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

Rodríguez-Muñoz, L; Rodighiero, G; Mancini, C; Pérez-González, PG; Rawle, TD; Egami, E; Mercurio, A; Rosati, P; Puglisi, A; Franceschini, A; Balestra, I; Baronchelli, I; Biviano, A; Ebeling, H; Edge, AC; Enia, AFM; Grillo, C; Haines, CP; Iani, E; Jones, T; Nonino, M; Valtchanov, I; Vulcani, B; Zemcov, M

doi:10.1093/mnras/sty3335

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

Rodríguez-Muñoz, L; Rodighiero, G; Mancini, C; Pérez-González, PG; Rawle, TD; Egami, E; Mercurio, A; Rosati, P; Puglisi, A; Franceschini, A; Balestra, I; Baronchelli, I; Biviano, A; Ebeling, H; Edge, AC; Enia, AFM; Grillo, C; Haines, CP; Iani, E; Jones, T; Nonino, M; Valtchanov, I; Vulcani, B; Zemcov, M

Authors

L Rodríguez-Muñoz

G Rodighiero

C Mancini

PG Pérez-González

TD Rawle

E Egami

A Mercurio

P Rosati

A Puglisi

A Franceschini

I Balestra

I Baronchelli

A Biviano

H Ebeling

Professor Alastair Edge alastair.edge@durham.ac.uk
Professor

AFM Enia

C Grillo

CP Haines

E Iani

T Jones

M Nonino

I Valtchanov

B Vulcani

M Zemcov

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.

Citation

Rodríguez-Muñoz, L., Rodighiero, G., Mancini, C., Pérez-González, P., Rawle, T., Egami, E., …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), 586-619. https://doi.org/10.1093/mnras/sty3335

Journal Article Type	Article
Acceptance Date	Dec 5, 2018
Online Publication Date	Feb 7, 2019
Publication Date	May 31, 2019
Deposit Date	May 29, 2019
Publicly Available Date	May 29, 2019
Journal	Monthly Notices of the Royal Astronomical Society
Print ISSN	0035-8711
Electronic ISSN	1365-2966
Publisher	Royal Astronomical Society
Peer Reviewed	Peer Reviewed
Volume	485
Issue	1
Pages	586-619
DOI	https://doi.org/10.1093/mnras/sty3335