increasing contamination by old binaries to the sample “Young". Moreover, a small number of main sequence stars with $G-G_{\rm RP} \leq $ 0.34 may be also field stars, which can be identified and excluded by their different kinematics.

We discussed the CMDs without considering a possible extinction towards the sample of our stars from the BS. One may expect that its influence is rather small since our stars are all nearby ($\varpi \geq 7 $mas). On the other hand, they are actually located within the Sco-Cen association and may not be far away from or behind gas and molecular clouds. However, from Figure \[HRDnew\_fig2.pdf\] we note a good agreement between the 400 Myr isochrone and the main sequence of older BS stars of intermediate masses, and there is no reason to assume a significant extinction towards the stars in the BS. To verify this result, we also considered CMDs in other pass-bands including the near-infrared (J, K$_S$) from 2MASS [@2006AJ....131.1163S], and Gaia BP. Nevertheless, any attempt to introduce a correction for de-reddening led to a poorer fittings of isochrones to observations in the CMDs. Of course we cannot exclude that some individual stars may be significantly reddened, especially if we 