Interferometric Imaging with the 32 Element Murchison Wide-Field Array
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Hewitt_Interferometric imaging.pdf
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Author(s)
Benkevitch, Leonid
Cappallo, Roger J.
Corey, Brian E.
Doeleman, Sheperd Samuel
Derome, Mark F.
Kincaid, Barton B.
Kratzenberg, Eric W.
Lonsdale, Colin John
McWhirter, Stephen R.
Oberoi, Divya
Date Issued
October 2010
Journal
Publications of the Astronomical Society of the Pacific
Publisher
University of Chicago Press, The
Citation
Ord, S. M. et al. “Interferometric Imaging with the 32 Element Murchison Wide-Field Array.” Publications of the Astronomical Society of the Pacific 122.897 (2010): 1353–1366.
Version
Author's final manuscript
Abstract
The Murchison Wide-Field Array (MWA) is a low-frequency radio telescope, currently under construction, intended to search for the spectral signature of the epoch of reionization (EOR) and to probe the structure of the solar corona. Sited in western Australia, the full MWA will comprise 8192 dipoles grouped into 512 tiles and will be capable of imaging the sky south of 40° declination, from 80 MHz to 300 MHz with an instantaneous field of view that is tens of degrees wide and a resolution of a few arcminutes. A 32 station prototype of the MWA has been recently commissioned and a set of observations has been taken that exercise the whole acquisition and processing pipeline. We present Stokes I, Q, and U images from two ~4 hr integrations of a field 20° wide centered on Pictoris A. These images demonstrate the capacity and stability of a real-time calibration and imaging technique employing the weighted addition of warped snapshots to counter extreme wide-field imaging distortions.
MIT Department
Haystack Observatory
MIT Kavli Institute for Astrophysics and Space Research
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Creative Commons Attribution-Noncommercial-Share Alike 3.0
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DOI of Published Version
https://doi.org/10.1086/657160
