The assembly of dusty galaxies at $z\ge 4$: statistical properties

Abstract

The recent discovery of high redshift dusty galaxies implies a rapid dust enrichment of their interstellar medium (ISM). To interpret these observations, we run a cosmological simulation in a 30$h^{-1}$ cMpc/size volume down to $z\approx 4$. We use the hydrodynamical code dustyGadget, which accounts for the production of dust by stellar populations and its evolution in the ISM. We find that the cosmic dust density parameter (${\Omega }_{\mathrm{d}}$) is mainly driven by stellar dust at $z\gtrsim 10$, so that mass- and metallicity-dependent yields are required to assess the dust content in the first galaxies. At $z\lesssim 9$ the growth of grains in the ISM of evolved systems (Log$(M_{\star }/M_{\odot })>8.5$) significantly increases their dust mass, in agreement with observations in the redshift range $4\lesssim z<8$. Our simulation shows that the variety of high redshift galaxies observed with ALMA can naturally be accounted for by modeling the grain-growth timescale as a function of the physical conditions in the gas cold phase. In addition, the trends of dust-to-metal (DTM) and dust-to-gas ($\mathcal{D}$) ratios are compatible with the available data. A qualitative investigation of the inhomogeneous dust distribution in a representative massive halo at $z\approx 4$ shows that dust is found from the central galaxy up to the closest satellites along polluted filaments with $\mathrm{Log}(\mathcal{D})\le -2.4$, but sharply declines at distances $d\gtrsim 30$ kpc along many lines of sight, where $\mathrm{Log}(\mathcal{D})\lesssim -4.0$.

arXiv commentAccepted for publication in MNRAS

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