  We have carried out an extensive observational study (from BIMA data) and
made a preliminary theoretical investigation of the molecular gas around HH2.
The molecular maps show a very complex morphological, kinematical and chemical
structure. The overall main conclusion of this work confirms the findings of
Paper I and II, by demonstrating that in addition to the strong photochemical
effects caused by penetration of the UV photons from HH2 into molecular cloud,
a range of complex radiative and dynamical interactions occur. Thus, despite
the apparent `quiescent' nature of the molecular cloud ahead of HH2, the
kinematical properties observed within the field of view suggest that it is
possibly being driven out by powerful winds from the VLA 1 protostar.
