which reduced the sample to 3946 objects. Finally we discarded three stars with relative errors of parallaxes larger than 10 per cent. In summary, from the originally 20,138 entries in our search cone 3,943 sources survived these filterings, forming an astrometrically clean sample. For the subsequent discussion we always refer to this sample as “the Basic Sample (BS)". [The stars of the BS are shown in Fig. \[SCOCEN\] as small cyan dots and outline the area of our search.]{}

Candidate selection {#candsel}
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In Fig. \[HRDnew\_fig2.pdf\] we show the Color Magnitude Diagram (CMD) of the 3,943 stars of the BS, where we plot the absolute magnitude $M_{\rm G}$ (using the parallaxes from DR2) versus the color $G-G_{\rm RP}$. For colors redder than about 0.4 mag two separate sequences show up, which we attribute to young stars (upper sequence) and old stars (lower sequence). We strengthen this in Fig. \[HRDnew\_fig2.pdf\], where we also plot the theoretical isochrones of CIFIST and Parsec [@2017ApJ...835...77M]. The red lines are the CIFIST isochrones for 10 Myr and 400 Myr, while the black lines are the 10 Myr and 400 Myr Parsec isochrones. From a comparison between the two sets of isochrones for different ages, we 