Towards a Comprehensive Fueling-Controlled Theory on the Growth of Massive Black Holes and Host Spheroids

TL;DR

This study uses high-resolution simulations to explore how gas fueling influences the growth of massive black holes and their host spheroids, revealing new insights into their scaling relations and star formation laws.

Contribution

It introduces a fueling-controlled theoretical framework that explains the black hole and spheroid growth relations through detailed gas dynamics and star formation processes.

Findings

Simulations naturally reproduce the M_BH - M_virial relation with low scatter.

A generalized Kennicutt-Schmidt Law for starbursts is validated.

The M_BH - sigma relation emerges as a consequence of the M_BH - M_virial relation.

Abstract

We study the relation between nuclear massive black holes and their host spheroid gravitational potential. Using AMR numerical simulations, we analyze how gas is transported in the nuclear (central kpc) regions of galaxies. We study the gas fueling onto the inner accretion disk (sub-pc scale) and the star formation in a massive nuclear disk like those generally found in proto-spheroids (ULIRGs, SCUBA Galaxies). These sub-pc resolution simulation of gas fueling that is mainly depleted by star formation naturally satisfy the `M_BH - $M_virial' relation, with a scatter considerably less than the observed one. We found a generalized version of Kennicutt-Schmidt Law for starbursts is satisfied, in which the total gas depletion rate (dot{M}_gas = dot{M}_BH + dot{M}_SF) is the one that scales as M_gas/t_orbital. We also found that the `M_BH - sigma' relation is a byproduct of the `M_BH - M_virial' relation in the fueling controlled scenario.