Bulletin of the Astronomical Society of India
J. L. Riding1,2*, D. A. Mitchell1,2 and R. L. Webster1,2
1School of Physics, The University of Melbourne, Parkville, VIC 3010, Australia
2ARC Centre of Excellence for All-sky Astrophysics (CAASTRO)
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The Murchison Widefield Array (MWA), like most low frequency arrays, has a large field of view which requires multisource calibration to account for direction dependent eects (DDEs). Often these fields contain sidelobes from extended sources which obscure weaker sources. This can limit the number of calibrators that can be reliably used to solve for array parameters and DDEs. Sources such as Fornax A are so bright they can critically limit the number of usable calibrators. One solution is to subtract out these sources before or during calibration using a model, in this case a shapelet model.
Keywords : techniques - image processing, interferometric