Description
Detailed modelling of the formation and evolution of dust is important to explain the high dust content in z~7 galaxies observed with ALMA, as well as the carbonaceous dust in z~8 galaxies observed with JWST. The latter is particularly difficult to explain with our current theories of dust formation, which depend on Asymptotic Giant Branch (AGB) stars to be the main factories of carbonaceous dust. As a significant amount of metals are predicted to be locked inside dust grains, this may have a substantial impact on mass-metallicity relations and our understanding of early chemical enrichment. Therefore, we introduce dust into our cosmological chemodynamical simulations, focusing on dust production in the early universe. We trace the mass of carbonaceous, iron, and silicate dust grains in the ISM from initial conditions. We increase dust mass through production in core-collapse supernovae and AGB stars, and accretion from gas phase metals. We destroy dust through star formation, supernova shock waves and thermal sputtering. We then compare our results to high redshift observations to reproduce high dust-to-stellar mass ratios and the early 'carbon bump' indicative of carbon dust produced by AGB stars. We analyse particularly the impact of dust on the early chemical evolution of galaxies.
