SEEDisCS

II. Molecular gas in galaxy clusters and their large-scale structure: low gas fraction galaxies, the case of CL1301.7−1139

¹ Institute of Physics, Laboratory of Astrophysics, École Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny, 1290 Versoix, Switzerland
e-mail: damien.sperone-longin@epfl.ch
² GEPI, Observatoire de Paris, PSL University, CNRS, 5 place Jules Janssen, 92190 Meudon, France
³ Observatoire de Paris, LERMA, CNRS, Sorbonne University, PSL Research Universty, 75014 Paris, France
⁴ Collège de France, 11 place Marcelin Berthelot, 75231 Paris, France
⁵ Dipartimento di Fisica e Astronomia, Alma Mater Studiorum Università di Bologna, Via Gobetti 93/2, 40129 Bologna, Italy
⁶ IRAM, Domaine Universitaire, 300 rue de la Piscine, 38406 Saint-Martin-d’Hères, France
⁷ Department of Physics and Astronomy, The University of Kansas, Lawrence, KS, USA
⁸ Steward Observatory and Department of Astronomy, University of Arizona, Tucson, AZ, USA
⁹ Department of Physics and Astronomy, Siena College, Loudonville, NY, USA
¹⁰ INAF – Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11, 34143 Trieste, Italy
¹¹ IPAC, Mail Code 100-22, Caltech, 1200 E. California Boulevard, Pasadena, CA, USA

Received: 30 March 2021
Accepted: 26 July 2021

Abstract

This paper is the second of a series that tackles the properties of molecular gas in galaxies residing in clusters and their related large-scale structures. Out of 21 targeted fields, 19 galaxies were detected in CO(3–2) with the Atacama Large Millimeter Array, including two detections within a single field. These galaxies are either bona fide members of the CL1301.7−1139 cluster (z = 0.4828, σ_cl = 681 km s⁻¹), or located within ∼7 × R₂₀₀, its virial radius. They have been selected to sample the range of photometric local densities around CL1301.7−1139, with stellar masses above log(M_star) = 10, and to be located in the blue clump of star-forming galaxies derived from the u, g, and i photometric bands. Unlike previous works, our sample selection does not impose a minimum star formation rate or detection in the far-infrared. As such and as much as possible, it delivers an unbiased view of the gas content of normal star-forming galaxies at z ∼ 0.5. Our study highlights the variety of paths to star formation quenching, and most likely the variety of physical properties (i.e., temperature, density) of the corresponding galaxy’s cold molecular gas. Just as in the case of CL1411.1−1148, although to a smaller extent, we identify a number of galaxies with lower gas fraction than classically found in other surveys. These galaxies can still be on the star-forming main sequence. When these galaxies are not inside the cluster virialised region, we provide hints that they are linked to their infall regions within ∼4 × R₂₀₀.