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Beam Size, Shape and Efficiencies for the ATNF Mopra Radio Telescope at 86–115 GHz

Published online by Cambridge University Press:  05 March 2013

Ned Ladd ,
Cormac Purcell ,
Tony Wong  and
Stuart Robertson
Ned Ladd*
Affiliation:
Physics Department, Bucknell University, Lewisburg PA 17837, USA
Cormac Purcell*
Affiliation:
School of Physics, University of New South Wales, Sydney NSW 2052, Australia
Tony Wong
Affiliation:
School of Physics, University of New South Wales, Sydney NSW 2052, Australia CSIRO Australia Telescope National Facility, Epping NSW 1710, Australia
Stuart Robertson
Affiliation:
CSIRO Australia Telescope National Facility, Epping NSW 1710, Australia
*
DCorresponding authors. Email: ladd@bucknell.edu; crp@phys.unsw.edu.au
DCorresponding authors. Email: ladd@bucknell.edu; crp@phys.unsw.edu.au
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Abstract

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We present data characterising the performance of the Mopra Radio Telescope during the period 2000–2004, including measurements of the beam size and shape, as well as the overall beam efficiency of the telescope. In 2004 the full width half maximum of the beam was measured to be 36 ± 3″ at 86 GHz, falling to 33 ± 2″ at 115 GHz. Based on our observations of Jupiter we measured the beam efficiency of the Gaussian main beam to be 0.49 ± 0.03 at 86 GHz and 0.42 ± 0.02 at 115 GHz. Sources with angular sizes of ∼80″ couple well to the main beam, while sources with angular sizes between ∼80″ and ∼160″ couple to the both the main beam and inner error beam. Measurements indicate that the inner error beam contains approximately one-third the power of the main beam. We also compare efficiency corrected spectra to measurements made at similar facilities and present standard spectra taken towards the molecular clouds Orion-KL and M17-SW.

Keywords

instrumentsinterstellar: moleculesradio sources: lines
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 22 , Issue 1 , 2005 , pp. 62 - 72
Copyright
Copyright © Astronomical Society of Australia 2005

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