The Supermassive Black Hole at the Heart of Centaurus A: Revealed by the Kinematics of Gas and Stars

At less than 4Mpc distance the radio galaxy NGC5128 (CentaurusA) is the prime example to study the supermassive black hole and its influence on the environment in great detail. To model and understand the feeding and feedback mechanisms one needs an accurate determination of the mass of the supermassive black hole. The aim of this review is to give an overview of the recent studies that have been dedicated to measure the black hole mass in CentaurusA from both gas and stellar kinematics. It shows how the advancement in observing techniques and instrumentation drive the field of black hole mass measurements and concludes that adaptive optics assisted integral field spectroscopy is the key to identify the effects of the AGN on the surrounding ionised gas. Using data from SINFONI at the ESO Very Large Telescope, the best-fit black hole mass is M_BH=4.5(+1.7,-1.0)×10⁷M_solar (from H₂ kinematics) and M_BH=(5.5+/-3.0)×10⁷M_solar (from stellar kinematics). This is one of the cleanest gas-versus-star comparisons of a M_BH determination, and brings CentaurusA into agreement with the M_BH-σ relation.