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High-resolution radio data of molecular gas in dwarf starburst galaxies

Published online by Cambridge University Press:  25 May 2016

David S. Meier ,
Jean L. Turner  and
Sara C. Beck
David S. Meier
Affiliation:
Department of Physics & Astronomy, UCLA, CA 90095-1562, USA
Jean L. Turner
Affiliation:
Department of Physics & Astronomy, UCLA, CA 90095-1562, USA
Sara C. Beck
Affiliation:
Department of Physics & Astronomy, Tel Aviv University, Ramat Aviv, Israel

Extract

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Star-formation in dwarf starburst galaxies can be quite intense for their sizes, especially in the very young ones characterized by Wolf-Rayet emission features. Since stars form out of molecular gas (H2), it is important to investigate in detail, where the molecular gas is relative to the star formation in such young starbursts. The molecular gas may also indicate what might have triggered the starburst. The ISM in dwarfs can be quite warm, is the molecular gas also warm? In an attempt to investigate the properties of molecular gas in WR galaxies we have obtained high resolution images of the J = 2–1 transitions of CO for two dwarf starbursts, NGC5253 and He2–10. Both galaxies are nearby dwarf starbursts with WR emission features (e.g., Conti 1991). NGC 5253 may be one of the youngest starbursts known (e.g., Rieke, Lebofsky & Walker 1988).

Type
Part 6. Starbursts in normal and active galaxies: their effects on the ISM and on chemical evolution
Information
Symposium - International Astronomical Union , Volume 193: Wolf-Rayet Phenomena in Massive Stars and Starburst Galaxies , 1999 , pp. 747 - 748
Copyright
Copyright © Astronomical Society of the Pacific 1999 

References

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