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Gas-phase abundances in galaxies are the products of those galaxies'evolutionary histories. The star-formation history (SFH) of a region mighttherefore be expected to influence that region's present day gaseousabundances. Here, we employ data from the MaNGA survey to explore how local gasmetallicities relate to star-formation histories of galaxy regions. We combineMaNGA emission line measurements with SFH classifications from absorption linespectra, to compare gas-phase abundances in star-forming regions with those inregions classified as starburst, post-starburst and green valley. We find thatstarburst regions contain gas that is more pristine than in normal star-formingregions, in terms of O/H and N/O; we further find that post-starburst regions(which have experienced stochastic SFHs) behave very similarly to ordinarystar-forming regions (which have experienced far smoother SFHs) in O/H-N/Ospace. We argue from this that gas is diluted significantly by pristine infallbut is then re-enriched rapidly after a starburst event, making gas-phaseabundances insensitive to the precise form of the SFH at late times. We alsofind that green-valley regions possess slightly elevated N/O abundances at agiven O/H; this is potentially due to a reduced star-formation efficiency insuch regions, but it could also point to late-time rejuvenation of green valleyregions in our sample.

SDSS-IV MaNGA: how do star-formation histories affect gas-phase abundances?