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Observations of evolution in the dust-to-metal ratio allow us to constrainthe dominant dust processing mechanisms. In this work, we present a study ofthe dust-to-metal and dust-to-gas ratios in a sub-sample of ~500 DustPediagalaxies. Using literature and MUSE emission line fluxes, we derived gas-phasemetallicities (oxygen abundances) for over 10000 individual regions anddetermine characteristic metallicities for each galaxy. We study how therelative dust, gas, and metal contents of galaxies evolve by using metallicityand gas fraction as proxies for evolutionary state. The global oxygen abundanceand nitrogen-to-oxygen ratio are found to increase monotonically as galaxiesevolve. Additionally, unevolved galaxies (gas fraction > 60%, metallicity 12 +log(O/H) < 8.2) have dust-to-metal ratios that are about a factor of 2.1 lower(a factor of six lower for galaxies with gas fraction > 80%) than the typicaldust-to-metal ratio (Md/MZ ~ 0.214) for more evolved sources. However, for highgas fractions, the scatter is larger due to larger observational uncertaintiesas well as a potential dependence of the dust grain growth timescale andsupernova dust yield on local conditions and star formation histories. We findchemical evolution models with a strong contribution from dust grain growthdescribe these observations reasonably well. The dust-to-metal ratio is alsofound to be lower for low stellar masses and high specific star formation rates(with the exception of some sources undergoing a starburst). Finally, themetallicity gradient correlates weakly with the HI-to-stellar mass ratio, theeffective radius and the dust-to-stellar mass ratio, but not with stellar mass.

A systematic metallicity study of DustPedia galaxies reveals evolution in the dust-to-metal ratios