On the origin of the galactic ridge recombination lines
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Radio recombination lines are known to be observable at positions along the galactic ridge which are free of discrete continuum sources. Based on the results of a recent survey of H272α lines it is shown that most of the observed galactic ridge recombination lines can be explained as emission from outer low-density envelopes of normal Hn regions. The distribution of low-density ionized gas and discrete HII regions as a function of the distance from the galactic centre is also derived.
Key wordsGalaxy recombination lines galactic ridge HII regions low-density envelopes distribution
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- Lockman, F. J. 1980, inRadio Recombination Lines, Ed. P. A. Shaver, D. Reidel, Dordrecht, p. 185.Google Scholar
- Sandage, A. R., Tammann, G. A. 1974,Astrophys. J.,156, 269.Google Scholar
- Schmidt, M. 1965, inStars and Stellar Systems, Eds A. Blaauw & M. Schmidt, Univ. Chicago Press, 5, 513.Google Scholar
- Shaver, P. A., Goss, W. M. 1970,Austr. J. Phys. Astrophys. Suppl. No. 14, 133.Google Scholar