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We present Gemini-S/GMOS-IFU optical spectroscopy of four regions near thecentre of the nearby (3.8 Mpc) dwarf starburst galaxy NGC 5253. This galaxy isfamous for hosting a radio supernebula containing two deeply embedded massivesuper star clusters, surrounded by a region of enhanced nitrogen abundance thathas been linked to the presence of WR stars. We detected 11 distinct sources ofred WR bump (CIV) emission over a 20" (~350 pc) area, each consistent with thepresence of ~1 WCE-type star. WC stars are not found coincident with thesupernebula, although WN stars have previously been detected here. We performeda multi-component decomposition of the H\alpha\ line across all four fields andmapped the kinematics of the narrow and broad (FWHM = 100-250 km/s) components.These maps paint a picture of localised gas flows, as part of multipleoverlapping bubbles and filaments driven by the star clusters throughout thestarburst. We confirm the presence of a strong H\alpha\ velocity gradient over~4.5" (~80 pc) coincident with the region of N/O enhancement, and high gasdensity known from previous study, and interpret this as an acceleratingionized gas outflow from the supernebula clusters. We measure the ionized gasabundances in a number of regions in the outer IFU positions and combine thesewith measurements from the literature to assess the radial abundancedistribution. We find that the O/H and N/H profiles are consistent with beingflat. Only the central 50 pc exhibits the well-known N/O enhancement, and wepropose that the unusually high densities/pressures in the supernebula regionhave acted to impede the escape of metal-enriched hot winds from the starclusters and allow them to mix with the cooler phases, thus allowing thesefreshly processed chemicals to be seen in the optical.

Piecing together the puzzle of NGC 5253: abundances, kinematics and WR stars