The main scientific goal is to detect water maser emission at
9 wavelengths in the range 116-196 microns towards a sample
of 4 well studied star-formation regions.  The existance of
these maser inversions have been predicted by Yates, Field
and Gray, in prep (Y94).  The solution of the radiative transfer
problem was performed using Accelerated Lambda Iteration
techniques, which yields precise quantitative solutions.
By measuring the fluxes (W  m(-2) of these masers
we will be able to test the numerical predictions of our
model, and place constraints on the density of molecular
hydrogen and water, and the kinetic temperature of the molecular
gas in the water masing regions.