Following the completion of each SHEVE experiment, a file containing the logged system temperatures, 
, from each antenna was produced in the format required by the Caltech calibration task CAL. The file also contained nominal values for the antenna gains, 
, and the correlator dependent constant, b. This a priori calibration information was then applied to the averaged and edited amplitudes output from the correlator for calibrator sources. The relationship between the correlated flux density, 
, on the i - j baseline, and the correlated amplitude, 
, is [Cohen et al. 1975]
The SHEVE calibrator sources are known to be unresolved on most of the Australian SHEVE baselines, with little extended structure on arcsecond scales.
The total flux densities of the calibrators were measured during the course of each SHEVE experiment and compared to the calibrated VLBI flux densities. For most experiments the a priori calibration put the VLBI flux density of the calibrator within 10% of its total flux density. For some experiments larger deviations were present on some baselines, usually due to departures from the nominal system characteristics. When this was the case, antenna based corrections were derived from the calibrator observations using amplitude closure relations and added to the calibration file as an improvement on the a priori calibration. The refined calibration file was then applied to the raw correlated amplitudes of the target sources to produce calibrated amplitudes. The overall flux density accuracy of the data presented in this thesis is approximately 10%.