Cosmic quenching and scaling laws for the evolution of supermassive black holes and host galaxies

TL;DR

This paper presents a theoretical framework for SMBH and galaxy coevolution based on a key parameter $ ext{"}varepsilon_b$ that governs gas flow and cooling, supported by simulations and leading to new scaling laws and growth stages.

Contribution

It introduces a novel parameter $ ext{"}varepsilon_b$ to unify SMBH and galaxy evolution, deriving scaling laws and growth phases from first principles and simulations.

Findings

$ ext{"}varepsilon_b$ scales as $(1+z)^{5/2}$ in the early universe.

New scaling laws relate galaxy mass, size, and velocity dispersion to $ ext{"}varepsilon_b$.

Three SMBH growth phases with distinct luminosity behaviors are identified.

Abstract

Observations suggest an SMBH-host coevolution. We consider the mass and energy flow in a bulge suffused by gases of varying temperatures. By assuming the rate of energy flow independent of the distance from the bulge center and the local virial equilibrium for permeated gases, a key parameter $\varepsilon_b$ was identified that quantifies the rate of mass and energy flow in gases and the efficiency of gas cooling and thus regulates the coevolution of SMBHs and hosts. Using Illustris simulations, we found $\varepsilon_b\propto (1+z)^{5/2}$. A higher $\varepsilon_b$ in the early Universe means a more efficient gas cooling that allows initial rapid growth of SMBHs and hosts. This simple theory, characterized by $\varepsilon_b$, provides the dominant mean cosmic evolution of SMBHs and hosts. All other transient phenomena may only contribute to the dispersion around mean evolution. Relevant scaling laws involving $\varepsilon_b$ were identified. For host galaxies, the mass-size relation $M_b\propto \varepsilon_b^{2/3}r_b^{5/3}G^{-1}$, dispersion-size relation $\sigma_b^2\propto(\varepsilon_b r_b)^{2/3}\propto (1+z)$, or the mass-dispersion relation $M_b\propto \varepsilon_b^{-1}G^{-1}\sigma_b^5$ were identified, where size $r_b\propto (1+z)^{-1}$. For SMBHs, three evolution phases were found involving an initial rapid growth stage with a rising luminosity $L_B\propto (\varepsilon_b M_{BH})^{4/5}$, a transition stage with a declining $L_B\propto \varepsilon_b^2 M_{BH} \propto (1+z)^5$, and a dormant stage with $L_B\propto (\varepsilon_b M_{BH})^{4/3}$. Results suggest a rapid initial super-Eddington growth with a new redshift-dependent luminosity limit $L_X\propto\varepsilon_b^{4/5}M_{BH}^{4/5}G^{-1/5}c$, in contrast to the Eddington limit. Analytical solutions are formulated for the BH and AGN mass functions and AGN duty cycle and predict a slope of -1/5 for the faint-end luminosity function.