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Located in the Perseus cluster, NGC 1271 is an early-type galaxy with a smalleffective radius of 2.2 kpc and a large stellar velocity dispersion of 276 km/sfor its K-band luminosity of 8.9x10^{10} L_sun. We present a mass measurementfor the black hole in this compact, high-dispersion galaxy using observationsfrom the integral field spectrograph NIFS on the Gemini North telescopeassisted by laser guide star adaptive optics, large-scale integral field unitobservations with PPAK at the Calar Alto Observatory, and Hubble SpaceTelescope WFC3 imaging observations. We are able to map out the stellarkinematics on small spatial scales, within the black hole sphere of influence,and on large scales that extend out to four times the galaxy's effectiveradius. We find that the galaxy is rapidly rotating and exhibits a sharp risein the velocity dispersion. Through the use of orbit-based stellar dynamicalmodels, we determine that the black hole has a mass of (3.0^{+1.0}_{-1.1}) x10^9 M_sun and the H-band stellar mass-to-light ratio is 1.40^{+0.13}_{-0.11}M_sun/L_sun (1-sigma uncertainties). NGC 1271 occupies the sparsely-populatedupper end of the black hole mass distribution, but is very different from theBrightest Cluster Galaxies (BCGs) and giant elliptical galaxies that areexpected to host the most massive black holes. Interestingly, the black holemass is an order of magnitude larger than expectations based on the galaxy'sbulge luminosity, but is consistent with the mass predicted using the galaxy'sbulge stellar velocity dispersion. More compact, high-dispersion galaxies needto be studied using high spatial resolution observations to securely determineblack hole masses, as there could be systematic differences in the black holescaling relations between these types of galaxies and the BCGs/giantellipticals, thereby implying different pathways for black hole and galaxygrowth.

The Black Hole in the Compact, High-dispersion Galaxy NGC 1271