  We present new images of the OMC-1 molecular hydrogen outflow, made using
long-slit spectroscopy in order to accurately subtract the underlying continuum
emission. These images reveal an extremely clumpy, quasi-spherical inner shell
that breaks up at larger radii into bow-shocks and trailing wakes in the
north-west, as originally described by Allen & Burton (1993); a fainter
counter-finger to the south-east is newly discovered in the present data. While
the outflow appears to be broadly bipolar, this is probably due to an
interaction between an initially spherical wind from the source and a
large-scale density enhancement surrounding it, rather than direct collimation
imposed close to the source. The clumpy appearance of the inner shell confirms
the prediction of the recent model of Stone, Xu, & Mundy (1995), in which a
spherical and time-varying wind fragments a swept-up shell, producing
high-velocity shrapnel, which in turn drives bow-shocks into the surrounding
gas, resulting in the observed "fingers". As an alternative to the single
varying source proposed by Stone et al., we speculate that several young
sources in the BN-KL cluster may have been responsible for first sweeping up
the shell and then fragmenting it.
