Fig. 4
Measurements of the eclipsing binaries V18 and V20 (left panels) and cluster CMDs (middle and right panels) compared to Victoria model isochrones and ZAHB loci following the procedure described in Sect. 3.2. Uncertainties shown in the left panels are 1σ and 3σ for mass and radius, and 1σ for Teff. GS_98 denotes the solar abundance pattern of Grevesse & Sauval (1998). The thick part of the ZAHB corresponds to masses with an RGB mass-loss from 0 to twice the mean mass loss found from asteroseismology (Miglio et al. 2012).
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