Abstract
Interest has developed rapidly in the astrophysics associated with far-infrared line emission from ionised regions, following the development of spectroscopic instruments and observing facilities appropriate to those wavelengths. The first detection of a far-infrared fine structure line was by Ward et al. (1975) with the 88 μm line of 0++. Subsequent instrumental development has improved the limiting sensitivity by a factor of about 1000, principally through the use of cooled Fabry-Perot etalons. These observations have sufficient spectral resolution to match the width of lines from exceptional regions, such as the galactic centre, equivalent to a velocity range of 100 km/sec. A resolution about 10 times better than this is required to match the lines from normal galactic HII regions and this performance was approached by Baluteau et al. (1976) using a Michelson interferometer.
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Emery, R.J., Kessler, M.F. (1984). Far-Infrared Spectroscopy of HII Regions. 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_19
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DOI: https://doi.org/10.1007/978-94-009-7251-3_19
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