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The internal distribution of heavy elements, in particular the radialmetallicity gradient, offers insight into the merging history of galaxies.Using our cosmological, chemodynamical simulations that include both detailedchemical enrichment and feedback from active galactic nuclei (AGN), we findthat stellar metallicity gradients in the most massive galaxies($\sim3\times10^{10}$M$_\odot$) are made flatter by mergers and are unable toregenerate due to the quenching of star formation by AGN feedback. The fittingrange is chosen on a galaxy-by-galaxy basis in order to mask satellitegalaxies. The evolutionary paths of the gradients can be summarised as follows;i) creation of initial steep gradients by gas-rich assembly, ii) passiveevolution by star formation and/or stellar accretion at outskirts, iii) suddenflattening by mergers. There is a significant scatter in gradients at a givenmass, which originates from the last path, and therefore from galaxy type. Somevariation remains at given galaxy mass and type because of the complexity ofmerging events, and hence we find only a weak environmental dependence. Ourearly-type galaxies (ETGs), defined from the star formation main sequencerather than their morphology, are in excellent agreement with the observedstellar metallicity gradients of ETGs in the SAURON and ATLAS3D surveys. Wefind small positive [O/Fe] gradients of stars in our simulated galaxies,although they are smaller with AGN feedback. Gas-phase metallicity and [O/Fe]gradients also show variation, the origin of which is not as clear as forstellar populations.

The Metallicity and Elemental Abundance Gradients of Simulated Galaxies, and their Environmental Dependence