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dc.contributor.authorOrd, S.
dc.contributor.authorMitchell, D.
dc.contributor.authorWayth, Randall
dc.contributor.authorGreenhill, L.
dc.contributor.authorBernadi, G.
dc.contributor.authorGleadow, A.
dc.contributor.authorEdgar, R.G.
dc.contributor.authorClarke, M.A.
dc.contributor.authorAllen, G.
dc.contributor.authorArcus, Wayne
dc.contributor.authorBenkevitch, L.
dc.contributor.authorBowman, J.D.
dc.contributor.authorBriggs, F.H.
dc.contributor.authorBunton, J.D.
dc.contributor.authorBurns, S.
dc.contributor.authorCappallo, R.J.
dc.contributor.authorColes, W.A.
dc.contributor.authorCorey, B.E.
dc.contributor.authorDeSouza, L.
dc.contributor.authorDoeleman, S.S.
dc.contributor.authorDerome, M.
dc.contributor.authorDeshpande, A.
dc.contributor.authorEmrich, D.
dc.contributor.authorGoeke, M.R.
dc.contributor.authorGopalakrishna, M.R.
dc.contributor.authorHerne, David
dc.contributor.authorHewitt, J.N.
dc.contributor.authorKamini, P.A.
dc.contributor.authorKaplan, D.L.
dc.contributor.authorKasper, J.C.
dc.contributor.authorKincaid, B.B.
dc.contributor.authorKocz, J.
dc.contributor.authorKowald, E.
dc.contributor.authorKratzenberg, E.
dc.contributor.authorKumar, D.
dc.contributor.authorLonsdale, C.
dc.contributor.authorLynch, Mervyn
dc.contributor.authorMcWhirter, S.
dc.contributor.authorMadhavi, S.
dc.contributor.authorMatejek, M.
dc.contributor.authorMorales, M.
dc.contributor.authorMorgan, E.
dc.contributor.authorOberoi, D.
dc.contributor.authorPathikulangara, J.
dc.contributor.authorPrabu, T.
dc.contributor.authorRogers, A.
dc.contributor.authorRoshi, A.
dc.contributor.authorSalah, J.
dc.contributor.authorSchinkel, A.
dc.contributor.authorUdaya, S.N.
dc.contributor.authorSrivani, K.
dc.contributor.authorStevens, J.
dc.contributor.authorTingay, Steven
dc.contributor.authorVaccarella, A.
dc.contributor.authorWaterson, Mark
dc.identifier.citationOrd, S.M. and Mitchell, D.A. and Wayth, R. and Greenhill, L.J. and Bernardi, G. and Gleadow, S. and Edgar, R.G. et al. 2010. Interferometric Imaging with the 32 Element Murchison Wide-Field Array. Astronomical Society of the Pacific. 122 (897): pp. 1353-1366.

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.

dc.publisherUniversity of Chicago Press
dc.titleInterferometric Imaging with the 32 Element Murchison Wide-Field Array
dc.typeJournal Article
dcterms.source.titlePublications of the Astronomical Society of the Pacific

Copyright © 2010. University of Chicago Press. All rights reserved.

curtin.departmentCurtin Institute of Radio Astronomy
curtin.accessStatusOpen access

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