Among the small class of gamma-ray binary systems, PSR B1259-63/LS 2883 is a peculiar case: It is one of two such systems for which the nature of the compact object is known, in this case being a pulsar, and its very eccentric 3.4-year orbit is suitable for frequent observations of periastron passages. Around the times of the periastron passages, bright emission is observed at all wavelengths, enabling detailed studies of particle acceleration and non-thermal photon emission in binary systems.

PSR B1259-63/LS 2883 was observed at very-high-energy (VHE) gamma rays with H.E.S.S. around the times of each periastron periastron passage from 2004 on until 2017. All available data were (re-)analysed using up-to-date analysis tools. Spectra and light curves of this variable gamma-ray emitter are derived from all available data, including phase-folded analysis results. Results from searches for super-orbital variability are presented. Lower limits on spectral cut-off energies are derived, indicating that PSR B1259-63/LS 2883 is an efficient emitter of VHE gamma rays.

In addition, a high-energy (HE) gamma-ray light curve derived from Fermi-LAT measurements is presented. Spectra measured contemporaneously in the HE and VHE gamma-ray domains are compared and discussed in a multi-component context.