Colours, Star formation Rates, and Environments of Star forming and Quiescent Galaxies at the Cosmic Noon

TL;DR

This study uses high-resolution cosmological simulations to analyze galaxy properties at z~2, revealing insights into star formation, colours, and morphology, with implications for understanding galaxy evolution during cosmic noon.

Contribution

It provides new simulation-based insights into the properties and evolution of massive and moderate-mass galaxies at cosmic noon, including their star formation and quiescence mechanisms.

Findings

Approximately half of massive galaxies at z~2 are quiescent.

Progenitors of quiescent galaxies are more massive and in larger haloes.

Simulations do not reproduce the reddest observed quiescent galaxies.

Abstract

We analyse the star formation rates (SFRs), colours, and dust extinctions of galaxies in massive (10^12.5-10^13.5 Msun) haloes at z~2 in high-resolution, cosmological zoom-in simulations as part of the Feedback in Realistic Environments (FIRE) project. The simulations do not model feedback from active galactic nuclei (AGN) but reproduce well the observed relations between stellar and halo mass and between stellar mass and SFR. About half (a third) of the simulated massive galaxies (massive central galaxies) at z~2 have broad-band colours classifying them as 'quiescent', and the fraction of quiescent centrals is steeply decreasing towards higher redshift, in agreement with observations. The progenitors of z~2 quiescent central galaxies are, on average, more massive, have lower specific SFRs, and reside in more massive haloes than the progenitors of similarly massive star forming centrals. The simulations further predict a morphological mix of galaxies that includes disk-dominated, irregular, and early-type galaxies. However, our simulations do not reproduce the reddest of the quiescent galaxies observed at z~2. We also do not find evidence for a colour bimodality, but are limited by our modest sample size. In our simulations, the star formation activity of central galaxies of moderate mass (Mstar~10^10-10^11 Msun) is affected by a combination of two distinct physical processes. Outflows powered by stellar feedback result in a short-lived (<100 Myr), but almost complete, suppression of star formation activity after which many galaxies quickly recover and continue to form stars at normal rates. In addition, galaxies residing in slowly growing haloes tend to experience a moderate reduction of their SFRs ('cosmological starvation'). The relative importance of these processes and AGN feedback is uncertain and will be explored in future work.