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Context. The distribution of elements in galaxies forms an importantdiagnostic tool to characterize the system's formation and evolution. This toolis however complex to use in practice, as galaxies are subject to a range ofsimultaneous physical processes active from pc to kpc scales. This rendersobservations of the full optical extent of galaxies down to sub-kpc scalesessential. Aims. Using the WiFeS integral field spectrograph, we previouslydetected abrupt and localized variations in the gas-phase oxygen abundance ofthe spiral galaxy HCG91c. Here, we follow-up on these observations to mapHCG91c's disk out to ~2Re at a resolution of 600pc, and characterize thenon-radial variations of the gas-phase oxygen abundance in the system. Methods.We obtained deep MUSE observations of the target under ~0.6 arcsec seeingconditions. We perform both a spaxel-based and aperture-based analysis of thedata to map the spatial variations of 12+log(O/H) across the disk of thegalaxy. Results. We confirm the presence of rapid variations of the oxygenabundance across the entire extent of the galaxy previously detected withWiFeS, for all azimuths and radii. The variations can be separated in twocategories: a) localized and associated with individual HII regions, and b)extended over kpc scales, and occurring at the boundaries of the spiralstructures in the galaxy. Conclusions. Our MUSE observations suggest that theenrichment of the interstellar medium in HGC91c has proceeded preferentiallyalong spiral structures, and less efficiently across them. Our datasethighlights the importance of distinguishing individual star-forming regionsdown to scales of a few 100pc when using integral field spectrographs tospatially resolve the distribution of oxygen abundances in a given system, andaccurately characterize azimuthal variations and intrinsic scatter.

Evidence for azimuthal variations of the oxygen abundance gradient tracing the spiral structure of the galaxy HCG91c