Molecules and dust in the Magellanic Clouds

Details Molecules and dust in the Magellanic Clouds Molecules and dust in the Magellanic Clouds

Sep 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984iaus..108..319i&link_type=abstract

IN: Structure and evolution of the Magellanic Clouds; Proceedings of the Symposium, Tuebingen, West Germany, September 5-8, 1983

Astronomy and Astrophysics

Astronomy

37

Cosmic Dust, Interstellar Matter, Magellanic Clouds, Molecular Clouds, Carbon Monoxide, Hydrogen Clouds, Hydroxyl Emission, Infrared Astronomy, Interstellar Extinction, Interstellar Masers

Scientific paper

Techniques for radio surveys of dust and molecular cloud emissions from the Magellanic Clouds are described, along with the contributions of the data to modeling star formation and the appearance and destruction of molecular material. The dust is observed in the UV and near-IR bands to detect the presence of molecules. Scans are further refined to map out regions of trace molecules by their transition emissions. Low dust concentrations in the Clouds permit line-of-sight adjustments to eliminate dust from the data. OH and H2O maser emissions then identify star nurseries. UV, near- and far-IR surveys are necessary, and seldom fully adequate, to discern the line-of-sight gas/dust ratios. Thermal IR data are in any case the most appropriate for mapping dust, and have served for characterizing the Small Magellanic Cloud as nearly transparent. The Large Magellanic Cloud is also fairly dust-depleted in comparison to the Galaxy's dust content.

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