The Murchison Widefield Array Prototype - Opening a new Window on the Low Frequency Radio Sun

Details The Murchison Widefield Array Prototype - Opening a new Window on the Low Frequency Radio Sun The Murchison Widefield Array Prototype - Opening a new Window on the Low Frequency Radio Sun

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh13b1964o&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH13B-1964

Astronomy and Astrophysics

Astrophysics

[6924] Radio Science / Interferometry, [6994] Radio Science / Instruments And Techniques, [7509] Solar Physics, Astrophysics, And Astronomy / Corona, [7534] Solar Physics, Astrophysics, And Astronomy / Radio Emissions

Scientific paper

The rich and unique diagnostic ability of low radio frequency (< 300 MHz) solar observations has long been appreciated but, owing to limitations of the existing instrumentation, have yet to be exploited to its full potential. In order to meet the demanding needs of solar science, a radio array must be capable of providing high fidelity, high dynamic range, snapshot images with high spectral resolution over a wide bandwidth. The steady march of technology has only now brought such capabilities within reach. The 32 element engineering prototype (32T) for the Murchison Widefield Array (MWA) is amongst the first of a new generation of radio arrays which can simultaneously achieve broad instantaneous spectral coverage, high spectral resolution, high temporal resolution and useful angular resolution with a high imaging fidelity. The MWA is being built at a remote and radio quiet Western Australian site with negligible terrestrial interference over its 80-300 MHz band and is expected to ultimately comprise 128 elements spread over a region 3 km in diameter. The MWA collaboration includes US, Australian and Indian institutions. The 32T solar images currently represent the state-of-the-art in high dynamic range solar imaging at low frequencies, offering an order of magnitude improvement over the earlier efforts. The unprecedented spectroscopic imaging capability, along with the imaging fidelity, of these data are already providing new insights into coronal dynamics (Oberoi et al., ApJ, 728, L27, 2011). Here we present some recent results to illustrate the powerful new capabilities that will be enabled by the MWA and other new generation radio interferometers over the next few years.

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