Speakers
Description
The evolution of dust is important for understanding galaxy evolution. More detailed models of dust formation are needed to reproduce observations of dust in galaxies at high redshift, which include high dust-to-stellar mass ratios in z~7 galaxies observed with ALMA. At the same time, the moderate amount of dust at z~14 seen with JWST requires processes such as dust destruction by the supernova reverse shock to reproduce in models. A better understanding of dust reddening and extinction is also necessary to more accurately analyse observations of galaxies. Therefore, we introduce a dust model into our cosmological hydrodynamical simulations. Our code is based on GADGET-3 but includes the latest nucleosynthesis yields to trace the evolution of elemental abundances in detail as well as all necessary baryon physics such as radiative cooling, AGN, star formation and supernova feedback. We trace the mass of carbon, iron, alumina and different species of silicate dust grains in the interstellar medium (ISM). Dust grains are produced by core-collapse supernovae and Asymptotic Giant Branch stars and are distributed into the ISM. The dust mass is further increased by accretion from the gas phase or decreased by star formation, supernova shock waves and thermal sputtering. We then compare our results with observations from both high redshift and the local universe.
