Dust evolution in zoom-in cosmological simulations of galaxy formation

GRANATO, G. L.; RAGONE FIGUEROA, C.; TAVERNA, ANTONELA; SILVA, LAURA; VALENTINI, MILENA; BORGANI, S.; MONACO, PIERLUIGI; MURANTE, GIUSEPPE; TORNATORE, LUCA

Marseille

Congreso; The Rise of Metals and Dust in Galaxies through Cosmic Time; 2020

University of Provence

We present cosmological zoom-in hydrodynamical simulations for the formation of disc galaxies, implementing dust evolutionand dust promoted cooling of hot gas. We couple an improved version of our previous treatment of dust evolution, which adoptsthe two-size approximation to estimate the grain-size distribution, with the MUPPI star formation and feedback subresolutionmodel. Our dust evolution model follows carbon and silicate dust separately. To distinguish differences induced by the chaoticbehaviour of simulations from those genuinely due to different simulation set-up, we run each model six times, after introducingtiny perturbations in the initial conditions. With this method, we discuss the role of various dust-related physical processesand the effect of a few possible approximations adopted in the literature. Metal depletion and dust cooling affect the evolutionof the system, causing substantial variations in its stellar, gas, and dust content. We discuss possible effects on the SpectralEnergy Distribution of the significant variations of the size distribution and chemical composition of grains, as predicted by oursimulations during the evolution of the galaxy. We compare dust surface density, dust-to-gas ratio, and small-to-large grain massratio as a function of galaxy radius and gas metallicity predicted by our fiducial run with recent observational estimates for threedisc galaxies of different masses. The general agreement is good, in particular taking into account that we have not adjusted ourmodel for this purpose.