EPJ Web Conf.
Volume 135, 20177th International Conference on Acoustic and Radio EeV Neutrino Detection Activities (ARENA 2016)
|Number of page(s)||4|
|Section||Planned Facilities for Radio Detection of Air Showers|
|Published online||15 March 2017|
The Giant Radio Array for Neutrino Detection
1 LPNHE, CNRS-IN2P3 and Universités Paris 6 & 7, BP200, 4 place Jussieu, 75252 Paris, France
2 Center for Cosmology and AstroParticle Physics, The Ohio State University, Columbus, OH 43210, USA
3 Physics institute, University of Säo Paulo, Rua do Matäo, trav. R, Cid. Universitária, Säo Paulo, Brazil
4 SUBATECH, CNRS-IN2P3, Université de Nantes, Ecole des Mines de Nantes, Nantes, France
5 Nikhef/Radboud University, Nijmegen, the Netherlands
6 Vrije Universiteit Brussel, Dienst ELEM, B-1050 Brussels, Belgium
7 Department of Astronomy, University of Maryland, College Park, MD, 20742
8 Key Lab of Particle Astrophysics, IHEP, Chinese Academy of Sciences, Beijing 100049, China
9 Oskar Klein Centre and Dept. of Physics, Stockholm University, SE-10691 Stockholm, Sweden
10 National Astronomical Observatory, Chinese Academy of Sciences, Beijing 100012, China
11 IAP, Sorbonne Universités, Paris 6 and CNRS, 98 bis bd Arago, 75014 Paris, France
12 Instituto Argentino de Radioastronomia, CCT La Plata-CONICET, 1894, Villa Elisa C.C. No. 5, Argentina
13 Dept. of Physics, Dept. of Astronomy & Astrophysics, Penn State University, University Park, PA, USA
14 LPC, CNRS-IN2P3, Université Blaise Pascal, BP 10448, 63000 Clermond-Ferrand, France
* e-mail: email@example.com
Published online: 15 March 2017
The Giant Radio Array for Neutrino Detection (GRAND) is a planned array of ~ 2·105 radio antennas deployed over ~ 200 000 km2 in a mountainous site. It aims primarly at detecting high-energy neutrinos via the observation of extensive air showers induced by the decay in the atmosphere of taus produced by the interaction of cosmic neutrinos under the Earth surface. GRAND aims at reaching a neutrino sensitivity of 5 · 10−11 E−2 GeV−1 cm−2 s−1 sr−1 above 3 · 1016 eV. This ensures the detection of cosmogenic neutrinos in the most pessimistic source models, and ~50 events per year are expected for the standard models. The instrument will also detect UHECRs and possibly FRBs. Here we show how our preliminary design should enable us to reach our sensitivity goals, and discuss the steps to be taken to achieve GRAND, while the compelling science case for GRAND is discussed in more details in .
© The Authors, published by EDP Sciences, 2017
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