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dc.contributor.authorWayth, R. B.
dc.contributor.authorLenc, E.
dc.contributor.authorBell, M. E.
dc.contributor.authorCallingham, J. R.
dc.contributor.authorDwarakanath, K. S.
dc.contributor.authorFranzen, T. M. O.
dc.contributor.authorFor, B. -Q.
dc.contributor.authorGaensler, B.
dc.contributor.authorHancock, P.
dc.contributor.authorHindson, L.
dc.contributor.authorHurley-Walker, N.
dc.contributor.authorJackson, C. A.
dc.contributor.authorJohnston-Hollitt, M.
dc.contributor.authorKapinska, A. D.
dc.contributor.authorMcKinley, B.
dc.contributor.authorMorgan, J.
dc.contributor.authorOffringa, A. R.
dc.contributor.authorProcopio, P.
dc.contributor.authorStaveley-Smith, L.
dc.contributor.authorWu, C.
dc.contributor.authorZheng, Q.
dc.contributor.authorTrott, C. M.
dc.contributor.authorBernardi, G.
dc.contributor.authorBowman, J. D.
dc.contributor.authorBriggs, F.
dc.contributor.authorCappallo, R. J.
dc.contributor.authorCorey, B. E.
dc.contributor.authorDeshpande, A. A.
dc.contributor.authorEmrich, D.
dc.contributor.authorGoeke, R.
dc.contributor.authorGreenhill, L. J.
dc.contributor.authorHazelton, B. J.
dc.contributor.authorKaplan, D. L.
dc.contributor.authorKasper, J. C.
dc.contributor.authorKratzenberg, E.
dc.contributor.authorLonsdale, C. J.
dc.contributor.authorLynch, M. J.
dc.contributor.authorMcWhirter, S. R.
dc.contributor.authorMitchell, D. A.
dc.contributor.authorMorales, M. F.
dc.contributor.authorMorgan, E.
dc.contributor.authorOberoi, D.
dc.contributor.authorOrd, S. M.
dc.contributor.authorPrabu, T.
dc.contributor.authorRogers, A. E. E.
dc.contributor.authorRoshi, A.
dc.contributor.authorShankar, N. Udaya
dc.contributor.authorSrivani, K. S.
dc.contributor.authorSubrahmanyan, R.
dc.contributor.authorTingay, S. J.
dc.contributor.authorWaterson, M.
dc.contributor.authorWebster, R. L.
dc.contributor.authorWhitney, A. R.
dc.contributor.authorWilliams, A.
dc.contributor.authorWilliams, C. L.
dc.date.accessioned2017-07-13T17:00:28Z
dc.date.available2017-07-13T17:00:28Z
dc.date.issued2015-06-22
dc.identifier.citationWayth , R B , Lenc , E , Bell , M E , Callingham , J R , Dwarakanath , K S , Franzen , T M O , For , B -Q , Gaensler , B , Hancock , P , Hindson , L , Hurley-Walker , N , Jackson , C A , Johnston-Hollitt , M , Kapinska , A D , McKinley , B , Morgan , J , Offringa , A R , Procopio , P , Staveley-Smith , L , Wu , C , Zheng , Q , Trott , C M , Bernardi , G , Bowman , J D , Briggs , F , Cappallo , R J , Corey , B E , Deshpande , A A , Emrich , D , Goeke , R , Greenhill , L J , Hazelton , B J , Kaplan , D L , Kasper , J C , Kratzenberg , E , Lonsdale , C J , Lynch , M J , McWhirter , S R , Mitchell , D A , Morales , M F , Morgan , E , Oberoi , D , Ord , S M , Prabu , T , Rogers , A E E , Roshi , A , Shankar , N U , Srivani , K S , Subrahmanyan , R , Tingay , S J , Waterson , M , Webster , R L , Whitney , A R , Williams , A & Williams , C L 2015 , ' GLEAM : The GaLactic and Extragalactic All-sky MWA survey ' , Publications of the Astronomical Society of Australia , vol. 32 , E025 . https://doi.org/10.1017/pasa.2015.26
dc.identifier.issn1323-3580
dc.identifier.otherPURE: 10291290
dc.identifier.otherPURE UUID: 358197fe-69ae-4fe7-aa24-b1da373660e5
dc.identifier.otherArXiv: http://arxiv.org/abs/1505.06041v1
dc.identifier.otherScopus: 84945189570
dc.identifier.urihttp://hdl.handle.net/2299/18919
dc.description© 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: http://creativecommons.org/licenses/by/4.0/
dc.description.abstractGLEAM, 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.en
dc.format.extent12
dc.language.isoeng
dc.relation.ispartofPublications of the Astronomical Society of Australia
dc.rightsOpen
dc.subjectastro-ph.IM
dc.subjectastro-ph.CO
dc.subjectastro-ph.GA
dc.titleGLEAM : The GaLactic and Extragalactic All-sky MWA surveyen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
dc.description.versiontypeFinal Published version
dcterms.dateAccepted2015-06-22
rioxxterms.versionVoR
rioxxterms.versionofrecordhttps://doi.org/10.1017/pasa.2015.26
rioxxterms.licenseref.urihttp://creativecommons.org/licenses/by/4.0/
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


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