Modelling the quenching of star formation activity from the evolution of the colour-magnitude relation in VIPERS

TL;DR

This study investigates how the bright edge of the colour-magnitude relation in galaxies evolves from redshift 0.5 to 1.1, revealing the necessity of quenching star formation to match observations and testing galaxy formation models.

Contribution

It introduces the bright edge concept to constrain galaxy quenching timescales and compares observations with models, highlighting the importance of quenching and feedback processes.

Findings

Quenching is necessary to reproduce the bright edge evolution.

Star formation stops randomly within 2.5 Gyr in the best-fit model.

Feedback from active galactic nuclei influences the bright edge evolution.

Abstract

We study the evolution of the colour-magnitude relation for galaxies in the VIMOS Public Extragalactic Redshift Survey (VIPERS) by introducing the concept of the bright edge, and use this to derive constraints on the quenching of star formation activity in galaxies over the redshift range $0.5 < z < 1.1$. The bright-edge of the colour-magnitude diagram evolves with little dependence on galaxy colour, and therefore on the amount of star formation taking place in bright galaxies. We modelled this evolution with delayed exponential star formation histories (SFHs), to better understand the time-scale of the turn-off in star formation activity. We show that using SFHs without quenching, the transition from the blue cloud to the red sequence is too slow. This indicates that a scenario purely driven by the consumption of the gas inside each galaxy does not reproduce the observed evolution of the colour-magnitude bright edge. Among the quenching scenarios explored, the one that best matches the observations assumes that galaxies stop their star formation at a randomly selected time with a uniform distribution up to $2.5$ Gyr. We argue that quenching is required over a wide range of stellar masses. Qualitatively similar evolution of the bright edge is found in the predictions of a semi-analytical galaxy formation model, but quantitatively there are marked differences with the observations. This illustrates the utility of the bright edge as a test of galaxy formation models. The evolution changes and no longer matches the observed trend if feedback from heating by active galactic nuclei is turned off.