The dust content of galaxies from z = 0 to z = 9
  We study the dust content of galaxies from $z=0$ to $z=9$ in semi-analytic
models of galaxy formation that include new recipes to track the production and
destruction of dust. We include condensation of dust in stellar ejecta, the
growth of dust in the interstellar medium (ISM), the destruction of dust by
supernovae and in the hot halo, and dusty winds and inflows. The rate of dust
growth in the ISM depends on the metallicity and density of molecular clouds.
Our fiducial model reproduces the relation between dust mass and stellar mass
from $z=0$ to $z=7$, the number density of galaxies with dust masses less than
$10^{8.3}\,\rm{M}_\odot$, and the cosmic density of dust at $z=0$. The model
accounts for the double power-law trend between dust-to-gas (DTG) ratio and
gas-phase metallicity of local galaxies and the relation between DTG ratio and
stellar mass. The dominant mode of dust formation is dust growth in the ISM,
except for galaxies with $M_*<10^7\,\rm{M}_\odot$, where condensation of dust
in supernova ejecta dominates. The dust-to-metal ratio of galaxies depends on
the gas-phase metallicity, unlike what is typically assumed in cosmological
simulations. Model variants including higher condensation efficiencies, a fixed
timescale for dust growth in the ISM, or no growth at all reproduce some of the
observed constraints, but fail to simultaneously reproduce the shape of dust
scaling relations and the dust mass of high-redshift galaxies.
