  HESS J1825-137 is a bright very-high-energy (VHE) gamma-ray source that has
been firmly established as a pulsar wind nebula (PWN), and one of the most
extended gamma-ray objects within this category. The progenitor supernova
remnant (SNR) for this PWN has not been firmly established. We carried out an
analysis of gamma-ray observations in the region of HESS J1825-137 with the
Fermi-LAT which reveal emission in the direction away from the Galactic plane.
The region lies beyond the PWN and reaches a distance from the pulsar
compatible with the supposed location of the SNR shock front. The spectrum of
the gamma-rays is hard with a photon index of $\sim 1.9$ in the 10-250 GeV
range. Several scenarios for the origin of the emission are discussed,
including the SNR as a source of high-energy particles and the "leakage"' of
leptons from the PWN.
