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- Always make an image first. This is mandatory if you have no idea of
the structure of your source but this is also useful since the image will
directly show you the calibration problems, which are in general much
more difficult to detect directly in the visibilities.
- Use any knowledge you can have on your source. For instance, fitting
a disk function is probably the most appropriate for barely resolved
planets and satellites.
- If your source is barely resolved and you have no a priori
knowledge of the source structure, you should start with the simplest
possible model (e.g. POINT) and complexify the model only
gradually (e.g. C_GAUSS, E_GAUSS, etc...). Verify how
the uncertainties on the fitted parameters evolves to decide which model
is most appropriate.
- Always be critical with the results. In particular, image and
deconvolve the residual table. You should obtain just noise if the