Abstract
This paper deals with the analysis of interstellar clouds through infrared and submillimeter observations. The determination of temperature, density, state of ionization and abundance of different chemical constituents is discussed for clouds exhibiting a range of optical depths. There is a preferred choice of spectral features useful for examining different types of gaseous complexes. The prospects for improving our understanding of chemical reaction schemes in interstellar clouds are outlined. Prime advances may be expected in improved data on the abundance of atoms; diatomic hydrides; other small, hydrogen-containing molecules; and their ions.
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Harwit, M. (1984). The Significance of Far-Infrared Spectra of the Interstellar Medium. 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_10
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DOI: https://doi.org/10.1007/978-94-009-7251-3_10
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