We report the spectroscopic confirmation of four further white dwarf members of Praesepe .
This brings the total number of confirmed white dwarf members to eleven making this the second largest collection of these objects in an open cluster identified to date .
This number is consistent with the high mass end of the initial mass function of Praesepe being Salpeter in form .
Furthermore , it suggests that the bulk of Praesepe white dwarfs did not gain a substantial recoil kick velocity from possible asymmetries in their loss of mass during the asymptotic giant branch phase of evolution .
By comparing our estimates of the effective temperatures and the surface gravities of WD0833+194 , WD0840+190 , WD0840+205 and WD0843+184 to modern theoretical evolutionary tracks we have derived their masses to be in the range 0.72 - 0.76M _ { \odot } and their cooling ages \sim 300Myrs .
For an assumed cluster age of 625 \pm 50Myrs the infered progenitor masses are between 3.3 - 3.5M _ { \odot } .
Examining these new data in the context of the initial mass-final mass relation we find that it can be adequately represented by a linear function ( a _ { 0 } =0.289 \pm 0.051 , a _ { 1 } =0.133 \pm 0.015 ) over the initial mass range 2.7M _ { \odot } to 6M _ { \odot } .
Assuming an extrapolation of this relation to larger initial masses is valid and adopting a maximum white dwarf mass of 1.3M _ { \odot } , our results support a minimum mass for core-collapse supernovae progenitors in the range \sim 6.8-8.6M _ { \odot } .