  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 HST}/ACS 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 5x5 arcsec field centered on
the nucleus of the cluster, as well as for a field 14 arcsecaway. We detect a
clear rise in the velocity dispersion from 18.6 km/s at 14 arcsec to 23 km/s 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} times 10^4 M_sun, 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.
