2022:
505:(PFB) boards that convert the 1.28 MHz coarse frequency channels into channels with 10 kHz frequency resolution in preparation for cross-correlation. Correlator boards then cross-multiply signals from all tiles to form visibility data. A distributed clock signal drives the coherence of receivers in the field and maintains timing for the correlator. This system is only capable of ingesting the data from 128 tiles and thus, while the array currently comprises 256 tiles, only half of the tiles are correlated at a time, giving rise to the two configurations discussed above. The MWA Collaboration plan to replace this correlator in the near future with a newer machine, capable of ingesting the data from all 256 tiles.
509:
database describing the observation scheduling of the
Instrument. M&C software commands several elements of the system including pointing and tracking of the beamformers, frequency selection of the receivers, correlation parameters for the correlator, and RTC/RTS functions, amongst others. The M&C system contributes to the MWA archive by storing instrument "metadata" into an external database. This includes both the instrument configurations for each observation and also housekeeping information collected from various hardware components.
195:
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520:. As of December 2018 the resultant initially calibrated data are then provided to the international astronomical community via the MWA node of the Australian All-Sky Virtual Observatory (ASVO). Significant processed data products produced by the MWA Collaboration such as the initial release of the GLEAM survey are also available via various international scientific databases for subsequent analysis and interpretation.
2082:
215:
29:
1972:
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685:(ARC), the Australian National Collaborative Research Infrastructure Strategy (NCRIS) administered by Astronomy Australia Ltd., and the Australia-India Strategic Research Fund Overview (AISRF). In addition, support for the MWA computer hardware was given through an IBM Shared University Research Grant awarded to Victoria University of Wellington and Curtin University (PIs: Johnston-Hollitt and Tingey).
345:'s Australian Square Kilometre Array Pathfinder (ASKAP) and one of two selected sites in Australia for the Square Kilometre Array (SKA). In addition to the geographic link, the MWA is one of four official SKA precursor telescopes – instruments that provide instrumental, scientific and operational information to help guide SKA developments, along with two sites in South Africa, HERA and MeerKAT.
2070:
2094:
486:-sampled at high precision. Digital elements in the receiver (after the digitizer) are used to transform the time-series data to the frequency domain with a 1.28 MHz resolution – 5 bits real and 5 bits imaginary for each resolution element. Sets of 1.28 MHz coarse frequency channels are transmitted via an optical fiber connection to the correlator subsystem, located in the
2046:
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new hexagonal super tiles in the compact configuration make use of the concept of "redundant spacings" to help calibrate the array to high precision for detection of the EoR. The extended configuration consists of nine Phase I receivers and 72 original tiles, plus an additional 56 new long baseline tiles that provide baselines distances of about 5 km.
353:
dipoles arranged in a 4x4 square. As part of a planned future roll out infrastructure on-site at the MRO was installed during Phase I to allow an eventual build-out to 256 tiles. The total cost of the first phase of the project was A$ 51 million. The Phase I array was largely driven by the second MWA director,
482:
eight tiles; cables between receivers and beamformers carry data, power and control signals. Power for the receivers is provided from a central generator. The receiver contains analogue elements to condition the signals in preparation for sampling and digitization. The frequency range 80–300 MHz is
528:
During Phase I, the MWA consortium initially comprised 110 individual researchers drawn from 12 institutions from
Australia, New Zealand, the United States and India. New Zealand joined the consortium in late 2011 and an additional two institutions from the United States were added in 2014 taking the
497:
In Phase II the MWA operated in two configurations, a compact configuration and an extended configuration of 128 tiles each. The compact configuration consists of seven Phase I receivers and 56 tiles, plus 72 new tiles arranged in two dense hexagonal configurations each of 36 close-packed tiles. The
493:
In Phase I the majority of the tiles (112) were scattered across a roughly 1.5 km core region, forming an array with very high imaging quality, and a field of view of several hundred square degrees at a resolution of several arcminutes. The remaining 16 tiles are placed at locations outside the
532:
Membership of the MWA consortium was substantially expanded for Phase II with the admission of Canada, China and Japan, though India left the consortium at this time. Nevertheless, at the start of Phase II the MWA had expanded to 21 partner organizations across six countries and had a membership of
481:
to produce tile beams on the sky. Beamformers sit next to the tiles in the field. The radio frequency (RF) signals from the tile-beams are transmitted to a receiver, each receiver being able to process the signals from a group of eight tiles. Receivers therefore sit in the field, close to groups of
348:
The MWA was initially conceived as a 512-tile instrument (512T) to be built in stages. The first stage was a 32-tile prototype (MWA-32T), which was constructed and operated with increasing capability over the period 2007–2011, testing telescope hardware and making preliminary science observations,
352:
The first phase of the telescope, the so-called "Phase I MWA" achieved full practical completion in late 2012 and completed commissioning on 20 June 2013, before moving into full operations. The Phase I MWA fully cross-correlates signals from 128 phased tiles, each of which consist of 16 crossed
360:
In 2017 the telescope received the planned upgrade, doubling both the number of antennas, resulting in an increase in resolution and sensitivity. This upgraded instrument is known as the "Phase II MWA". Phase II was practically completed in
October 2017 and officially launched on 23 April 2018.
