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We present measurements of the [NII]/Ha ratio as a probe of gas-phase oxygenabundance for a sample of 419 star-forming galaxies at z=0.6-2.7 from theKMOS3D near-IR multi-IFU survey. The mass-metallicity relation (MZR) isdetermined consistently with the same sample selection, metallicity tracer, andmethodology over the wide redshift range probed by the survey. We find goodagreement with long-slit surveys in the literature, except for the low-massslope of the relation at z~2.3, where this sample is less biased than previoussamples based on optical spectroscopic redshifts. In this regime we measure asteeper slope than some literature results. Excluding the AGN contribution fromthe MZR reduces sensitivity at the high mass end, but produces otherwiseconsistent results. There is no significant dependence of the [NII]/Ha ratio onSFR or environment at fixed redshift and stellar mass. The IFU data allowspatially resolved measurements of [NII]/Ha, from which we can infer abundancegradients for 180 galaxies, thus tripling the current sample in the literature.The observed gradients are on average flat, with only 15 gradientsstatistically offset from zero at >3sigma. We have modelled the effect ofbeam-smearing, assuming a smooth intrinsic radial gradient and known seeing,inclination and effective radius for each galaxy. Our seeing-limitedobservations can recover up to 70% of the intrinsic gradient for the largest,face-on disks, but only 30% for the smaller, more inclined galaxies. We do notfind significant trends between observed or corrected gradients and any stellarpopulation, dynamical or structural galaxy parameters, mostly in agreement withexisting studies with much smaller sample sizes. In cosmological simulations,strong feedback is generally required to produce flat gradients at highredshift.

The evolution of metallicity and metallicity gradients from z=2.7-0.6 with KMOS3D