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arxiv: 1101.0620 · v1 · pith:47I4VI5Jnew · submitted 2011-01-03 · 🌌 astro-ph.SR

First Spectroscopic Imaging Observations of the Sun at Low Radio Frequencies with the Murchison Widefield Array Prototype

Divya Oberoi , Lynn D. Matthews , Iver H. Cairns , David Emrich , Vasili Lobzin , Colin J. Lonsdale , Edward H. Morgan , T. Prabu
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Harish Vedantham Randall B. Wayth Andrew Williams Christopher Williams Stephen M. White G. Allen Wayne Arcus David Barnes Leonid Benkevitch Gianni Bernardi Judd D. Bowman Frank H. Briggs John D. Bunton Steve Burns Roger C. Cappallo M. A. Clark Brian E. Corey M. Dawson David DeBoer A. De Gans Ludi deSouza Mark Derome R. G. Edgar T. Elton Robert Goeke M. R. Gopalakrishna Lincoln J. Greenhill Bryna Hazelton David Herne Jacqueline N. Hewitt P. A. Kamini David L. Kaplan Justin C. Kasper Rachel Kennedy Barton B. Kincaid Jonathan Kocz R. Koeing Errol Kowald Mervyn J. Lynch S. Madhavi Stephen R. McWhirter Daniel A. Mitchell Miguel F. Morales A. Ng Stephen M. Ord Joseph Pathikulangara Alan E. E. Rogers Anish Roshi Joseph E. Salah Robert J. Sault Antony Schinckel N. Udaya Shankar K. S. Srivani Jamie Stevens Ravi Subrahmanyan D. Thakkar Steven J. Tingay J. Tuthill Annino Vaccarella Mark Waterson Rachel L. Webster Alan R. Whitney
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classification 🌌 astro-ph.SR
keywords radiofrequencyemissionobservationsarrayfeaturesfirstimaging
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We present the first spectroscopic images of solar radio transients from the prototype for the Murchison Widefield Array (MWA), observed on 2010 March 27. Our observations span the instantaneous frequency band 170.9-201.6 MHz. Though our observing period is characterized as a period of `low' to `medium' activity, one broadband emission feature and numerous short-lived, narrowband, non-thermal emission features are evident. Our data represent a significant advance in low radio frequency solar imaging, enabling us to follow the spatial, spectral, and temporal evolution of events simultaneously and in unprecedented detail. The rich variety of features seen here reaffirms the coronal diagnostic capability of low radio frequency emission and provides an early glimpse of the nature of radio observations that will become available as the next generation of low frequency radio interferometers come on-line over the next few years.

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  1. The Murchison Widefield Array Phase III upgrade: Sensitivity Doubled, Number of Baselines Quadrupled, Flexibility Enhanced, and EoR Observations Optimised

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    MWA Phase III upgrade adds receivers and uses MWAX correlator to support full 256-tile correlation, doubling sensitivity and quadrupling baselines.