Central Dynamics of Globular Clusters: the Case for a Black Hole in ω Centauri

• Published in: Proceedings of the International Astronomical Union Vol. 3; no. S246; pp. 341 - 345
• Main Authors: Noyola, Eva, Gebhardt, Karl, Bergmann, Marcel
• Format: Journal Article
• Language: English
• Published: Cambridge, UK Cambridge University Press 01.09.2007
• Subjects: Anisotropy; Astronomy; Black holes; Contributed Papers; Dwarf galaxies; Globular clusters; Kinematics; Relaxation time; Star clusters; Stellar evolution; Surface brightness; globular clusters: individual (Omega Centauri); Galaxy: kinematics and dynamics
• DOI: 10.1017/S1743921308015895
• ISSN: 1743-9213

The globular cluster ω Centauri is one of the largest and most massive members of the Galactic system. Its classification as a globular cluster has been challenged making it a candidate for being the stripped core of an accreted dwarf galaxy; this and the fact that it has one of the largest velocity dispersions for star clusters in our galaxy makes it an interesting candidate for harboring an intermediate mass black hole. We measure the surface brightness profile from integrated light on an HST/ACS image, and find a central power-law cusp of logarithmic slope -0.08. We also analyze Gemini GMOS-IFU kinematic data for a 5”x5” field centered on the nucleus of the cluster, as well as for a field 14″ away. We detect a clear rise in the velocity dispersion from 18.6 kms−1 at 14″ to 23 kms−1 in the center. Given the very large core in ω Cen (2.58'), an increase in the dispersion in the central 10″ is difficult to attribute to stellar remnants, since it requires too many dark remnants and the implied configuration would dissolve quickly given the relaxation time in the core. However, the increase could be consistent with the existence of a central black hole. Assuming a constant M/L for the stars within the core, the dispersion profile from these data and data at larger radii implies a black hole mass of 4.0+0.75−1.0×104M⊙. We have also run flattened, orbit-based models and find a similar mass. In addition, the no black hole case for the orbit model requires an extreme amount of radial anisotropy, which is difficult to preserve given the short relaxation time of the cluster.