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We investigate the physical and chemical processes at work during theformation of a massive protostar based on the observation of water in anoutflow from a very young object previously detected in H2 and SiO in the IRAS17233-3606 region. We estimated the abundance of water to understand itschemistry, and to constrain the mass of the emitting outflow. We present newobservations of shocked water obtained with the HIFI receiver onboard Herschel.We detected water at high velocities in a range similar to SiO. Weself-consistently fitted these observations along with previous SiO datathrough a state-of-the-art, one-dimensional, stationary C-shock model. We foundthat a single model can explain the SiO and H2O emission in the red and bluewings of the spectra. Remarkably, one common area, similar to that found for H2emission, fits both the SiO and H2O emission regions. This shock modelsubsequently allowed us to assess the shocked water column density,N(H2O)=1.2x10^{18} cm^{-2}, mass, M(H2O)=12.5 M_earth, and its maximumfractional abundance with respect to the total density, x(H2O)=1.4x10^{-4}. Thecorresponding water abundance in fractional column density units ranges between2.5x10^{-5} and 1.2x10^{-5}, in agreement with recent results obtained inoutflows from low- and high-mass young stellar objects.

Water emission from the high-mass star-forming region IRAS 17233-3606. High water abundances at high velocities