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: http://www.eso.org/~chummel/oyster/manual/node250.html
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A collection of procedures capable of imaging interferometric data. These were written to develop an algorithm for combining multi-channel data by accounting for the wavelength dependence of the image if composed of black-body radiators (or stellar atmospheres). A corresponding multi-channel CLEAN was implemented together with a self-calibration routine, following a difference mapping scheme. In the latter, a model (list of CLEAN components) is built-up incrementally between phase self-calibrations. The CLEAN algorithm is controlled with a slider widget to adjust the number of components to be added to the model, updating the residual image for each component added or subtracted.
PEARL will work with the complex visibilities, which have to be initialized with the observed visibility and closure phase data using the set_complexvis procedure. For testing purposes, if PEARL is called directly after computing model visibilities with calcmodel, the complex visibilities used by PEARL correspond exactly to the model.
The PEARL widget has two HELP buttons for further information on how to use it. The final PEARL image consists of a white light image and two maps, one of the effective temperature and the other one of the surface gravity. Together, these fully constrain images of stellar surfaces and multiple stellar systems.