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Radio studies of the distribution of ionized gas

Published online by Cambridge University Press:  14 August 2015

Felix J. Lockman
Felix J. Lockman*
Affiliation:
Department of Terrestrial Magnetism, Carnegie Institution of Washington

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Although radio recombination line and continuum observations are very useful for investigating galactic structure, it is well to remember their limitations. First, they only provide measurements of coordinates and velocities; a kinematic model is needed to derive the distance and thus the actual location of every nebula. In some directions, particularly all longitudes from ℓ=0°, kinematic distance estimates are prone to systematic errors arising from velocity crowding or uncertainties in the rotation curve, and are of little use in quantitative studies. I will only discuss the distribution of radio nebulae in the inner ∼100° of the galactic plane, since in this area kinematic analyses can give reasonable results and, in any case, here we must rely on radio observations for most of our information.

Type
II. THE DISK COMPONENT
Information
Symposium - International Astronomical Union , Volume 84: The Large-Scale Characteristics of the Galaxy , 1979 , pp. 73 - 79
Copyright
Copyright © Reidel 1979 

References

Bowers, P.F.: 1978, Astron. Astrophys. 64, pp. 307–318.Google Scholar
Burton, W.B.: 1971, Astron. Astrophys. 10, pp. 76–96.Google Scholar
Burton, W.B.: 1976, Ann. Rev. Astron. Astrophys. 14, pp. 275–306.Google Scholar
Caswell, J.L.: 1972, Aust. J. Phys. 25, pp. 443–450.Google Scholar
Cohen, R.S. and Thaddeus, P.: Astrophys. J. 217, pp. L155–L159.Google Scholar
Dickel, J.R. and Milne, D.K.: 1972, Aust. J. Phys. 25, pp. 539–544.CrossRefGoogle Scholar
Hart, L. and Pedlar, A.: 1976, Mon. Not. Roy. Astron. Soc. 176, pp. 547–559.Google Scholar
Hart, L.: 1977, in van Woerden, H. (ed.), “Topics in Interstellar Matter”, Reidel, Dordrecht.Google Scholar
Lockman, F.J.: 1976, Astrophys. J. 209, pp. 429–444.Google Scholar
Lockman, F.J.: 1977, Astron. J. 82, 408–413.Google Scholar
Lockman, F.J.: 1979, Astrophys. J. (in the press).Google Scholar
Mezger, P.G.: 1970, in Becker, W. and Contopoulos, G. (eds.), “The Spiral Structure of Our Galaxy”, Reidel, Dordrecht.Google Scholar
Quiroga, R.: 1974, Astrophys. Space Sci. 27, pp. 323–342.Google Scholar
Reifenstein, E.C., Wilson, T.L., Burke, B.F., Mezger, P.G. and Alterhoff, W.J.: 1970, Astron. Astrophys. 4, pp. 257–377.Google Scholar
Wilson, T.L., Mezger, P.G., Gardner, F.F. and Milne, D.K.: 1970, Astron. Astrophys. 6, pp. 364–384.Google Scholar