2010A&A...518L.120N

The far-IR/sub-mm spectral mapping facility provided by the Herschel-PACS and HIFI instruments has made it possible to obtain, for the first time, images of H₂O emission with a spatial resolution comparable to ground based mm/sub-mm observations. In the framework of the Water In Star-forming regions with Herschel (WISH) key program, maps in water lines of several outflows from young stars are being obtained, to study the water production in shocks and its role in the outflow cooling. This paper reports the first results of this program, presenting a PACS map of the o-H₂O 179µm transition obtained toward the young outflow L1157. The 179µm map is compared with those of other important shock tracers, and with previous single-pointing ISO, SWAS, and Odin water observations of the same source that allow us to constrain the H₂O abundance and total cooling. Strong H₂O peaks are localized on both shocked emission knots and the central source position. The H₂O 179µm emission is spatially correlated with emission from H₂ rotational lines, excited in shocks leading to a significant enhancement of the water abundance. Water emission peaks along the outflow also correlate with peaks of other shock-produced molecular species, such as SiO and NH₃. A strong H₂Opeak is also observed at the location of the proto-star, where none of the other molecules have significant emission. The absolute 179 µm intensity and its intensity ratio to the H₂O 557GHz line previously observed with Odin/SWAS indicate that the water emission originates in warm compact clumps, spatially unresolved by PACS, having a H₂O abundance of the order of 10^–4. This testifies that the clumps have been heated for a time long enough to allow the conversion of almost all the available gas-phase oxygen into water. The total H₂O cooling is ∼10^–1L_☉, about 40% of the cooling due to H₂ and 23% of the total energy released in shocks along the L1157 outflow.