Quantifying the suppression of the (un)-obscured star formation in galaxy cluster cores at 0.2≲ z ≲0.9
Pérez-González, P G
Rawle, T D
Edge, A C
Enia, A F M
Haines, C P
AffiliationUniv Arizona, Steward Observ
MetadataShow full item record
PublisherOXFORD UNIV PRESS
CitationL Rodríguez-Muñoz, G Rodighiero, C Mancini, P G Pérez-González, T D Rawle, E Egami, A Mercurio, P Rosati, A Puglisi, A Franceschini, I Balestra, I Baronchelli, A Biviano, H Ebeling, A C Edge, A F M Enia, C Grillo, C P Haines, E Iani, T Jones, M Nonino, I Valtchanov, B Vulcani, M Zemcov, 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, Volume 485, Issue 1, May 2019, Pages 586–619, https://doi.org/10.1093/mnras/sty3335
RightsCopyright © 2019 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society.
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AbstractWe 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.
VersionFinal published version
SponsorsUniversita degli studi di Padova -Dipartimento di Fisica e Astronomia 'G. Galilei' [1.05.01.88.04]; Spanish Government MINECO [AYA2015-70815-ERC, AYA2015-63650-P]; STFC; [ST/P00541/1]