Contents of: VI/111/./abstract/TWILSON_ORICLUMP.abs

The following document lists the file abstract/TWILSON_ORICLUMP.abs from catalogue VI/111.
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The dense cores in Orion are the nearest high mass star formation region;
to study high mass star formation, one MUST study Orion. Radio molecular
line measurements show that the cloud cores in the Orion region have
physical characteristics which are different from dense cores in dark
clouds. We have started a large scale radio survey of ammonia lines
and millimeter dust continuum emission of the maxima in the Orion cloud,
outside the Orion KL region. To the north of Orion KL, the 'S' shaped cloud
is well defined with a number of cores. It is more diffuse and has fewer
regions to the south of Orion KL. We plan to study 10 fairly isolated regions
regions north of Orion KL, 15 close to but outside KL, and 10 south of KL to
determine the abundances of OH, CO, H2, CH and the atomic species CII, OI,
NII, SiI, SiII, SI, SIII and NeII. These results cannot be obtained in the
radio range, and will be used to determine abundances, and the energy
balance and will complement our centimeter and millimeter data. The Orion
cloud is a prototype of high mass star formation regions, and thus will
serve as a model for studies of star forming regions in distant galaxies,
and also as a comparison with our ISO project to study galactic center
clouds. For the distant galaxies, where the angular resolution and
sensitivity are much lower, our radio an ISO data will serve as a
'rosetta stone' to decode these results.  Although not a direct continuation
of our galactic center proposal, this proposal is a direct follow up and
in this sense, is indeed a continuation.

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