  We present results of VLBI observations of the water masers associated with
IRAS 4A and IRAS 4B in the NGC 1333 star-forming region taken in four epochs
over a two month period. Both objects have been classified as extremely young
sources and each source is known to be a multiple system. Using the Very Long
Baseline Array, we detected 35 masers in Epoch I, 40 masers in Epoch II, 35 in
Epoch III, and 24 in Epoch IV. Only one identified source in each system
associates with these masers. These data are used to calculate proper motions
for the masers and trace the jet outflows within 100 AU of IRAS 4A2 and IRAS
4BW. In IRAS 4A2 there are two groups of masers, one near the systemic cloud
velocity and one red-shifted. They expand linearly away from each other at
velocities of 53 km/s. In IRAS 4BW, masers are observed in two groups that are
blue-shifted and red-shifted relative to the cloud velocity. They form complex
linear structures with a thickness of 3 mas (1 AU at a distance of 320 pc) that
expand linearly away from each other at velocities of 78 km/s. Neither of the
jet outflows traced by the maser groups align with the larger scale outflows.
We suggest the presence of unresolved companions to both IRAS 4A2 and 4BW.
