I review recent studies about the gravitational potential and stellar dynamics of M 87 in particular, and the dynamics of the stars in the presence of a super-massive central black hole, in general.
At large radii, investigations of both the X-ray emitting gas and the velocity distribution of globular clusters indicate the presence of large amounts of non-luminous matter, possibly belonging to the inner parts of the Virgo cluster.
At small radii, there is no evidence from the stellar kinematics, at most a hint, for the existence of a central point mass, whereas the gas dynamics reveal the presence of a highly concentrated mass in the centre of M 87, possibly a super-massive black hole (bh). Given the existence of such a central mass, the stellar kinematics indicate a strong tangential anisotropy of the stellar motion inside a few arcesconds. The implications of this result for the evolution and formation history of M 87 and its central bh are discussed. I also discuss in more general terms the structural changes that a highly concentrated central mass can induce in its parent galaxy.
Black Hole Velocity Dispersion Elliptical Galaxy Planetary Nebula Central Black Hole
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.
This is a preview of subscription content, log in to check access.