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The rate of long-duration gamma ray bursts (GRBs) has been identified as apotential proxy for the star formation rate (SFR) across redshift, but theexact relationship depends on GRB progenitor models (single versus binary). Thesingle-progenitor collapsar model accounts for the preference towardslow-metallicity GRB progenitors, but is in apparent tension with somehigh-metallicity GRB host galaxy measurements. As a possible solution, weconsider the scenario where high-metallicity GRB hosts harbour low metallicityregions in which GRB progenitors form. For this, we use the IllustrisTNGcosmological hydrodynamical simulation to investigate the internal metallicitydistribution of GRB hosts, implementing in post-processing different GRBformation models. Predictions (GRB rate, host metallicities and stellar masses)are compared to the high-completeness GRB legacy surveys BAT6 and SHOALS and asample of high-redshift GRB-DLA metallicities, allowing us to compute theirrelative likelihoods. When the internal metallicity distribution of galaxies isignored, the best-fitting model requires a metallicity-independent channel, aspreviously proposed by Trenti, Perna & Jimenez. However, when the internalmetallicity distribution is considered, a basic metallicity bias model with acutoff at $Z_{max}=0.35Z_\odot$ is the best fitting one. Current data areinsufficient to discriminate among more detailed metallicity bias models, suchas weak metallicity dependence of massive binaries vs stronger metallicity biasof collapsars. An increased sample of objects, and direct measurements of hoststellar masses at redshift $z>2$ would allow to further constrain the origin oflong GRBs.

One star, two stars, or both? Investigating metallicity-dependant models for Gamma-Ray Burst progenitors with the IllustrisTNG simulation