Open Access

Fig. 13.

image

Mass distribution of our GDR2 candidate members plus the WDs progenitors as recovered from the COLIBRI isochrone. For comparison, we also show the empirical determination of the mass distribution from: (i) the Pleiades cluster from Bouy et al. (2015b), and (ii) the Hyades cluster from Goldman et al. (2013) for masses above 0.15 M, and Bouvier et al. (2008) for masses below 0.15 M.

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