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GRB 190114C is the first GRB for which the detection of very-high energyemission up to the TeV range has been reported. It is still unclear whetherenvironmental properties might have contributed to the production of these veryhigh-energy photons, or if it is solely related to the released GRB emission.The relatively low redshift of the GRB (z=0.425) allows us to study the hostgalaxy of this event in detail, and to potentially identify idiosyncrasies thatcould point to progenitor characteristics or environmental propertiesresponsible for such a unique event. We use ultraviolet, optical, infrared andsubmillimetre imaging and spectroscopy obtained with HST, VLT and ALMA toobtain an extensive dataset on which the analysis of the host galaxy is based.The host system is composed of a close pair of interacting galaxies (Delta v =50 km s^-1), both of which are well-detected by ALMA in CO(3-2). The GRBoccurred within the nuclear region (~170 pc from the centre) of the lessmassive but more star-forming galaxy of the pair. The host is more massive(log(M/M_odot)=9.3) than average GRB hosts at that redshift and the location ofthe GRB is rather unique. The enhanced star-formation rate was probablytriggered by tidal interactions between the two galaxies. Our ALMA observationsindicate that both host galaxy and companion have a high molecular gasfraction, as has been observed before in interacting galaxy pairs. The locationof the GRB within the core of an interacting galaxy with an extinguishedline-of-sight is indicative of a denser environment than typically observed forGRBs and could have been crucial for the generation of the very-high-energyphotons that were observed.

GRB 190114C in the nuclear region of an interacting galaxy -- A detailed host analysis using ALMA, HST and VLT