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By observing bright and compact astronomical sources while also taking datawith the 183 GHz Water Vapour Radiometers, ALMA will be able to measure the`empirical' relationship between fluctuations in the phase of the astronomicalsignal and the fluctuations of sky brightness around 183 GHz. Simulations ofsuch measurements assuming only thermal noise in the astronomical and WVRreceivers are presented and it is shown that accurate determination of theempirical relationship should be possible in a relatively short time. It isthen proposed that the best way of using these empirical coefficients is toinclude them as a constraint on a physical model of the atmosphere -- thisallows them to be used for longer period of time, increasing the efficiency ofobserving. This approach fits naturally into the analysis framework presentedin the previous memo, which has now been extended to implement it. Thetechnique is illustrated via simulations and on a short data set collected atthe SMA.

Inference of Coefficients for Use in Phase Correction II: Using the Observed Correlation Between Phase and Sky Brightness Fluctuations