The V,B − V CMD of NGC 6791 compared to the isochrone and ZAHB from Fig. 4 extended to bluer colours. Only stars with a non-zero proper motion probability in preliminary measurements of Kyle Cudworth (priv. comm.) are shown. Circles represent stars which were selected as suspected HB stars in the proper motion study by Platais et al. (2011). The open circle, which belongs to this group, is the star 2–17. The square represents a cluster member that does not show the seismic signature of a RC star and has a seismic mass which is larger than that of the RGB stars (Miglio et al. 2012; Corsaro et al. 2012). Also shown is an extended ZAMS and main-sequence evolutionary tracks for stars with masses of 1.4 and 2.2 M_⊙ taking into account convective core overshooting as in VandenBerg et al. (2006). The ends of the tracks are connected to show the terminal age main sequence (TAMS) in this mass interval. The dashed line is the 2.2 M_⊙ track shifted down along the ZAMS to estimate the mass of 2–17. Numbers indicate masses at the given positions.