Table 3.
Equivalent widths (EW) of the lines used in this analysis, as measured off the Keck HIRES spectrum discussed in Simón-Díaz et al. (2020).
| Ion | Wavelength (Å) | EW (mÅ) | X (solar) |
|---|---|---|---|
| Si II | 4128.0 | 79.1 ± 1.0 | 2.39 ± 0.12 |
| Si II | 4130.8 | 82.4 ± 1.0 | 1.74 ± 0.06 |
| Si II | 6347.0 (b) | 157.0 ± 3.0 | 6.16 ± 0.44 |
| Si II | 6371.3 | 118.0 ± 3.0 | 4.14 ± 0.42 |
| Si III | 4552.6 (b) | 11.1 ± 1.0 | 2.40 ± 0.43 |
| Si III | 4567.8 | 7.8 ± 1.0 | 1.98 ± 0.48 |
| Si III | 4574.7 | 3.7 ± 0.5 | 1.72 ± 0.38 |
| Mg II | 4481.2 | 203.6 ± 3.0 | 3.91 ± 0.32 |
| N II | 3995.0 | 28.2 ± 1.0 | 26.93 ± 2.61 |
| N II | 4447.0 | 9.2 ± 1.0 | 16.52 ± 3.41 |
| N II | 4607.1 | 12.4 ± 1.0 | 35.66 ± 4.43 |
| N II | 4613.8 | 7.2 ± 1.0 | 18.73 ± 4.91 |
| N II | 4630.5 | 20.0 ± 1.0 | 40.84 ± 4.29 |
| C II | 3918.9 | 11.2 ± 1.0 | 0.40 ± 0.07 |
| C II | 3920.6 | 14.7 ± 1.0 | 0.33 ± 0.04 |
| C II | 4267.1 | 28.2 ± 1.0 | 0.23 ± 0.02 |
| C II | 6578.0 | 2.8 ± 1.0 | 0.04 ± 0.02 |
| C II | 6582.8 | 3.3 ± 1.0 | 0.08 ± 0.03 |
Notes. The abundances (X) are relative to solar, and are determined for the model with Teff = 12 500 K, log g = 3.0 and for Bstr star contributing 55% of the total V-band flux. Abundance uncertainties reflect observational errors, though uncertainties in vt dominate the overall error budget leading to uncertainties of ∼0.1 dex for C and N, and ∼0.2 dex for Mg and Si. The superscript (b) denotes lines that are blended with other lines in the data.
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