Quenching Global Star Formation: Dominance of Gravitational Shock Heating at z<2

TL;DR

This study demonstrates that gravitational shock heating, including halo self-quenching and hot environments, primarily drives the decline in cosmic star formation rate from redshift 2 to 0, explaining cosmic downsizing.

Contribution

It identifies gravitational shock heating as the dominant mechanism for star formation suppression at z<2, contrasting with the minor role of photoheating and highlighting the need for additional feedback effects at higher redshifts.

Findings

Steep decline in SFR density from z~2 to 0 explained by shock heating.

Cosmic downsizing reproduced by decreasing SFR in galaxies from z=2 to 0.

Halo mass of star-forming galaxies continues to increase from z=2 to 0.

Abstract

We systematically study, in the context of the standard cold dark matter model, star-formation suppression effects of two important known physical processes---photoheating due to reionization of the intergalactic medium and gravitational shock heating due to formation of massive halos and large-scale structure---on the global evolution of star formation rate (SFR) density and the so-called cosmic downsizing phenomenon in the redshift range z=0-6. We show that the steep decline of cosmic SFR density from z~2 to z=0 can be primarily explained by gravitational shock heating in two forms: massive halo self-quenching and hot environment. Simultaneously, we show a decreasing trend in the average SFR of star-forming galaxies from z=2 to z=0, reproducing the observed cosmic downsizing at z<2. Nevertheless, the average halo mass of star-forming galaxies is found to continue upsizing from z=2 to z=0. In stark contrast to z<2, both photoheating and gravitational shock heating effects are found to play a minor role in suppressing star formation. Additional negative feedback effects are required to reconcile our model with observations at z>2. Internal feedback from stellar evolution and supermassive black hole growth are the natural candidates for this role, as galaxies at z>2 are more moderate in mass but stronger in star formation and are thus more vulnerable. Our physical model can be used to treat star formation in cosmological N-body simulations.