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18-25 GHz low-noise Line Receiver for the Tidbinbilla 64-m Antenna

Published online by Cambridge University Press:  25 April 2016

D. L. Jauncey
Affiliation:
Division of Radiophysics, CSIRO, Sydney
M. J. Batty
Affiliation:
Division of Radiophysics, CSIRO, Sydney
G. J. Gay
Affiliation:
Division of Radiophysics, CSIRO, Sydney
C. R. Moore
Affiliation:
Division of Radiophysics, CSIRO, Sydney
P. J. Batelaan
Affiliation:
Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
R. Clauss
Affiliation:
Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
D. Dickinson
Affiliation:
Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
S. Gulkis
Affiliation:
Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
M. Klein
Affiliation:
Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
T. Kuiper
Affiliation:
Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
G. Morris
Affiliation:
Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
D. Neff
Affiliation:
Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
W. B. Ricketts
Affiliation:
Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
P. Swanson
Affiliation:
Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California

Extract

A K-band (18-25 GHz) reflected-wave ruby maser (Moore and Clauss 1979) has been borrowed from the National Radio Astronomy Observatory for radio astronomy use on the NASA 64-m antenna of the Deep Space Network at the Tidbinbilla Tracking Station, near Canberra. The purpose of the installation is to provide additional sensitive spectral line, continuum, and VLBI capabilities in the southern hemisphere. Previous measurements at 22.3 GHz (λ = 13.5 mm) determined that the Tidbinbilla 64-m antenna has a peak aperture efficiency of ˜22%, a well-behaved beam shape and consistent pointing (Fourikis and Jauncey 1979). Before installing the maser on the antenna a cooled (circulator) switch was added to provide a beam-switching capability, and a spectral line receiver following the maser was incorporated. The system was assembled and tested at JPL in late 1980 and installed at Tidbinbilla early in 1981. We give here a brief description and present some of the first line observations made in February and March 1981. Extensive line and continuum observations are planned with the present system and a program is under way to determine the telescope pointing characteristics.

Type
Contributions
Copyright
Copyright © Astronomical Society of Australia 1981

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References

Batchelor, R. A., Caswell, J. L., Goss, W. M., Haynes, R. F., Knowles, S. H. and Wellington, K. J. Aust. J. Phys., 33, 139 (1980).CrossRefGoogle Scholar
Batchelor, R. A., and 14 others Leti. Astron. J. (USSR Acad. Sci.), 2, 467 (1976).Google Scholar
Fourikis, N. and Jauncey, D. L. Proc. Astron. Soc. Aust., 3, 353 (1979).CrossRefGoogle Scholar
Moore, C. R. and Clauss, R. C. IEEE Trans. Microwave Theory Tech., MTT-27, 249 (1979).CrossRefGoogle Scholar
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18-25 GHz low-noise Line Receiver for the Tidbinbilla 64-m Antenna
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