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We identify the nature of high redshift long Gamma-Ray Bursts (LGRBs) hostgalaxies by comparing the observed abundance ratios in the interstellar mediumwith detailed chemical evolution models accounting for the presence of dust. Wecompare abundance data from long Gamma-Ray Bursts afterglow spectra toabundance patterns as predicted by our models for different galaxy types. Weanalyse [X/Fe] abundance ratios (where X is C, N, O, Mg, Si, S, Ni, Zn) asfunctions of [Fe/H]. Different galaxies (irregulars, spirals, spheroids) are,in fact, characterised by different star formation histories, which producedifferent [X/Fe] vs. [Fe/H] relations ("time-delay model"). This allows us toidentify the star formation history of the host galaxies and to infer their age(i.e. the time elapsed from the beginning of star formation) at the time of theGRB events. Unlike previous works, we use newer models in which we adoptupdated stellar yields and prescriptions for dust production, accretion anddestruction. We consider a sample of seven LGRB host galaxies. Our resultssuggest that two of them (GRB 050820, GRB 120815A) are star forming spheroids,two (GRB 081008, GRB 161023A) are spirals and three (GRB 090926A, GRB 050730,GRB 120327A) are irregulars. The inferred ages of the considered host galaxiesspan from 10 Myr to slightly more than 1 Gyr.

Galactic archaeology at high redshift: inferring the nature of GRB host galaxies from abundances