been rated as a member of Praesepe by @2019MNRAS.483.3098S. All WDs by @2019MNRAS.483.3098S are confirmed by us with the exception of which did not pass the quality cuts in Sec. \[prep\]. Three white dwarfs, , and in the tidal tails have not been mentioned before as being related to Praesepe, but now we can confirm their provenance from Praesepe.

![Number density $D$, mass density $\rho$, and average mass per star $\overline{m}$ as a function of the logarithm of the distance from the centre ${r_{c}}$. A bin size of 2 pc in steps of 1 pc is used within 10 pc; beyond this the bin size is increased to 4 pc to get a better signal-to-noise ratio. From top to bottom: the number density $D$ as a green curve, the observed mass density (blue curve) and a density distribution (black dashed line) from a Plummer model (Eq. \[pluden\]) with $M_t$ = 483 $\rm{M}_{\odot}$ and ${r_{co}}$ = 3.7 pc, the average mass per star ($\rho/D$) as a red line. []{data-label="Figure4"}](Figure4.pdf){width="49.00000%"}

A short comparison between Praesepe and the Hyades {#Praehya}
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In Fig. \[Figure5\] we show the location on the sky of Praesepe (yellow pluses) and the Hyades (cyan pluses) as well as 