Contrasting the chemical and physical evolution of isolated and clustered pre-protostellar cores

Details Contrasting the chemical and physical evolution of isolated and clustered pre-protostellar cores Contrasting the chemical and physical evolution of isolated and clustered pre-protostellar cores

Apr 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006atnf.prop..269f&link_type=abstract

ATNF proposal C1566, Semester: April, 2006

Physics

Galactic, Atca

Scientific paper

The process by which dense filaments in molecular clouds further fragment into solar-mass sized centrally condensed cores is currently a matter of debate. We have previously mapped the most massive star-forming cores in the Ophiuchus molecular cloud in NH3 emission at high spatial and spectral resolution with the ATCA. Our results differ from those obtained in observations of isolated pre-protostellar cores, where submillimeter and NH3 line emission are found to correlate well. To study this correlation in light of our recent observations, we propose to expand our study of the fragmentation and evolution of dense gas in Ophiuchus by making pointed NH3 observations of less massive (~ solar mass), isolated cores visible in dust continuum emission. These observations will complete a survey of the densest cores and filaments in the central star-forming region of Ophiuchus. Combining the results of observations towards isolated cores with the data in hand of the larger Oph filaments, which are forming multiple cores, will enable us to compare the physical process of fragmentation and collapse of dense gas in both isolated and clustered regions in the same molecular cloud.

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