Left: Color‐velocity distribution of foreground dwarfs from the Galactic Besançon model (Robin et al. 2003), at a projected distance of 160 kpc to M31. The solid lines illustrate the cuts we used to assess the number of undetectable blue dwarfs in our M31 giant sample. Also indicated are the observed photometric errors. Right: Velocity distributions of our observed stars (shaded and dashed histograms) with ﹩V-i^{\prime }\leq 1﹩ and the expected blue dwarfs from the Besançon model (solid histogram). The fraction of unresolvable blue dwarfs in our giant sample is well below 3% and negligible.