Abstract
The near infrared vibration rotation (v-r) bands of CO and H2 provide a powerful tool for the study of physical conditions in molecular clouds. They cluster individual v-r transitions, encompassing a wide range of excitation energy and line strength, into a relatively narrow frequency interval which can be observed with uniform instrumental techniques, often with a single instrument. Precise line frequencies and transition probabilities are available for both CO and H2. The v-r lines are not seen in emission from cool (T ≲ 200K) cloud material because their upper states (E/k ≳ 3000K) are not collisionally populated at such temperatures. However, the H2 transitions are emitted by shocked regions where T is ≳ 2000K and the CO transitions are seen in absorption against embedded continuum sources.
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Hall, D.N.B. (1984). Near-IR Spectroscopy of H2 and CO in Molecular Clouds. In: Kessler, M.F., Phillips, J.P. (eds) Galactic and Extragalactic Infrared Spectroscopy. Astrophysics and Space Science Library, vol 108. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-7251-3_17
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DOI: https://doi.org/10.1007/978-94-009-7251-3_17
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