Abstract details

Simulations of the chemical evolution of the Local Group dwarf galaxies will be presented, explaining the differences in gas and stellar chemical properties between spheroidal and irregular classes of dwarfs in terms of their proximity to their central host galaxy. Empirically-derived spatial and temporal star formation histories are imposed on Galactic Chemical Evolution models which track the loss of ejecta from low- and intermediate-mass stars, multiple supernovae classes, compact object (neutron star and black hole) mergers. For the first time, a self-consistent treatment of the neutron capture contribution from intermediate mass stars has been considered in tandem with the traditional light, alpha, and iron-peak elements, clearly demonstrating the critical role of the former to the evolution of dwarf galaxies. Nucleosynthetic constraints are provided which suggest that dwarfs are not fossil relics of the epoch of reionisation. Further, the link between dwarf galaxy interstellar media abundance patterns, supergalactic winds, and the chemical fingerprint of quasar absorbers in the intergalactic medium, will be highlighted.