  We follow the collapse in axisymmetry of a uniformly rotating, supermassive
star (SMS) to a supermassive black hole (SMBH) in full general relativity. The
initial SMS of arbitrary mass $M$ is marginally unstable to radial collapse and
rotates at the mass-shedding limit. The collapse proceeds homologously early on
and results in the appearance of an apparent horizon at the center. Although
our integration terminates before final equilibrium is achieved, we determine
that the final black hole will contain about 90% of the total mass of the
system and have a spin parameter $J/M^2 \sim 0.75$. The remaining gas forms a
rotating disk about the nascent hole.
