Measurements of V56 and the eclipsing binaries V18 and V20 (left panels) and cluster CMDs (middle and right panels) compared to Victoria model isochrones and ZAHB loci as described in Brogaard et al. (2012). Uncertainties shown in the left panels are 1σ and 3σ for mass and radius of V18 and V20, but only 1σ for V56, and 1σ for all T_eff values. 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 zero to twice the mean mass loss found from asteroseismology by Miglio et al. (2012).