Table 3
Main results of CMFGEN modeling of Mercer 30 cluster members.
| ID | Teff [kK] | log g | νLSR [ km s-1 ] | X H a | Y He a | (H − KS)0 | R T | M ⋆ / M ⊙ | log (L⋆/L⊙) | log QH | |
|
|
|||||||||||
| Mc30-1 | 32.2 | 3.1c | var. (binary)b | 0.43 | 0.57 | −0.047 | 49.4 | 99c | 6.51 | 50.15 | |
| Mc30-2 | 21.2 | 2.4c | 38 | 0.61 | 0.37 | 0.011 | 79.8 | 51c | 6.02 | 48.84 | |
| Mc30-3 | 39.3 | 3.80 | 22 | 0.71 | 0.28 | −0.112 | 222.0 | 73 | 5.83 | 49.54 | |
| Mc30-5 | 36.7 | 3.80 | 20 | 0.71 | 0.28 | −0.110 | 172.9 | 19 | 5.13 | 48.75 | |
| Mc30-6a | 29.9 | 3.1c | var. (binary)b | 0.71 | 0.28 | 0.003 | 61.1 | 62c | 6.13 | 49.67 | |
| Mc30-6b | 30.5 | 3.1c | 42 | 0.71 | 0.28 | −0.063 | 61.9 | 54c | 6.03 | 49.61 | |
| Mc30-7 | 41.4 | 3.6c | var. (binary)b | 0.33 | 0.66 | 0.036 | 26.6 | 60c | 6.24 | 50.06 | |
| Mc30-8 | 38.1 | 3.5c | 31 | 0.42 | 0.57 | 0.097 | 18.5 | 49c | 6.07 | 49.86 | |
| Mc30-9 | 34.5 | 3.50 | var. (binary)b | 0.71 | 0.28 | −0.107 | 189.8 | 61 | 5.83 | 49.44 | |
| Mc30-10 | 39.5 | 3.65 | var. (binary)b | 0.71 | 0.28 | −0.096 | 178.1 | 42 | 5.75 | 49.51 | |
| Mc30-11 | 36.8 | 3.65 | 35 | 0.71 | 0.28 | −0.102 | 178.1 | 73 | 5.87 | 49.53 | |
| Mc30-13 | 36.3 | 3.65 | var. (binary)b | 0.71 | 0.28 | −0.086 | 189.8 | 46 | 5.64 | 49.30 | |
| Mc30-18 | 35.5 | 3.65 | var. (binary)b | 0.71 | 0.28 | −0.098 | 99.2 | 34 | 5.48 | 49.08 | |
| Mc30-19 | 36.0 | 3.50 | 34 | 0.71 | 0.28 | −0.104 | 253.0 | 40 | 5.72 | 49.40 | |
| Mc30-22 | 32.5 | 3.80 | 25 | 0.71 | 0.28 | −0.111 | 382.8 | 17 | 4.87 | 48.19 | |
Notes.
The varying radial velocities of binary stars are shown in Table 5.
Models with dense winds whose surface gravities cannot be reliably inferred; masses have been estimated using the method of Gräfener et al. (2011) (see text for a detailed description).
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