Table 3.
Comparison between the stellar parameters derived in this study (Table 2) with their Bayesian estimates from Stock et al. (2018).
| HD | HIP | Tcolour | Teff | log(L/L⊙) | Mass |
log g | ||||
|---|---|---|---|---|---|---|---|---|---|---|
| (K) | (K) | (M⊙) | (M⊙) | |||||||
| (1) | (2) | (1) | (2) | (1) | (2) | (1) | (2) | |||
| 27497 | 20268 | RGB | 5141 | 5134 | 1.75 | 1.78 | 3.0 | 2.64 | 3.0 | 2.88 |
| HB | 5141 | 5074 | 1.75 | 1.79 | 3.0 | 2.24 | 3.0 | 2.77 | ||
| 116292 | 65301 | RGB | 4837 | 4896 | 1.76 | 1.84 | 2.5 | 2.23 | 2.77 | 2.66 |
| HB | 4837 | 4908 | 1.76 | 1.84 | 2.0 | 1.93 | 2.67 | 2.61 | ||
| 212320 | 110532 | RGB | 5660 | 4814 | 1.92 | 1.98 | – | 1.89 | – | 2.43 |
| HB | 5660 | 4825 | 1.92 | 1.96 | – | 1.64 | – | 2.37 | ||
Notes. (1): This work; (2): Stock et al. (2018). There are two different estimates, one corresponding to the location on the RGB, and the other to the location on the Horizontal Branch (HB, or “red clump”).
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