  We present the results of Keck Telescope laser adaptive optics integral field
spectroscopy with OSIRIS of the innermost regions of the NGC 1333 SVS 13
outflow that forms the system of Herbig-Haro objects 7-11. We find a bright 0.2
arc sec long microjet traced by the emission of shock-excited [FeII]. Beyond
the extent of this jet, we find a series of bubbles and fragments of bubbles
that are traced in the lower excitation H_2 1-0 S(1) line. While the most
recent outflow activity is directed almost precisely (PA ~145 deg) to the
south-east of SVS 13, there is clear indication that prior bubble ejections
were pointed in different directions. Within these variations, a clear
connection of the newly observed bubble ejection events to the well-known,
poorly collimated HH 7-11 system of Herbig-Haro objects is established.
Astrometry of the youngest of the expanding shock fronts at 3 epochs covering a
time span of over two years gives kinematic ages for two of these. The
kinematic age of the youngest bubble is slightly older than the historically
observed last photometric outburst of SVS 13 in 1990, consistent with that
event launching the bubble and some deceleration of its expansion. A
re-evaluation of historic infrared photometry and new data show that SVS 13 has
not yet returned to its brightness before that outburst and thus shows a
behavior similar to FUor outbursts, albeit with a smaller amplitude. We
postulate that the creation of a series of bubbles and the changes in outflow
direction are indicative of a precessing disk and accretion events triggered by
a repetitive phenomenon possibly linked to the orbit of a close binary
companion. We have tried, but failed to detect, the kinematic signature of
rotation of the microjet in the [FeII] emission line at 1.644 micrometers.
