  Pulsar wind nebulae (PWNe) are among the most extreme particle accelerators
in galaxies, are recognized as multi-TeV electron/positron sources, and are one
of the dominant classes of Galactic gamma-ray sources. Vela X is a nearby PWN
at 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 of
the brightest known sources of TeV gamma rays. The bulk of the gamma-ray
emission measured using H.E.S.S. coincides with an elongated structure known
from X-ray observations and dubbed the cocoon, that seemingly emanates from the
region of the pulsar wind termination shock. The spectral energy distribution
of the cocoon peaks at around 10 TeV, and then presents a cutoff that can be
precisely 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 the
same responsible for the X-ray synchrotron emission at energies $> 1$ keV.
Therefore, Vela X provides a unique test case, in which we can constrain the
densities and spectra of accelerated leptons in the cutoff regime, as well as
the magnetic field properties, with minimal modeling assumptions. Thanks to the
proximity/large apparent size of the source, this can be done in a
spatially-resolved fashion across the PWN. We will present an analysis of
H.E.S.S. data combined with X-ray data from the Suzaku space telescope. We will
discuss implications for the mechanisms behind particle acceleration and
transport, constrain the strength of the magnetic field in different locations
in the nebula, and probe for magnetic field turbulence.
