  We present black hole mass measurements from kinematic modeling of
high-spatial resolution integral field spectroscopy of the inner regions of 9
nearby (ultra-)luminous infrared galaxies in a variety of merger stages. These
observations were taken with OSIRIS and laser guide star adaptive optics on the
Keck I and Keck II telescopes, and reveal gas and stellar kinematics inside the
spheres of influence of these supermassive black holes. We find that this
sample of black holes are overmassive ($\sim10^{7-9}$ M$_{Sun}$) compared to
the expected values based on black hole scaling relations, and suggest that the
major epoch of black hole growth occurs in early stages of a merger, as opposed
to during a final episode of quasar-mode feedback. The black hole masses
presented are the dynamical masses enclosed in $\sim$25pc, and could include
gas which is gravitationally bound to the black hole but has not yet lost
sufficient angular momentum to be accreted. If present, this gas could in
principle eventually fuel AGN feedback or be itself blown out from the system.
