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A frequent analysis case in astronomy is that of rotating, flattened, structures. A typical example is that of proto-planetary disks around young stars, and the second category is galactic disks.
In such circumstances, once the relation between rotation velocity and radius is known, it is possible to recover radial profiles with better accuracy, by stacking spectra from a given radius after correction from their projected velocities.
This is the purpose of the KEPLER command. By default, it assumes a Keplerian velocity profile, but the use can specify any arbitrary (parametric) rotation curve. See HELP KEPLER for details.