we show the Colour-absolute-magnitude diagram (CAMD) $M_G$ versus $G_{BP} - G_{RP}$ of the 1393 stars of the Praesepe Sample. The stars are colour-coded according to their contamination value $p_{cont}$. We also present a PARSEC-(version 1.2S)-isochrone [@2014MNRAS.444.2525C] with Z = 0.02 and $\log \rm{t}$ = 8.85, and $E(B-V)$ = 0.027 mag . The Gaia passbands from were used; we also applied the corrections to the Gaia $G$-magnitudes given in the same paper. We note here that the tails are spread over a wide part of space and, hence, the assumption of a unique reddening is not fully appropriate for tail stars. Nevertheless, over a wide range of $G_{BP} - G_{RP}$, the isochrone gives a reasonable fit to the observations except for the low-mass stars redder than about $G_{BP} - G_{RP}$ = 2.8 mag. Anyway, we used the isochrone shown in Fig. \[Figure3\] to roughly estimate individual masses via a mass-luminosity relation in the 3 Gaia photometric bands, neglecting binary issues. The incompleteness of our sample beyond $G$ $\approx$ 18 mag (see Sec. \[prep\]) creates incompleteness at $M_G$ $\approx$ 11.8 mag near the cluster centre, and brighter or fainter in the tails, depending on the individual parallax of the stars. Via our 