508:
The MWA is operated remotely through an interface to a
Monitor and Control (M&C) software package resident on a dedicated computer located within the CSIRO Data Processing Facility at the MWA site. The M&C software maintains a state-based description of the hardware and an event-driven
476:
consists of a four by four regular grid of dual-polarization dipole elements arranged on a 4m x 4m steel mesh ground plane. Each antenna (with its 16 dipoles) is known as a "tile". Signals from each dipole pass through a low noise amplifier (LNA) and are combined in an analogue
373:
The MWA is an inherently versatile instrument with a very large field of view, on the order of 30 degrees across, able to cover a wide range of scientific goals. In Phase I the array provided a wealth of scientific papers covering topics such as detection of
378:(s) in the Galactic plane, limits on radio emission from extra-solar planets, observations of haloes and relics in galaxy clusters to detection of transient radio sources and space debris tracking. Two of the most significant results from the Phase I MWA were:
676:
Funding for the MWA to date has been provided by partner institutions and by allocations from national funding agencies: the New
Zealand Ministry of Economic Development (now the Ministry of Business, Innovation and Employment), the United States
341:, at the Murchison Radio-astronomy Observatory (MRO), 800 kilometres (500 mi) north of Perth. This location offers a quiet radio environment and stable climate for observations. The MRO is also the site of
361:
Installation of the additional antennas and commissioning of the array was led by the third MWA director, Randall Wayth and operation of the Phase II instruments have been led by the current director,
270:. 'Widefield' refers to its very large field of view (on the order of 30 degrees across). Operating in the frequency range 70–300 MHz, the main scientific goals of the MWA are to detect
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270 individual scientists. The expansion of the collaboration was largely the work of the then MWA Board Chair (January 2014 – January 2018) and current MWA director,
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Data are transferred from the site to the MWA archive located at the end of a high-bandwidth network connection. The primary MWA data archive is located in
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total number of Phase I partner organizations to 14. By the end of Phase I there were 160 individual research scientists involved in the MWA.
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is a long periodicity (1,091.170 second / 18m11s) object, that provided a bright pulse of energy for up to a minute, and is some 4,000
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464:. The object was discovered by Tyrone O'Doherty as part of his undergraduate honours project supervised by Dr Hurley-Walker.
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812:. Bulletin of the American Astronomical Society, Vol. 43. American Astronomical Society. Retrieved on 2 December 2012.
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core, yielding baseline distances of about 3 km to allow higher angular resolution observations.
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Data
Processing Facility near the MWA site. MWA shares the CSIRO facility with the ASKAP program.
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at right ascension 16h 27m 59.5s, declination −52°35′04.3". The object produces pulses at 154
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448:. Scaling this to 1.4 GHz would indicate S1.4 GHz = 3.5 Jy and, therefore, a
401:
sources at 20 frequencies between 70 and 230 MHz that was carried out by the MWA.
