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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/3890
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dc.contributor.authorLonsdale, C.J.-
dc.contributor.authorDeshpande, A.A.-
dc.contributor.authorGopalakrishna, M.R.-
dc.contributor.authorKamini, P.A.-
dc.contributor.authorKumar, Deepak-
dc.contributor.authorMadhavi, S.-
dc.contributor.authorPrabu, T.-
dc.contributor.authorRoshi, Anish D.-
dc.contributor.authorUdaya Shankar, N.-
dc.contributor.authorSrivani, K.S.-
dc.contributor.author+33 Co-authors-
dc.date.accessioned2010-01-15T07:48:34Z-
dc.date.available2010-01-15T07:48:34Z-
dc.date.issued2009-08-
dc.identifier.citationProceedings of the IEEE, 2009, Vol.97, p1497-1506en
dc.identifier.issn0018-9219-
dc.identifier.urihttp://hdl.handle.net/2289/3890-
dc.descriptionOpen Access.en
dc.description.abstractThe Murchison Widefield Array is a dipole-based aperture array synthesis telescope designed to operate in the 80-300 MHz frequency range. It is capable of a wide range of science investigations but is initially focused on three key science projects: detection and characterization of three-dimensional brightness temperature fluctuations in the 21 cm line of neutral hydrogen during the epoch of reionization (EoR) at redshifts from six to ten; solar imaging and remote sensing of the inner heliosphere via propagation effects on signals from distant background sources; and high-sensitivity exploration of the variable radio sky. The array design features 8192 dual-polarization broadband active dipoles, arranged into 512 ldquotilesrdquo comprising 16 dipoles each. The tiles are quasi-randomly distributed over an aperture 1.5 km in diameter, with a small number of outliers extending to 3 km. All tile-tile baselines are correlated in custom field-programmable gate array based hardware, yielding a Nyquist-sampled instantaneous monochromatic uv coverage and unprecedented point spread function quality. The correlated data are calibrated in real time using novel position-dependent self-calibration algorithms. The array is located in the Murchison region of outback Western Australia. This region is characterized by extremely low population density and a superbly radio-quiet environment, allowing full exploitation of the instrumental capabilities.en
dc.language.isoenen
dc.publisherIEEEen
dc.relation.urihttp://adsabs.harvard.edu/abs/2009IEEEP..97.1497Len
dc.relation.urihttp://arxiv.org/abs/0903.1828en
dc.relation.urihttp://dx.doi.org/10.1109/JPROC.2009.2017564en
dc.rights© 2009 IEEE. This material is posted here with permission of the IEEE. Such permission of the IEEE does not in any way imply IEEE endorsement of any of Raman Research Institute's's products or services. Internal or personal use of this material is permitted. However, permission to reprint/republish this material for advertising or promotional purposes or for creating new collective works for resale or redistribution must be obtained from the IEEE by writing to pubs-permissions@ieee.org. By choosing to view this document, you agree to all provisions of the copyright laws protecting it.en
dc.subjectantenna arraysen
dc.subjectastronomyen
dc.subjectcalibrationen
dc.subjectimagingen
dc.subjectionosphereen
dc.titleThe Murchison widefield arrary: design overviewen
dc.typeArticleen
Appears in Collections:Research Papers (A&A)

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