Simulating the dust content of galaxies: successes and failures

We present full-volume cosmological simulations, using the moving-mesh code AREPO to the coevolution of dust and galaxies. We extend the dust model in AREPO to include sputtering of grains and investigate the evolution of the dust mass function, the cosmic of dust beyond the interstellar medium and the dependence of dust-to-stellar mass on galactic properties. The simulated dust mass function is well described by a Schechter and lies closest to observations at z = 0. The radial scaling of projected dust surface density to distances of 10 Mpc around galaxies with magnitudes 17 < i < 21 is similar to that seen Sloan Digital Sky Survey data, albeit with a lower normalization. At z=0, the predicted dust of dust ≈1. 3×10^ (−6) lies in the range of dust values seen in low-redshift observations. find that the dust-to-stellar mass ratio anticorrelates with stellar mass for galaxies living the star formation main sequence. Moreover, we estimate the 850 μm number density for simulated galaxies and analyse the relation between dust-to-stellar flux and mass at z = 0. At high redshift, our model fails to produce enough dust-rich galaxies, and tension is not alleviated by adopting a top-heavy initial mass function. We do not capture decline in dust from z = 2 to 0, which suggests that dust production mechanisms more dependent on star formation may help to produce the observed number of dusty near the peak of cosmic star formation.