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arxiv: 1212.5151 · v2 · submitted 2012-12-20 · 🌌 astro-ph.IM · astro-ph.CO· astro-ph.GA· astro-ph.SR

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Science with the Murchison Widefield Array

Judd D. Bowman , Iver Cairns , David L. Kaplan , Tara Murphy , Divya Oberoi , Lister Staveley-Smith , Wayne Arcus , David G. Barnes
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Gianni Bernardi Frank H. Briggs Shea Brown John D. Bunton Adam J. Burgasser Roger J. Cappallo Shami Chatterjee Brian E. Corey Anthea Coster Avinash Deshpande Ludi deSouza David Emrich Philip Erickson Robert F. Goeke B. M. Gaensler Lincoln J. Greenhill Lisa Harvey-Smith Bryna J. Hazelton David Herne Jacqueline N. Hewitt Melanie Johnston-Hollitt Justin C. Kasper Barton B. Kincaid Ronald Koenig Eric Kratzenberg Colin J. Lonsdale Mervyn J. Lynch Lynn D. Matthews S. Russell McWhirter Daniel A. Mitchell Miguel F. Morales Edward H. Morgan Stephen M. Ord Joseph Pathikulangara Prabu Thiagaraj Ronald A. Remillard Timothy Robishaw Alan E. E. Rogers Anish A. Roshi Joseph E. Salah Robert J. Sault N. Udaya Shankar K. S. Srivani Jamie B. Stevens Ravi Subrahmanyan Steven J. Tingay Randall B. Wayth Mark Waterson Rachel L. Webster Alan R. Whitney Andrew J. Williams Christopher L. Williams J. Stuart B. Wyithe
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classification 🌌 astro-ph.IM astro-ph.COastro-ph.GAastro-ph.SR
keywords arraymurchisonwidefieldsciencetelescopeastrophysicshemispherelow-frequency
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Significant new opportunities for astrophysics and cosmology have been identified at low radio frequencies. The Murchison Widefield Array is the first telescope in the Southern Hemisphere designed specifically to explore the low-frequency astronomical sky between 80 and 300 MHz with arcminute angular resolution and high survey efficiency. The telescope will enable new advances along four key science themes, including searching for redshifted 21 cm emission from the epoch of reionisation in the early Universe; Galactic and extragalactic all-sky southern hemisphere surveys; time-domain astrophysics; and solar, heliospheric, and ionospheric science and space weather. The Murchison Widefield Array is located in Western Australia at the site of the planned Square Kilometre Array (SKA) low-band telescope and is the only low-frequency SKA precursor facility. In this paper, we review the performance properties of the Murchison Widefield Array and describe its primary scientific objectives.

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  1. Mitigating residual foregrounds and systematic errors in SKA1-Low AA* EoR observations via Bayesian Gaussian Process Regression

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    Bayesian GPR recovers the 21cm signal within 2σ credible intervals for most k-modes (0.06 to 1.0 h/Mpc) in SKA1-Low simulations that include realistic residual foregrounds and systematics.