RT Journal Article
T1 Quantifying the suppression of the (un)-obscured star formation in galaxy cluster cores at 0.2  </~ z </~ 0.9
A1 Rodríguez Muñoz, L.
A1 Rodighiero, G.
A1 Mancini, C.
A1 Pérez González, Pablo Guillermo
A1 Rawle, T.D.
A1 Egami, E.
A1 Mercurio, A.
A1 Rosati, P.
A1 Puglisi, A.
A1 Franceschini, A.
A1 Balestra, I.
A1 Baronchelli, I.
A1 Biviano, A.
A1 Ebeling, H.
A1 Edge, A,C,
A1 Enia, A.F.M.
A1 Grillo, C.
A1 Haines, C.P.
A1 Iani, E.
A1 Jones, T.
A1 Nonino, M.
A1 Valtchanov, I.
A1 Vulcani, B.
A1 Zemcov, M.
AB We quantify the star formation (SF) in the inner cores (R/R_(200) ≤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∗ > 10^(10) Mꙩ) 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 intermediatez 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.
PB Oxford University Press.
SN 0035-8711
YR 2019
FD 2019-05
LK https://hdl.handle.net/20.500.14352/13587
UL https://hdl.handle.net/20.500.14352/13587
LA eng
NO © 2019 The Author(s). The authors thank Françoise Combes, Carlos López-Sanjuan, Dieter Lutz, Bianca Poggianti, and Alvio Renzini for their suggestions to improve this work. We acknowledge funding from the INAF PRINSKA 2017 program 1.05.01.88.04. LR-M acknowledges funding support from the Università degli studi di Padova – Dipartimento di  Fisica e Astronomia ‘G. Galilei’. GR and CM acknowledge support from an INAF PRIN-SKA 2017 grant. PGP-G acknowledges funding support from the Spanish Government MINECO under grants AYA2015-70815-ERC and AYA2015-63650-P. ACE acknowledges support from STFC grant ST/P00541/1. AM acknowledges funding from the INAF PRIN-SKA 2017 program 1.05.01.88.04. Analyses were performed in R 3.4.0 (R Core Team 2018).
NO Ministerio de Economía y Competitividad (MINECO)
NO INAF PRINSKA 2017 program
NO Università degli studi di Padova – Dipartimento di  Fisica e Astronomia ‘G. Galilei’
NO INAF
NO STFC
DS Docta Complutense
RD 5 abr 2025