Nuclear Black Hole Formation in Clumpy Galaxies at High Redshift

Abstract

Massive stellar clumps in high redshift galaxies interact and migrate to the center to form a bulge and exponential disk in <1 Gyr. Here we consider the fate of intermediate mass black holes (BHs) that might form by massive-star coalescence in the dense young clusters of these disk clumps. We find that the BHs move inward with the clumps and reach the inner few hundred parsecs in only a few orbit times. There they could merge into a supermassive BH by dynamical friction. The ratio of BH mass to stellar mass in the disk clumps is approximately preserved in the final ratio of BH to bulge mass. Because this ratio for individual clusters has been estimated to be ~10^{-3}, the observed BH-to-bulge mass ratio results. We also obtain a relation between BH mass and bulge velocity dispersion that is compatible with observations of present-day galaxies.

10 pages, 3 figures, accepted by ApJ

References in corpus (5)

• Rapid Formation of Supermassive Black Hole Binaries in Galaxy Mergers with Gas
• Cosmic Evolution of Black Holes and Spheroids. III. The M-sigma relation in the last six billion years
• Cosmic Evolution of Black Holes and Spheroids. II: Scaling Relations at z=0.36
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Cited by in corpus (4)

• Formation of Massive Galaxies at High Redshift: Cold Streams, Clumpy Disks and Compact Spheroids
• Bulge Formation by the Coalescence of Giant Clumps in Primordial Disk Galaxies
• The SINS Survey: Broad Emission Lines in High-Redshift Star-Forming Galaxies
• Black hole spin and radio loudness in a LCDM universe