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Large fractions of metals are missing from the observable gas-phase in theinterstellar medium (ISM) because they are incorporated into dust grains, aphenomenon called dust depletion. The study of dust depletion in the ISM isimportant to investigate the origin and evolution of metals and cosmic dust.Here we aim at characterizing the dust depletion of several metals from theMilky Way to distant galaxies. We collect ISM metal column densities fromabsorption-line spectroscopy in the literature, and in addition, we determineTi and Ni column densities from a sample of 70 damped Lyman-$\alpha$ absorbers(DLAs) towards quasars, observed with UVES/VLT. We use ISM relative abundancesto estimate the dust depletion of 18 metals (C, P, O, Cl, Kr, S, Ge, Mg, Si,Cu, Co, Mn, Cr, Ni, Al, Ti, Zn and Fe) for different environments (the MilkyWay, the Magellanic Clouds (MCs), DLAs towards quasars and towards gamma-raybursts). We observe linear relations between the depletion of each metal andthe strength of dust depletion, which we trace with the observed [Zn/Fe]. Inthe neutral ISM of the MCs we find small deviations from linearity observed asan overabundance of the $\alpha$-elements Ti, Mg, S and an underabundance ofMn. The deviations disappear if we assume that all OB stars observed towardsthe MCs in our sample have an $\alpha$-element enhancement and Mnunderabundance. This may imply that the MCs have been recently enriched in$\alpha$-elements, potentially due to recent bursts of star formation. Theobserved strong correlations of the depletion sequences of the metals all theway from low metallicity QSO-DLAs to the Milky Way suggest that cosmic dust hasa common origin, independently of the star formation history, which variessignificantly between these different galaxies. This supports the importance ofgrain growth in the ISM as a significant process of dust production.

Dust depletion of metals from local to distant galaxies I: Peculiar nucleosynthesis effects and grain growth in the ISM