  We present here a preliminary report and commentary of recently processed
observations of Ha emission towards the Magellanic Bridge. These data have been
analysed in an attempt to quantify the extent to which the stellar population
is capable of reshaping the local ISM. We find that the Ha emission regions are
small, weak and sparsely distributed, consistent with a relatively quiescent
and inactive ISM where radiative and collisional ionisation is inefficient and
sporadic. This suggests that energetic processes at the small scale (i.e. ~tens
of pc) do not dominate the energy balance within the ISM of the Bridge, which
therefore hosts a pristine turbulent structure, otherwise inaccessible within
our own Galaxy. We find Ha emission that is well correlated with detected
12CO(1-0) line emission (a proxy for molecular hydrogen), as well as other
easily identified ring-like HI features.
