found that the brighter part of the CMD is appropriately described by the Parsec isochrones, whereas the CIFIST isochrones better fit the pre-main-sequence part for stars less massive than 1.4M$_{\odot}$. [Here we note that the CIFIST isochrones use the pre-launch filter profiles of @Jordi10, while the Parsec isochrones use the profiles of @Evans18, both in the Vega system.]{}

The difference between the two observed sequences is too large to be explained by unresolved binaries of main sequence stars in this field. Consequently, the upper sequences must be attributed to young pre-main sequence stars. To separate the old and young population we made a cut along the 40 Myr CIFIST isochrone from the faintest stars up to the locus ( $G-G_{\rm RP}$, $M_{\rm G}$) = (0.34, 3.22), corresponding to 1.4 M$_{\odot}$, and continue on the Parsec 40 Myr isochrone for brighter stars. The actual separation is shown in Fig. \[HRDnew\_fig3.pdf\]. We additionally discarded a small number of scattered stars which we attribute to older red giants. The sub-sample of young stars (2,659) in the BS is called “Young", the complement (1,284 stars) “Old". We note that beginning at the turnover at ( $G-G_{\rm RP}$, $M_{\rm G}$) = (0.75,6.0) there may be 