A two-phase model of galaxy formation: I. The growth of galaxies and supermassive black holes

TL;DR

This paper presents a two-phase galaxy formation model that explains the growth of galaxies and supermassive black holes by considering the dynamics of gas in dark matter halos, feedback effects, and reproduces key observational correlations.

Contribution

The model introduces a two-phase process for galaxy and SMBH growth, emphasizing the role of turbulent gas and feedback during the fast halo formation phase, which is a novel approach.

Findings

Reproduces observed SMBH-galaxy-halo mass correlations.

Matches the number densities and evolution of galaxies and SMBHs.

Highlights the importance of feedback during the fast phase.

Abstract

We develop a model for galaxy formation and the growth of supermassive black holes (SMBHs), based on the fact that cold dark matter (CDM) halos form their gravitational potential wells through a fast phase with rapid change in the potential, and that the high universal baryon fraction makes cooled gas in halos self-gravitating and turbulent before it can form rotation-supported disks. Gas fragmentation produces sub-clouds so dense that cloud-cloud collision and drag on clouds are not significant, producing a dynamically hot system of sub-clouds that form stars and move ballistically to feed the central SMBH. Active galactic nucleus (AGN) and supernova (SN) feedback is effective only in the fast phase, and the cumulative effects are to regulate star formation and SMBH growth, as well as to reduce the amount of cold gas in halos to allow the formation of globally stable disks. Using a set of halo assembly histories, we demonstrate that the model can reproduce a number of observations, including correlations among SMBH mass, stellar mass of galaxies and halo mass, the number densities of galaxies and SMBH, as well as their evolution over the cosmic time.