  We have expanded the sample of observed white dwarfs in the rich open cluster
NGC 2099 (M37) with the Keck Low-Resolution Imaging Spectrometer. Of 20 white
dwarf candidates, the spectroscopy shows 19 to be true white dwarfs with 14 of
these having high S/N. We find 11 of these 14 to be consistent with singly
evolved 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$3 to
4 M$_\odot$. This region of the initial final mass relation (IFMR) has large
scatter and a slope that remains to be precisely determined. With this large
sample of white dwarfs that belong to a single age and metallicity population,
we find an initial-final mass relation of (0.171$\pm$0.057)M$_{\rm
initial}$+0.219$\pm$0.187 M$_\odot$, significantly steeper than the linear
relation adopted over the full observed white dwarf mass range in many previous
studies. Comparison of this new relation from the solar metallicity NGC 2099 to
18 white dwarfs in the metal-rich Hyades and Praesepe shows that their IFMR
also has a consistently steep slope. This strong consistency also suggests that
there is no significant metallicity dependence of the IFMR at this mass and
metallicity range. As a result, the IFMR can be more reliably determined with
this broad sample of 29 total white dwarfs giving M$_{\rm
final}$=(0.163$\pm$0.022)M$_{\rm initial}$+0.238$\pm$0.071 M$_\odot$ from
M$_{\rm initial}$ of 3 to 4 M$_\odot$. A steep IFMR in this mass range
indicates that the full IFMR is nonlinear.
