Monte Carlo models of Omega Centauri grow intermediate-mass black hole seeds of 500 to 5000 solar masses to about 50,000 solar masses by mergers with 30 to 40 solar mass black holes.
The Metallicity Distribution Function of Omega Centauri
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abstract
We explore the metallicity distribution function (MDF) of red giant stars in Omega Centauri from a catalogue of Washington M, T_2 and DDO51 photometry covering over 1.1 deg^2 outside the cluster core. Using updated calibrations of giant branch isometallicity loci in this filter system, photometric metallicities, guided by previously published spectroscopic abundances, are derived. Several methods are employed to correct the MDF for contamination by Galactic stars, including: (1) use of the surface gravity sensitivity of the (M-DDO51) color index to eliminate foreground dwarf stars, (2) radial velocities, and (3) membership probabilities from proper motions. The contamination-corrected MDF for Omega Cen shows a range of enrichment levels spanning nearly 2 dex in [Fe/H], and with peaks at [Fe/H]=-1.6, -1.2, and -0.9.
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Growing the Intermediate-mass Black Hole in Omega Centauri
Monte Carlo models of Omega Centauri grow intermediate-mass black hole seeds of 500 to 5000 solar masses to about 50,000 solar masses by mergers with 30 to 40 solar mass black holes.