A³COSMOS: A census on the molecular gas mass and extent of main-sequence galaxies across cosmic time

¹ Argelander-Institut für Astronomie, Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany
e-mail: twan@uni-bonn.de
² AIM, CEA, CNRS, Université Paris-Saclay, Université Paris Diderot, Sorbonne Paris Cité, 91191 Gif-sur-Yvette, France
³ Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
⁴ Max-Planck-Institut für extraterrestrische Physik, Gießenbachstraße 1, 85748 Garching b. München, Germany
⁵ National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville 22903, USA
⁶ Cosmic Dawn Center (DAWN), Copenhagen, Denmark
⁷ Niels Bohr Institute, University of Copenhagen, Lyngbyvej 2, 2100 Copenhagen Ø, Denmark

Received: 24 September 2021
Accepted: 17 January 2022

Abstract

Aims. We aim to constrain for the first time the mean mass and extent of the molecular gas of a mass-complete sample of normal > 10¹⁰ M_⊙ star-forming galaxies at 0.4 < z < 3.6.

Methods. We apply an innovative uv-based stacking analysis to a large set of archival Atacama Large Millimeter/submillimeter Array (ALMA) observations using a mass-complete sample of main-sequence (MS) galaxies. This stacking analysis, performed on the Rayleigh-Jeans dust continuum emission, provides accurate measurements of the mean mass and extent of the molecular gas of galaxy populations, which are otherwise individually undetected.

Results. The molecular gas mass of MS galaxies evolves with redshift and stellar mass. At all stellar masses, the molecular gas fraction decreases by a factor of ∼24 from z ∼ 3.2 to z ∼ 0. At a given redshift, the molecular gas fraction of MS galaxies decreases with stellar mass at roughly the same rate that their specific star-formation rate (SFR/M_⋆) decreases. The molecular gas depletion time of MS galaxies remains roughly constant at z > 0.5 with a value of 300–500 Myr, but increases by a factor of ∼3 from z ∼ 0.5 to z ∼ 0. This evolution of the molecular gas depletion time of MS galaxies can be predicted from the evolution of their molecular gas surface density and a seemingly universal MS-only Σ_Mmol − Σ_SFR relation with an inferred slope of ∼1.13, the so-called Kennicutt–Schmidt (KS) relation. The far-infrared size of MS galaxies shows no significant evolution with redshift or stellar mass, with a mean circularized half-light radius of ∼2.2 kpc. Finally, our mean molecular gas masses are generally lower than previous estimates, likely due to the fact that literature studies were largely biased toward individually detected MS galaxies with massive gas reservoirs.

Conclusions. To first order, the molecular gas content of MS galaxies regulates their star formation across cosmic time, while variation in their star-formation efficiency plays a secondary role. Despite a large evolution of their gas content and star-formation rates, MS galaxies have evolved along a seemingly universal MS-only KS relation.