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|
|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|
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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