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Table 3

Excerpt from the list of Fe, O, and S abundances derived for each star in our sample.

Name [Fe I/H] ± σ [Fe II/H] ± σ [Fe/H] ± σ (std) N [O/H] ± σ (std) N [S/H] ± σ (std) N Nf Nh Nu NS
AA Gem −0.18 ± 0.10 −0.17 ± 0.11 −0.18 ± 0.10 1 −0.24 ± 0.08 1 −0.34 ± 0.11 1 0 0 1 0
AASer 0 0 0 0 0 1 0
1Car −0.04 ± 0.11 −0.04 ± 0.16 −0.04 ± 0.11 1 0 −0.08 ± 0.13 1 1 0 0 0
ζ Gem 0.01 ± 0.01 0.01 ± 0.01 0.01 ± 0.01 (0.06) 131 0.03 ± 0.01 (0.09) 129 −0.03 ± 0.01 (0.05) 131 0 47 0 84

Notes. The first three columns give the target name and the iron abundances from neutral and ionized lines, which are either the same values as in Table 2 for stars with a single spectrum or the weighted mean and standard errors computed using the abundances from multiple spectra. Column (4) lists the iron abundances and their uncertainties, either calculated as a weighted mean from Cols. (2) and (3) or adopted from Col. (2) when only one spectrum was available. For stars with multiple spectra, the standard deviation is also shown within parentheses, which was calculated using individual abundances from Fe I and Fe II lines together. Column (5) gives the number of spectra for which we were able to derive the iron abundances and the atmospheric parameters. Columns from (6)–(9) list the oxygen and sulfur abundances (again, either the same values as in Table 2 for stars with a single spectrum, or the weighted mean and standard errors computed using the abundances from multiple spectra), the standard deviations calculated for stars with multiple spectra, and the number of spectra used. The four last columns show the number of optical spectra available from each spectrograph: NF: FEROS, NH: HARPS, NU: UVES, and NS: STELLA.

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