Table 2
Parameters of the stellar sample.
| Target | Sp. type | B−V | Teff [K] | log ɡ | [Fe/H] | υ sin i [km s−1] | M⋆ [M⊙] | R⋆[R⊙] | L⋆[L⊙] | References |
|---|---|---|---|---|---|---|---|---|---|---|
| Gl 229 | M1V | 1.48 | 3733± 50 | 5.02 ± 0.25 | −0.05 + 0.25 | 2.6 ± 1.0 | 0.58 ±− |  |
– | 1,2,3,4 |
| HD 36003 | K5V | 1.14 | 4647 ± 88 | 4.31 ± 0.21 | −0.2 ± 0.06 | 2.063 ± 0.116 | 0.75 ± 0.008 | 0.7 ± 0.02 | – | 4,5,6 |
| HD 85512 | K6V | 1.18 | 4715 ± 102 | 4.39 ± 0.28 | −0.32 ± 0.03 | 2.194 ± 0.118 |  |
 |
– | 4,5,6 |
| HD 154577 | K2.5V | 0.89 | 4881 ± 44 | 4.61+0.06 | −0.56 ± 0.03 | 0.2 ± 0.3 |  |
0.68 ± 0.02 | – | 4,7 |
| HD 215152 | K3V | 0.99 | 4935 ± 76 | 4.4 ±0.14 | −0.1 ± 0.04 | 1.922 ± 0.059 | 0.77 ± 0.015 | 0.73 ± 0.02 | – | 5,6,8 |
| HD 211038 | G9.5IV | 0.90 | 5009 ± 44 | 3.87 + 0.06 | −0.13 ± 0.03 | 2.7 ± 0.5 |  |
 |
– | 4,7 |
| HD 192310 | K2V | 0.91 | 5080 ± 25 | 4.55 ± 0.03 | 0.0 ± 0.02 | 2.0 ± 0.3 |  |
 |
– | 4,7 |
| HD 128621 | K1V | 0.88 | 5178 ± 22 | 4.56 ± 0.03 | 0.15 ± 0.01 | 0.9 ± 0.3 |  |
0.88 ±0.02 | – | 4,7 |
| HD 21693 | G9V | 0.78 | 5430 ± 26 | 4.37 ± 0.04 | 0.0 ± 0.02 | 1.988 ± 0.289 | 0.676 ± 0.028 | 0.888 ±0.017 | 0.618 ±0.02 | 5,6 |
| HD 56274 | G7V | 0.57 | 5681 ± 44 | 4.47 ± 0.06 | −0.5 ± 0.03 | 1.7 ± 0.5 | – | – | – | 7 |
| HD 189567 | G2V | 0.64 | 5713 ± 25 | 4.45 ± 0.03 | –0.18 ± 0.02 | 1.2 ± 0.3 |  |
1.04 ±0.03 | – | 4,7 |
| HD 45184 | G2V | 0.62 | 5810 ± 44 | 4.37 ± 0.06 | 0.03 ± 0.03 | 2.5 ± 0.5 |  |
 |
– | 4,7 |
Notes. The columns indicate the target name, spectral type, B–V color, effective temperature, surface gravity, metallicity, projected rotational velocity, mass, radius, luminosity, and references. The stars are ordered by effective temperature. For HD 21693, the mass and radius were computed using the effective temperature, surface gravity, and luminosity, as is described in the text.
References. 1: Kuznetsov et al. (2019), 2: Hojjatpanah et al. (2020), 3: Tuomi et al. (2014), 4: Takeda et al. (2007), 5: Sousa et al. (2008), 6: Soto & lenkins (2018), 7: Valenti & Fischer (2005), 8: Delisle et al. (2018).
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