1925:
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2014:
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The "Galactic and
Extragalactic All-sky MWA" (or "GLEAM") is a survey of 300,000
330:
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The first detection of plasma tubes in the ionosphere by undergraduate student,
2110:
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317:, the MWA is one of four precursors to the international project known as the
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The MWA Project is composed of the following project partners as of 2018:
1935:
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Sydney
University physics undergraduate maps huge plasma tubes in the sky
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Special
Astrophysical Observatory of the Russian Academy of Science
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294:, as well as map the extragalactic radio sky. It is located at the
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where initial testing had been conducted then moved southwest to
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799:. American Astronomical Society. Retrieved on 2 December 2012.
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The
Murchison Widefield Array (MWA): Current Status and Plans
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342:
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How an undergraduate discovered tubes of plasma in the sky
749:. Murchison Widefield Array. Retrieved on 2 December 2012.
453:
279:
1311:
Combined Array for Research in Millimeter-wave Astronomy
824:. Adventures in Astronomy. Retrieved on 2 December 2012.
933:
A radio transient with unusually slow periodic emission
1986:
835:"Australia unveils telescope to warn of solar flares"
436:
galaxy. The derived position is in the constellation
1415:Multi-Element Radio Linked Interferometer Network
926:
858:
856:
214:
2118:
2132:Astronomical observatories in Western Australia
1301:Canadian Hydrogen Intensity Mapping Experiment
853:
349:including initial observations of EoR fields.
985:
444:of peak flux densities of up to S154MHz = 45
418:re-analyzed 2018 GLEAM data and announced in
1291:Australian Square Kilometre Array Pathfinder
501:The original correlator subsystem comprises
303:Australian Square Kilometre Array Pathfinder
1085:500 meter Aperture Spherical Telescope
115:3.75, 1 m (80, 300 MHz)
992:
978:
943:https://doi.org/10.1038/s41586-021-04272-x
590:National Astronomical Observatory of Japan
193:
172:
159:
145:
131:
101:
47:
27:
456:^−1. It is speculated to be similar to a
1405:Molonglo Observatory Synthesis Telescope
1242:Warkworth Radio Astronomical Observatory
810:MWA Observations of Candidate EoR Fields
2119:
890:
761:. CSIRO. Retrieved on 2 December 2012.
1906:Cosmic microwave background radiation
1643:Pushchino Radio Astronomy Observatory
1365:Large Latin American Millimeter Array
973:
912:
296:Murchison Radio-astronomy Observatory
223:Location of Murchison Widefield Array
158:3 km (9,842 ft 6 in)
43:Murchison Radio-astronomy Observatory
1971:
1619:National Radio Astronomy Observatory
1513:Westerbork Synthesis Radio Telescope
543:
311:Hydrogen Epoch of Reionization Array
16:Radio telescope in Western Australia
1611:Mullard Radio Astronomy Observatory
999:
887:, 1 June 2015, accessed 8 June 2015
871:, 5 June 2015, accessed 7 June 2015
523:
171:512 m (5,510 sq ft)
13:
1445:Northern Extended Millimeter Array
841:. Raw Story Media. 1 December 2012
827:
695:List of astronomical observatories
610:University of California, Berkeley
600:Swinburne University of Technology
467:
410:In January 2022, a team led by Dr
305:(ASKAP), also at the MRO, and two
14:
2163:
1281:Australia Telescope Compact Array
1103:Caltech Submillimeter Observatory
1046:Very Long Baseline Interferometry
951:
740:The MWA Site in Western Australia
658:Victoria University of Wellington
653:University of Wisconsin–Milwaukee
595:Shanghai Astronomical Observatory
388:Astronomical Society of Australia
2104:
2092:
2080:
2068:
2056:
2044:
2032:
2020:
2008:
1996:
1970:
1961:
1960:
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721:. MIT Haystack Observatory. 2013
272:neutral atomic Hydrogen emission
234:
213:
206:
1335:Giant Metrewave Radio Telescope
1203:UTR-2 decameter radio telescope
874:
648:University of Western Australia
1435:Northern Cross Radio Telescope
1271:Atacama Large Millimeter Array
941:, 601, pages 526–530 (2022),
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802:
789:
764:
752:
733:
711:
556:Australian National University
405:
329:The MWA was to be situated at
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1:
705:
1885:Gravitational-wave astronomy
1463:Primeval Structure Telescope
772:"Precursors and Pathfinders"
518:Pawsey Supercomputing Centre
7:
1797:Christiaan Alexander Muller
1663:Vermilion River Observatory
1571:Algonquin Radio Observatory
1036:Astronomical interferometer
719:"Murchison Widefield Array"
688:
683:Australian Research Council
679:National Science Foundation
10:
2168:
2152:Interferometric telescopes
1137:Large Millimeter Telescope
935:, N. Hurley-Walker et al,
426:GLEAM-X J162759.5−523504.3
368:
143:radio interferometer
33:An individual MWA-32T tile
1956:
1893:
1855:
1709:
1674:
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1425:Murchison Widefield Array
1345:Green Bank Interferometer
1253:
1169:RATAN-600 Radio Telescope
1075:
1060:
1052:Astronomical radio source
1007:
964:Murchison Widefield Array
922:. ICRAR. 24 October 2016.
