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Table A.2.

Gaia benchmark stars parameters from NLTE fit (max S/N) and reference study (Jofré et al. 2015), except where noted.

Star Teff,K log(g),dex [Fe/H],dex Vmic, km s−1
fit, ref fit, ref fit, ref fit, ref
HD 107328 4384, 4496 ± 59 1.90, 2.09 ± 0.14 −0.60, −0.38 ± 0.16 1.71, 1.65 ± 0.26
HD 220009 4336, 4275 ± 54 1.86, 1.47 ± 0.14 −0.79, −0.79 ± 0.13 1.42, 1.49 ± 0.14
ksiHya 5045, 5044 ± 38 3.01, 2.87 ± 0.02 −0.05, 0.11 ± 0.20 1.54, 1.40 ± 0.32
muLeo 4462, 4474 ± 60 2.45, 2.51 ± 0.09 0.01, 0.20 ± 0.15 1.54, 1.28 ± 0.26
HD 122563 4771, 4636 ± 37 (1) 1.29, 1.42 ± 0.01 (2) −2.56, −2.52 ± 0.11 (3) 2.53, 1.92 ± 0.11
HD 140283 5888, 5787 ± 48 (1) 3.63, 3.57 ± 0.12 −2.39, −2.34 ± 0.03 (3) 2.16, 1.56 ± 0.20
delEri 5006, 4954 ± 26 3.61, 3.75 ± 0.02 −0.00, 0.01 ± 0.05 1.15, 1.10 ± 0.22
epsFor 5070, 5123 ± 78 3.28, 3.52 ± 0.07 −0.65, −0.65 ± 0.10 1.14, 1.04 ± 0.13
18Sco 5838, 5810 ± 80 4.32, 4.44 ± 0.03 0.02, −0.02 ± 0.03 1.27, 1.07 ± 0.20
alfCenB 5167, 5231 ± 20 4.33, 4.53 ± 0.03 0.14, 0.17 ± 0.10 1.06, 0.99 ± 0.31
muAra 5743, 5902 ± 66 4.05, 4.30 ± 0.03 0.22, 0.30 ± 0.13 1.32, 1.17 ± 0.13
betVir 6259, 6083 ± 41 4.06, 4.10 ± 0.02 0.18, 0.19 ± 0.07 1.51, 1.33 ± 0.09
epsEri 5079, 5076 ± 30 4.54, 4.60 ± 0.03 −0.14, −0.14 ± 0.06 1.11, 1.14 ± 0.05
etaBoo 6183, 6099 ± 28 3.84, 3.80 ± 0.02 0.27, 0.27 ± 0.08 1.52, 1.52 ± 0.19
HD 22879 5907, 5868 ± 89 3.98, 4.27 ± 0.03 −0.80, −0.91 ± 0.05 1.24, 1.05 ± 0.19
HD 49933 6718, 6635 ± 91 4.16, 4.20 ± 0.03 −0.36, −0.46 ± 0.08 1.51, 1.46 ± 0.35
HD 84937 6481, 6356 ± 97 3.91, 4.15 ± 0.06 −2.00, −1.99 ± 0.02 (3) 1.76, 1.39 ± 0.24
Procyon 6686, 6554 ± 84 3.91, 3.99 ± 0.02 0.03, −0.04 ± 0.08 1.83, 1.66 ± 0.11
tauCet 5349, 5414 ± 21 4.26, 4.49 ± 0.01 −0.52, −0.54 ± 0.03 1.00, 0.89 ± 0.28

⟨ref-fit⟩ −29 ± 88 0.09 ± 0.16 0.02 ± 0.09 −0.16 ± 0.18

Notes. In order to be consistent with our reference solar [Fe/H] scale, we subtracted 0.05 dex from Jofré et al. (2015) and 0.03 dex from Amarsi et al. (2016) metallicities.

References. (1)Karovicova et al. (2018). (2)Creevey et al. (2019). (3)Amarsi et al. (2016).

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