Fig. 1.
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Comparison of isochrones for a range of ages from 50 Myr to 1 Gyr for the BHAC15 (dashed lines) and PARSEC models (solid lines). The polynomial fit used as a colour–mass relation is shown in magenta. While we only plot the relation for G − RP > −0.2, the fit extends to bluer colours in order to cover the most massive stars in our input catalogue.
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