View Item 

Interferometric Imaging with the 32 Element Murchison Wide-Field Array

Access Status
Open access
Authors
Ord, S.
Mitchell, D.
Wayth, Randall
Greenhill, L.
Bernadi, G.
Gleadow, A.
Edgar, R.G.
Clarke, M.A.
Allen, G.
Arcus, Wayne
Benkevitch, L.
Bowman, J.D.
Briggs, F.H.
Bunton, J.D.
Burns, S.
Cappallo, R.J.
Coles, W.A.
Corey, B.E.
DeSouza, L.
Doeleman, S.S.
Derome, M.
Deshpande, A.
Emrich, D.
Goeke, M.R.
Gopalakrishna, M.R.
Herne, David
Hewitt, J.N.
Kamini, P.A.
Kaplan, D.L.
Kasper, J.C.
Kincaid, B.B.
Kocz, J.
Kowald, E.
Kratzenberg, E.
Kumar, D.
Lonsdale, C.
Lynch, Mervyn
McWhirter, S.
Madhavi, S.
Matejek, M.
Morales, M.
Morgan, E.
Oberoi, D.
Pathikulangara, J.
Prabu, T.
Rogers, A.
Roshi, A.
Salah, J.
Schinkel, A.
Udaya, S.N.
Srivani, K.
Stevens, J.
Tingay, Steven
Vaccarella, A.
Waterson, Mark
Date
2010
Type
Journal Article

Metadata
Show full item record
Citation
Ord, 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.
Source Title
Publications of the Astronomical Society of the Pacific
DOI
ISSN
School
Curtin Institute of Radio Astronomy
Remarks

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

URI
Collection
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.