  Using NASA's Submillimeter Wave Astronomy Satellite (SWAS) we have examined
the production of water in quiescent and shocked molecular gas through a survey
of the 556.936 GHz transition of ortho-H2O in the NGC 1333 molecular core.
These observations reveal broad emission lines associated with the IRAS~2,
IRAS~4, IRAS~7, and HH7-11 outflows. Towards 3 positions we detect narrow (~2-3
km/s) emission lines clearly associated with the ambient gas. The SWAS
observations, with a resolution of 4', are supplemented with observations from
the Infrared Space Observatory (ISO) and by an unbiased survey of a 17' x 15'
area, with 50" resolution, in the low-J transitions of CO, 13CO, C18O, N2H+,
CH3OH, and SiO.
  Using these combined data sets, with consistent assumptions, we find
beam-averaged o-H2O abundances of > 10^{-6} relative to H2O for all four
outflows. A comparison of SWAS and ISO water data is consistent with
non-dissociative shock models, provided the majority of the 557 GHz emission
arises from cool post-shock material with enhanced abundances. In the ambient
gas the o-H2O abundance is found to lie between 0.1-1 x 10^{-7} relative to H2
and is enhanced when compared to cold pre-stellar molecular cores. A comparison
of the water emission with tracers of dense condensations and shock chemistry
finds no clear correlation. However, the water emission appears to be
associated with the presence of luminous external heating sources which power
the reflection nebula and the photodissociation (PDR) region. Simple PDR models
are capable of reproducing the water and high-J 13CO emission, suggesting that
a PDR may account for the excitation of water in low density undepleted gas as
suggested by Spaans & van Dishoeck (2001).
