Table 4
Comparison of candidate masses using both evolutionary models with isochrones and Weidner & Vink (2010) models.
| VFTS | log (Teff) | log (L) | Age | Mass | MassWV10 |
| [K] | [L⊙] | [Myr] | [M⊙] | [M⊙] | |
|
|
|||||
| 089 | 4.58 | 4.91 | 1.5 | 25 | 33 |
| 123 | 4.58 | 4.91 | 1.5 | 25 | 33 |
| 208 | 4.57 | 5.62 | 3.5 | 43 | 46 |
| 216 | 4.63 | 5.79 | 2.2 | 57 | 53 |
| 382 | 4.62 | 5.04 | 0.0 | 29 | 48 |
| 385 | 4.62 | 5.36 | 1.8 | 37 | 48 |
| 392 | 4.58 | 4.82 | 0.0 | 24 | 33 |
| 398 | 4.60 | 5.36 | 2.5 | 36 | 36 |
| 470 | 4.58 | 4.81 | 0.0 | 24 | 44 |
| 488 | 4.59 | 5.10 | 2.0 | 29 | 36 |
| 537 | 4.61 | 4.88 | 0.0 | 25 | 44 |
| 577 | 4.59 | 4.97 | 1.0 | 27 | 36 |
| 581 | 4.62 | 5.01 | 0.0 | 29 | 48 |
| 706 | 4.58 | 4.96 | 2.0 | 26 | 33 |
| 849 | 4.57 | 4.91 | 2.5 | 24 | 30 |
Notes. Derived properties of our isolated candidates (O-stars) from comparisons with evolutionary models and isochrones with a metallicity appropriate to that of the LMC (Meynet et al. 1994; Lejeune et al. 1997). Although the masses differ to those in the last column from Weidner & Vink (2010), our key conclusions are unaffected.
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