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We have expanded the sample of observed white dwarfs in the rich open clusterNGC 2099 (M37) with the Keck Low-Resolution Imaging Spectrometer. Of 20 whitedwarf candidates, the spectroscopy shows 19 to be true white dwarfs with 14 ofthese having high S/N. We find 11 of these 14 to be consistent with singlyevolved cluster members. They span a mass range of $\sim$0.7 to 0.95 M$_\odot$,excluding a low-mass outlier, corresponding to progenitor masses of $\sim$3 to4 M$_\odot$. This region of the initial final mass relation (IFMR) has largescatter and a slope that remains to be precisely determined. With this largesample of white dwarfs that belong to a single age and metallicity population,we find an initial-final mass relation of (0.171$\pm$0.057)M$_{\rminitial}$+0.219$\pm$0.187 M$_\odot$, significantly steeper than the linearrelation adopted over the full observed white dwarf mass range in many previousstudies. Comparison of this new relation from the solar metallicity NGC 2099 to18 white dwarfs in the metal-rich Hyades and Praesepe shows that their IFMRalso has a consistently steep slope. This strong consistency also suggests thatthere is no significant metallicity dependence of the IFMR at this mass andmetallicity range. As a result, the IFMR can be more reliably determined withthis broad sample of 29 total white dwarfs giving M$_{\rmfinal}$=(0.163$\pm$0.022)M$_{\rm initial}$+0.238$\pm$0.071 M$_\odot$ fromM$_{\rm initial}$ of 3 to 4 M$_\odot$. A steep IFMR in this mass rangeindicates that the full IFMR is nonlinear.

Initial-Final Mass Relation for 3 to 4 M$_\odot$ Progenitors of White Dwarfs from the Single Cluster NGC 2099