Both H.E.S.S. and MAGIC Cherenkov telescopes have observed very-high energy (VHE) gamma-ray emission from W41, a 105 years-old supernova remnant (SNR). The origin of this emission is still uncertain. Different scenarios, notably interaction with a molecular cloud or pulsar wind nebulae, have been proposed, in relation to 13 CO emission and X-ray pulsar candidates spatially coincident with the VHE excess. The improvement in event reconstruction and selection developed by the H.E.S.S. collaboration allows us to analyse this source with an unprecedented gamma-ray angular resolution. Furthermore, thanks to 5 time more H.E.S.S. data since the discovery paper, it is now possible to examine more precisely the spatial distribution of the VHE gamma-rays from W41 in com-parison with radio data. Informations provided by the 1-year Fermi-LAT catalogue will be included in the discussion of possible scenarios. The nearby SNR G22.7-0.2 (̃0.6° from W41, well within the H.E.S.S. field of view) appears to coincide with CO emission and is thus another potential VHE gamma-ray emitter.