Table 3
Summary of isochrone properties relevant for the mass derivation.
| Isochrone name | Description | Wolf-Rayet mass | Stars with ambiguous mass assignments | |||
| PMS → MS | MS → post-MS | |||||
| mass range | No. of stars | mass range | No. of stars | |||
| (M⊙) | (M⊙) | (M⊙) | ||||
|
|
||||||
| 3 Myr Padova | MSa + PMSb | 85–100 | 2.1–5.5 | 150 | 42.3–84.4 | 11 |
| 4 Myr Padova | MSa + PMSb | 51–65 | 1.9–4.6 | 146 | 39.9–50.8 | 5 |
| 5 Myr Padova | MSa + PMSb | 37–40 | 1.8–4.0 | 146 | 33.5–35.4 | 3 |
| 4 Myr Geneva | MSc | 48–60 | 45.8–47.3 | 0 | ||
Notes.
Padova isochrone with solar metallicity for m > 4 M⊙ (Marigo et al. 2008).
Pre-main sequence parts of the isochrones (m ≤ 4 M⊙) are derived from Pisa-FRANEC PMS stellar models (Degl’Innocenti et al. 2008; see Gennaro et al. 2011, for the combination with the Padova isochrones).
Geneva isochrone with solar metallicity and enhanced mass loss for high mass stars, M > 15 M⊙ (Lejeune & Schaerer 2001).
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