M$_\odot$ were inside 11.25 pc. Considering the fact that @2007AJ....134.2340K did not have available accurately measured trigonometric parallaxes, the coincidence of their tidal radius with ours is quite satisfactory. From their 1010 80$\%$-members we found 785 among our 1393 stars. From the remaining 225, only 77 passed the cuts in Sec.\[prep\], but were not selected as members when using our criteria.

Using the individual masses we determine the radial density and mass profiles of the cluster. In Fig. \[Figure4\] we present the number density $D$, the mass density $\rho$ , and the average mass per star as a function of the distance from the centre $r_{c}$. The bottom panel of Fig. \[Figure4\] reveals the mass segregation in Praesepe; the average mass per star ($\rho/D$) decreases from 1.17 $\rm{M}_{\odot}$ close to the centre to about 0.46 $\rm{M}_{\odot}$ at the tidal radius $r_t$. Again the apparent increase of the average mass per star towards larger distances from the centre is attributed to incompleteness at the low mass end. The mass density of Praesepe, shown in the middle part of Fig. \[Figure4\], is fitted to a Plummer model [@1915MNRAS..76..107P], where the mass density follows the equation $$\rho({r_{c}}) = \frac{3M_t}{4\pi{r_{co}}^3}\frac{1}{[1+(r_c/{r_{co}})^2]^{5/2}}.
\label{pluden}$$ Here $r_{co}$ is 