Detailed dust modelling in the L-Galaxies semi-analytic model of galaxy
  formation
  We implement a detailed dust model into the L-Galaxies semi-analytical model
which includes: injection of dust by type II and type Ia supernovae (SNe) and
AGB stars; grain growth in molecular clouds; and destruction due to
supernova-induced shocks, star formation, and reheating. Our grain growth model
follows the dust content in molecular clouds and the inter-cloud medium
separately, and allows growth only on pre-existing dust grains. At early times,
this can make a significant difference to the dust growth rate. Above $z\sim8$,
type II SNe are the primary source of dust, whereas below $z\sim8$, grain
growth in molecular clouds dominates, with the total dust content being
dominated by the latter below $z\sim6$. However, the detailed history of galaxy
formation is important for determining the dust content of any individual
galaxy. We introduce a fit to the dust-to-metal (DTM) ratio as a function of
metallicity and age, which can be used to deduce the DTM ratio of galaxies at
any redshift. At $z\lesssim3$, we find a fairly flat mean relation between
metallicity and the DTM, and a positive correlation between metallicity and the
dust-to-gas (DTG) ratio, in good agreement with the shape and normalisation of
the observed relations. We also match the normalisation of the observed stellar
mass -- dust mass relation over the redshift range of $0-4$, and to the dust
mass function at $z=0$. Our results are important in interpreting observations
on the dust content of galaxies across cosmic time, particularly so at high
redshift.
