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(abridged) Data and results from the WISH key program are summarized,designed to provide a legacy data set to address its physics and chemistry.WISH targeted ~80 sources along the two axes of luminosity and evolutionarystage: from low- to high-mass protostars and from pre-stellar cores toprotoplanetary disks. Lines of H2O, HDO, OH, CO and [O I] were observed withthe HIFI and PACS instruments, complemented by molecules that probe UV, X-rayor grain chemistry. Most of the far-infrared water emission from protostars isfound to be compact, originating from warm outflowing and shocked gas at highdensity and temperature in at least two physical components. This gas is notprobed by low-J CO lines, only by J>14. Water is a significant, but notdominant, coolant. Its abundance is universally low, of order H2O/H2=2E-6,pointing to shock and outflow cavity models that include UV radiation at100-1000 times the ISRF. In cold quiescent pre-stellar cores and envelopes, thewater abundance structure is accurately probed through velocity-resolved lineprofiles, confirming basic chemistry networks. The gaseous HDO/H2O ratio of0.025, much higher than that of bulk ice, is representative of the outerphotodesorbed ice layers and cold chemistry. Water abundances in the inner hotcores are high, but with variations from 5E-6 to 2E-4. Combined analyses ofwater gas and ice show that up to 50% of the oxygen budget may be missing, withpossible explanations discussed. Water vapor emission from disks is weak,indicating that water ice is locked up in larger pebbles early on and thatthese pebbles have settled and drifted inward by the Class II stage.Quantitatively, many oceans of water ice are available. Extragalactic low-J H2Oemission is mostly compact and collisionally excited. Prospects for future mid-to far-infrared missions are given.

Water in star-forming regions (WISH): Physics and chemistry from clouds to disks as probed by Herschel spectroscopy