the peak pixel of the map in the instrument units. The flux density of the calibrator in one beam, S$_{beam}$, was calculated by assuming a gaussian beam.

Over the various observing runs, we used Mars, Uranus, and Neptune as calibrators. As described above, we also used several secondary calibrators to check the pointing when none of the planets were available. While they are adequate for checking the pointing, we did not use them as calibrators both because their flux densities are not as well known as for the planets and because they are not as bright as the planets and thus produce larger measurement uncertainties. Table \[caltable\] presents C$_{beam}$, C$_{20}$, C$_{40}$ for each observation of one of the three planets listed above. Table \[caltable2\] lists the average and standard deviation of the FCFs for each run. It is clear from these tables that the FCFs are consistent both within and between each run. We were unable to observe any of these three planets in March 2005, but since the FCFs are seen to be consistent between the various observing runs, we used the average FCFs over all of the runs (listed in Table \[caltable2\]) to calibrate data taken during this 