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The galaxy cluster CLG0218.3-0510 at z=1.62 is one of the most distant galaxyclusters known, with a rich muti-wavelength data set that confirms a maturegalaxy population already in place. Using very deep, wide area (20x20 Mpc)imaging by Spitzer/MIPS at 24um, in conjunction with Herschel 5-band imagingfrom 100-500um, we investigate the dust-obscured, star-formation properties inthe cluster and its associated large scale environment. Our galaxy sample of693 galaxies at z=1.62 detected at 24um (10 spectroscopic and 683 photo-z)includes both cluster galaxies (i.e. within r <1 Mpc projected clustercentricradius) and field galaxies, defined as the region beyond a radius of 3 Mpc. Thestar-formation rates (SFRs) derived from the measured infrared luminosity rangefrom 18 to 2500 Ms/yr, with a median of 55 Ms/yr, over the entire radial range(10 Mpc). The cluster brightest FIR galaxy, taken as the centre of the galaxysystem, is vigorously forming stars at a rate of 256$\pm$70 Ms/yr, and thetotal cluster SFR enclosed in a circle of 1 Mpc is 1161$\pm$96 Ms/yr. Weestimate a dust extinction of about 3 magnitudes by comparing the SFRs derivedfrom [OII] luminosity with the ones computed from the 24um fluxes. We find thatthe in-falling region (1-3 Mpc) is special: there is a significant decrement(3.5x) of passive relative to star-forming galaxies in this region, and thetotal SFR of the galaxies located in this region is lower (130 Ms/yr/Mpc2) thananywhere in the cluster or field, regardless of their stellar mass. In acomplementary approach we compute the local galaxy density, Sigma5, and find notrend between SFR and Sigma5. However, we measure an excess of star-forminggalaxies in the cluster relative to the field by a factor 1.7, that lendssupport to a reversal of the SF-density relation in CLG0218.

Star formation in the cluster CLG0218.3-0510 at z=1.62 and its large-scale environment: the infrared perspective