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We present an analysis of the chemical abundance properties of $\approx$650star-forming galaxies at $z \approx0.6-1.8$. Using integral-field observationsfrom the $K$-band Multi-Object Spectrograph (KMOS), we quantify the[NII]/H$\alpha$ emission-line ratio, a proxy for the gas-phase Oxygen abundancewithin the interstellar medium. We define the stellar mass-metallicity relationat $z \approx0.6-1.0$ and $z \approx1.2-1.8$ and analyse the correlationbetween the scatter in the relation and fundamental galaxy properties (e.g.H$\alpha$ star-formation rate, H$\alpha$ specific star-formation rate, rotationdominance, stellar continuum half-light radius and Hubble-type morphology). Wefind that for a given stellar mass, more highly star-forming, larger andirregular galaxies have lower gas-phase metallicities, which may beattributable to their lower surface mass densities and the higher gas fractionsof irregular systems. We measure the radial dependence of gas-phase metallicityin the galaxies, establishing a median, beam smearing-corrected, metallicitygradient of $ \Delta Z/ \Delta R=0.002 \pm0.004$ dex kpc$^{-1}$, indicating onaverage there is no significant dependence on radius. The metallicity gradientof a galaxy is independent of its rest-frame optical morphology, whilstcorrelating with its stellar mass and specific star-formation rate, inagreement with an inside-out model of galaxy evolution, as well as its rotationdominance. We quantify the evolution of metallicity gradients, comparing thedistribution of $\Delta Z/ \Delta R$ in our sample with numerical simulationsand observations at $z \approx0-3$. Galaxies in our sample exhibit flattermetallicity gradients than local star-forming galaxies, in agreement withnumerical models in which stellar feedback plays a crucial role redistributingmetals.

The Evolution of Gas-Phase Metallicity and Resolved Abundances in Star-forming Galaxies at $z \approx0.6-1.8$