Chemodynamics of a Simulated Disc Galaxy: Initial Mass Functions and
  SNIa Progenitors
  We trace the formation and advection of several elements within a
cosmological adaptive mesh refinement simulation of an L* galaxy. We use nine
realisations of the same initial conditions with different stellar Initial Mass
Functions (IMFs), mass limits for type-II and type-Ia supernovae (SNII, SNIa)
and stellar lifetimes to constrain these sub-grid phenomena. Our code includes
self-gravity, hydrodynamics, star formation, radiative cooling and feedback
from multiple sources within a cosmological framework. Under our assumptions of
nucleosynthesis we find that SNII with progenitor masses of up to 100 Msun are
required to match low metallicity gas oxygen abundances. Tardy SNIa are
necessary to reproduce the classical chemical evolution knee in [O/Fe]-[Fe/H]:
more prompt SNIa delayed time distributions do not reproduce this feature.
Within our framework of hydrodynamical mixing of metals and galaxy mergers we
find that chemical evolution is sensitive to the shape of the IMF and that
there exists a degeneracy with the mass range of SNII. We look at the abundance
plane and present the properties of different regions of the plot, noting the
distinct chemical properties of satellites and a series of nested discs that
have greater velocity dispersions, are more alpha-rich and metal poor with age.
