 | 12 | 0.08 ± 0.08 | (1) |
| NGC6067 | 0.02 | 0.26 | 3 | 0.12 ± 0.13 | (1) |
| NGC6134 | 0.07 | 0.03 | 3 | 0.11 ± 0.07 | (1) |
| NGC6208 | −0.20 | 0.04 | 2 | −0.01 | (4) |
| NGC6281 | −0.07 | 0.03 | 2 | −0.05 ± 0.01 | (2) |
| NGC6425 | −0.03 | 0.02 | 2 | 0.09 | (4) |
| NGC6494 | −0.05 | 0.02 | 4 | −0.04± 0.08 | (1) |
| NGC6633 | −0.09 | 0.01 | 3 | −0.06 ± 0.02 | (5) |
| NGC6705 | 0.07 | 0.02 | 29 | 0.12 ± 0.05 | (6) |
Notes. N represents the number of stars in each cluster excluding non-members. The literature iron metallicity and their references are shown in the last columns.
Refeгences. (1) Heiter et al. (2014), (2) Casamiquela et al. (2021), (3) Alonso-Santiago et al. (2019), (4) Bossini et al. (2019), (5) Spina et al. (2017), (6) Magrini et al. (2014), and (7) Jacobson et al. (2011).
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