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Galactic structure at meter wavelengths

Published online by Cambridge University Press:  14 August 2015

B. Y. Mills
B. Y. Mills*
Affiliation:
Radiophysics Laboratory, Commonwealth Scientific and Industrial Research Organization, Sydney, Australia

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The study of meter-wave radiation from the Milky Way has been hampered, until recently, by the difficulty of obtaining sufficiently high resolution. Observations using interferometers had early indicated the probability of fine structure in the radiation distribution, but the interpretation of these observations was not unique. It was not until the Sydney 3.5-m cross-type radio telescope (beamwidth 50 minutes of arc) was put into operation in 1954 that it became possible to study the distribution of meter wave emission in detail. The observational program with this instrument, together with most of the data analysis relating to the galactic emission, has now been completed and some of the results have already been described [1, 2]. It seems appropriate at this time to give a rather detailed account of the results of this completed work and to discuss its astronomical and astrophysical significance.

Type
Part IV: The Large-Scale Structure of Galaxies
Information
Symposium - International Astronomical Union , Volume 9: Paris Symposium on Radio Astronomy , 1959 , pp. 431 - 446
Copyright
Copyright © Stanford University Press 1959 

References

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