ARA

    Overview

    The Askaryan Radio Array (ARA) is a radio detector array, currently under development at the South Pole, designed for the detection of ultra-high-energy cosmic neutrinos using the emission of radio waves produced by their interaction with Antarctic ice. The goal is to detect the cosmogenic neutrino flux at energies above 1017 eV. Plans are underway for further construction at the South Pole during the 2017-18 season.

    Research Topics

    • Detection of ultra-high-energy cosmic neutrinos 
     

    Senior Personnel

    Albrecht Karle, principal investigator, professor 
    John Kelley, staff scientist, detector operations and analysis 
    Michael DuVernois, staff scientist, on-ice lead for instrumentation 
     
    Complete list of ARA personnel at WIPAC
     

    WIPAC contributions

    ARA collaborators at UW–Madison are primarily responsible for the integration, testing, drilling, and installation of the ARA instrumentation at the South Pole.  Pending further funding, WIPAC will support the integration and testing of three additional stations as well as the deployment and commissioning of two more stations at the South Pole.  

    The scientific team is working on detector simulations, including neutrino interaction and photon propagation, data analysis, software development, event reconstruction tools, triggering studies, and  detector operations.  

    Select Publications

    Performance of two Askaryan Radio Array stations and first results in the search for ultra-high energy neutrinos
    ARA Collaboration: P. Allison et al
    (Journal Article) e-print archive arXiv: 1507.08991[astro-ph.HE], July 2015
    arxiv.org

    First Constraints on the Ultra-High Energy Neutrino Flux from a Prototype Station of the Askaryan Radio Array
    ARA Collaboration: P. Allison et al
    (Journal Article) e-print: arXiv:1404.5285v2 [astro-ph.HE]
    arxiv.org

    Design and Initial Performance of the Askaryan Radio Array Protoype EeV Neutrino Detector at the South Pole
    ARA Collaboration: P. Allison et al
    (Journal Article) Astropart. Phys. 35 (2012) 457-477; e-print: arXiv:1105.2854 [astro-ph.IM]
    arxiv.org

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