Effects of AGN feedback on LCDM galaxies

TL;DR

This paper investigates how AGN feedback influences galaxy formation and evolution in a semi-analytic model, successfully reproducing various observed galaxy properties and luminosity functions across different redshifts.

Contribution

The study introduces an improved semi-analytic model that incorporates detailed black hole growth mechanisms and AGN feedback effects, aligning model predictions with multiple observational data.

Findings

AGN feedback suppresses gas cooling at low redshifts.

Model reproduces galaxy luminosity functions and star formation rates from z=0 to z=5.

Early-type massive galaxies form by z>1, matching observed bimodal color distribution.

Abstract

We study the effects of Active Galactic Nuclei (AGN) feedback on the formation and evolution of galaxies in a semi-analytic model of galaxy formation. This model is an improved version of the one described by Cora (2006), which now considers the growth of black holes (BHs) as driven by (i) gas accretion during merger-driven starbursts and mergers with other BHs, (ii) accretion during starbursts triggered by disc instabilities, and (iii) accretion of gas cooled from quasi-hydrostatic hot gas haloes. It is assumed that feedback from AGN operates in the later case. The model has been calibrated in order to reproduce observational correlations between BH mass and mass, velocity dispersion, and absolute magnitudes of the galaxy bulge. AGN feedback has a strong impact on reducing or even suppressing gas cooling, an effect that becomes important at lower redshifts. This phenomenon helps to reproduce the observed galaxy luminosity function (LF) in the optical and near IR bands at z=0, and the cosmic star formation rate and stellar mass functions over a wide redshift range (0<z<5). It also allows to have a population of massive galaxies already in place at z>1, which are mostly early-type and have older and redder stellar populations than lower mass galaxies, reproducing the observed bimodality in the galaxy colour distribution, and the morphological fractions. The evolution of the optical QSO LF is also reproduced, provided that the presence of a significant fraction of obscured QSOs is assumed. We explore the effects of AGN feedback during starbursts and new recent prescriptions for dynamical friction time-scales. (ABRIDGED)