Science with the Murchison Widefield Array

By Judd D. Bowman, I. Cairns, D. Kaplan, T. Murphy, D. Oberoi, L. Staveley-Smith, W. Arcus, David G. Barnes, G. Bernardi, Frank H. Briggs and 51 more. Publications Astronomical Society of Australia, 2012

263 citations recorded by the source corpus.

Abstract Significant new opportunities for astrophysics and cosmology have been identified at low radio frequencies. The Murchison Widefield Array is the first telescope in the southern hemisphere designed specifically to explore the low-frequency astronomical sky between 80 and 300 MHz with arcminute angular resolution and high survey efficiency. The telescope will enable new advances along four key science themes, including searching for redshifted 21-cm emission from the EoR in the early Universe; Galactic and extragalactic all-sky southern hemisphere surveys; time-domain astrophysics; and solar, heliospheric, and ionospheric science and space weather. The Murchison Widefield Array is located in Western Australia at the site of the planned Square Kilometre Array (SKA) low-band telescope and is the only low-frequency SKA precursor facility. In this paper, we review the performance properties of the Murchison Widefield Array and describe its primary scientific objectives.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/472d4bfce590b3de012b11bb3cb7898aa1376663

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In Astronomy and Astrophysics

1. A. Mesinger
2. M. McQuinn
3. L. Hernquist
4. S. Furlanetto
5. C. Carilli
6. B. Greig
7. P. Hopkins
8. Volker Springel

In Nuclear and High Energy Physics

1. A. Mesinger
2. M. McQuinn
3. C. Carilli
4. S. Furlanetto
5. Judd D. Bowman
6. B. Greig
7. J. Aguirre
8. Miguel F. Morales

Citations in the corpus

• wsclean: an implementation of a fast, generic wide-field imager for radio astronomy (2014, methodology): “However, MWA’s EoR observations (Bowman et al. 2013) require more advanced deconvolution techniques.”
• GaLactic and Extragalactic All-sky Murchison Widefield Array (GLEAM) survey - I. A low-frequency extragalactic catalogue (2016, background): “More details of the science enabled by wide- band low-frequency observations, and specifically the MWA, can be found in Bowman et al. (2013).”
• Inferring the astrophysics of reionization and cosmic dawn from galaxy luminosity functions and the 21-cm signal (2018, unknown): “Ongoing interferometer experiments aiming to detect the power spectrum of the signal include the Murchison Wide Field Array (MWA4; Bowman et al. 2013; Tingay et al. 2013), Low Frequency Array (LOFAR5; van Haarlem et al. 2013), Precision Array for Probing Epoch of Reionisation (PAPER6; Parsons et…”
• Calibration requirements for detecting the 21 cm epoch of reionization power spectrum and implications for the SKA (2016, background): “…(PAPER; Parsons et al. 2010)1, the LOw Frequency ARray (LOFAR; Yatawatta et al. 2013; van Haarlem et al. 2013)2, the Murchison Widefield Array (MWA; Lonsdale et al. 2009; Tingay et al. 2013; Bowman et al. 2013)3, the Hydrogen Epoch of Reionization Array (HERA; Pober et al. 2014)4, and ?”
• Hydrogen Epoch of Reionization Array (HERA) (2016, background): “…the Donald C. Backer Precision Array for Probing the Epoch of Reionization (PAPER; Parsons et al. 2010), the Murchison Widefield Array (MWA; Bowman et al. 2013; Tingay et al. 2013), the MIT EoR experiment (MITEoR; Zheng et al. 2014) and the Experiment to Detect the Global EoR Step (EDGES;…”
• Upper Limits on the 21 cm Epoch of Reionization Power Spectrum from One Night with LOFAR (2017, methodology): “To date, a number of experiments have been seeking to measure this high-redshift 21-cm emission, using LOFAR (van Haarlem et al. 2013), the GMRT (Paciga et al. 2011), the MWA (Tingay et al. 2013; Bowman et al. 2013), PAPER (Parsons et al. 2010) and the 21CMA (Zheng et al. 2016).”
• LOFAR: The LOw-Frequency ARray (2013, background): “…(10−88 MHz) (see Kassim et al. 2010; Lazio et al. 2010; Taylor et al. 2012, and examples therein) and MWA (80−300 MHz) (see Rightley et al. 2009; Oberoi et al. 2011; Bowman et al. 2013; Tingay et al. 2013b, and examples therein), both of which provide powerful solar observing capabilities.”
• New Limits on 21cm EoR From PAPER-32 Consistent with an X-Ray Heated IGM at z=7.7 (2013, background): “Other such telescopes include the Giant Metre-wave Radio Telescope (GMRT; Paciga et al. 2013)12, the LOw Frequency ARray (LOFAR; Yatawatta et al. 2013)13, and the Murchison Widefield Array (MWA; Bowman et al. 2013; Tingay et al. 2013)14.”
• COSMIC REIONIZATION AND EARLY STAR-FORMING GALAXIES: A JOINT ANALYSIS OF NEW CONSTRAINTS FROM PLANCK AND THE HUBBLE SPACE TELESCOPE (2015, background): “Our results offer extra hope for efforts to make redshifted 21-cm measurements of neutral hydrogen in the IGM, as the experimental foregrounds are weakest at low redshifts (e.g., van Haarlem et al. 2013; Bowman et al. 2013; Pober et al. 2014).”
• WHAT NEXT-GENERATION 21 cm POWER SPECTRUM MEASUREMENTS CAN TEACH US ABOUT THE EPOCH OF REIONIZATION (2013, background): “…the LOw Frequency ARray (LOFAR; Yatawatta et al. 2013; van Haarlem et al. 2013)17, the Murchison Widefield Array (MWA; Tingay et al. 2013; Bowman et al. 2013)18, and the Donald C. Backer Precision Array for Probing the Epoch of Reionization (PAPER; Parsons 17 http://www.lofar.org/ 18…”