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The Molonglo Observatory Transient Event Recorder

Published online by Cambridge University Press:  25 April 2016

M. I. Large ,
A. E. Vaughan ,
J. M. Durdin  and
A. G. Little
M. I. Large
Affiliation:
School of Physics, University of Sydney
A. E. Vaughan
Affiliation:
School of Mathematics and Physics, Macquarie University
J. M. Durdin
Affiliation:
School of Physics, University of Sydney
A. G. Little
Affiliation:
School of Physics, University of Sydney
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Extract

In its normal synthesis mode of operation, the Molonglo Observatory Synthesis Telescope (MOST) tracks a region of sky for a period of 12 hours with 64 real-time fan beams having high sensitivity at 843 MHz (Mills 1981). It thus provides an excellent opportunity to monitor the sky at the same time for transient radio events. During a 12 hour synthesis observation the fan beams rotate 180° on the field. Thus any sources producing occasional radio transients can be located by analysing the positions of the beams on which the events are recorded. Futhermore, by rejecting events which occur simultaneously on non-adjacent beams, local terrestrial sources of impulsive interference may be eliminated. This technique for recognizing extra-terrestrial sources was of considerable value in the first Molonglo pulsar search when only two beams were used.

Type
Contributions
Information
Publications of the Astronomical Society of Australia , Volume 5 , Issue 4 , 1984 , pp. 569 - 574
Copyright
Copyright © Astronomical Society of Australia 1984

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References

Allan, J. R., Progress in Elementary Particle and Cosmic Ray Physics, Vol X (eds Wilson, J. G. and Wouthuysen, S. A.) Chapter 3, North Holland Publishing Company (1971).Google Scholar
Ashworth, M., Lyne, A. G. and Smith, F. G., Nature, 301, 313 (1983).Google Scholar
Backer, D. C., Kulkarni, S. R., Heiles, C., Davis, M. M. and Goss, W. M., Nature, 300, 615 (1982).Google Scholar
Daishido, T., Ohkawa, T., Yokoyama, T., Asuma, K., Kikuchi, H., Nagane, K., Hirabayashi, H. and Komatsu, S., Indirect Imaging, Proc. URSI/IAU symposium, Sydney 1983 (ed Roberts, J. A.) p. 81, C.U.P. (1984).Google Scholar
Huguenin, G. R. and Moore, E. L., Astrophys. J., 187, L57 (1974).Google Scholar
Large, M. I. and Vaughan, A. E., Mon. Not. R. Astron, Soc., 151, 277 (1971).Google Scholar
Manchester, R. N., Lyne, A. G., Taylor, J. H., Durdin, J. M., Large, M. I. and Little, A. G., Mon. Not. R. Astron. Soc., 185, 409 (1978).Google Scholar
Manchester, R. N. and Taylor, J. H., Astron. J., 86, 1953 (1981).Google Scholar
Meikle, W. P. S. and Colgate, S. A., Astrophys. J., 220, 1076 (1978).Google Scholar
Mills, B. Y., Proc. Astron. Soc. Aust., 4, 156 (1981).CrossRefGoogle Scholar
O’Sullivan, J. D., Ekers, R. D. and Shaver, P. A., Nature, 276, 590 (1978).Google Scholar