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We present the results of a programme of scanning and mapping observations ofastronomical masers and Jupiter designed to characterise the performance of theMopra Radio Telescope at frequencies between 16-50 GHz using the 12-mm and 7-mmreceivers. We use these observations to determine the telescope beam size, beamshape and overall telescope beam efficiency as a function of frequency. We findthat the beam size is well fit by $\lambda$/$D$ over the frequency range with acorrelation coefficient of ~90%. We determine the telescope main beamefficiencies are between ~48-64% for the 12-mm receiver and reasonably flat at~50% for the 7-mm receiver. Beam maps of strong H$_2$O (22 GHz) and SiO masers(43 GHz) provide a means to examine the radial beam pattern of the telescope.At both frequencies the radial beam pattern reveals the presence of threecomponents, a central `core', which is well fit by a Gaussian and constitutesthe telescopes main beam, and inner and outer error beams. At both frequenciesthe inner and outer error beams extend out to approximately 2 and 3.4 times thefull-width half maximum of the main beam respectively. Sources with angularsizes a factor of two or more larger than the telescope main beam will coupleto the main and error beams, and therefore the power contributed by the errorbeams needs to be considered. From measurements of the radial beam powerpattern we estimate the amount of power contained in the inner and outer errorbeams is of order one-fifth at 22 GHz rising slightly to one-third at 43 GHz.

Characterisation of the Mopra Radio Telescope at 16--50 GHz