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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/6290
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dc.contributor.authorWayth, R.B.-
dc.contributor.authorLenc, E.-
dc.contributor.authorDeshpande, A.A.-
dc.contributor.authorPrabu, T.-
dc.contributor.authorUdaya Shankar, N.-
dc.contributor.authorSrivani, K.S.-
dc.contributor.authorSubrahmanyan, Ravi-
dc.contributor.authorDwarakanath, K.S.-
dc.contributor.author+30 Co-authors-
dc.date.accessioned2015-09-09T08:26:43Z-
dc.date.available2015-09-09T08:26:43Z-
dc.date.issued2015-06-22-
dc.identifier.citationPublications of the Astronomical Society of Australia,2015,Vol.32, e025en
dc.identifier.issn1323-3580-
dc.identifier.issn1448-6083(online)-
dc.identifier.urihttp://hdl.handle.net/2289/6290-
dc.descriptionRestricted Access. An open-access version is available at arXiv.org (one of the alternative locations)en
dc.description.abstractGLEAM, the GaLactic and Extragalactic All-sky MWA survey, is a survey of the entire radio sky south of declination + 25° at frequencies between 72 and 231 MHz, made with the 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 × 2.2/cos (δ + 26.7°) arcmin with sensitivity to structures up to ~ 10° 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.language.isoenen
dc.publisherCambridge University Press for Astronomical Society of Australiaen
dc.relation.urihttp://adsabs.harvard.edu/abs/2015PASA...32...25Wen
dc.relation.urihttp://arxiv.org/abs/1505.06041en
dc.relation.urihttp://dx.doi.org/10.1017/pasa.2015.26en
dc.rights2015 Astronomical Society of Australiaen
dc.titleGLEAM: The galactic and extragalactic all-sky MWA surveyen
dc.typeArticleen
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