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Insights on molecular cloud structure

Published online by Cambridge University Press:  27 April 2011

João Alves ,
Marco Lombardi  and
Charles Lada
João Alves
Affiliation:
University of Vienna, Türkenschanzstrasse 17, 1180 Vienna, Austria email: joao.alves@univie.ac.at
Marco Lombardi
Affiliation:
ESO, Karl-Schwarzschild-Strasse 2, D-85748 Garching bei München, Germany University of Milan, Department of Physics, via Celoria 16, I-20133 Milan, Italy
Charles Lada
Affiliation:
Harvard-Smithsonian Center for Astrophysics, MS42, 60 Garden St., Cambridge, MA 02138
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Abstract

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Stars form in the densest regions of clouds of cold molecular hydrogen. Measuring structure in these clouds is far from trivial as 99% of the mass of a molecular cloud is inaccessible to direct observation. Over the last decade we have been developing an alternative, more robust density tracer technique based on dust extinction measurements towards background starlight. The new technique does not suffer from the complications plaguing the more conventional molecular line and dust emission techniques, and when used with these can provide unique views on cloud chemistry and dust grain properties in molecular clouds. In this brief communication we summarize the main results achieved so far using this technique.

Keywords

ISM: cloudsdustextinctionstructurestars: formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S270: Computational Star Formation , May 2010 , pp. 99 - 102
Copyright
Copyright © International Astronomical Union 2011

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