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Science with ASKAP

The Australian square-kilometre-array pathfinder

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Abstract

The 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.

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Notes

  1. Note that the Bower et al. [35] predictions are based on Millennium Simulation merger trees [244], and the mass resolution of the simulation is such that the cold gas mass fraction is underestimated at high redshifts.

  2. Although this technique increases the likelihood of finding radio galaxies at high redshift, it severely biases the resultant samples to only those with unusually steep spectra. As a result, we currently know very little any population of normal-spectrum radio galaxies at high redshift.

  3. The SUMSS-NVSS USS sample was selected with a 15mJy flux density limit imposed at 843 MHz.

  4. Obviously much deeper surveys could be reached in longer integrations, but the resulting Stokes I images would be heavily confused. Also, an initial RM grid from ASKAP would provide such a large leap forward in our understanding of the polarized sky, that we would need to properly digest these new data before knowing how best to survey deeper.

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Authors and Affiliations

  1. Australia Telescope National Facility, Commonwealth Scientific and Industrial Research Organisation, P.O. Box 76, Epping, New South Wales, 1710, Australia

    S. Johnston, R. Braun, P. Edwards, R. Ekers, I. Feain, G. Hobbs, C. Jackson, B. Koribalski, R. Manchester, N. McClure-Griffiths, R. Norris, C. Phillips & A. Tzioumis

  2. Department of Physics and Astronomy, University of Calgary, Calgary, Alberta, T2N 1N4, Canada

    R. Taylor, J. Brown, R. Kothes & J. Stil

  3. Centre for Astrophysics and Supercomputing, Swinburne University of Technology, P.O. Box 218, Hawthorn, Victoria, 3122, Australia

    M. Bailes, C. Blake, A. Deller, V. Kilborn, A. Lenc & C. Power

  4. Department of Physics and Astronomy, York University, Toronto, Ontario, M3J 1P3, Canada

    N. Bartel & M. Bietenholz

  5. Institute for Computational Cosmology, University of Durham, Durham, DH1 3LE, UK

    C. Baugh

  6. Hartebeesthoek Radio Observatory, P.O. Box 443, Krugersdorp, 1740, South Africa

    M. Bietenholz

  7. School of Physics, The University of Sydney, Sydney, New South Wales, 2006, Australia

    S. Chatterjee, B. Gaensler, A. Hopkins & E. Sadler

  8. Center for Astrophysics and Space Astronomy, University of Colorado, 389 UCB, Boulder, CO, 80309-0389, USA

    J. Darling

  9. Observatorio Astronomico Nacional, Alcara de Henares, Spain

    R. Dodson

  10. School of Mathematics and Physics, University of Tasmania, Private Bag 21, Hobart, Tasmania, 7001, Australia

    S. Ellingsen & J. Lovell

  11. Astronomy Department, University of California-Berkeley, Berkeley, CA, 94720, USA

    M. Haverkorn

  12. School of Chemistry & Physics, University of Adelaide, Adelaide, South Australia, 5006, Australia

    C. James & R. Protheroe

  13. Department de Physique et Observatoire du Mont Megantic, Universite Laval, Quebec City, Quebec, G1K 7P4, Canada

    G. Joncas

  14. Department of Physics, McGill University, Montreal, Quebec, H3A 2T8, Canada

    V. Kaspi

  15. Dominion Radio Astrophysical Observatory, Herzberg Institute of Astrophysics, National Research Council, Penticton, British Columbia, Canada

    T. Landecker & M. Wolleben

  16. Astronomy Department, California Institute of Technology, Pasadena, CA, 91125, USA

    J.-P. Macquart

  17. Department of Physics, La Trobe University, Melbourne, Victoria, 3086, Australia

    D. Matthews

  18. Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, Ontario, M5S 3H8, Canada

    U.-L. Pen

  19. Mount Stromlo and Siding Spring Observatory, Private Bag, Weston Creek, Canberra, Australian Capital Territory, 2601, Australia

    B. Schmidt

  20. Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, British Columbia, V6T 1Z1, Canada

    I. Stairs & J. Wall

  21. School of Physics, University of Western Australia, Crawley, Western Australia, 6009, Australia

    L. Staveley-Smith

  22. Department of Imaging and Applied Physics, Curtin University of Technology, Bentley, Western Australia, Australia

    S. Tingay

  23. Manly Astrophysics Workshop Pty Ltd, Manly, New South Wales, 2095, Australia

    M. Walker

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  1. S. Johnston
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  48. M. Walker
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  49. J. Wall
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Correspondence to S. Johnston.

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J. Wall is the overall editor.

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Johnston, S., Taylor, R., Bailes, M. et al. Science with ASKAP. Exp Astron 22, 151–273 (2008). https://doi.org/10.1007/s10686-008-9124-7

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