885:The Sydney Morning Herald
663:Western Sydney University
260:Murchison Widefield Array
245:
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22:Murchison Widefield Array
1635:Onsala Space Observatory
1627:Nançay Radio Observatory
1603:Jodrell Bank Observatory
1503:Very Long Baseline Array
1179:Sardinia Radio Telescope
643:University of Washington
535:Melanie Johnston-Hollitt
363:Melanie Johnston-Hollitt
240:Related media on Commons
1865:Submillimetre astronomy
1477:Australia, South Africa
1329:Event Horizon Telescope
619:University of Melbourne
452:L1.4 GHz = 4×10^31
2142:Square Kilometre Array
1587:Green Bank Observatory
1473:Square Kilometre Array
776:Square Kilometre Array
759:Square Kilometre Array
503:Poly-phase Filter Bank
319:Square Kilometre Array
274:from the cosmological
1880:High-energy astronomy
1767:Sebastian von Hoerner
1375:Long Wavelength Array
1321:European VLBI Network
1261:Allen Telescope Array
1161:Qitai Radio Telescope
745:13 April 2012 at the
633:University of Toronto
412:Natasha Hurley-Walker
309:in South Africa, the
276:Epoch of Reionization
1948:Solar radio emission
1737:Jocelyn Bell Burnell
1595:Haystack Observatory
1129:Green Bank Telescope
1113:Effelsberg Telescope
966:at Wikimedia Commons
898:"MWA – GLEAM Survey"
624:University of Sydney
571:Kagoshima University
278:(EoR), to study the
168:Collecting area
140:Telescope style
1921:Pulsar timing array
1727:Edward George Bowen
1717:Elizabeth Alexander
1579:Arecibo Observatory
1483:Submillimeter Array
1385:Low-Frequency Array
1355:Korean VLBI Network
1221:Southern Hemisphere
1132:(West Virginia, US)
638:University of Tokyo
614:Breakthrough Listen
576:Kumamoto University
552:(Lead Organization)
292:transient phenomena
89:26.7033°S 116.671°E
85: /
23:
2147:Shire of Murchison
2137:Harvard University
1901:Aperture synthesis
1870:Infrared astronomy
1807:Joseph Lade Pawsey
1777:Kenneth Kellermann
1747:Nan Dieter-Conklin
1455:One-Mile Telescope
1234:Parkes Observatory
432:from Earth in the
21:
2003:Western Australia
1984:
1983:
1926:Radio propagation
1875:Optical astronomy
1772:Karl Guthe Jansky
1582:(Puerto Rico, US)
1557:
1556:
1349:West Virginia, US
1098:(Puerto Rico, US)
1095:Arecibo Telescope
962:Media related to
673:
672:
605:Tohoku University
581:Nagoya University
550:Curtin University
416:Curtin University
394:for her research.
386:. Ms Loi won the
339:Western Australia
256:
255:
94:-26.7033; 116.671
61:Western Australia
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952:External links
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399:extragalactic
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355:Steven Tingay
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188:.mwatelescope
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19:
2087:Solar System
1856:Astronomy by
1817:Arno Penzias
1757:Cyril Hazard
1424:
1399:South Africa
1190:(Uzbekistan)
1030:Radio window
936:
928:
914:
902:. Retrieved
892:
876:
866:
843:. Retrieved
838:
829:
817:
808:(May 2011).
