outside 2 $r_t$ and in the tails. For these groups we found a contamination of 0.83 stars (group a), 0.69 stars (group b), and 46.1 stars or 11.8% (group c). These values refer only to the contamination within our 5-D approach. At this stage it is also appropriate to estimate the possible field star contamination that comes from the fact that we did not consider radial velocities for estimating membership, since radial velocity data are only measured for a small sub-set of stars in the BS. Nevertheless, for 245 stars in the PrS radial velocities are available in Gaia DR2. Only 8 of them (3.3%) have radial velocities inconsistent with Praesepe’s space velocity. The contamination increases from 1.2% within the tidal radius to 10% outside 2 $r_t$. Combining these 2 kinds of contamination we expect a total contamination between about 50 to 100 stars for our Praesepe Sample.

![Colour-absolute-magnitude diagram (CAMD) $M_G$ versus $G_{BP} - G_{RP}$ of the 1393 stars of Praesepe and its tails. Stars are colour-coded by their $p_{cont}$. In addition we plot a PARSEC isochrone (Z = 0.02) with $\log \rm{t}$ = 8.85, and $E(B-V)$ = 0.027 mag.[]{data-label="Figure3"}](Figure3.pdf){width="49.00000%"}

Astrophysical properties of Praesepe {#CAMDs}
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In Fig. \[Figure3\] 