The murchison widefield array: Solar science with the low frequency SKA precursor

SJ Tingay; D Oberoi; I Cairns; A Donea; R Duffin; W Arcus; G Bernardi; JD Bowman; F Briggs; JD Bunton; RJ Cappallo; BE Corey; A Deshpande; L Desouza; D Emrich; BM Gaensler; R Goeke; LJ Greenhill; BJ Hazelton; D Herne; JN Hewitt; M Johnston-Hollitt; DL Kaplan; JC Kasper; JA Kennewell; BB Kincaid; R Koenig; E Kratzenberg; CJ Lonsdale; MJ Lynch; SR McWhirter; DA Mitchell; MF Morales; E Morgan; SM Ord; J Pathikulangara; T Prabu; RA Remillard; AEE Rogers; A Roshi; JE Salah; RJ Sault; N Udaya-Shankar; KS Srivani; J Stevens; R Subrahmanyan; M Waterson; RB Wayth; RL Webster; AR Whitney; A Williams; CL Williams; JSB Wyithe

Journal article

The murchison widefield array: Solar science with the low frequency SKA precursor

SJ Tingay, D Oberoi, I Cairns, A Donea, R Duffin, W Arcus, G Bernardi, JD Bowman, F Briggs, JD Bunton, RJ Cappallo, BE Corey, A Deshpande, L Desouza, D Emrich, BM Gaensler, R Goeke, LJ Greenhill, BJ Hazelton, D Herne Show all

Journal of Physics Conference Series | IOP PUBLISHING LTD | Published : 2013

DOI: 10.1088/1742-6596/440/1/012033

Open access

Abstract

The Murchison Widefield Array is a low frequency (80-300 MHz) SKA Precursor, comprising 128 aperture array elements (known as tiles) distributed over an area of 3 km diameter. The MWA is located at the extraordinarily radio quiet Murchison Radioastronomy Observatory in the mid-west of Western Australia, the selected home for the Phase 1 and Phase 2 SKA low frequency arrays. The MWA science goals include: 1) detection of fluctuations in the brightness temperature of the diffuse redshifted 21 cm line of neutral hydrogen from the epoch of reionisation; 2) studies of Galactic and extragalactic processes based on deep, confusion-limited surveys of the full sky visible to the array; 3) time domain..

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