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Urquhart, J.S.; Thompson, M.A.; Morgan, L.K. and White, Glenn J.
(2006).
DOI: https://doi.org/10.1017/S1743921307002712
URL: http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?b...
Abstract
We present the results of an in-depth study of four bright-rimmed clouds (BRCs), SFO 58, SFO 68, SFO 75 and SFO 76 (Sugitani & Ogura 1994), conducted with the Swedish-ESO Submillimetre Telescope, Australia Telescope Compact Array and the Mopra millimetre telescope. BRCs are small molecular clouds are located on the periphery of evolved HII regions and are thought to be sites where star formation may have been triggered through the process of radiative-driven implosion (RDI). If these BRCs are star-forming regions, as suggested by their association with an infrared point source with colours consistent with embedded protostars, their simple geometries and isolation within their HII regions makes them ideal laboratories in which triggered star formation processes can be studied. We present the results of CO millimetre line, radio continuum, ammonia (1,1) and 1.2 mm continuum observations. Using these observations we evaluate the pressure balance between the ionised surface layers and the molecular cloud and determine the current state of star formation within each cloud. 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, H2O 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.
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