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We present the first observation of cluster-scale radial metallicitygradients from star-forming galaxies. We use the DEIMOS spectrograph on theKeck II telescope to observe two CLASH clusters at z~0.35: MACS1115+0129 andRXJ1532+3021. Based on our measured interstellar medium (ISM) properties ofstar-forming galaxies out to a radius of 2.5 Mpc from the cluster centre, wefind that the galaxy metallicity decreases as a function of projectedcluster-centric distance (-0.15+/-0.08 dex/Mpc) in MACS1115+01. On themass-metallicity relation (MZR), star-forming galaxies in MACS1115+01 areoffset to higher metallicity (~0.2 dex) than the local SDSS galaxies at a fixedmass range. In contrast, the MZR of RXJ1532+30 is consistent with the localcomparison sample. RXJ1532+30 exhibits a bimodal radial metallicitydistribution, with one branch showing a similar negative gradient asMACS1115+01 (-0.14+/-0.05 dex/Mpc) and the other branch showing a positiveradial gradient. The positive gradient branch in RXJ1532+30 is likely caused byeither interloper galaxies or an in-plane merger, indicating that cluster-scaleabundance gradients probe cluster substructures and thus the dynamical state ofa cluster. Most strikingly, we discover that neither the radial metallicitygradient nor the offset from the MZR is driven by the stellar mass. We compareour observations with Rhapsody-G cosmological hydrodynamical zoom-insimulations of relaxed galaxy clusters and find that the simulated galaxycluster also exhibits a negative abundance gradient, albeit with a shallowerslope (-0.04+/-0.03 dex/Mpc). Our observations suggest that the negative radialgradient originates from ram-pressure stripping and/or strangulation processesin the cluster environments.

Radial Distribution Of ISM Gas-phase Metallicity In CLASH Clusters at z~0.35: A New Outlook On Environmental Impact On Galaxy Evolution