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The evolution of the cosmic dust content and the cycle between metals anddust in the interstellar medium (ISM) play a fundamental role in galaxyevolution. The chemical enrichment of the Universe can be traced through theevolution of the dust-to-metals ratio (DTM) and the dust-to-gas ratio (DTG)with metallicity. We use a novel method to determine mass estimates of the DTM,DTG and dust composition based on our previous measurements of the depletion ofmetals in different environments (the Milky Way, the Magellanic Clouds, anddamped Lyman-$\alpha$ absorbers, DLAs, toward quasars and towards gamma-raybursts, GRBs), which were calculated from the relative abundances of metals inthe ISM through absorption-line spectroscopy column densities observed mainlyfrom VLT/UVES and X-shooter, and HST/STIS. We derive the dust extinction fromthe estimated dust depletion ($A_{V, \rm depl}$) and compare with the $A_{V}$from extinction. We find that the DTM and DTG ratios increase with metallicityand with the dust tracer [Zn/Fe]. This suggests that grain growth in the ISM isa dominant process of dust production. The increasing trend of the DTM and DTGwith metallicity is in good agreement with a dust production and evolutionmodel. Our data suggest that the stellar dust yield is much lower than themetal yield and thus that the overall amount of dust in the warm neutral mediumthat is produced by stars is much lower. We find that $A_{V,\rm depl}$ isoverall lower than $A_{V, \rm ext}$ for the Milky Way and a few MagellanicClouds lines of sight, a discrepancy that is likely related to the presence ofcarbonaceous dust. We show that the main elements that contribute to the dustcomposition are, O, Fe, Si, Mg, C, S, Ni and Al for all the environments.Abundances at low dust regimes suggest the presence of pyroxene and metalliciron in dust.

Dust depletion of of metals from local to distant galaxies II: Cosmic dust-to-metal ratio and dust composition