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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



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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