Molecular Line Observations in the Magellanic Clouds

Details Molecular Line Observations in the Magellanic Clouds Molecular Line Observations in the Magellanic Clouds

Jan 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005hia....13..854r&link_type=abstract

Highlights of Astronomy, Vol. 13, as presented at the XXVth General Assembly of the IAU - 2003 [Sydney, Australia, 13 - 26 July

Astronomy and Astrophysics

Astronomy

Scientific paper

We will review the present knowledge of molecular line studies an its relation tointerstellar medium properties in the Large and Small Magellanic Cloud. The physical and chemical properties of the molecular gas together withthe abundance of different molecular species will be discussed. The Magellanic Clouds interstellar medium (ISM) is known for its lowermetallicity with respect to our Galaxy. The C abundance is 0.25 solar in the LMC and 0.10 in the SMC respectively.In addition they showa low gas to dust ratio and therefore the elemental and molecular abundance estimates are less affected by dust extinction. Thus these galaxies provide an excellent laboratory for the study of the effects of metallicity variations on the properties of the interstellar medium. Implications to ISM properties in systems in the early universe will be explored.

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