| dc.description.abstract | This thesis presents molecular line and radio continuum observations of the giant molecular
cloud (GMC) complex known as G305. The energy input from high-mass stars in the form
of powerful winds and ionising radiation is one of the primary feedback mechanisms in GMCs.
This feedback is thought to play a dual role both dispersing and destroying the natal environment
but also sweeping up and compressing molecular gas and potentially triggering new episodes
of star formation. Despite their importance to the evolution of GMCs and galaxies as a whole,
the physical processes behind the formation and evolution of high-mass stars remains poorly
understood. We therefore set out to obtain wide-field observations of the ionised and molecular
environment to study the impact of high-mass stars on the evolution of G305.
Observations conducted with the Mopra telescope of the molecular gas traced by NH3 in the
(1,1), (2,2) and (3,3) transition and CO (12CO, 13CO and C18O J = 1–0) reveals the reservoir
for future star formation in G305 and allows the physical properties and kinematics of the region
to be studied. We identify 15 large molecular clouds and 57 smaller molecular clumps towards
G305. The physical properties of the molecular gas are consistent with G305 being amongst
the most massive a vigorous star forming regions in the Galaxy. We find a total molecular gas
mass of 2:5–6:5 105M indicating that there is a large reservoir for future star formation.
By considering virial equilibrium within the molecular clumps we discover that only 14% of the
molecular clumps in G305 are gravitationally unstable, however these clumps contain > 30% of
the molecular mass in G305 suggesting there is scope for considerable future star formation.
To study the ionised environment towards G305 we have obtained some of the largest and most
detailed wide-area mosaics with the Australia Telescope Compact Array to date. These radio
continuum observations were performed simultaneously at 5.5 and 8.8 GHz and by applying
two imaging techniques we are able to resolve HII regions from the ultra-compact to classical
evolutionary phase. This has allowed high-mass star formation within G305 to be traced over
the extent and lifetime of the complex. We discover that more than half of the observable
total ionising flux in G305 is associated with embedded high-mass star formation around the
periphery of a central cavity that has been driven into the molecular gas by a cluster of optically
visible massive stars. By considering the contribution of embedded and visible massive stars to
the observed radio continuum we suggest that more than 45 massive stars exist within G305.
Combination of these two studies and recent and ongoing star formation provides the most
in depth view of G305 to date and allows the star formation history and impact of high-mass
stars to be investigated. We find compelling morphological evidence that suggests triggering
is responsible for at least some of the observed high-mass star formation and construct a star
formation history for the region. | en_US |
