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The Interstellar Medium in Galaxies pp 67–120Cite as

Molecular Clouds in Spiral Galaxies

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Part of the book series: Astrophysics and Space Science Library ((ASSL,volume 161))

Abstract

Observations of the 2.6mm CO emission in more than 200 galaxies are used to deduce the molecular content, the yield in young stars per unit molecular gas mass, and the H2/HI ratio as a function of radius in individual galaxies and globally as a function of morphological type, luminosity, and environment. New evidence indicates that the molecular masses for spiral galaxies are accurate to better than a factor of 2, that the ratio of molecular to atomic gas mass decreases by a factor of ~20 among spiral galaxies from type SO/a to Sd/m, and that the mean yield of high mass stars per unit mass of molecular gas in spiral galaxies is constant as a function of type.

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Authors and Affiliations

  1. Department of Physics and Astronomy, University of Massachusetts, 01003, Amherst, MA, USA

    Judith S. Young

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  1. Judith S. Young
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  1. Wyoming Infrared Observatory, Laramie, USA

    Harley A. Thronson Jr.

  2. Royal Observatory, Edinburgh, UK

    Harley A. Thronson Jr.

  3. Joint Institute for Laboratory Astrophysics, University of Colorado, USA

    J. Michael Shull

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Young, J.S. (1990). Molecular Clouds in Spiral Galaxies. In: Thronson, H.A., Shull, J.M. (eds) The Interstellar Medium in Galaxies. Astrophysics and Space Science Library, vol 161. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-0595-5_4

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  • DOI: https://doi.org/10.1007/978-94-009-0595-5_4

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