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The chemical enrichment in the interstellar medium (ISM) of galaxies isregulated by several physical processes: stellar evolution, grain formation anddestruction, galactic inflows and outflows. Understanding such processes isessential to follow the chemical enrichment of galaxies through the cosmicepochs, and to interpret the observations. Despite the importance of suchtopics, the efficiency of the different processes driving the evolution ofbaryons in galaxies, remain controversial. We revise the current description ofmetal and dust evolution in local low-metallicity dwarf galaxies and we developa description for Lyman Break Galaxies. Our main goal is to reproduce i) thepeak in the mass of dust over the mass of stars (sMdust) observed within fewhundred Myrs; ii) the decrease of the sMdust at later time. The spectral energydistribution of the galaxies is fitted with the "Code Investigating GALaxiesEmission" (CIGALE), through which the stellar and dust masses, and the starformation rate are estimated. For some of the dwarf galaxies, the metal and gascontent are also available. We run different calculations of chemical evolutionin galaxies, and we fit the observed properties through the model predictions.We show that i) a top-heavy initial mass function that favours massive starsand a dust condensation fraction for Type II Supernovae (SNe II) of 50% or morehelp to reproduce the peak of sMdust observed after 100 Myrs since thebeginning of the cycle; ii) galactic outflows play a crucial role inreproducing the decline in sMdust with age, and they are more efficient thangrain destruction from SNe II; iii) a star formation efficiency (mass of gasconverted into stars) of few per cent is required to explain the metallicity oflocal dwarf galaxies; iv) dust growth in the ISM is not necessary to reproducethe sMdust and, if present, its effect is erased by galactic outflows.

The gas, metal and dust evolution in low-metallicity local and high-redshift galaxies