The weak dependence of velocity dispersion on disk fractions, mass-to-light ratio and redshift: Implications for galaxy and black hole evolution

TL;DR

This study investigates the weak dependence of galaxy velocity dispersion on various factors, using semi-empirical models and simulations to understand galaxy and black hole evolution across redshifts.

Contribution

It introduces a comprehensive semi-empirical approach to model velocity dispersion considering mass-to-light ratio gradients and compares results with hydrodynamic simulations, revealing insights into galaxy evolution.

Findings

Velocity dispersion weakly depends on bulge-to-total ratio for B/T > 0.25.

Dark matter fraction influences velocity dispersion evolution.

Models show consistent results with hydrodynamic simulations.

Abstract

Velocity dispersion ($\sigma$) is a key driver for galaxy structure and evolution. We here present a comprehensive semi-empirical approach to compute $\sigma$ via detailed Jeans modelling assuming both a constant and scale-dependent mass-to-light ratio $M^*/L$. We compare with a large sample of local galaxies from MaNGA and find that both models can reproduce the Faber-Jackson (FJ) relation and the weak dependence of $\sigma$ on bulge-to-total ratio $B/T$ (for $B/T\gtrsim 0.25$). The dynamical-to-stellar mass ratio within $R\lesssim R_e$ can be fully accounted for by a gradient in $M^*/L$. We then build velocity dispersion evolutionary tracks $\sigma_{ap}[M^*,z]$ (within an aperture) along the main progenitor dark matter haloes assigning stellar masses, effective radii and Sersic indices via a variety of abundance matching and empirically motivated relations. We find: 1) clear evidence for downsizing in $\sigma_{ap}[M^*,z]$ along the progenitor tracks; 2) at fixed stellar mass $\sigma\propto(1+z)^{0.2-0.3}$ depending on the presence or not of a gradient in $M^*/L$. We extract $\sigma_{ap}[M^*,z]$ from the TNG50 hydrodynamic simulation and find very similar results to our models with constant $M^*/L$. The increasing dark matter fraction within $R_e$ tends to flatten the $\sigma_{ap}[M^*,z]$ along the progenitors at $z \gtrsim 1$ in constant $M^*/L$ models, while $\sigma_{ap}[M^*,z]$ have a steeper evolution in the presence of a stellar gradient. We then show that a combination of mergers and gas accretion are likely responsible for the constant or increasing $\sigma_{ap}[M^*,z]$ with time. Finally, our $\sigma_{ap}[M^*,z]$ are consistent with a nearly constant and steep $M_{bh}-\sigma$ relation at $z\lesssim 2$, with black hole masses derived from the $L_X-M^*$ relation.