Other
Scientific paper
Jul 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008hst..prop11779u&link_type=abstract
HST Proposal ID #11779. Cycle 17
Other
Scientific paper
Although predicted by theory more than 30 years ago, the possible existence and properties of intermediate-mass black holes {IMBHs} could not be probed by observations up until very recently. IMBHs are expected theoretically to form at the centers of dense star clusters through various dynamical processes and indeed the most promising observational signatures for IMBHs are in the cores of dense globular clusters {GCs}, where the evidence now comes from both the stellar velocity distribution and the surface brightness profile near the cluster center. However, interpretation of the data and, in particular, constraints on central IMBH masses, require the use of detailed cluster dynamical models. Here we propose to model GCs that harbor IMBHs with our state-of-the-art Monte Carlo cluster code. This Monte Carlo code is orders of magnitude faster than other, "direct summation" N-Body codes, and now incorporates all relevant physical processes, including both stellar dynamics and stellar evolution, thereby allowing us for the first time to make detailed and direct comparisons with observations. By directly comparing our predicted velocity dispersion and surface brightness profiles with observations, we will be able to place strong constraints on the masses of a central IMBH. In particular, with our detailed dynamical models we should be able to unambiguously prove or disprove the presence of a 40,000 solar mass IMBH at the center of omega Cen, suggested by recent HST data of Noyola et al. {2008}.;
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