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Physical parameters in extragalactic star forming regions

Published online by Cambridge University Press:  03 August 2017

R. Mauersberger ,
C. Henkel  and
L. J. Sage
R. Mauersberger
Affiliation:
MPIfR, Auf dem Hügel 69, D-5300 Bonn, F.R.G.
C. Henkel
Affiliation:
MPIfR, Auf dem Hügel 69, D-5300 Bonn, F.R.G.
L. J. Sage
Affiliation:
MPIfR, Auf dem Hügel 69, D-5300 Bonn, F.R.G.

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To use a molecule as a diagnostic of a single star forming region, one has to observe it in different transitions. That is especially true for galaxies, where the beam filling factor is small and unknown. From studies of Galactic objects, the CS molecule is a good tracer of dense gas. Toward the IR galaxies NGC 253, IC 342 and M 82, Mauersberger and Henkel (1989) observed the J=2—1, 3—2 and 5—4 transitions of CS at 3, 2 and 1.3 mm wavelength, repectively. They also measured emission of the isotope C34S, which has an abundance ∼ 1/23 that of the main isotope. This study revealed that the H2 densities in the circumnuclear gas exceed 104, and, in the case of NGC 253, 105 cm−3. In all three cases, the distribution of the dense gas traced out by CS follows the CO distribution.

Type
Poster Sessions
Information
Symposium - International Astronomical Union , Volume 147: Fragmentation of Molecular Clouds and Star Formation , 1991 , pp. 458 - 459
Copyright
Copyright © Kluwer 1991 

References

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