University of Hertfordshire

GLEAM: The GaLactic and Extragalactic All-sky MWA survey

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  • R. B. Wayth
  • E. Lenc
  • M. E. Bell
  • J. R. Callingham
  • K. S. Dwarakanath
  • T. M. O. Franzen
  • B. -Q. For
  • B. Gaensler
  • P. Hancock
  • L. Hindson
  • N. Hurley-Walker
  • C. A. Jackson
  • M. Johnston-Hollitt
  • A. D. Kapinska
  • B. McKinley
  • J. Morgan
  • A. R. Offringa
  • P. Procopio
  • L. Staveley-Smith
  • C. Wu
  • And 35 others
  • Q. Zheng
  • C. M. Trott
  • G. Bernardi
  • J. D. Bowman
  • F. Briggs
  • R. J. Cappallo
  • B. E. Corey
  • A. A. Deshpande
  • D. Emrich
  • R. Goeke
  • L. J. Greenhill
  • B. J. Hazelton
  • D. L. Kaplan
  • J. C. Kasper
  • E. Kratzenberg
  • C. J. Lonsdale
  • M. J. Lynch
  • S. R. McWhirter
  • D. A. Mitchell
  • M. F. Morales
  • E. Morgan
  • D. Oberoi
  • S. M. Ord
  • T. Prabu
  • A. E. E. Rogers
  • A. Roshi
  • N. Udaya Shankar
  • K. S. Srivani
  • R. Subrahmanyan
  • S. J. Tingay
  • M. Waterson
  • R. L. Webster
  • A. R. Whitney
  • A. Williams
  • C. L. Williams
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Original languageEnglish
Article numberE025
Number of pages12
JournalPublications of the Astronomical Society of Australia
Publication statusPublished - 22 Jun 2015


GLEAM, the GaLactic and Extragalactic All-sky MWA survey, is a survey of the entire radio sky south of declination +25 deg at frequencies between 72 and 231 MHz, made with the Murchison Widefield Array (MWA) using a drift scan method that makes efficient use of the MWA's very large field-of-view. We present the observation details, imaging strategies and theoretical sensitivity for GLEAM. The survey ran for two years, the first year using 40 kHz frequency resolution and 0.5 s time resolution; the second year using 10 kHz frequency resolution and 2 s time resolution. The resulting image resolution and sensitivity depends on observing frequency, sky pointing and image weighting scheme. At 154 MHz the image resolution is approximately 2.5 x 2.2/cos(DEC+26.7) arcmin with sensitivity to structures up to ~10 deg in angular size. We provide tables to calculate the expected thermal noise for GLEAM mosaics depending on pointing and frequency and discuss limitations to achieving theoretical noise in Stokes I images. We discuss challenges, and their solutions, that arise for GLEAM including ionospheric effects on source positions and linearly polarised emission, and the instrumental polarisation effects inherent to the MWA's primary beam.


© Astronomical Society of Australia 2015; published by Cambridge University Press. This is an Open Access article distributed in accordance with the terms of the Creative Commons Attribution (CC BY 4.0) license, which permits others to distribute, remix, adapt and build upon this work, for commercial use, provided the original work is properly cited. See:


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