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The nearby lenticular galaxy NGC 1277 is thought to host one of the largestblack holes known, however the black hole mass measurement is based on lowspatial resolution spectroscopy. In this paper, we present Gemini Near-infraredIntegral Field Spectrometer observations assisted by adaptive optics. We mapout the galaxy's stellar kinematics within ~440 pc of the nucleus with anangular resolution that allows us to probe well within the region where thepotential from the black hole dominates. We find that the stellar velocitydispersion rises dramatically, reaching ~550 km/s at the center. Throughorbit-based, stellar-dynamical models we obtain a black hole mass of (4.9 \pm1.6) x 10^9 Msun (1-sigma uncertainties). Although the black hole massmeasurement is smaller by a factor of ~3 compared to previous claims based onlarge-scale kinematics, NGC 1277 does indeed contain one of the most massiveblack holes detected to date, and the black hole mass is an order of magnitudelarger than expectations from the empirical relation between black hole massand galaxy luminosity. Given the galaxy's similarities to the higher redshift(z~2) massive quiescent galaxies, NGC 1277 could be a relic, passively evolvingsince that period. A population of local analogs to the higher redshiftquiescent galaxies that also contain over-massive black holes may suggest thatblack hole growth precedes that of the host galaxy.

A 5x10^9 Solar Mass Black Hole in NGC 1277 from Adaptive Optics Spectroscopy