Table A.1
Information about 54 spectroscopically known stars with Teff and log L/L⊙ estimated by Crowther et al. (2016, second and third columns).
| HSH95 | Teff [kK] | log L/L⊙ | age [Myr] | E(J−K) | Ks | J | Minitial | Mact | N2 | N1 |
|
|
||||||||||
| 3 |
|
|
|
|
11.07 ± 0.04 | 11.33 ± 0.13 |
|
|
3 | 1 |
| 5 |
|
|
|
|
11.32 ± 0.04 | 11.55 ± 0.13 |
|
|
3 | 0 |
| 20 |
|
|
|
|
12.73 ± 0.04 | 12.75 ± 0.13 |
|
|
2 | 0 |
| 24 |
|
|
|
|
13.05 ± 0.04 | 12.95 ± 0.13 |
|
|
3 | 0 |
| 27 |
|
|
|
|
13.27 ± 0.04 | 13.18 ± 0.13 |
|
|
1 | 1 |
| 21 |
|
|
|
|
13.09 ± 0.04 | 13.00 ± 0.13 |
|
|
1 | 1 |
| 86 |
|
|
|
|
14.80 ± 0.05 | 14.80 ± 0.13 |
|
|
2 | 0 |
| 66 |
|
|
|
|
14.42 ± 0.04 | 14.31 ± 0.13 |
|
|
2 | 0 |
| 6 |
|
|
|
|
11.44 ± 0.04 | 11.77 ± 0.13 |
|
|
2 | 1 |
| 58 |
|
|
|
|
13.91 ± 0.04 | 13.78 ± 0.13 |
|
|
0 | 0 |
| 70 |
|
|
|
|
14.20 ± 0.04 | 14.06 ± 0.13 |
|
|
1 | 1 |
| 30 |
|
|
|
|
13.65 ± 0.04 | 13.62 ± 0.13 |
|
|
2 | 0 |
| 89 |
|
|
|
|
14.69 ± 0.04 | 14.62 ± 0.13 |
|
|
2 | 0 |
| 62 |
|
|
|
|
14.35 ± 0.04 | 14.28 ± 0.13 |
|
|
4 | 0 |
| 19 |
|
|
|
|
13.05 ± 0.04 | 13.24 ± 0.13 |
|
|
2 | 1 |
| 50 |
|
|
|
|
13.96 ± 0.04 | 13.82 ± 0.13 |
|
|
2 | 0 |
| 90 |
|
|
|
|
14.83 ± 0.05 | 14.88 ± 0.13 |
|
|
1 | 0 |
| 141 |
|
|
|
|
15.40 ± 0.05 | 15.33 ± 0.13 |
|
|
4 | 0 |
| 80 |
|
|
|
|
14.77 ± 0.04 | 14.71 ± 0.13 |
|
|
1 | 0 |
| 35 |
|
|
|
|
14.00 ± 0.04 | 14.04 ± 0.13 |
|
|
2 | 0 |
| 78 |
|
|
|
|
14.68 ± 0.04 | 14.76 ± 0.13 |
|
|
0 | 0 |
| 73 |
|
|
|
|
14.38 ± 0.04 | 14.24 ± 0.13 |
|
|
2 | 0 |
| 92 |
|
|
|
|
14.87 ± 0.04 | 14.96 ± 0.13 |
|
|
1 | 0 |
| 143 |
|
|
|
|
15.11 ± 0.04 | 14.93 ± 0.13 |
|
|
4 | 0 |
| 112 |
|
|
|
|
14.78 ± 0.04 | 14.61 ± 0.13 |
|
|
3 | 1 |
| 135 |
|
|
|
|
15.32 ± 0.04 | 15.17 ± 0.13 |
|
|
3 | 1 |
| 69 |
|
|
|
|
14.39 ± 0.04 | 14.29 ± 0.13 |
|
|
3 | 0 |
| 52 |
|
|
|
|
14.20 ± 0.04 | 14.10 ± 0.13 |
|
|
2 | 0 |
| 48 |
|
|
|
|
13.58 ± 0.04 | 13.41 ± 0.13 |
|
|
3 | 0 |
| 94 |
|
|
|
|
14.85 ± 0.04 | 14.69 ± 0.13 |
|
|
2 | 0 |
