Table 3
Stellar parameters of the sample stars.
| ID# | Object | Teff | log g | y | ξ | υ sin i | ζ | RV | E (B − V) | B.C. | MV | Mbol | Mevol | R | log L/L⊙ | log τevol | dspec | dGaia(a) |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| kK | (cgs) | km s−1 | mag | mag | mag | mag | M⊙ | R⊙ | yr | pc | pc | |||||||
| 1 | Sher 25 | 20.9 | 2.61 | 0.117 | 16 | 60 | 35 | 3.40 | 1.66 | −1.920 | −7.05 | −8.97 | 25.5 | 42 | 5.48 | 6.86 | 5440 | 5740 |
| ± 0.5 | 0.06 | 0.015 | 2 | 5 | 5 | 0.1 | 0.03 | 0.34 | 0.34 | 1.7 | 7 | 0.14 | 0.04 | 700 | 800 420 | |||
| 2 | HD 13854 | 20.5 | 2.62 | 0.111 | 15 | 57 | 47 | 3.02 | 0.52 | −1.871 | −6.91 | −8.78 | 23.7 | 40 | 5.41 | 6.88 | 2320 | 2140 |
| ± 0.3 | 0.04 | 0.010 | 2 | 6 | 5 | 0.1 | 0.03 | 0.21 | 0.22 | 1.0 | 4 | 0.09 | 0.03 | 200 | 110 100 | |||
| 3 | HD 14956 | 19.2 | 2.37 | 0.127 | 16 | 49 | 55 | 2.69 | 0.97 | −1.722 | −7.55 | −9.27 | 27.2 | 57 | 5.60 | 6.81 | 2680 | 2720 |
| ± 0.3 | 0.04 | 0.010 | 2 | 7 | 5 | 0.1 | 0.03 | 0.24 | 0.24 | 1.5 | 7 | 0.10 | 0.03 | 250 | 150 130 | |||
| 4 | HD 91316 | 21.7 | 2.87 | 0.092 | 15 | 43 | 62 | 2.81 | 0.09 | −2.007 | −6.19 | −8.20 | 19.9 | 28 | 5.18 | 6.96 | 900 | 660 |
| ± 0.2 | 0.04 | 0.009 | 2 | 5 | 5 | 0.1 | 0.03 | 0.20 | 0.20 | 1.0 | 3 | 0.08 | 0.04 | 70 | 170 140 | |||
| 4a(b,c) | −5.51 | −7.52 | 10.6 | 20 | 4.90 | … | … | |||||||||||
| ± | 0.52 | 0.53 | 5.3 | 5 | 0.21 | … | … | |||||||||||
| 5 | HD 114199 | 25.6 | 3.42 | 0.119 | 14 | 135 | 50 | 3.21 | 0.59 | −2.436 | −4.86 | −7.29 | 15.7 | 13 | 4.81 | 7.03 | 3070 | 2630 |
| ± 0.4 | 0.05 | 0.010 | 2 | 9 | 10 | 0.1 | 0.03 | 0.27 | 0.27 | 2.0 | 2 | 0.11 | 0.05 | 340 | 100 100 | |||
| 6 | HD 152235 | 21.6 | 2.68 | 0.085 | 16 | 59 | 50 | 3.00 | 0.80 | −2.006 | −6.89 | −8.89 | 24.5 | 38 | 5.45 | 6.87 | 1460 | 1620 |
| ± 0.3 | 0.05 | 0.008 | 2 | 4 | 5 | 0.1 | 0.03 | 0.24 | 0.25 | 1.3 | 4 | 0.10 | 0.04 | 140 | 130 90 | |||
Notes. Uncertainties are 1σ-values, except where noted otherwise. (a)Gaia Collaboration (2016, 2021) – distances and uncertainties correspond to ‘photogeometric distances’ and associated 14th and 86th confidence percentiles (Bailer-Jones et al. 2021).(b) Alternative solution, adopting the Gaia distance for the calculation of the fundamental stellar parameters instead of the spectroscopic distance, starting from MV. (c)HD 91316 is in fact a binary star with the V magnitude difference of the two components in the range ~1 to 1.5 mag at similar Teff as discussed in Sect. 5. As the Gaia parallax is likely affected by the binary orbital motion (indicated by a high Renormalised Unit Weight Error of 2.457) and in the absence of a second line system, a further determination of the parameters of the binary components is beyond the scope of the present paper.
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