Rodríguez Muñoz, L.Rodighiero, G.Mancini, C.Pérez González, Pablo GuillermoRawle, T.D.Egami, E.Mercurio, A.Rosati, P.Puglisi, A.Franceschini, A.Balestra, I.Baronchelli, I.Biviano, A.Ebeling, H.Edge, A,C,Enia, A.F.M.Grillo, C.Haines, C.P.Iani, E.Jones, T.Nonino, M.Valtchanov, I.Vulcani, B.Zemcov, M.2023-06-172023-06-172019-050035-871110.1093/mnras/sty3335https://hdl.handle.net/20.500.14352/13587© 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).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.engjournal articlehttp://dx.doi.org/10.1093/mnras/sty3335https://academic.oup.comopen access52Stellar mass functionInfrared luminosity functionsKeck spectroscopic surveyArray camera IracDeep field-southFormation historiesRedshift surveyStarburst galaxiesFormation ratesEnvironmental dependenceAstrofísica