at the four frequencies, respectively.

Data are first checked for obvious interference or telescope problems, flagged if necessary and then are processed using [miriad]{}[^3] scripts to ensure consistency. Visibility data are calibrated in both phase and amplitude and images formed using baselines longer than 3 k$\lambda$. These images are cleaned and sources above a threshold identified. A table of source positions and integrated and peak flux densities is output for each frequency. At least at the two higher frequencies, SNR 1987A is resolved and so integrated flux densities are quoted. An unresolved source, J0536-6919, is present on all images with an observed flux density ranging between 80 mJy at 1.4 GHz and 6 mJy at 8.6 GHz and serves as a check on the system calibration. Its J2000 position determined from the 4.8 GHz observations since day 4000 is R.A. $05^{\rm h}\;36^{\rm m}\;04\fs789 \pm 0\fs005$, Dec. $-69^{\circ}\;18'\;44\farcs81 \pm 0\farcs02$. At 8.6 GHz it lies at about 1.5 primary beam radii from the pointing centre, so it’s flux density measurements at this frequency are not very reliable. Measured flux densities for SNR 1987A are given in Appendix 1.

Figure \[fg:fluxes\] shows the measured flux densities of SNR 1987A at the four 