  We present the results of radio continuum and molecular line observations
conducted using the Mopra millimetre-wave telescope and Australia Telescope
Compact Array. These observations reveal the presence of a dense core embedded
within each cloud, and the presence of a layer of hot ionised gas coincided
with their bright-rims. The ionised gas has electron densities significantly
higher than the critical density above which an ionised boundary layer can form
and be maintained, strongly supporting the hypothesis that these clouds are
being photoionised by the nearby OB star(s). From an evaluation of the pressure
balance between the ionised and molecular gas, SFO 58 and SFO 68 are identified
as being in a post-pressure balance state, while SFO 75 and SFO 76 are more
likely to be in a pre-pressure balance state. We find secondary evidence for
the presence of ongoing star formation within SFO 58 and SFO 68, such as
molecular outflows, OH, H$_2$O and methanol masers, and identify a potential
embedded UC HII region, but find no evidence for any ongoing star formation
within SFO 75 and SFO 76. Our results are consistent with the star formation
within SFO 58 and SFO 68 having been triggered by the radiatively driven
implosion of these clouds.