| 115 |
|
|
|
|
15.46 ± 0.04 | 15.53 ± 0.13 |
|
|
1 | 0 |
| 132 |
|
|
|
|
15.36 ± 0.04 | 15.38 ± 0.13 |
|
|
2 | 0 |
| 36 |
|
|
|
|
12.96 ± 0.04 | 12.86 ± 0.13 |
|
|
1 | 0 |
| 173 |
|
|
|
|
15.63 ± 0.04 | 15.70 ± 0.13 |
|
|
3 | 0 |
| 75 |
|
|
|
|
14.78 ± 0.04 | 14.84 ± 0.13 |
|
|
2 | 0 |
| 114 |
|
|
|
|
15.26 ± 0.04 | 15.33 ± 0.13 |
|
|
1 | 0 |
| 108 |
|
|
|
|
15.59 ± 0.04 | 15.71 ± 0.13 |
|
|
2 | 0 |
| 31 |
|
|
|
|
13.62 ± 0.04 | 13.69 ± 0.13 |
|
|
1 | 0 |
| 49 |
|
|
|
|
13.98 ± 0.04 | 13.94 ± 0.13 |
|
|
1 | 0 |
| 46 |
|
|
|
|
13.29 ± 0.04 | 13.11 ± 0.13 |
|
|
3 | 0 |
| 47 |
|
|
|
|
13.32 ± 0.04 | 13.17 ± 0.13 |
|
|
3 | 0 |
| 40 |
|
|
|
|
13.72 ± 0.04 | 13.61 ± 0.13 |
|
|
1 | 0 |
| 116 |
|
|
|
|
15.45 ± 0.04 | 15.86 ± 0.13 |
|
|
1 | 1 |
| 118 |
|
|
|
|
14.64 ± 0.04 | 14.42 ± 0.13 |
|
|
2 | 0 |
| 42 |
|
|
|
|
14.11 ± 0.04 | 14.30 ± 0.13 |
|
|
0 | 0 |
| 55 |
|
|
|
|
14.15 ± 0.04 | 14.15 ± 0.13 |
|
|
0 | 0 |
| 71 |
|
|
|
|
14.70 ± 0.04 | 14.80 ± 0.13 |
|
|
1 | 0 |
| 121 |
|
|
|
|
15.47 ± 0.04 | 15.50 ± 0.13 |
|
|
1 | 0 |
| 9 |
|
|
|
|
11.66 ± 0.04 | 11.67 ± 0.13 |
|
|
1 | 0 |
| 65 |
|
|
|
|
13.85 ± 0.04 | 13.67 ± 0.13 |
|
|
1 | 0 |
| 134 |
|
|
|
|
15.71 ± 0.04 | 15.90 ± 0.13 |
|
|
1 | 0 |
| 64 |
|
|
|
|
13.84 ± 0.04 | 13.69 ± 0.13 |
|
|
0 | 0 |
| 45 |
|
|
|
|
13.63 ± 0.04 | 13.37 ± 0.13 |
|
|
1 | 0 |
| 123 |
|
|
|
|
15.61 ± 0.04 | 15.88 ± 0.13 |
|
|
0 | 0 |
Notes. Using PARSEC evolutionary isochrones (0.1 to 8 Myr), we estimated the age, color excess, and initial and actual stellar masses (columns four, five, eight, and nine). IRDIS Ks and J magnitudes are given in columns six and seven. N2 and N1 are the number of visual companions for each source in a radius of 0.2′′ and 0.1′′, respectively. The identifications (ID) of the sources are from Hunter et al. (1995). Note that we are also limited by the evolutionary tracks up to 350 M⊙, which explains zero error bars for very bright stars.
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