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19 March 2024 |
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GLEAM: The GaLactic and Extragalactic All-sky MWA survey | 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
; 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
; | Date: |
22 May 2015 | Abstract: | 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. | Source: | arXiv, 1505.6041 | Services: | Forum | Review | PDF | Favorites |
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