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Quantifying the suppression of the (un)-obscured star formation in galaxy cluster cores at 0.2≲ z ≲0.9.

Rodríguez-Muñoz, L. and Rodighiero, G. and Mancini, C. and Pérez-González, P. G. and Rawle, T. D. and Egami, E. and Mercurio, A. and Rosati, P. and Puglisi, A. and Franceschini, A. and Balestra, I. and Baronchelli, I. and Biviano, A. and Ebeling, H. and Edge, A. C. and Enia, A. F. M. and Grillo, C. and Haines, C. P. and Iani, E. and Jones, T. and Nonino, M. and Valtchanov, I. and Vulcani, B. and Zemcov, M. (2019) 'Quantifying the suppression of the (un)-obscured star formation in galaxy cluster cores at 0.2≲ z ≲0.9.', Monthly notices of the Royal Astronomical Society., 485 (1). pp. 586-619.

Abstract

We quantify the star formation (SF) in the inner cores (⁠R/R200 ≤0.3) of 24 massive galaxy clusters at 0.2≲ z ≲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 (⁠M∗>1010 M⊙) 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 (⁠F⁠) of star-forming galaxies (SFGs) and the rate at which they form stars (⁠SFR and sSFR=SFR/M∗⁠). On average, the F of SFGs is a factor ∼2 smaller in cluster cores than in the field. Furthermore, SFGs present average SFR and sSFR typically ∼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 ∼0.9, with shorter time-scale processes being very likely responsible for a fraction of the missing SFG population.

Item Type:Article
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Status:Peer-reviewed
Publisher Web site:https://doi.org/10.1093/mnras/sty3335
Publisher statement:© 2019 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society.
Date accepted:05 December 2018
Date deposited:29 May 2019
Date of first online publication:07 February 2019
Date first made open access:29 May 2019

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