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The dust abundance of the interstellar medium plays an important role ingalaxy physics, the chemical evolution of matter and the absorption andre-emission of stellar light. The last years have seen a surge in observationaland theoretical studies constraining the dust-abundance of galaxies up to$z\sim5$. In this work we gather the latest observational measurements (with afocus on absorption studies covering metallicities in the range $6.8 < 12 +\log{(O/H)}<9$) and theoretical predictions (from six different galaxyformation models) for the dust-to-gas (DTG) and dust-to-metal (DTM) ratio ofgalaxies. The observed trend between DTG and DTM and gas-phase metallicity canbe described by a linear relation and shows no evolution from $0<z<5$.Importantly, the fit to the DTG-metallicity relation provides a refined toolfor robust dust-based gas mass estimates inferred from millimeterdust-continuum observations. The lack of evolution in the observed relationsare indicative of a quickly reached balance (already when the Universe was 1.2Gyr old) between the formation and destruction of dust and a constant timescalefor star-formation at fixed metallicities over cosmic time. None of the modelsis able to reproduce the observed trends over the entire range in metallicityand redshift probed. The comparison between models and simulations furthermorerules out some of the current implementations for the growth and destruction ofdust in galaxy formation models and places tight constraints on the predictedtimescale for star-formation.

Observed cosmic evolution of galaxy dust properties with metallicity and tensions with models