The dominance of quenching through cosmic times

Abstract

The evolution with cosmic time of the star formation rate density (SFRD) and of the "Main Sequence" star formation rate-stellar mass relations are two well established observational facts. In this paper the implications of these two relations combined are analytically explored, showing that quenching of star formation must start already at very early cosmic times and the quenched fraction then dominates ever since over the star forming one. Thus, a simple picture of the cosmic evolution of the global SFRD is derived, in terms of the interplay between star formation and its quenching.

To appear on MNRAS-Letters; 6 pages, 2 figures

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• The VLA-COSMOS 3 GHz Large Project: Evolution of specific star formation rates out to $z\sim 5$
• Stochastic modelling of star-formation histories II: star-formation variability from molecular clouds and gas inflow
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• Rejuvenated galaxies with very old bulges at the origin of the bending of the main sequence and of the "green valley"
• The emergence of passive galaxies in the early Universe
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• An alternate approach to measure specific star formation rates at 2<z<7
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• From haloes to galaxies -- II. The fundamental relations in star formation and quenching
• Cosmic Star Formation: a simple model of the SFRD(z)
• The quenched mass portion of star-forming galaxies and the origin of the star formation sequence slope
• Correlation of the rate of Type Ia supernovae with the parent galaxy properties: Light and shadows
• Galaxy Manifold: Characterizing and understanding galaxies with two parameters
• ZFIRE: The Beginning of the End for Massive Galaxies at z ~ 2 and Why Environment Matters