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The detection of the first electromagnetic counterpart to the binary neutronstar (BNS) merger remnant GW170817 established the connection between short$\gamma$-ray bursts and BNS mergers. It also confirmed the forging of heavyelements in the ejecta (a so-called kilonova) via the r-processnucleosynthesis. The appearance of non-thermal radio and X-ray emission, aswell as the brightening, which lasted more than 100 days, were somewhatunexpected. Current theoretical models attempt to explain this temporalbehavior as either originating from a relativistic off-axis jet or akilonova-like outflow. In either scenario, there is some ambiguity regardinghow much energy is transported in the non-thermal electrons versus the magneticfield of the emission region. Combining the VLA (radio) and Chandra (X-ray)measurements with observations in the GeV-TeV domain can help break thisambiguity, almost independently of the assumed origin of the emission. Here wereport for the first time on deep H.E.S.S. observations of GW170817 / GRB170817A between 124 and 272 days after the BNS merger with the full H.E.S.S.array of telescopes, as well as on an updated analysis of the prompt (<5 days)observations with the upgraded H.E.S.S. phase-I telescopes. We discussimplications of the H.E.S.S. measurement for the magnetic field in the contextof different source scenarios.

Probing the magnetic field in the GW170817 outflow using H.E.S.S. observations