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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/5759
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dc.contributor.authorBernard, G.-
dc.contributor.authorUdaya Shankar, N.-
dc.contributor.authorSubrahmanyan, Ravi-
dc.contributor.authorDeshpande, A.A.-
dc.contributor.authorPrabu, T.-
dc.contributor.authorRoshi, Anish D.-
dc.contributor.authorSrivani, K.S.-
dc.date.accessioned2013-08-29T10:10:00Z-
dc.date.available2013-08-29T10:10:00Z-
dc.date.issued2013-07-
dc.identifier.citationThe Astrophysical journal, 2013, Vol.771, p105en
dc.identifier.issn0004-637X-
dc.identifier.issn1538-4357-(Online)-
dc.identifier.urihttp://hdl.handle.net/2289/5759-
dc.descriptionRestricted Access. An open-access version is available at arXiv.org (one of the alternative locations)en
dc.description.abstractWe present a Stokes I, Q and U survey at 189 MHz with the Murchison Widefield Array 32 element prototype covering 2400 deg2. The survey has a 15.6 arcmin angular resolution and achieves a noise level of 15 mJy beam-1. We demonstrate a novel interferometric data analysis that involves calibration of drift scan data, integration through the co-addition of warped snapshot images, and deconvolution of the point-spread function through forward modeling. We present a point source catalog down to a flux limit of 4 Jy. We detect polarization from only one of the sources, PMN J0351-2744, at a level of 1.8% ± 0.4%, whereas the remaining sources have a polarization fraction below 2%. Compared to a reported average value of 7% at 1.4 GHz, the polarization fraction of compact sources significantly decreases at low frequencies. We find a wealth of diffuse polarized emission across a large area of the survey with a maximum peak of ~13 K, primarily with positive rotation measure values smaller than +10 rad m-2. The small values observed indicate that the emission is likely to have a local origin (closer than a few hundred parsecs). There is a large sky area at α >= 2h30m where the diffuse polarized emission rms is fainter than 1 K. Within this area of low Galactic polarization we characterize the foreground properties in a cold sky patch at (α, δ) = (4h, -27.°6) in terms of three-dimensional power spectra.en
dc.language.isoenen
dc.publisherIOP Sciences for The American Astronomical Societyen
dc.relation.urihttp://adsabs.harvard.edu/abs/2013ApJ...771..105Ben
dc.relation.urihttp://arxiv.org/abs/1305.6047en
dc.relation.urihttp://dx.doi.org/10.1088/0004-637X/771/2/105en
dc.rights2013 American Astronomical Societyen
dc.subjectdiffuse radiation ISMen
dc.subjectMagnetic fieldsen
dc.subjectpolarization radio continuumen
dc.subjectsurveys techniquesen
dc.subjectinterferometicen
dc.titleA 189 MHz, 2400 deg2 polarization survey with the Murchison wide field array 32-element prototypeen
dc.typeArticleen
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