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Rodriguez-Munoz, L.; Rodighiero, G.; Mancini, C.; Perez-Gonzalez, P. G.; Rawle, 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. (2019): Quantifying the suppression of the (un)-obscured star formation in galaxy cluster cores at 0.2 less than or similar to z less than or similar to 0.9. In: Monthly Notices of the Royal Astronomical Society, Vol. 485, No. 1: pp. 586-619
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We quantify the star formation (SF) in the inner cores (R/R-200 <= 0.3) of 24 massive galaxy clusters at 0.2 less than or similar to z less than or similar to 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) M-circle dot) 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 similar to 2 smaller in cluster cores than in the field. Furthermore, SFGs present average SFR and sSFR typically similar to 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 similar to 0.9, with shorter time-scale processes being very likely responsible for a fraction of the missing SFG population.