Dust evolution in cosmological simulations
  We study the evolution of dust in a cosmological volume using a
hydrodynamical simulation in which the dust production is coupled with the
MUPPI (MUlti Phase Particle Integrator) sub-resolution model of star formation
and feedback. As for the latter, we keep as reference the model setup
calibrated previously to match the general properties of Milky Way like
galaxies in zoom-in simulations. However, we suggest that an increase of the
star formation efficiency with the local dust to gas ratio would better
reproduce the observed evolution of the cosmic star formation density.
Moreover, the paucity of quenched galaxies at low redshift demands a stronger
role of AGN feedback. We tune the parameters ruling direct dust production from
evolved stars and accretion in the inter stellar medium to get scaling
relations involving dust, stellar mass and metallicity in good agreement with
observations. In low mass galaxies the accretion process is inefficient. As a
consequence, they remain poorer in silicate and small grains than higher mass
ones. We reproduce reasonably well the few available data on the radial
distribution of dust outside the galactic region, supporting the assumption
that the dust and gas dynamics are well coupled at galactic scales.
