Science with ASKAP

By Simon Johnston, R. Taylor, M. Bailes, N. Bartel, C. Baugh, M. Bietenholz, Chris Blake, Robert Braun, Jo-Anne C. Brown, S. Chatterjee and 40 more. 2008

323 citations recorded by the source corpus.

AbstractThe future of cm and m-wave astronomy lies with the Square Kilometre Array (SKA), a telescope under development by a consortium of 17 countries. The SKA will be 50 times more sensitive than any existing radio facility. A majority of the key science for the SKA will be addressed through large-area imaging of the Universe at frequencies from 300 MHz to a few GHz. The Australian SKA Pathfinder (ASKAP) is aimed squarely in this frequency range, and achieves instantaneous wide-area imaging through the development and deployment of phase-array feed systems on parabolic reflectors. This large field-of-view makes ASKAP an unprecedented synoptic telescope poised to achieve substantial advances in SKA key science. The central core of ASKAP will be located at the Murchison Radio Observatory in inland Western Australia, one of the most radio-quiet locations on the Earth and one of the sites selected by the international community as a potential location for the SKA. Following an introductory description of ASKAP, this document contains 7 chapters describing specific science programmes for ASKAP. In summary, the goals of these programmes are as follows: The detection of a million galaxies in atomic hydrogen emission across 75% of the sky out to a redshift of 0.2 to understand galaxy formation and gas evolution in the nearby Universe.The detection of synchrotron radiation from 60 million galaxies to determine the evolution, formation and population of galaxies across cosmic time and enabling key cosmological tests.The detection of polarized radiation from over 500,000 galaxies, allowing a grid of rotation measures at 10′ to explore the evolution of magnetic fields in galaxies over cosmic time.The understanding of the evolution of the interstellar medium of our own Galaxy and the processes that drive its chemical and physical evolution.The high-resolution imaging of intense, energetic phenomena by enlarging the Australian and global Very Long Baseline networks.The discovery and timing of a thousand new radio pulsars.The characterization of the radio transient sky through detection and monitoring of transient sources such as gamma ray bursts, radio supernovae and intra-day variables.The combination of location, technological innovation and scientific program will ensure that ASKAP will be a world-leading radio astronomy facility, closely aligned with the scientific and technical direction of the SKA. A brief summary chapter emphasizes the point, and considers discovery space.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/b6fd80a3b5db00d9562131b746d8ef115304b506

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Citations in the corpus

• The Australia Telescope Compact Array Broadband Backend (CABB): Description & First Results ⋆ (2011, background): “With its expected 30 square degrees field of view at 1.4 GHz, provided by novel phased array feeds, ASKAP will be a fast 21-cm survey machine, designed to carry out large-scale H i spectral line, transients and radio continuum surveys of the sky (Johnston et al. 2007, 2008).”
• Radio and millimeter continuum surveys and their astrophysical implications (2009, background): “They will realize dramatic improvements in survey speed and sensitivity; ASKAP for example, is expected to produce a survey similar to the NVSS (Condon et al. 1998) in sky coverage, but bettering it by a factor of 50 in sensitivity and of 5 in angular resolution (Johnston et al. 2008).”
• The 6dF Galaxy Survey: final redshift release (DR3) and southern large-scale structures (2009, background): “Deep HI surveys planned for next-generation radio telescopes (Blake et al. 2004; van Driel 2005; Rawlings 2006; Johnston et al. 2008) will also benefit from this redshift information as they probe the gas content of the local southern universe over comparable volumes.”
• Cosmic evolution of the atomic and molecular gas contents of galaxies (2011, background): “…dramatically over the next decade with the nextgeneration of radio and sub-millimeter telescopes such as the Australian SKA Pathfinder (ASKAP; Johnston et al. 2008), the Karoo Array Telescope (MeerKAT; Booth et al. 2009) and the Square Kilometre Array (SKA; Schilizzi et al. 2008) which aim…”
• THE LAST OF FIRST: THE FINAL CATALOG AND SOURCE IDENTIFICATIONS (2015, unknown): “For 95% completeness, WODAN will therefore require an optical matching radius of 4.8 arcsec and ASKAPEMU will require 3 arcsec.”
• COSMIC MICROWAVE BACKGROUND CONSTRAINTS ON THE DURATION AND TIMING OF REIONIZATION FROM THE SOUTH POLE TELESCOPE (2011, methodology): “These efforts include the MWA (Bowman et al. 2005), LOFAR (Harker et al. 2012), GMRT (Pen et al. 2009), PAPER (Parsons et al. 2010) and SKA (Johnston et al. 2008).”
• On the origin of a highly dispersed coherent radio burst (2012, background): “…repeat, and as the numbers detected should rise dramatically with the onset of the ‘all-sky transient monitoring’ capabilities of LOFAR (Stappers et al. 2011), the VLA (Perley et al. 2011), MeerKAT (Booth et al. 2009), ASKAP (Johnston et al. 2008) and ultimately the SKA (Colegate & Clarke 2011).”
• The Detection of an Extremely Bright Fast Radio Burst in a Phased Array Feed Survey (2017, background): “1 see http://www.astronomy.swin.edu.au/pulsar/frbcat/ The Australian SKA Pathfinder (ASKAP; Johnston et al. 2008; Schinckel et al. 2012) is a next-generation wide-field telescope potentially capable of detecting FRBs at a rate an order of magnitude higher than previously possible.”
• The Westerbork SINGS survey - II Polarization, Faraday rotation, and magnetic fields (2009, background): “Detection of such a contribution would require a much more extensive sampling of the RM sky, such as envisioned for the Square Kilometre Array and its Pathfinders (e.g. Johnston et al. 2008).”
• 3D BAROLO: a new 3D algorithm to derive rotation curves of galaxies (2015, methodology): “Indeed, already planned Hi survey, such as WALLABY and DINGO with ASKAP (Johnston et al. 2008), LADUMA with MeerKAT (Booth et al. 2009) and WNSHS with WSRT/APERTIF (Verheijen et al. 2008), are expected to observe thousands of galaxies with spatial resolution comparable to the WHISP galaxies.”
• Short-Duration Gamma-Ray Bursts (2013, background): “However, ASKAP’s limited angular resolution of about 10′′ will lead to source confusion at the level of the anticipated signal,∼ 0.05− 0.1 mJy (Johnston et al. 2008).”
• Evolution of the atomic and molecular gas content of galaxies (2013, background): “…such as the Atacama Large Millimeter Array (ALMA; Wootten & Thompson 2009) and the Square Kilometer Array (SKA; Carilli & Rawlings 2004) and its pathfinders the Karoo Array Telescope (MeerKAT; Booth et al. 2009) and the Australian SKA Pathfinder (ASKAP; Johnston et al. 2008) coming online.”
• LATE-TIME COSMOLOGY WITH 21 cm INTENSITY MAPPING EXPERIMENTS (2014, unknown): “Parkes: A single 64 m dish (with 13 beams) in NSW, Australia (ATNF 2014).”
• On the impact of empirical and theoretical star formation laws on galaxy formation (2010, background): “Telescopes such as ALMA, James Webb Space Telescope and extremely large telescopes will make possible measurements of very low SFRs such as those predicted here for the passive galaxy population, while observations with ALMA, ASKAP, MeerKAT and eventually SKA will be critical for measuring the molec”