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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