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Theme: User Experience for astronomical software
The CLEAN algorithm, first published by Högbom (1974) and its later variants such as Multiscale CLEAN (msCLEAN) by Cornwell (2008), has been the most popular tool for deconvolution in interferometric imaging used by aperture synthesis radio telescopes. CLEAN effectively removes the telescopes point spread function from the observed images. We have compared source fluxes produced by different implementations of msCLEAN (WSCLEAN, CASA) with a prototype implementation of msCLEAN for the SKA on two datasets. The first is a simulation of multiple point sources of known intensity, where none of the software packages detected all the simulated point sources to within 1.0% of the simulated values. The second is of supernova remnant 3C 391 taken by the Very Large Array (VLA), where none of the software packages produced images which agreed to within 1.0% of each other.