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

    258730.pdf (1.543Mb)
    Access Status
    Open access
    Authors
    Sokolowski, M.
    Colegate, T.
    Sutinjo, A.
    Ung, D.
    Wayth, R.
    Hurley-Walker, N.
    Lenc, E.
    Pindor, B.
    Morgan, J.
    Kaplan, D.
    Bell, M.
    Callingham, J.
    Dwarakanath, K.
    For, B.
    Gaensler, B.
    Hancock, Paul
    Hindson, L.
    Johnston-Hollitt, M.
    Kapinska, A.
    McKinley, B.
    Offringa, A.
    Procopio, P.
    Staveley-Smith, L.
    Wu, C.
    Zheng, Q.
    Date
    2017
    Type
    Journal Article
    
    Metadata
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    Citation
    Sokolowski, M. and Colegate, T. and Sutinjo, A. and Ung, D. and Wayth, R. and Hurley-Walker, N. and Lenc, E. et al. 2017. Calibration and Stokes Imaging with Full Embedded Element Primary Beam Model for the Murchison Widefield Array. Publications of the Astronomical Society of Australia. 34: Article ID e062.
    Source Title
    Publications of the Astronomical Society of Australia
    DOI
    10.1017/pasa.2017.54
    ISSN
    1323-3580
    School
    Curtin Institute of Radio Astronomy (Physics)
    Remarks

    © Astronomical Society of Australia 2017; published by Cambridge University Press

    URI
    http://hdl.handle.net/20.500.11937/60169
    Collection
    • Curtin Research Publications
    Abstract

    The Murchison Widefield Array (MWA), located in Western Australia, is one of the low-frequency precursors of the international Square Kilometre Array (SKA) project. In addition to pursuing its own ambitious science program, it is also a testbed for wide range of future SKA activities ranging from hardware, software to data analysis. The key science programs for the MWA and SKA require very high dynamic ranges, which challenges calibration and imaging systems. Correct calibration of the instrument and accurate measurements of source flux densities and polarisations require precise characterisation of the telescope's primary 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 % in Stokes Q. We present a new simulation-based Full Embedded Element (FEE) model which is the most rigorous realisation yet of the MWA's primary beam model. It enables efficient calculation of the MWA beam response in arbitrary directions without necessity of spatial interpolation. In the new model, every dipole in the MWA tile (4 x 4 bow-tie dipoles) is simulated separately, taking into account all mutual coupling, ground screen and soil effects, and therefore accounts 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 and used false Stokes parameter leakage as a metric to compare the models. We have determined that the FEE model reduced the magnitude and declination-dependent behaviour of false polarisation in Stokes Q and V while retaining low levels of false polarisation in Stokes U.

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