As galaxies assemble and evolve they form stars. Since each cycle of star formation boosts the metal content of the galaxy, chemical abundances provide a fossil record of a galaxy’s star-forming history.
Modern simulations of galaxy evolution make predictions about the chemical evolution of galaxies, though competing simulations differ. Meanwhile, providing observations with absolute levels of accuracy that can discriminate between competing models has proved to be challenging.
In this meeting, we aim to bring together observers studying a wide variety of abundance tracers (hot stars, cool stars, nebulae), to explore the strengths and weaknesses of each technique, and the regimes under which they are the most reliable. Simultaneously, we will assemble theorists from competing groups to discuss their numerical results to identify the most robust theoretical predictions. The ultimate goal of the programme is to devise a set of experiments that will allow us to make conclusive quantitative tests of the theory of galaxy evolution.