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Large Scale Dissociation of Molecular Gas and Star Formation in M83

Published online by Cambridge University Press:  04 August 2017

R. J. Allen ,
P. D. Atherton  and
R.P.J. Tilanus
R. J. Allen
Affiliation:
Kapteyn Astronomical Institute, University of Groningen, The Netherlands Astronomy Department, University of Illinois, Urbana, Illinois USA
P. D. Atherton
Affiliation:
Kapteyn Astronomical Institute, University of Groningen, The Netherlands Queensgate Instruments Ltd. Sunbury-on-Thames, U.K.
R.P.J. Tilanus
Affiliation:
Queensgate Instruments Ltd. Sunbury-on-Thames, U.K.

Extract

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Observations of the distribution of the CO-molecule in several prominent late-type galaxies indicate that the central HI depressions may very well be filled in with molecular gas. One such galaxy is M83 (NGC 5236) and, although the angular resolution of the CO-observations is insufficient to discern details on the scale of a spiral arm, it is known that CO is concentrated in the central regions within a radius of 1′. Furthermore, at a resolution of 50″, the CO profile at the position of the nucleus is as bright in M83 as it is for example in NGC 6946, IC 346 and M51.

Type
II. Large Scale Processes of Star Formation
Information
Symposium - International Astronomical Union , Volume 115: Star Forming Regions , 1987 , pp. 628
Copyright
Copyright © Reidel 1987