Table 6
Stellar parameters of all stars investigated in this paper.
| Parameter [Unit] | NEXA | Interferometry | PySME | Parameter [Unit] | NEXA | Interferometry | PySME |
|---|---|---|---|---|---|---|---|
| ϵ Eri | M/H, υ sin i | Teff, log g, M/H | HD 179949 | M/H, υ sin i | |||
| Teff [K] |  [1] |
5077 ± 35 [2] | 4949 ± 2 ± 191 | Teff [K] |  [1] |
– | 6301 ± 2 ± 242 |
| log g [log (cm s−2)] |  [1] |
4.61 ± 0.02 [2] | 4.210 ± 0.003 ± 0.63 | log g [log(cm s−2)] |  [1] |
– | 4.410 ± 0.003 ± 0.80 |
| [M/H] [dex] | −0 : 05 ± 0.10 [1] | −0.06 ± 0.10 [2] | −0.220 ± 0.002 ± 0.25 | [M/H] [dex] | 0.2 ± 0.1 [1] | – | 0.130 ± 0.001 ± 0.19 |
| υmic [km s−1] | (1) | – | 0.870 ± 0.004 ± 0.7 | υmic [km s−1] | (1) | – | 1.510 ± 0.004 ± 0.5 |
| υmac [km s−1] | (4) | – | 3.27 ±0.01 ± 1.8 | υmac [km s−1] | (4) | – | 7.82 ± 0.05 ± 3.0 |
| υ sin i [km s−1] | 2.4 ± 0.5 [3] | – | 0.0 ± 4.4 ± 189 | υ sin i [km s−1] | 6.52 [7] | – | 4.19 ± 0.07 ± 4.7 |
| HN Peg | M/H | Teff, log g, M/H | HD 189733 | M/H, υ sin i | Teff, log g, M/H | ||
| Teff [K] |  [1] |
5860 ± 83 [2] | 5941 ± 2 ± 222 | Teff [K] |  [1] |
5024 ± 60 [2] | 4910 ± 2 ± 203 |
| log g [log(cm s−2)] |  [1] |
4.43 ± 0.05 [2] | 4.370 ± 0.003 ± 0.61 | log g [log(cm s−2)] |  [1] |
4.51 ± 0.05 [2] | 4.120 ± 0.004 ± 0.65 |
| [M/H] [dex] | −0.03 ± 0.01 [1] | −0.16 ± 0.10 [2] | −0.160 ±0.001 ±0.18 | [M/H] [dex] | 0.20 ± 0.10 [1] | 0.07 ± 0.05 [2] | −0.130 ± 0.002 ± 0.27 |
| υmic [km s−1] | (1) | – | 1.480 ±0.004 ±0.6 | υmic [km s−1] | (1) | – | 0.940 ± 0.004 ± 0.7 |
| υmac [km s−1] | (4) | – | 7.46 ± 0.05 ± 5.2 | υmac [km s−1] | (4) | – | 4.52 ± 0.01 ±2.1 |
| υ sin i [km s−1] |  [4] |
– | 9.29 ± 0.03 ± 3.4 | υ sin i [km s−1] | 3.5 ± 1.0 [8] | – | 0.0 ± 1.4 ± 289 |
| HD 102195 | M/H, υ sin i | Teff, log g, M/H | 55 Cnc | M/H, υ sin i | Teff, log g, M/H | ||
| Teff [K] |  [1] |
5277 ± 60 [2] | 5223 ± 2 ± 197 | Teff [K] |  [1] |
5172 ± 18 [2] | 5140 ± 2± 228 |
| log g [log(cm s−2)] |  [1] |
4.50 ± 0.05 [2] | 4.350 ± 0.004 ± 0.64 | log g [log(cm s−2)] |  [1] |
4.43 ± 0.02 [2] | 4.370 ± 0.004 ± 0.74 |
| [M/H] [dex] | 0.05 ± 0.10 [1] | 0.10 ± 0.05 [2] | −0.070 ± 0.002 ± 0.23 | [M/H] [dex] | 0.35 ± 0.10 [1] | 0.35 ± 0.10 [2] | 0.260 ± 0.002 ± 0.28 |
| υmic [km s−1] | (1) | – | 1.110 ±0.004 ±0.6 | υmic [km s−1] | (1) | – | 0.800 ± 0.005 ± 0.7 |
| υmac [km s−1] | (4) | – | 3.87 ±0.01 ± 1.8 | υmac [km s−1] | (4) | – | 2.92 ± 0.04 ± 1.8 |
| υ sin i [km s−1] | 2.6 [5] | – | 0.0 ± 0.9 ± 220 | υ sin i [km s−1] | < 1.23 ±0.01 [9] | – | 0.0 ± 4.4 ± 189 |
| HD 130322 | M/H, υ sin i | WASP 18 | M/H, υ sin i | ||||
| Teff [K] |  [i] |
– | 5285 ± 2 ± 212 | Teff [K] |  [1] |
– | 6443 ± 2 ± 328 |
| log g [log(cm s−2)] |  [1] |
– | 4.440 ± 0.004 ± 0.60 | log g [log(cm s−2)] |  [1] |
– | 4.230 ± 0.003 ± 1.01 |
| [M/H] [dex] | 0.02 ± 0.10 [1] | – | −0.110 ±0.002 ±0.22 | [M/H] [dex] | 0.1 ± 0.1 [1] | – | 0.120 ± 0.001 ± 0.22 |
| υmic [km s−1] | (1) | – | 0.870 ± 0.004 ± 0.6 | υmic [km s−1] | (1) | – | 1.580 ± 0.004 ± 0.7 |
| υmac [km s−1] | (4) | – | 2.85 ±0.01 ± 1.8 | υmac [km s−1] | (4) | – | 8.87 ± 0.06 ± 7.3 |
| υ sin i [km s−1] | 0.5 ± 0.5 [6] | – | 0.0 ± 0.9 ± 167 | υ sin i [km s−1] | 11.0 ± 1.5 [8] | – | 10.70 ± 0.04 ± 4.7 |
Notes. For PySME both the fit uncertainty and the model uncertainty are given (see Sect. 2.7). Two sets of literature values are given. The first is from the NASA Exoplanet Archive (NEXA). These are used as initial values for the fitting procedure. The micro- and macroturbulence parameters are given in brackets ( ); as there are no existing literature values, we use general estimates instead. In the second set of values the Teff and log g are derived by interferometry if that data is available, or spectroscopy otherwise. These are used in the comparison in Sect. 6. We note that for 55 Cnc the analysis is independent of the IDL SME analysis discussed in Sect. 4.3, which used a different continuum normalization, line list, and NLTE coefficients, but instead follows the same steps as for the other targets.
References. [1] Stassun et al. (2019), [2] Yee et al. (2017), [3] Valenti & Fischer (2005), [4] Swastik et al. (2021), [5] Melo et al. (2007), [6] Hinkel et al. (2015), [7] Tsantaki et al. (2014), [8] Bonomo et al. (2017), [9] Bourrier et al. (2018).
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