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The Murchison Widefield Array (MWA), located in Western Australia, is one ofthe low-frequency precursors of the international Square Kilometre Array (SKA)project. In addition to pursuing its own ambitious science program, it is alsoa testbed for wide range of future SKA activities ranging from hardware,software to data analysis. The key science programs for the MWA and SKA requirevery high dynamic ranges, which challenges calibration and imaging systems.Correct calibration of the instrument and accurate measurements of source fluxdensities and polarisations require precise characterisation of the telescope'sprimary beam. Recent results from the MWA GaLactic Extragalactic All-sky MWA(GLEAM) survey show that the previously implemented Average Embedded Element(AEE) model still leaves residual polarisations errors of up to 10-20 % inStokes Q. We present a new simulation-based Full Embedded Element (FEE) modelwhich is the most rigorous realisation yet of the MWA's primary beam model. Itenables efficient calculation of the MWA beam response in arbitrary directionswithout necessity of spatial interpolation. In the new model, every dipole inthe MWA tile (4 x 4 bow-tie dipoles) is simulated separately, taking intoaccount all mutual coupling, ground screen and soil effects, and thereforeaccounts for the different properties of the individual dipoles within a tile.We have applied the FEE beam model to GLEAM observations at 200 - 231 MHz andused false Stokes parameter leakage as a metric to compare the models. We havedetermined that the FEE model reduced the magnitude and declination-dependentbehaviour of false polarisation in Stokes Q and V while retaining low levels offalse polarisation in Stokes U.

Calibration and Stokes Imaging with Full Embedded Element Primary Beam Model for the Murchison Widefield Array