the so-called core radius of a cluster. Using the tidal mass of $M_t$ = 483 $\rm{M}_{\odot}$ the best fit to the observed density distribution (blue line) in Fig. \[Figure4\] is obtained with a core radius $r_{co}$ of 3.7 pc. In the two upper panels of Fig. \[Figure4\] the core radius is seen as the distance where the slope in the density and mass distributions changes. The corresponding Plummer model (dashed line in Fig. \[Figure4\]) shows good agreement with observations. The ratio of the half-mass radius ${r_h}$ to ${r_{co}}$ in Praesepe is 1.297 which is in remarkable coincidence with the theoretical ratio of 1.305 for a Plummer model [see @1975ApJ...200..339S].

Fig. \[Figure3\] shows the presence of white dwarfs (WD) in Praesepe and its tails. In total, we find 13 white dwarfs with 9 of them inside the tidal radius of 10.77 pc. We disregard here the two objects with $M_G \approx 14$ mag and $G_{BP} - G_{RP}$ near 1. Twelve out of 13 objects are known in SIMBAD as white dwarfs or blue proper motion stars. One star is not known as a WD in SIMBAD, but it fits perfectly to the loci of the other white dwarfs and has recently 