Table 3.
Derived mean-reduced equivalent widths from different methods and cluster metallicities.
| NGC |  |
 |
 |
 |
[Fe/H] |
|---|---|---|---|---|---|
| 104 | 5.59 | 5.66 | 5.60 | 5.63 | −0.69 |
| 362 | 4.84 | 4.82 | 4.76 | 4.78 | −1.05 |
| 1851 | 4.99 | 4.97 | 4.91 | 4.94 | −1.19 |
| 1904 | – | – | – | 3.80 | −1.61 |
| 2808 | 5.05 | 5.04 | 4.99 | 5.02 | −1.13 |
| 3201 | 4.39 | 4.29 | 4.22 | 4.24 | −1.46 |
| 5139 | – | – | 3.74 | 3.77 | −1.56 |
| 5286 | 3.57 | 3.64 | 3.52 | 3.55 | −1.63 |
| 5904 | 4.79 | 4.76 | 4.67 | 4.69 | −1.15 |
| 6093 | 3.46 | 3.51 | 3.53 | 3.55 | −1.73 |
| 6218 | – | – | 4.58 | 4.60 | −1.35 |
| 6254 | 4.17 | 4.06 | 4.09 | 4.11 | −1.65 |
| 6266 | – | – | – | 5.07 | −1.11 |
| 6293 | – | – | – | 2.37 | −1.86 |
| 6388 | 5.67 | 5.70 | 5.81 | 5.82 | −0.57 |
| 6441 | 5.64 | 5.66 | 5.79 | 5.78 | −0.49 |
| 6522 | – | – | – | 4.83 | −1.35 |
| 6541 | 3.48 | 3.52 | 3.41 | 3.44 | −1.80 |
| 6624 | 5.71 | 5.72 | 5.68 | 5.70 | −0.36 |
| 6656 | 3.45 | 3.51 | 3.50 | 3.52 | −1.91 |
| 6681 | 4.18 | 4.21 | 4.20 | 4.23 | −1.54 |
| 6752 | 4.09 | 4.10 | 4.06 | 4.08 | −1.44 |
| 7078 | 1.99 | 2.15 | 2.02 | 2.05 | −2.28 |
| 7089 | 3.95 | 3.98 | 3.90 | 3.93 | −1.58 |
| 7099 | 2.32 | 2.46 | 2.38 | 2.40 | −2.28 |
Notes. The index “HB” denotes results from the linear relation using stars with V − VHB < +0.2 as discussed in Sect. 4.2, while “all” uses the results for all RGB stars using a quadratic relation from Sect. 4.3. Finally, “M” uses the absolute magnitude in F606W instead of V − VHB and “lum” the luminosity, both as presented in Sect. 4.4. The uncertainties for the reduced EWs are usually of the order 0.1 − 0.4 dex, the metallicities are taken from Dias et al. (2016).
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