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(Abridged) Long gamma-ray bursts (LGRB) have been suggested as promisingtracers of star formation owing to their association with the core-collapse ofmassive stars. The goal of this work is to characterise the population of hostgalaxies of LGRBs at 1 < z < 2, investigate the conditions in which LGRBs format these redshifts and assess their use as tracers of star formation. Weperform a spectro-photometric analysis to determine the stellar mass, starformation rate, specific star formation rate and metallicity of the complete,unbiased host galaxy sample of the Swift/BAT6 LGRB sample at 1 < z < 2. Wecompare the distribution of these properties to the ones of typicalstar-forming galaxies from the MOSDEF and COSMOS2015 Ultra Deep surveys, withinthe same redshift range. We find that, similarly to z < 1, LGRBs do notdirectly trace star formation at 1 < z < 2, and they tend to avoid high-mass,high-metallicity host galaxies. We also find evidence for an enhanced fractionof starbursts among the LGRB host sample with respect to the star-formingpopulation of galaxies. Nonetheless we demonstrate that the driving factorruling the LGRB efficiency is metallicity. The LGRB host distributions can bereconciled with the ones expected from galaxy surveys by imposing a metallicityupper limit of 12+logOH ~ 8.55. Metallicity rules the LGRB productionefficiency, which is stifled at Z > 0.7 Zsun. Under this hypothesis we canexpect LGRBs to trace star formation at z > 3, once the bulk of the starforming galaxy population are characterised by metallicities below this limit.The moderately high metallicity threshold found is in agreement with theconditions necessary to rapidly produce a fast-rotating Wolf-Rayet star a inclose binary system, and could be accommodated by single star models underchemically homogeneous mixing with very rapid rotation and weak magneticcoupling.

astronomy and astrophysics

Are LGRBs biased tracers of star formation? Clues from the host galaxies  of the $Swift$/BAT6 complete sample of bright LGRBs III: Stellar masses, star  formation rates and metallicities at $z>1$