Hostname: page-component-8448b6f56d-mp689 Total loading time: 0 Render date: 2024-04-24T10:38:11.668Z Has data issue: false hasContentIssue false
  • English
  • Français

Some Highlights of Interferometry in early Radio Astronomy

Published online by Cambridge University Press:  12 April 2016

Woodruff T. Sullivan III
Woodruff T. Sullivan III*
Affiliation:
Department of Astronomy FM-20, University of Washington, Seattle, WA 98195USA

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Two important episodes in the early development of interferometry in radio astronomy are traced in detail. The first is the use of the sea-cliff interferometer at the Radiophysics Laboratory in Sydney, first by Pawsey for solar observations and later by Bolton for radio star surveys. The second is the development of the Michelson interferometer and the phase switch by Ryle in Cambridge. This also was employed for important observations of the sun and radio stars.

Type
History
Information
International Astronomical Union Colloquium , Volume 131: Radio Interferometry: Theory, Techniques, and Applications , 1991 , pp. 132 - 149
Copyright
Copyright © Astronomical Society of the Pacific 1991

References

Bolton, J.G. (1948). “Discrete sources of galactic radio frequency noise.” Nature 162: 141–2.Google Scholar
Bolton, J.G. and Stanley, G.J. (1948a). “Variable source of radio frequency radiation in the constellation of Cygnus.” Nature 161: 312–3.CrossRefGoogle Scholar
Bolton, J.G. and Stanley, G.J. (1948b). “Observations on the variable source of cosmic radio frequency radiation in the constellation of Cygnus.” Austral. J. Sci. Res. A1: 58–69.Google Scholar
Bolton, J.G. and Stanley, G.J. (1949). “The position and probable identification of the source of galactic radio-frequency radiation TaurusA.” Austral. J. Sci. Res. A2: 139-48.Google Scholar
Bolton, J.G., Stanley, G.J. and Slee, O.B. (1949). “Positions of three discrete sources of galactic radio-frequency radiation.” Nature 164: 101-2.CrossRefGoogle Scholar
Bolton, J.G. (1982). “Radio astronomy at Dover Heights.” Proc. Astron. Soc. Australia 4: 349-58.CrossRefGoogle Scholar
Christiansen, W.N. (1984). “The first decade of solar radio astronomy in Australia.” pp. 113-31 in Sullivan (1984a).CrossRefGoogle Scholar
Eckersley, T.L. (1938). “A wireless interferometer.” Nature 141: 369-70.CrossRefGoogle Scholar
Edge, D.O. and Mulkay, M.J. (1976). Astronomy Transformed: The Emergence of Radio Astronomy in Britain. New York: John Wiley and Sons.Google Scholar
Hanbury Brown, R. (1974). The Intensity Interferometer. London: Taylor and Francis.Google Scholar
Hey, J.S., Parsons, S.J. and Phillips, J.W. (1946). “Fluctuations in cosmic radiation at radio-frequencies.” Nature 158: 234.CrossRefGoogle ScholarPubMed
Hey, J.S. (1973). The Evolution of Radio Astronomy. London: Elek Science.Google Scholar
McCready, L.L., Pawsey, J.L. and Payne-Scott, R. (1947). “Solar radiation at radio frequencies and its relation to sunspots.” Proc. Roy. Soc. A190: 357-75.Google ScholarPubMed
Mills, B.Y. (1952). “The distribution of the discrete sources of cosmic radio radiation.” Austral. J. Sci. Res. A5: 266-87.Google Scholar
Erratum: Austral. J. Physics, Vol. 6, p. 125 (1953).Google Scholar
Mills, B.Y. (1984). “Radio sources and the log N - log S controversy.” pp. 147-65 in Sullivan (1984a).CrossRefGoogle Scholar
Reber, G. (1958). “Early radio astronomy at Wheaton, Illinois.” Proc. IRE 46: 15–23. also reprinted in Sullivan (1984a).CrossRefGoogle Scholar
Ryle, M. and Smith, F.G. (1948). “A new intense source of radio-frequency radiation in the constellation of Cassiopeia.” Nature 162: 462-3.Google Scholar
Ryle, M. and Vonberg, D.D. (1946). “Solar radiation on 175 Mc./s.” Nature 158: 339-40.CrossRefGoogle Scholar
Ryle, M. and Vonberg, D.D. (1948). “An investigation of radio-frequency radiation from the sun.” Proc. Roy. Soc. A193: 98–120.Google ScholarPubMed
Ryle, M., Smith, F.G. and Elsmore, B. (1950). “A preliminary survey of the radio stars in the Northern Hemisphere.” Mon. Not. RAS 110: 508-23.erratum: Vol. 111, p. 641 (1951).CrossRefGoogle Scholar
Ryle, M. (1952). “A new radio interferometer and its application to the observation of weak radio stars.” Proc. Roy. Soc. A211: 351-75.Google Scholar
Scheuer, P.A.G. (1984). “The development of aperture synthesis at Cambridge.” pp. 249-65 in Sullivan (1984a).CrossRefGoogle Scholar
Scheuer, P.A.G. (1990). “Radio source counts.” pp. 331-45 in Modern Cosmology in Retrospect, (ed. Bertotti, R. et al.). Cambridge: Cambridge Univ. Press.Google Scholar
Sullivan, W.T., III (1984a) (Ed.). The Early Years of Radio Astronomy: Reflections Fifty Years after Jansky. Cambridge: Cambridge University Press.CrossRefGoogle Scholar
Sullivan, W.T., III (1984b). “Karl Jansky and the discovery of extraterrestrial radio waves.” pp. 3–42 in Sullivan (1984a).CrossRefGoogle Scholar
Sullivan, W.T., III (1988). “Early years of Australian radio astronomy.” pp. 308-44 in Australian Science in the Making, (ed. Home, R.W.). Sydney: Cambridge University Press.Google Scholar
Sullivan, W.T., III (1990). “The entry of radio astronomy into cosmology: Radio stars and Martin Ryle’s 2C survey.” pp. 309-30 in Modern Cosmology in Retrospect, (ed. Bertotti, R. et al.). Cambridge: Cambridge Univ. Press.Google Scholar