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Molecular Mass Distribution in the Outer Galaxy

Published online by Cambridge University Press:  25 May 2016

Sean J. Carey,
Kathryn N. Mead and
Marc L. Kutner
Sean J. Carey
Affiliation:
Rensselaer Polytechnic Institute, Troy, NY, 12180, USA carey@charon.phys.rpi.edu
Kathryn N. Mead
Affiliation:
NRAO, Tucson, AZ, USA
Marc L. Kutner
Affiliation:
NRAO, Tucson, AZ, USA

Extract

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The extent and nature of molecular material in the outer Galaxy (R > R⊙) has been an open, interesting question since the discovery of molecular material in the outer Galaxy (Kutner & Mead, 1981). From large scale CO surveys, two estimates of the total molecular mass have been made with the same result, M(H2) = 6 × 108 M⊙ (Wouterloot et al., 1990), (Digel et al., 1990). Both estimates have a strong bias towards large, star forming (warm) clouds. Wouterloot et al. used the IRAS point source catalog as a finder chart for their observations and the inner Galaxy mass distribution to scale their result. Digel et al. conducted an unbiased survey with a large (8.8 arcminute) beam which underestimated the amount of material in small clouds due to the effects of beam dilution.

Information

Type
Chapter 7: How are we to Understand the Small Scale Structure of the ISM?
Information
Symposium - International Astronomical Union , Volume 169: Unsolved Problems of the Milky Way , 1996, pp. 607 - 608
Copyright
Copyright © Kluwer 1996 

References

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