Dust Formation in Milky Way-like Galaxies
  We introduce a dust model for cosmological simulations implemented in the
moving-mesh code AREPO and present a suite of cosmological hydrodynamical
zoom-in simulations to study dust formation within galactic haloes. Our model
accounts for the stellar production of dust, accretion of gas-phase metals onto
existing grains, destruction of dust through local supernova activity, and dust
driven by winds from star-forming regions. We find that accurate stellar and
active galactic nuclei feedback is needed to reproduce the observed
dust-metallicity relation and that dust growth largely dominates dust
destruction. Our simulations predict a dust content of the interstellar medium
which is consistent with observed scaling relations at $z = 0$, including
scalings between dust-to-gas ratio and metallicity, dust mass and gas mass,
dust-to-gas ratio and stellar mass, and dust-to-stellar mass ratio and gas
fraction. We find that roughly two-thirds of dust at $z = 0$ originated from
Type II supernovae, with the contribution from asymptotic giant branch stars
below 20 per cent for $z \gtrsim 5$. While our suite of Milky Way-sized
galaxies forms dust in good agreement with a number of key observables, it
predicts a high dust-to-metal ratio in the circumgalactic medium, which
motivates a more realistic treatment of thermal sputtering of grains and dust
cooling channels.
