In this work, we investigate the chemical dependence of the progenitors of long gamma-ray bursts. Using hydrodynamical cosmological simulations consistent with the concordance Λ-CDM model which include star formation, chemical enrichment and supernova feedback in a self-consistent way, and assuming that these bursts are produced by a subset of massive stars (possibly with distinct chemical properties), we compute the LGRB rate at different redshifts. Introducing prescriptions for their peak isotropic luminosity function and intrinsic spectrum, and using a Monte Carlo scheme to model their detectability by different high-energy observatories, we compute the distributions of the burst observables (peak flux, spectral peak energy) and compare them to actual data. Our preliminary results show that a possible chemical dependence for LGRBs progenitors cannot be ruled out, but it might be more complex than the usually assumed metallicity cut-off.
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