System design and validation of Central Redundant Array Mega-Tile (CRAM)
Exploration of the 21cm signal during the Cosmic Dawn and the Epoch of Reionisation (EoR) can unravel the mysteries of the early Universe when the first stars and galaxies were born and ionised, respectively. However, the 21 cm signal is exceptionally weak, and thus, the detection amidst the bright...
| Main Authors: | , , , |
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| Format: | Journal Article |
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2024
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| Online Access: | http://purl.org/au-research/grants/arc/CE170100013 http://hdl.handle.net/20.500.11937/96509 |
| _version_ | 1848766161998577664 |
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| author | Selvaraj, Aishwarya Wayth, Randall B. Trott, Cathryn M. Bhatia, G.S. |
| author_facet | Selvaraj, Aishwarya Wayth, Randall B. Trott, Cathryn M. Bhatia, G.S. |
| author_sort | Selvaraj, Aishwarya |
| building | Curtin Institutional Repository |
| collection | Online Access |
| description | Exploration of the 21cm signal during the Cosmic Dawn and the Epoch of Reionisation (EoR) can unravel the mysteries of the early Universe when the first stars and galaxies were born and ionised, respectively. However, the 21 cm signal is exceptionally weak, and thus, the detection amidst the bright foregrounds is extremely challenging. The Murchison Widefield Array (MWA) aims to measure the brightness temperature fluctuations of neutral hydrogen from the early Universe. The MWA telescope observes the radio sky with a large field of view (FoV) that causes the bright galaxies, especially near the horizon, to contaminate the measurements. These foregrounds contaminating the EoR datasets must be meticulously removed or treated to detect the signal successfully. The Central Redundant Array Mega-Tile (CRAM) is a zenith-pointing new instrument, installed at the centre of the MWA Phase II southern hexagonal configuration, comprising of 64 dipoles in an configuration with a FoV half the width of the MWA's at every frequency under consideration. The primary objective of this new instrument is to mitigate the impact of bright radio sources near the field centre in accordance with the reduced primary beamshape and to reduce the contamination of foreground sources near the horizon with the reduced sidelobe response of the larger array configuration. In this paper, we introduce the new instrument to the community and present the system architecture and characteristics of the instrument. Using the first light observations, we determine the CRAM system temperature and system performance. |
| first_indexed | 2025-11-14T11:46:45Z |
| format | Journal Article |
| id | curtin-20.500.11937-96509 |
| institution | Curtin University Malaysia |
| institution_category | Local University |
| last_indexed | 2025-11-14T11:46:45Z |
| publishDate | 2024 |
| recordtype | eprints |
| repository_type | Digital Repository |
| spelling | curtin-20.500.11937-965092025-01-15T05:52:17Z System design and validation of Central Redundant Array Mega-Tile (CRAM) Selvaraj, Aishwarya Wayth, Randall B. Trott, Cathryn M. Bhatia, G.S. Exploration of the 21cm signal during the Cosmic Dawn and the Epoch of Reionisation (EoR) can unravel the mysteries of the early Universe when the first stars and galaxies were born and ionised, respectively. However, the 21 cm signal is exceptionally weak, and thus, the detection amidst the bright foregrounds is extremely challenging. The Murchison Widefield Array (MWA) aims to measure the brightness temperature fluctuations of neutral hydrogen from the early Universe. The MWA telescope observes the radio sky with a large field of view (FoV) that causes the bright galaxies, especially near the horizon, to contaminate the measurements. These foregrounds contaminating the EoR datasets must be meticulously removed or treated to detect the signal successfully. The Central Redundant Array Mega-Tile (CRAM) is a zenith-pointing new instrument, installed at the centre of the MWA Phase II southern hexagonal configuration, comprising of 64 dipoles in an configuration with a FoV half the width of the MWA's at every frequency under consideration. The primary objective of this new instrument is to mitigate the impact of bright radio sources near the field centre in accordance with the reduced primary beamshape and to reduce the contamination of foreground sources near the horizon with the reduced sidelobe response of the larger array configuration. In this paper, we introduce the new instrument to the community and present the system architecture and characteristics of the instrument. Using the first light observations, we determine the CRAM system temperature and system performance. 2024 Journal Article http://hdl.handle.net/20.500.11937/96509 10.1017/pasa.2024.33 http://purl.org/au-research/grants/arc/CE170100013 http://purl.org/au-research/grants/arc/FT180100321 http://creativecommons.org/licenses/by/4.0/), fulltext |
| spellingShingle | Selvaraj, Aishwarya Wayth, Randall B. Trott, Cathryn M. Bhatia, G.S. System design and validation of Central Redundant Array Mega-Tile (CRAM) |
| title | System design and validation of Central Redundant Array Mega-Tile (CRAM) |
| title_full | System design and validation of Central Redundant Array Mega-Tile (CRAM) |
| title_fullStr | System design and validation of Central Redundant Array Mega-Tile (CRAM) |
| title_full_unstemmed | System design and validation of Central Redundant Array Mega-Tile (CRAM) |
| title_short | System design and validation of Central Redundant Array Mega-Tile (CRAM) |
| title_sort | system design and validation of central redundant array mega-tile (cram) |
| url | http://purl.org/au-research/grants/arc/CE170100013 http://purl.org/au-research/grants/arc/CE170100013 http://hdl.handle.net/20.500.11937/96509 |