Abstract
High-energy neutrino astronomy will probe the working of the most violent phenomena in the Universe. The Giant Radio Array for Neutrino Detection (GRAND) project consists of an array of $\sim10^5$ radio antennas deployed over $\sim$200000km$^2$ in a mountainous site. It aims at detecting high-energy neutrinos via the measurement of air showers induced by the decay in the atmosphere of $\tau$ leptons produced by the interaction of the cosmic neutrinos under the Earth surface. Our objective with GRAND is to reach a neutrino sensitivity of $3\times10^{-11}E^{-2}$GeV$^{-1}$cm$^{-2}$s$^{-1}$sr$^{-1}$ above $3 \times10^{16}$eV. This sensitivity ensures the detection of cosmogenic neutrinos in the most pessimistic source models, and about 100 events per year are expected for the standard models. GRAND would also probe the neutrino signals produced at the potential sources of UHECRs. We show how our preliminary design should enable us to reach our sensitivity goals, and present the experimental characteristics. We assess the possibility to adapt GRAND to other astrophysical radio measurements. We discuss in this token the technological options for the detector and the steps to be taken to achieve the GRAND project.
Highlights
Detection methodCosmic ν s can produce particles underground through charged current interaction. s travel to the surface of the Earth and decay in the atmosphere, generating Earth-skimming extensive air showers (EAS)1 [1, 2]
High-energy neutrino astronomy will probe the working of the most violent phenomena in the Universe
We present here a preliminary evaluation of the potential of Giant Radio Array for Neutrino Detection (GRAND) for the detection of cosmic neutrinos
Summary
Cosmic ν s can produce particles underground through charged current interaction. s travel to the surface of the Earth and decay in the atmosphere, generating Earth-skimming extensive air showers (EAS)1 [1, 2]. Coherent electromagnetic radiation is associated to the shower development at frequencies of a few to hundreds of MHz at a detectable level for showers with E 1017 eV. Radio antennas are ideal instruments for this purpose. They offer practical advantages (limited unit cost, easiness of deployment, ...) that allow the deployment of an array over very large areas, as required by the expected low neutrino rate. An extension of the antenna bandwidth up to 200 or 300 MHz would enable to observe the Cherenkov ring associated with the air shower, that represents a sizable fraction of the total electromagnetic signal and may provide an unambiguous signature for background rejection
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