  The source HESS J1809-193 was discovered in 2006 in data of the Galactic
Plane survey, followed by several re-observations. It shows a hard gamma-ray
spectrum and the emission is clearly extended. Its vicinity to PSR J1809-1917,
a high spin-down luminosity pulsar powerful enough to drive the observed
gamma-ray emission, makes it a plausible candidate for a TeV Pulsar Wind Nebula
(PWN). On the other hand, in this region of the sky a number of faint,
radio-emitting supernova remnants can be found, making a firm conclusion on the
source type difficult.
  Here we present a detailed morphological study of recent H.E.S.S. data and
compare the result with X-ray measurements taken with Chandra and radio data.
The association with a PWN is likely, but contributions from supernova remnants
cannot be ruled out.
