Realisation of a low frequency SKA Precursor: The Murchison Widefield Array
The Murchison Widefield Array is a low frequency (80 - 300 MHz) SKA Precursor, comprising 128 aperture array elements distributed over an area of 3 km diameter. The MWA is located at the extraordinarily radio quiet Murchison Radioastronomy Observatory in the mid-west of Western Australia, the select...
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| Format: | Conference Paper |
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Proceedings of Science
2012
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| Online Access: | http://pos.sissa.it/archive/conferences/163/036/RTS2012_036.pdf http://hdl.handle.net/20.500.11937/4255 |
| _version_ | 1848744464168779776 |
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| author | Tingay, Steven Emrich, David Ord, Stephen Crosse, Brian Arcus, Wayne Colegate, Timothy Hall, Peter Herne, David Lynch, Mervyn Schlagenhaufer, Franz Tremblay, Steven Wayth, Randall Waterson, Mark Williams, Andrew |
| author2 | - |
| author_facet | - Tingay, Steven Emrich, David Ord, Stephen Crosse, Brian Arcus, Wayne Colegate, Timothy Hall, Peter Herne, David Lynch, Mervyn Schlagenhaufer, Franz Tremblay, Steven Wayth, Randall Waterson, Mark Williams, Andrew |
| author_sort | Tingay, Steven |
| building | Curtin Institutional Repository |
| collection | Online Access |
| description | The Murchison Widefield Array is a low frequency (80 - 300 MHz) SKA Precursor, comprising 128 aperture array elements distributed over an area of 3 km diameter. The MWA is located at the extraordinarily radio quiet Murchison Radioastronomy Observatory in the mid-west of Western Australia, the selected home for the Phase 1 and Phase 2 SKA low frequency arrays. The MWA science goals include: 1) detection of fluctuations in the brightness temperature of the diffuse redshifted 21 cm line of neutral hydrogen from the epoch of reionisation; 2) studies of Galactic and extragalactic processes based on deep, confusion-limited surveys of the full sky visible to the array; 3) time domain astrophysics through exploration of the variable radio sky; and 4) solar imaging and characterisation of the heliosphere and ionosphere via propagation effects on background radio source emission. This paper will focus on a brief discussion of the as-built MWA system, highlighting several novel characteristics of the instrument, and a brief progress report (as of June 2012) on the final construction phase. Practical completion of the MWA is expected in November 2012, with commissioning commencing from approximately August 2012 and operations commencing near mid 2013. A brief description of recent science results from the MWA prototype instrument is given. |
| first_indexed | 2025-11-14T06:01:53Z |
| format | Conference Paper |
| id | curtin-20.500.11937-4255 |
| institution | Curtin University Malaysia |
| institution_category | Local University |
| last_indexed | 2025-11-14T06:01:53Z |
| publishDate | 2012 |
| publisher | Proceedings of Science |
| recordtype | eprints |
| repository_type | Digital Repository |
| spelling | curtin-20.500.11937-42552017-01-30T10:37:49Z Realisation of a low frequency SKA Precursor: The Murchison Widefield Array Tingay, Steven Emrich, David Ord, Stephen Crosse, Brian Arcus, Wayne Colegate, Timothy Hall, Peter Herne, David Lynch, Mervyn Schlagenhaufer, Franz Tremblay, Steven Wayth, Randall Waterson, Mark Williams, Andrew - glalactic SKA low-frequency solar MRO EOR MWA The Murchison Widefield Array is a low frequency (80 - 300 MHz) SKA Precursor, comprising 128 aperture array elements distributed over an area of 3 km diameter. The MWA is located at the extraordinarily radio quiet Murchison Radioastronomy Observatory in the mid-west of Western Australia, the selected home for the Phase 1 and Phase 2 SKA low frequency arrays. The MWA science goals include: 1) detection of fluctuations in the brightness temperature of the diffuse redshifted 21 cm line of neutral hydrogen from the epoch of reionisation; 2) studies of Galactic and extragalactic processes based on deep, confusion-limited surveys of the full sky visible to the array; 3) time domain astrophysics through exploration of the variable radio sky; and 4) solar imaging and characterisation of the heliosphere and ionosphere via propagation effects on background radio source emission. This paper will focus on a brief discussion of the as-built MWA system, highlighting several novel characteristics of the instrument, and a brief progress report (as of June 2012) on the final construction phase. Practical completion of the MWA is expected in November 2012, with commissioning commencing from approximately August 2012 and operations commencing near mid 2013. A brief description of recent science results from the MWA prototype instrument is given. 2012 Conference Paper http://hdl.handle.net/20.500.11937/4255 http://pos.sissa.it/archive/conferences/163/036/RTS2012_036.pdf Proceedings of Science fulltext |
| spellingShingle | glalactic SKA low-frequency solar MRO EOR MWA Tingay, Steven Emrich, David Ord, Stephen Crosse, Brian Arcus, Wayne Colegate, Timothy Hall, Peter Herne, David Lynch, Mervyn Schlagenhaufer, Franz Tremblay, Steven Wayth, Randall Waterson, Mark Williams, Andrew Realisation of a low frequency SKA Precursor: The Murchison Widefield Array |
| title | Realisation of a low frequency SKA Precursor: The Murchison Widefield Array |
| title_full | Realisation of a low frequency SKA Precursor: The Murchison Widefield Array |
| title_fullStr | Realisation of a low frequency SKA Precursor: The Murchison Widefield Array |
| title_full_unstemmed | Realisation of a low frequency SKA Precursor: The Murchison Widefield Array |
| title_short | Realisation of a low frequency SKA Precursor: The Murchison Widefield Array |
| title_sort | realisation of a low frequency ska precursor: the murchison widefield array |
| topic | glalactic SKA low-frequency solar MRO EOR MWA |
| url | http://pos.sissa.it/archive/conferences/163/036/RTS2012_036.pdf http://hdl.handle.net/20.500.11937/4255 |