The ATLAS3D Project-- VIII: Modelling the Formation and Evolution of Fast and Slow Rotator Early-Type Galaxies within $\Lambda$CDM

TL;DR

This paper presents a simple hierarchical model within the $ ext{Lambda}$CDM framework that explains the formation and evolution of fast and slow rotator early-type galaxies, matching observed fractions and growth histories.

Contribution

It introduces a model linking stellar disc mass fraction to angular momentum, reproduces observed galaxy rotation classifications, and explains their different growth histories.

Findings

Slow rotators mainly have $M_* > 10^{10.5} M_ ext{sun}$ and form through major mergers.

Fast rotators typically have fewer mergers and less than 50% stellar mass accreted from satellites.

Gas cooling shutdown in massive galaxies leads to different growth pathways for fast and slow rotators.

Abstract

We propose a simple model for the origin of fast and slow rotator early-type galaxies (ETG) within the hierarchical $\Lambda$CDM scenario, that is based on the assumption that the mass fraction of stellar discs in ETGs is a proxy for the specific angular momentum expressed via $\lambda_R$. Within our model we reproduce the fraction of fast and slow rotators as a function of magnitude in the \atl survey, assuming that fast rotating ETGs have at least 10% of their total stellar mass in a disc component. In agreement with \atl observations we find that slow rotators are predominantly galaxies with $ M_* > 10^{10.5}$ M$_{\odot}$ contributing $\sim 20%$ to the overall ETG population. We show in detail that the growth histories of fast and slow rotators are different, supporting the classification of ETGs into these two categories. Slow rotators accrete between $\sim 50% -90%$ of their stellar mass from satellites and their most massive progenitors have on average up to 3 major mergers during their evolution. Fast rotators in contrast, accrete less than 50% and have on average less than one major merger in their past. We find that the underlying physical reason for the different growth histories is the slowing down and ultimately complete shut-down of gas cooling in massive galaxies. Once cooling and associated star formation in disc stops, galaxies grow via infall from satellites. Frequent minor mergers thereby, destroy existing stellar discs via violent relaxation and also tend to lower the specific angular momentum of the main stellar body, lowering $\lambda_R$ into the slow rotator regime. Abridged...