Distribution of absolute magnitudes MG for the stars from Fig. 3 (panels a) and b)) within the colour range 1.0 ≤ (B−V) ≤ 1.1. The thick green solid line shows the distribution of MG derived from Gaia DR1 parallaxes, while the thin blue line shows the same for the Hipparcos parallaxes. The distributions are represented as kernel density estimates, using an Epanechnikov kernel (Epanechnikov 1969) with a band-width of 0.2 mag.
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