We study the star-forming ( SF ) population of galaxies within a sample of 209 IR-selected galaxy clusters at 0.3 \leq z \leq 1.1 in the ELAIS-N1 and XMM-LSS fields , exploiting the first HSC-SSP data release .
The large area and depth of these data allows us to analyze the dependence of the SF fraction , f _ { SF } , on stellar mass and environment separately .
Using R / R _ { 200 } to trace environment , we observe a decrease in f _ { SF } from the field towards the cluster core , which strongly depends on stellar mass and redshift .
The data show an accelerated growth of the quiescent population within the cluster environment : the f _ { SF } vs. stellar mass relation of the cluster core ( R / R _ { 200 } \leq 0.4 ) is always below that of the field ( 4 \leq R / R _ { 200 } < 6 ) .
Finally , we find that environmental and mass quenching efficiencies depend on galaxy stellar mass and distance to the center of the cluster , demonstrating that the two effects are not separable in the cluster environment .
We suggest that the increase of the mass quenching efficiency in the cluster core may emerge from an initial population of galaxies formed “ in situ. ” The dependence of the environmental quenching efficiency on stellar mass favors models in which galaxies exhaust their reservoir of gas through star formation and outflows , after new gas supply is truncated when galaxies enter the cluster .