Table 4
Metal abundances ε(X) = log(X/H) + 12 and metallicity Z (by mass) of the sample stars.
| ID# | Object | C | N | O | Ne | Mg | Al | Si | S | Ar | Fe | Z |
|---|---|---|---|---|---|---|---|---|---|---|---|---|
| 1 | Sher 25 | 8.01 (5) | 8.73 (23) | 8.64 (20) | 8.31 (7) | 7.42 (1) | 6.35 (4) | 7.81: (8) | 7.47:(6) | … | 7.53 (8) | 0.016 |
| ±0.11 | 0.09 | 0.08 | 0.08 | … | 0.04 | 0.11 | 0.03 | … | 0.13 | 0.002 | ||
| 2 | HD 13854 | 7.98 (6) | 8.30 (34) | 8.52 (26) | 8.11 (5) | 7.25 (1) | 6.17 (4) | 7.76:(10) | 7.33:(3) | 6.45 (1) | 7.30 (12) | 0.010 |
| ±0.07 | 0.10 | 0.07 | 0.09 | … | 0.08 | 0.07 | 0.05 | … | 0.09 | 0.002 | ||
| 3 | HD 14956 | 7.76 (7) | 8.70 (27) | 8.53 (16) | 8.08 (8) | 7.37 (1) | 6.30 (3) | 7.79:(9) | 7.34:(7) | … | 7.45 (7) | 0.013 |
| ±0.07 | 0.13 | 0.09 | 0.07 | … | 0.05 | 0.09 | 0.05 | … | 0.11 | 0.002 | ||
| 4 | HD 91316 (a) | 7.94 (11) | 8.35 (43) | 8.44 (30) | 8.06 (11) | 7.50 (4) | 6.27 (4) | 7.60 (9) | 7.20 (4) | 6.57 (5) | 7.27 (17) | 0.010 |
| ±0.08 | 0.08 | 0.08 | 0.06 | 0.29 | 0.03 | 0.09 | 0.05 | 0.04 | 0.09 | 0.002 | ||
| 5 | HD 114199 | 8.11 (4) | 8.45 (19) | 8.53 (20) | 8.24 (4) | 7.46 (1) | 6.57 (1) | 7.53 (6) | 7.05 (1) | … | 7.61 (9) | 0.012 |
| ±0.08 | 0.07 | 0.07 | 0.06 | … | … | 0.06 | … | … | 0.09 | 0.002 | ||
| 6 | HD 152235 | 8.30 (5) | 7.85 (22) | 8.70 (27) | 8.15 (8) | 7.39 (1) | 6.29 (4) | 7.72 (9) | 7.22 (3) | 6.62 (1) | 7.44 (7) | 0.013 |
| ±0.09 | 0.09 | 0.12 | 0.06 | … | 0.06 | 0.15 | 0.03 | … | 0.12 | 0.002 | ||
| CAS (b) | 8.35 | 7.79 | 8.76 | 8.09 | 7.56 | 6.30 | 7.50 | 7.14 | 6.50 | 7.52 | 0.014 | |
| ±0.04 | 0.04 | 0.05 | 0.05 | 0.05 | 0.07 | 0.06 | 0.06 | 0.08 | 0.03 | 0.002 | ||
Notes. Uncertainties are 1σ-values from the line-to-line scatter. Numbers in parentheses quantify number of lines analysed. A colon is inserted for abundances with a suspected systematic overestimation (see Sect. 4.3 for details).(a) Abundances are only indicative. The second continuum from the companion star needs to be considered for a proper abundance determination, which will result in higher abundances and metallicity. However, this is beyond the scope of the present work.(b)Cosmic abundance standard (CAS, Nieva & Przybilla 2012; Przybilla et al. 2013).
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