Angular momentum transfer and the size - mass relation in early - type galaxies

TL;DR

This paper models how angular momentum transfer influences the size-mass relation in early-type galaxies, linking anisotropic velocity distributions to observed deviations from simple theoretical predictions.

Contribution

It introduces an analytic model connecting angular momentum transfer to the size-mass relation via anisotropic distribution functions in early-type galaxies.

Findings

The model reproduces the observed size-mass relation slope.

Anisotropy profiles with tangential and radial regions match observations.

Angular momentum transfer explains deviations from canonical size-mass predictions.

Abstract

Early - type galaxies (ETGs) define a narrow strip in the size - mass plane because of the observed correlation between the effective radius $R_{eff}$ and the total stellar mass $M_{\star}$. When expressed in logarithmic units, a linear relation, $\log{R_{eff}} \propto \gamma \log{M_{\star}}$, is indeed observationally found, but the slope $\gamma$ deviates from the canonical $\gamma = 1/2$ value which can be naively predicted for a spherically symmetric isotropic system. We propose here that a transfer of angular momentum to the stellar component induces an anisotropy in the velocity space thus leading to a modified distribution function (DF). Assuming an Osipkov - Merritt like anisotropic DF, we derive an analytic relation between the slope $\gamma$ of the size - mass relation and the slope $\alpha$ of the angular momentum term in the DF. With this simple model, we are then able to recover the observed $\gamma$ value provided $\alpha$ is suitably set. It turns out that an anisotropy profile which is tangential inside $\sim 0.6 r_a$ and radial outside, with $r_a$ the anisotropy radius, is able to reproduce the observed size - mass relation observed for massive ($M_{\star} \ge 2 \times 10^{10} \ h^{-1} {\rm M}_{\odot}$) elliptical galaxies.