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The masses of the supermassive black-holes found in galaxy bulges arecorrelated with a multitude of galaxy properties, leading to suggestions thatgalaxies and black-holes may evolve together. The number of reliably measuredblack-hole masses is small, and the number of methods for measuring them islimited, holding back attempts to understand this co-evolution. Directlymeasuring black-hole masses is currently possible with stellar kinematics (inearly-type galaxies), ionised-gas kinematics (in some spiral and early-typegalaxies) and in rare objects which have central maser emission. Here we reportthat by modelling the effect of a black-hole on the kinematics of molecular gasit is possible to fit interferometric observations of CO emission and therebyaccurately estimate black hole masses. We study the dynamics of the gas in theearly-type galaxy NGC4526, and obtain a best fit which requires the presence ofa central dark-object of 4.5(+4.2-3.0)x10^8 Msun (3 sigma confidence limit).With next generation mm-interferometers (e.g. ALMA) these observations could bereproduced in galaxies out to 75 megaparsecs in less the 5 hours of observingtime. The use of molecular gas as a kinematic tracer should thus allow one toestimate black-hole masses in hundreds of galaxies in the local universe, manymore than accessible with current techniques.

A black-hole mass measurement from molecular gas kinematics in NGC4526