Résumé
The H.E.S.S. source 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 Pulsar Wind Nebula. 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. We will present a morphological study of recent data of the source taken with H.E.S.S. We will compare the results with Chandra X-ray data and discuss possible radio counterparts. This may lead to the answer to the question of the nature of HESS J1809-193.