  We present near-infrared integral field spectroscopy of the central
kiloparsec of NGC 1275 at the heart of the Perseus cluster of galaxies,
obtained with the UIST IFU on UKIRT. The nuclear ro-vibrational H_2 emission is
spatially resolved and is likely to originate approximately 50 pc from the
active nucleus. The Pa-alpha emission is, by contrast, spatially unresolved.
The requirements for thermal excitation of the H_2 by nuclear X-radiation, its
kinematics on sub-arcsec scales, and its stability against self-gravity,
together suggest that the observed H_2 is part of a clumpy disk rotating about
the radio-jet axis. The sharp jump in H_2 velocity across the nucleus implies a
black hole mass of 3.4E8 M(Solar), with a systematic error of 0.18 dex due to
the uncertainty in the radio jet inclination. This agrees well with the value
implied by the empirical correlation between black hole mass and stellar
velocity dispersion for nearby elliptical galaxies, and is ~100 times the
stellar mass in this region.
