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    Overview of lunar detection of ultra-high energy particles and new plans for the SKA

    Access Status
    Open access via publisher
    Authors
    James, C.
    Alvarez-Muñiz, J.
    Bray, J.
    Buitink, S.
    Dagkesamanskii, R.
    Ekers, Ronald
    Falcke, H.
    Gayley, K.
    Huege, T.
    Mevius, M.
    Mutel, R.
    Scholten, O.
    Spencer, R.
    Ter Veen, S.
    Winchen, T.
    Date
    2017
    Type
    Conference Paper
    
    Metadata
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    Citation
    James, C. and Alvarez-Muñiz, J. and Bray, J. and Buitink, S. and Dagkesamanskii, R. and Ekers, R. and Falcke, H. et al. 2017. Overview of lunar detection of ultra-high energy particles and new plans for the SKA.
    Source Title
    EPJ Web of Conferences
    DOI
    10.1051/epjconf/201713504001
    ISBN
    9782759890156
    School
    Curtin Institute of Radio Astronomy (Engineering)
    URI
    http://hdl.handle.net/20.500.11937/57019
    Collection
    • Curtin Research Publications
    Abstract

    © 2017 The Authors, published by EDP Sciences. The lunar technique is a method for maximising the collection area for ultra-high-energy (UHE) cosmic ray and neutrino searches. The method uses either ground-based radio telescopes or lunar orbiters to search for Askaryan emission from particles cascading near the lunar surface. While experiments using the technique have made important advances in the detection of nanosecond-scale pulses, only at the very highest energies has the lunar technique achieved competitive limits. This is expected to change with the advent of the Square Kilometre Array (SKA), the low-frequency component of which (SKA-low) is predicted to be able to detect an unprecedented number of UHE cosmic rays. In this contribution, the status of lunar particle detection is reviewed, with particular attention paid to outstanding theoretical questions, and the technical challenges of using a giant radio array to search for nanosecond pulses. The activities of SKA's High Energy Cosmic Particles Focus Group are described, as is a roadmap by which this group plans to incorporate this detection mode into SKA-low observations. Estimates for the sensitivity of SKA-low phases 1 and 2 to UHE particles are given, along with the achievable science goals with each stage. Prospects for near-future observations with other instruments are also described.

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