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We follow the collapse in axisymmetry of a uniformly rotating, supermassivestar (SMS) to a supermassive black hole (SMBH) in full general relativity. Theinitial SMS of arbitrary mass $M$ is marginally unstable to radial collapse androtates at the mass-shedding limit. The collapse proceeds homologously early onand results in the appearance of an apparent horizon at the center. Althoughour integration terminates before final equilibrium is achieved, we determinethat the final black hole will contain about 90% of the total mass of thesystem and have a spin parameter $J/M^2 \sim 0.75$. The remaining gas forms arotating disk about the nascent hole.Comment: 12 pages, to appear in ApJ

Collapse of a Rotating Supermassive Star to a Supermassive Black Hole: Fully Relativistic Simulations