Table B.1
Results from the SME fit of CFHT-ESpaDoNS and TBL-NARVAL spectra.
| star | Teff | log g | [Fe/H] | vmic | v sin i | A(C) | A(O)NLTE | A(Fe) | FIP bias |
|---|---|---|---|---|---|---|---|---|---|
| [K] | [cgs] | [km s−1] | [km s−1] | ||||||
| 70 Oph A | 5320 ± 40 | 4.52 ± 0.06 | -0.02 ± 0.07 | 1.12 ± 0.02 | 3.7 ± 0.05 | 8.49 | 8.90 | 7.42 | -0.49 ± 0.07a |
| 70 Oph B | 4400 | 4.47 | -0.02 | 1.85 | 6.4 | 8.79 | 8.81 | 7.60 | 0.12 ± 0.23a |
| β Com | 6090 ± 60 | 4.41 ± 0.05 | -0.03 ± 0.05 | 1.28 ± 0.1 | 5.1 ± 0.05 | 8.35 | 8.61 | 7.45 | -0.54 ± 0.30b |
| EK Dra | 5840 ± 100 | 4.57 ± 0.20 | -0.01 ± 0.10 | 1.6 ± 0.05 | 18.3 ± 0.1 | 8.50 | 8.87 | 7.53 | -0.13 ± 0.15a,b |
| ϵ Eri | 5050 ± 10 | 4.48 ± 0.05 | -0.11 ± 0.01 | 0.99 ± 0.01 | 3.7 ± 0.2 | 8.53 | 8.97 | 7.49 | -0.22 ± 0.06a |
| η Lep | 6920 ± 70 | 4.19 ± 0.02 | -0.09 ± 0.05 | 1.83 ± 0.2 | 19 ± 0.2 | 8.27 | 9.40 | 7.45 | -0.63 ± 0.5a |
| κ Cet | 5740 ± 20 | 4.48 ± 0.01 | -0.02 ± 0.06 | 1.25 ± 0.03 | 5.7 ± 0.1 | 8.45 | 8.80 | 7.45 | -0.46 ± 0.07b |
| χ1 Ori | 6020 ± 10 | 4.45 ± 0.03 | -0.06 ± 0.05 | 1.21 ± 0.05 | 9.7 ± 0.1 | 8.35 | 8.62 | 7.47 | -0.38 ± 0.09b |
| ξ Boo A | 5550 ± 100 | 4.66 ± 0.20 | -0.19 ± 0.10 | 1.29 ± 0.1 | 5.5 ± 0.2 | 8.50 | 8.90 | 7.48 | -0.29 ± 0.03a |
| Sun (Moon) | 5840 ± 60 | 4.44 ± 0.10 | -0.06 ± 0.10 | 1.13 ± 0.05 | 2.7 ± 0.1 | 8.44 | 8.65 | 7.44 | – |
| π1 UMa | 5950 ± 70 | 4.53 ± 0.10 | -0.12 ± 0.10 | 1.4 ± 0.05 | 10 ± 0.1 | 8.36 | 8.69 | 7.47 | -0.27 ± 0.18a,b |
| π3 Ori | 6430 ± 40 | 4.25 ± 0.01 | -0.05 ± 0.01 | 1.37 ± 0.1 | 17.8 ± 0.2 | 8.18 | 8.67 | 7.43 | -0.23 ± 0.19a |
| τ Boo A | 6370 ± 30 | 4.14 ± 0.04 | 0.16 ± 0.10 | 1.34 ± 0.2 | 16.2 ± 0.2 | 8.20 | 8.64 | 7.45 | -0.17 ± 0.20a |
| λ And | 4510 | 2.57 | -0.56 | 1.26 | 9.2 | 8.42 | 10.19 | 7.33 | -1.02 ± 0.69c |
| β Cet | 4720 | 2.65 | -0.15 | 1.58 | 6.3 | 8.22 | 9.16 | 7.35 | -0.79 ± 0.46d |
| σ Gem | 4630 | 2.79 | -0.10 | 1.62 | 27.4 | 8.37 | 9.69 | 7.34 | -0.58 ± 0.26e |
Notes. Error bars (except for the FIP bias) are calculated as the standard deviation of the results from multiple spectra and are omitted when only a single spectrum was available. This represents the internal precision of the method, not the true accuracy. The oxygen abundances already include the NLTE correction from Kovalev et al. (2018).
Sources of coronal abundances: a Wood et al. (2018), b Telleschi et al. (2005), c Audard et al. (2003), d García-Alvarez et al. (2006), e Huenemoerder et al. (2013).
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