Dark matter halos and the M-\sigma relation for supermassive black holes

TL;DR

This paper models the connection between dark matter halos and supermassive black holes, predicting the observed M- relation at z=0 based on quasar feedback and halo evolution.

Contribution

It introduces a model linking dark matter halo properties at various redshifts to the local M- relation, incorporating quasar feedback physics and cosmological halo evolution.

Findings

Predicted M- relation matches local data for z_qso  2-4.

The M- relation is non-linear in log-log space.

Model highlights the impact of halo evolution and feedback on SMBH scaling relations.

Abstract

We develop models of two-component spherical galaxies to establish scaling relations linking the properties of spheroids at $z=0$ (total stellar masses, effective radii $R_e$ and velocity dispersions within $R_e$) to the properties of their dark-matter halos at both $z=0$ and higher redshifts. . Our main motivation is the widely accepted idea that the accretion-driven growth of supermassive black holes (SMBHs) in protogalaxies is limited by quasar-mode feedback and gas blow-out. The SMBH masses, $M_{\rm{BH}}$, should then be connected to the dark-matter potential wells at the redshift $z_{\rm{qso}}$ of the blow-out. We specifically consider the example of a power-law dependence on the maximum circular speed in a protogalactic dark-matter halo: $M_{\rm{BH}}\propto V^4_{\rm{d,pk}}$, as could be expected if quasar-mode feedback were momentum-driven. For halos with a given $V_{\rm{d,pk}}$ at a given $z_{\rm{qso}}\ge 0$, our model scaling relations give a typical stellar velocity dispersion $\sigma_{\rm{ap}}(R_e)$ at $z=0$. Thus, they transform a theoretical $M_{\rm{BH}}$-$V_{\rm{d,pk}}$ relation into a prediction for an observable $M_{\rm{BH}}$-$\sigma_{\rm{ap}}(R_e)$ relation. We find the latter to be distinctly non-linear in log-log space. Its shape depends on the generic redshift-evolution of halos in a {$\Lambda$}CDM cosmology and the systematic variation of stellar-to-dark matter mass fraction at $z=0$, in addition to any assumptions about the physics underlying the $M_{\rm{BH}}$-$V_{\rm{d,pk}}$ relation. Despite some clear limitations of the form we use for $M_{\rm{BH}}$ versus $V_{\rm{d,pk}}$, and even though we do not include any SMBH growth through dry mergers at low redshift, our results for $M_{\rm{BH}}$-$\sigma_{\rm{ap}}(R_e)$ compare well to data for local early types if we take $z_{\rm{qso}} \sim$ 2-4.