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(Abridged) We explore the massive cluster XMMXCSJ2215.9-1738 at z~1.5 withKMOS spectroscopy of Halpha and [NII] covering a region that corresponds toabout one virial radius. Using published spectroscopic redshifts of 108galaxies in and around the cluster we computed the location of galaxies in theprojected velocity vs. position phase-space to separate our cluster sample intoa virialized region of objects accreted longer ago (roughly inside half R200)and a region of infalling galaxies. We measured oxygen abundances for tencluster galaxies with detected [NII] lines in the individual galaxy spectra andcompared the MZR of the galaxies inside half R200 with the infalling galaxiesand a field sample at similar redshifts. We find that the oxygen abundances ofindividual z~1.5 star-forming cluster galaxies inside half R200 are comparable,at the respective stellar mass, to the higher local SDSS metallicity values. Wefind that the [NII]/Halpha line ratios inside half R200 are higher by 0.2 dexand that the resultant metallicities of the galaxies in the inner part of thecluster are higher by about 0.1 dex, at a given mass, than the metallicities ofinfalling galaxies and of field galaxies at z~1.5. The enhanced metallicitiesof cluster galaxies at z~1.5 inside half R200 indicate that the density of theICM in this massive cluster becomes high enough toward the cluster center suchthat the ram pressure exceeds the restoring pressure of the hot gas reservoirof cluster galaxies. This can remove the gas reservoir initiating quenching;although the galaxies continue to form stars, albeit at slightly lower rates,using the available cold gas in the disk which is not stripped.

Cluster induced quenching of galaxies in the massive cluster XMMXCSJ2215.9-1738 at z~1.5 traced by enhanced metallicities inside half R200