Gemini and Hubble Space Telescope Evidence for an Intermediate-Mass Black Hole in omega Centauri
Publication date: 03 April 2008
Authors: Noyola, E. et al.
Journal: ApJ preprint, doi:10.1086/529002
Copyright: The American Astronomical Society
The globular cluster omega Centauri is one of the largest and most massive members of the galactic system. However, its classification as a globular cluster has been challenged making it a candidate for being the stripped core of an accreted dwarf galaxy; this together with 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 HSTACS image of the center, 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 km s-1 at 14" to 23 km s-1 in the center. A rise in the velocity dispersion could be due to a central black hole, a central concentration of stellar remnants, or a central orbital structure that is radially biased.We discuss each of these possibilities. An isotropic, spherical dynamical model implies a black hole mass of 4.0+0.75-1.0 x 104 MSun, and excludes the no black hole case at greater than 99% significance. We have also run flattened, orbit-based models and find similar results. While our preferred model is the existence of a central black hole, detailed numerical simulations are required to confidently rule out the other possibilities.Link to publication