TY - GEN
T1 - The Giant Radio Array for Neutrino Detection
AU - The GRAND collaboration
AU - Martineau-Huynh, Olivier
AU - Bustamante, Mauricio
AU - Carvalho, Washington
AU - Charrier, Didier
AU - De Jong, Sijbrand
AU - De Vries, Krijn D.
AU - Fang, Ke
AU - Feng, Zhaoyang
AU - Finley, Chad
AU - Gou, Quanbu
AU - Gu, Junhua
AU - Hu, Hongbo
AU - Kotera, Kumiko
AU - Le Coz, Sandra
AU - Medina, Clementina
AU - Murase, Kohta
AU - Niess, Valentin
AU - Oikonomou, Foteini
AU - Timmermans, Charles
AU - Wang, Zhen
AU - Wu, Xiangping
AU - Zhang, Yi
PY - 2017/3/15
Y1 - 2017/3/15
N2 - 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 [1].
AB - 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 [1].
UR - https://www.scopus.com/pages/publications/85017118321
UR - https://www.scopus.com/inward/citedby.url?scp=85017118321&partnerID=8YFLogxK
U2 - 10.1051/epjconf/201713502001
DO - 10.1051/epjconf/201713502001
M3 - Conference contribution
T3 - EPJ Web of Conferences
BT - 7th International Conference on Acoustic and Radio EeV Neutrino Detection Activities, ARENA 2016
A2 - Buitink, Stijn
A2 - Horandel, Jorg R.
A2 - De Jong, Sijbrand
A2 - Lahmann, Robert
A2 - Nahnhauer, Rolf
A2 - Scholten, Olaf
PB - EDP Sciences
T2 - 7th International Conference on Acoustic and Radio EeV Neutrino Detection Activities, ARENA 2016
Y2 - 7 June 2016 through 10 June 2016
ER -