Table B.1
Alternate stellar parameters and abundances, based solely on metallic and He lines.
| Parameter | Value | Solar | # |
|---|---|---|---|
| Teff (K) | 14 189 ± 492 | ||
| log g | 3.43 ± 0.21 | ||
| v sin i (km s−1) | 64.8 ± 7.1 | ||
| vmic (km s−1) | 2.19 ± 0.83 | ||
| He | − 1.11 ± 0.18 | -1.07 | 3 |
| C | − 3.61 ± 0.15 | -3.57 | 1 |
| O | − 3.40 ± 0.11 | -3.31 | 2 |
| Ne | − 3.30 ± 0.23 | -4.07 | 2 |
| Mg | − 4.63 ± 0.14 | -4.40 | 4 |
| Al | − 5.96 ± 0.37 | -5.55 | 3 |
| Si | − 4.79 ± 0.15 | -4.49 | 5 |
| P | − 5.02 ± 0.24 | -6.59 | 5 |
| S | − 5.20 ± 0.21 | -4.88 | 4 |
| Ti | − 6.53 ± 0.20 | -7.05 | 2 |
| Cr | < −6.3 | -6.36 | 1 |
| Mn | − 6.21 ± 0.26 | -6.57 | 2 |
| Fe | − 4.47 ± 0.21 | -4.50 | 4 |
| Ni | − 5.51 ± 0.14 | -5.78 | 2 |
| Ga | < −6.9 | -8.96 | 1 |
| Pr | < −8.8 | -11.28 | 1 |
| Nd | − 9.13 ± 0.40 | -10.58 | 1 |
| Hg | < −7.5 | -10.83 | 1 |
Notes. Solar abundances from Asplund et al. (2009) are listed for comparison. The number of individual spectral windows used to constrain a given element is indicated in the last column. These results are less precise than, but consistent with, the results using the Balmer lines for Teff and log g (Table 2).
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