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Table 3
Adopted parameters and bolometric luminosities for the cool supergiants.
| Hosek | Damineli | |||||
|---|---|---|---|---|---|---|
| ID | SpT |
Teff (K) |
AKs (mag) |
log(L/L⊙) (dex) |
AKs (mag) |
log(L/L⊙) (dex) |
| W237 | M3-4I | 3550 | 0.54 | 5.20 | 0.66 | 5.24 |
| W20 | M3-4I | 3550 | 0.76 | 4.98 | 0.93 | 5.04 |
| W75 | M1 Ia | 4000 | 1.01 | 5.14 | 1.24 | 5.22 |
| W26 | M1-1.5 Ia | 3780 | 0.54 | 5.35 | 0.66 | 5.39 |
| W4 | F3 Ia+ | 6700 | 0.49 | 5.25 | 0.61 | 5.29 |
| W8a | F8 Ia+ | 6200 | 1.26 | 5.47 | 1.55 | 5.56 |
| W32 | F5 Ia+ | 6500 | 0.61 | 5.45 | 0.74 | 5.49 |
| W16a | A5 Ia+ | 8200 | 0.63 | 5.40 | 0.77 | 5.45 |
| W12a | F1 Ia+ | 7150 | 0.66 | 5.22 | 0.81 | 5.27 |
| W265 | F1-5 Ia+ | 6750 | 0.69 | 5.18 | 0.69 | 5.23 |
Notes. Extinction and luminosities are derived using the extinction laws of Hosek et al. (2018) and Damineli et al. (2016). For reference, Beasor et al. (2021) adopted a cluster average extinction of AK = 0.74 ± 0.08 for Wd1.
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