The Halo Occupation Distribution of Black Holes

Mathematics – Logic

Scientific paper

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Scientific paper

Using hydrodynamic cosmological simulations that directly follow black hole growth we investigate the halo occupation distribution (HOD) of black holes. Similar to the HOD of galaxies/subhalos, we find that the black hole occupation number can be described by the power law N_BH proportional to 1+(M_Host)^α where α evolves mildly with redshift, indicating that a given mass halo at low redshift tends to host fewer BHs than at high redshift (as expected as a result of galaxy and BH mergers). We further show how to divide the occupation number into contributions from black holes residing in central and satellite galaxies within the halo. The distribution of black holes masses and luminosities within halos tends to consist of a single massive, bright BH (distributed about a peak mass strongly correlated with the host mass), and a collection of relatively low-mass secondary BHs with weaker correlation to host mass. We examine the spatial distribution of black holes within their host halos, and find they typically follow a power-law radial distribution that is much more centrally concentrated than the subhalo distribution. We further show that black hole feedback becomes increasingly important at low redshifts, which can lead to suppression of the central quasar luminosity and increased scatter in the correlation between quasar luminosity and host halo mass. Overall, this HOD formalism provides the most complete tool for characterizing the distribution of black holes within host halos and galaxies, and can be used in semi-analytic and theoretical models and as a framework for interpreting observational black hole measurements.

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