804:
795:(May 2011).
791:
779:. Retrieved
775:
766:
754:
735:
723:. Retrieved
713:
675:
667:
539:
531:
527:
511:
507:
500:
496:
492:
471:
424:that object
419:
409:
372:
359:
351:
347:
328:
300:
290:, and radio
263:
259:
257:
18:
2075:Outer space
2063:Spaceflight
1936:Wow! signal
1827:Martin Ryle
1822:Grote Reber
1752:Frank Drake
1693:(Australia)
1527:Space-based
1517:Netherlands
1389:Netherlands
1359:South Korea
1237:(Australia)
1187:Suffa RT-70
904:30 November
781:22 November
725:17 February
430:light-years
406:Discoveries
376:H II region
337:in outback
325:Development
313:(HERA) and
284:heliosphere
268:radio array
92: /
80:116°40′16″E
68:Coordinates
57:Location(s)
2121:Categories
1858:EM methods
1078:telescopes
1076:Individual
945:2022-01-27
845:2 December
822:We did it!
706:References
479:beamformer
450:luminosity
288:ionosphere
111:Wavelength
77:26°42′12″S
2039:Astronomy
2015:Australia
1842:Paul Wild
1675:Multi-use
1655:(SAORAS,
1429:Australia
1417:(MERLIN,
1409:Australia
1295:Australia
1285:Australia
1214:(Ukraine)
1206:(Ukraine)
1116:(Germany)
434:Milky Way
392:Bok Prize
127:2007–2012
123:2007–2012
1966:Category
1802:Jan Oort
1701:(Canada)
1685:(Canada)
1638:(Sweden)
1630:(France)
1574:(Canada)
1544:Spektr-R
1387:(LOFAR,
1367:(LLAMA,
1324:(Europe)
1313:(CARMA,
1303:(CHIME,
1293:(ASKAP,
1140:(Mexico)
1124:(Russia)
1008:Concepts
743:Archived
689:See also
462:magnetar
384:Cleo Loi
155:Diameter
2111:Science
2099:Schools
2027:Physics
1989:Portals
1976:Commons
1515:(WSRT,
1505:(VLBA,
1465:(PaST,
1407:(MOST,
1395:MeerKAT
1337:(GMRT,
1283:(ATCA,
1273:(ALMA,
1226:HartRAO
1198:(Japan)
1182:(Italy)
1164:(China)
1156:(India)
1087:(FAST,
1040:History
1014:Units (
920:"GLEAM"
516:at the
484:Nyquist
474:antenna
472:An MWA
369:Science
321:(SKA).
315:MeerKAT
298:(MRO).
181:Website
125: (
39:Part of
1710:People
1657:Russia
1647:Russia
1548:Russia
1495:(VLA,
1485:(SMA,
1475:(SKA,
1449:France
1427:(MWA,
1377:(LWA,
1357:(KVN,
1347:(GBI,
1305:Canada
1263:(ATA,
1173:Russia
1105:(CSO,
1048:(VLBI)
1020:jansky
938:Nature
681:, the
668:
458:pulsar
421:Nature
282:, the
233:
45:
2051:Stars
1538:Japan
1534:HALCA
1467:China
1439:Italy
1339:India
1331:(EHT)
1275:Chile
1089:China
900:. MWA
700:LOFAR
566:CSIRO
514:Perth
488:CSIRO
438:Norma
390:2015
343:CSIRO
247:[
120:Built
63:, AUS
1931:SETI
1698:PARL
1682:DRAO
1666:(US)
1622:(US)
1614:(UK)
1606:(UK)
1598:(US)
1590:(US)
1458:(UK)
1245:(NZ)
1148:(UK)
1067:List
1018:and
1016:watt
906:2016
847:2012
783:2020
727:2013
454:ergs
258:The
190:.org
460:or
442:MHz
414:of
280:Sun
264:MWA
186:www
2123::
1507:US
1487:US
1419:UK
1107:US
855:^
837:.
774:.
537:.
446:Jy
365:.
357:.
1991::
1659:)
1649:)
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1546:(
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1371:)
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1171:(
1109:)
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1028:(
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993:e
986:t
979:v
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612:/
262:(
251:]
129:)
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