Abstract
Molecular clouds are the active, star forming component of the interstellar medium. In this article, we review the theoretical and empirical basis for using the 2.6 mm CO emission line as a tracer of H2 and we summarize the galactic distribution and properties of the molecular clouds. [All quantitative estimates are reduced to the recent IAU adopted value of Ro=8.5 kpc.]
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Scoville, N.Z., Sanders, D.B. (1987). H2 in the Galaxy. In: Hollenbach, D.J., Thronson, H.A. (eds) Interstellar Processes. Astrophysics and Space Science Library, vol 134. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-3861-8_2
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DOI: https://doi.org/10.1007/978-94-009-3861-8_2
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