a total of 100 M$_\odot$ in low-mass stars with $m$ &lt; 0.25 M$_\odot$ would be contained in the inner part of the cluster, the tidal radius would only rise to 11.5 pc. In models of star clusters the Lagrangian radius for 50% of the cluster mass, plays an important role and is called half-mass radius $r_h$. Estimated from a tidal mass of 483 $\rm{M}_{\odot}$, the half-mass radius $r_h$ is 4.8 pc at the present state of evolution of Praesepe.

@2007AJ....134.2340K made an inventory of the Praesepe cluster about a decade ago. They used data from the SDSS, 2MASS, USNOB1.0, and UCAC-2.0 surveys, and analysed proper motions and photometry over 300 $\deg^2$ on the sky. They found 1010 stars in Praesepe being candidate members with probability &gt; 80$\%$. These authors also estimated the total mass of the cluster to be 550 $\pm$ 40 M$_\odot$ and a tidal radius of 11.5 $\pm$ 0.3 pc. The small disagreement between our tidal radius and that from @2007AJ....134.2340K comes partly from their assumed values of $A$ = 14.4 $\rm{kms}^{-1}\rm{kpc}^{-1}$ and $B$ = -12.0 $\rm{kms}^{-1}\rm{kpc}^{-1}$. With the values from @2017MNRAS.468L..63B, @2007AJ....134.2340K would have got $r_t$ = 11.25 pc given that their derived total mass of 550 