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A Dirty WindowThe Relationship Between CO and H2

A Dirty Window: The Relationship Between CO and H2 [The CO(1-0) transition is the most important molecular emission line for studying molecular gas in the ISM. Unfortunately, it is nearly always optically thick, and so determining N(CO) and, more importantly, N(H2) is complicated. Over the years several empirical techniques have been worked out for using the CO(1-0) line to determine the physically relevant quantity, N(H2). In this chapter we discuss these techniques with particular emphasis on determining the conversion factor (called XCO) for diffuse and translucent molecular gas. The chapter closes with some comments on using the CO(1-0) line to trace dark gas.] http://www.deepdyve.com/assets/images/DeepDyve-Logo-lg.png

A Dirty WindowThe Relationship Between CO and H2

Part of the Astrophysics and Space Science Library Book Series (volume 442)
Magnani, Loris; Shore, Steven N.
Springer Journals — Apr 9, 2017
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Publisher
Springer Berlin Heidelberg
Copyright
© Springer-Verlag GmbH Germany 2017
ISBN
978-3-662-54348-1
Pages
205 –225
DOI
10.1007/978-3-662-54350-4_8
Publisher site
See Chapter on Publisher Site

Abstract

[The CO(1-0) transition is the most important molecular emission line for studying molecular gas in the ISM. Unfortunately, it is nearly always optically thick, and so determining N(CO) and, more importantly, N(H2) is complicated. Over the years several empirical techniques have been worked out for using the CO(1-0) line to determine the physically relevant quantity, N(H2). In this chapter we discuss these techniques with particular emphasis on determining the conversion factor (called XCO) for diffuse and translucent molecular gas. The chapter closes with some comments on using the CO(1-0) line to trace dark gas.]

Published: Apr 9, 2017

Keywords: Molecular Cloud; Column Density; Galactic Plane; Dark Cloud; Antenna Temperature

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