Murchison Widefield Array

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Murchison Widefield Array
MWA 32T Tile.jpg
An individual MWA-32T tile
ObservatoryMurchison Radio-astronomy Observatory Edit this on Wikidata
Location(s)Western Australia, Australia Edit this at Wikidata
Coordinates26°42′12″S 116°40′16″E / 26.7033°S 116.671°E / -26.7033; 116.671Coordinates: 26°42′12″S 116°40′16″E / 26.7033°S 116.671°E / -26.7033; 116.671 Edit this at Wikidata
Wavelength3.75, 1 m (80, 300 MHz)
Built2007 Edit this on Wikidata–2012 Edit this on Wikidata (2007 Edit this on Wikidata–2012 Edit this on Wikidata) Edit this at Wikidata
Telescope styleradio interferometer Edit this on Wikidata
Diameter3 km (9,842 ft 6 in) Edit this at Wikidata
Collecting area512 m2 (5,510 sq ft) Edit this at Wikidata
Websitewww.mwatelescope.org Edit this at Wikidata
Murchison Widefield Array is located in Australia
Murchison Widefield Array
Location of Murchison Widefield Array

The Murchison Widefield Array (MWA) is a joint project between an international consortia of organisations to construct and operate a low-frequency radio array. Operating in the frequency range 70–300 MHz, the main scientific goals of the MWA are to detect neutral atomic Hydrogen emission from the cosmological Epoch of Reionization (EoR), to study the sun, the heliosphere, the Earth's ionosphere, and radio transient phenomena, as well as map the extragalactic radio sky.

Development[edit]

The MWA was to be situated at Mileura Station where initial testing had been conducted[1] then moved southwest to Boolardy station in outback Western Australia, at the Murchison Radio-astronomy Observatory (MRO), 800 kilometres north of Perth. This location offers a quiet radio environment and stable climate for observations.[2] The MRO is also the site of CSIRO's Australian Square Kilometre Array Pathfinder[3] (ASKAP) and one of two selected sites 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.

The MWA was initially conceived as a 512-tile instrument (512T) [4] 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, including initial observations of EoR fields.[5]

The first phase of the telescope, the so-called 'Phase I MWA' achieved full practical completion in late 2012 [6] and completed commissioning on 20 June 2013, before moving into full operations. The Phase I MWA was the first so-called large-N array, fully cross-correlating signals from 128 phased tiles, each of which consist of 16 crossed 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.[7] The Phase I array was largely driven by the 2nd MWA Director, Professor Steven Tingay.

In 2017 the telescope received the planned substantial upgrade, doubling both the number of antennas and the resolution of the instrument; increasing the sensitivity by a factor of approximately 10. 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. Instillation of the additional antennas and commissioning of the array was led by the third MWA Director, Dr Randall Wayth.

Science[edit]

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 provide a wealth of scientific papers covering topics such as detection of HII regions 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:

1) The first detection of plasma tubes in the ionosphere by undergraduate student, Cleo Loi,[8].[8] Ms Loi won the Astronomical Society of Australia 2015 Bok Prize for her research.[9][8]

2) The "GaLactic and Extragalactic All-sky MWA" (or "GLEAM") is a survey of 300,000 extragalactic sources at 20 frequencies between 70 and 230 MHz that was carried out by the MWA.[10][11]


System overview[edit]

An MWA antenna consists of a four by four regular grid of dual-polarisation 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 beamformer to produce tile beams on the sky. Beamformers sit next to the tiles in the field. The radio frequency (RF) signals for 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 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 digitisation. The frequency range 80–300 MHz is Nyquist-sampled at high precision. Digital elements in the receiver (after the digitiser) 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 fibre connection to the correlator subsystem, located in the CSIRO Data Processing Facility near the MWA site. MWA shares the CSIRO facility with the ASKAP program.

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 core, yielding baseline distances of about 3 km to allow higher angular resolution observations.

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 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 which provide baselines distances of about 5 km.

The original correlator subsystem comprises Poly-phase Filter Bank (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.

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 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.

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 Perth at the Pawsey supercomputing cnetre. The resultant qualified data will then be provided to, and stored by, the various scientific databases for subsequent distribution to the respective scientific communities for analysis and interpretation.


Project partners[edit]

During Phase I, the MWA consortium initially comprised 110 individual researchers drawn from 12 institutions from Australia, NZ, the US, and India. New Zealand joined the consortium in late 2011 and an additional two institutions from the US were added in 2014 taking the total number of Phase I partner organisations to 14. By the end of Phase I there were 160 individual research scientists involved in the MWA.

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 organisations across 6 countries and had a membership of 270 individual scientists. The expansion of the collaboration was largely the work of the then MWA Board Chair (Jan 2014 - Jan 2018) and current MWA Director, Professor Melanie Johnston-Hollitt.

The MWA Project is composed of the following project partners as of 2018:

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 US National Science Foundation, the Australian Research Council (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 compute hardware was given through an IBM Shared University Research Grant awarded to Victoria University of Wellington and Curtin University (PIs: Johnston-Hollitt and Tingay).


See also[edit]

References[edit]

  1. ^ "Murchison Widefield Array". MIT Haystack Observatory. 2013. Retrieved 17 February 2013.
  2. ^ The MWA Site in Western Australia Archived 13 April 2012 at the Wayback Machine.. Murchison Widefield Array. Retrieved on 2 December 2012.
  3. ^ Square Kilometre Array. CSIRO. Retrieved on 2 December 2012.
  4. ^ (May 2011). The Murchison Widefield Array (MWA): Current Status and Plans. American Astronomical Society. Retrieved on 2 December 2012.
  5. ^ (May 2011). MWA Observations of Candidate EoR Fields. Bulletin of the American Astronomical Society, Vol. 43. American Astronomical Society. Retrieved on 2 December 2012.
  6. ^ We did it!. Adventures in Astronomy. Retrieved on 2 December 2012.
  7. ^ "Australia unveils telescope to warn of solar flares". The Raw Story. Raw Story Media. 1 December 2012. Retrieved 2 December 2012.
  8. ^ a b c How an undergraduate discovered tubes of plasma in the sky, Tara Murphy, The Conversation, 5 June 2015, accessed 7 June 2015
  9. ^ Sydney University physics undergraduate maps huge plasma tubes in the sky, Marcus Strom, Sydney Morning Herald, 1 June 2015, accessed 8 June 2015
  10. ^ "MWA – GLEAM Survey". MWA. Retrieved 30 November 2016.
  11. ^ "GLEAM". ICRAR. 24 October 2016.