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Pulsar wind nebulae (PWNe) are among the most extreme particle acceleratorsin galaxies, are recognized as multi-TeV electron/positron sources, and are oneof the dominant classes of Galactic gamma-ray sources. Vela X is a nearby PWNat 290 pc from the Earth with large apparent size ($>1^\circ$). The H.E.S.S.array of imaging atmospheric Cherenkov telescopes has detected Vela X as one ofthe brightest known sources of TeV gamma rays. The bulk of the gamma-rayemission measured using H.E.S.S. coincides with an elongated structure knownfrom X-ray observations and dubbed the cocoon, that seemingly emanates from theregion of the pulsar wind termination shock. The spectral energy distributionof the cocoon peaks at around 10 TeV, and then presents a cutoff that can beprecisely measured with H.E.S.S. owing to the extreme brightness of the source.Electrons radiating inverse-Compton gamma rays in the cutoff region are thesame responsible for the X-ray synchrotron emission at energies $> 1$ keV.Therefore, Vela X provides a unique test case, in which we can constrain thedensities and spectra of accelerated leptons in the cutoff regime, as well asthe magnetic field properties, with minimal modeling assumptions. Thanks to theproximity/large apparent size of the source, this can be done in aspatially-resolved fashion across the PWN. We will present an analysis ofH.E.S.S. data combined with X-ray data from the Suzaku space telescope. We willdiscuss implications for the mechanisms behind particle acceleration andtransport, constrain the strength of the magnetic field in different locationsin the nebula, and probe for magnetic field turbulence.

The Vela X pulsar wind nebula through the eyes of H.E.S.S. and Suzaku