Quantifying the suppression of the (un)-obscured star formation in galaxy cluster cores at 0.2$\lesssim$$z$$\lesssim$0.9

Abstract

We quantify the star formation (SF) in the inner cores ($\mathcal{R}$/$R_{200}$$\le$0.3) of 24 massive galaxy clusters at 0.2$\lesssim$$z$$\lesssim$0.9 observed by the $Herschel$ Lensing Survey and the Cluster Lensing and Supernova survey with $Hubble$. These programmes, covering the rest-frame ultraviolet to far-infrared regimes, allow us to accurately characterize stellar mass-limited (${\mathcal{M}}_{\ast }$$>$$10^{10}$ $M_{\odot }$) samples of star-forming cluster members (not)-detected in the mid- and/or far-infrared. We release the catalogues with the photometry, photometric redshifts, and physical properties of these samples. We also quantify the SF displayed by comparable field samples from the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey. We find that in intermediate-$z$ cluster cores, the SF activity is suppressed with respect the field in terms of both the fraction ($\mathcal{F}$) of star-forming galaxies (SFG) and the rate at which they form stars ($\mathcal{S}\mathcal{F}\mathcal{R}$ and $s\mathcal{S}\mathcal{F}\mathcal{R}=\mathcal{S}\mathcal{F}\mathcal{R}/{\mathcal{M}}_{\ast }$). On average, the $\mathcal{F}$ of SFGs is a factor $\sim$$2$ smaller in cluster cores than in the field. Furthermore, SFGs present average $\mathcal{S}\mathcal{F}\mathcal{R}$ and $s\mathcal{S}\mathcal{F}\mathcal{R}$ typically $\sim$0.3 dex smaller in the clusters than in the field along the whole redshift range probed. Our results favour long time-scale quenching physical processes as the main driver of SF suppression in the inner cores of clusters since $z$$\sim$0.9, with shorter time-scale processes being very likely responsible for a fraction of the missing SFG population.

arXiv comment34 pages, 13 figures, 15 tables; accepted for publication in MNRAS

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