Fig. 2
Histogram with 100 bins of the brightness distribution in our M dwarf sample. The red line shows the distribution according to the Besançon model (Robin et al. 2003). Our fields include more bright stars than predicted by the Besançon model, but the number of stars is in good agreement for stars with magnitudes i′ ≥ 14.5 mag. We further detail our stellar classification method in Sect. 3.
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