“…For instance, HESS Cherenkov minimal fluency detection at ∼TeV energy is ∼ 0, 1 eV cm -2 s -122 while the future Cherenkov Telescope Array (CTA, a km 2 array) would reach 10 -2 eV cm -2 s -1 . 23 For the The Large High Altitude Air Shower Observatory (LHAASO) project the array will encounter the best threshold at 100 TeV reaching 6, 2•10 −3 eV cm -2 s -1 sensitivity. 24 This implies that if the conversion ν µ → µ has a probability of 10 -4 , as much as it results at ≃ 10 13 eV, than the signal (∼ 30 eV cm -2 s -1 sr -1 ) would be at detection threshold 3 • 10 −3 eV cm -2 s -1 sr -1 .…”
Section: Muons Decay In Flight Feeding the Unique Neutrino Induced Te...mentioning
open a new wonderful passe-partout keyhole for neutrino, been seen along the Moon. The lunar solid angle is small and the muon or tau expected rate is rare, but future largest tau radio array as GRAND one might well discover such neutrino imprint.
“…For instance, HESS Cherenkov minimal fluency detection at ∼TeV energy is ∼ 0, 1 eV cm -2 s -122 while the future Cherenkov Telescope Array (CTA, a km 2 array) would reach 10 -2 eV cm -2 s -1 . 23 For the The Large High Altitude Air Shower Observatory (LHAASO) project the array will encounter the best threshold at 100 TeV reaching 6, 2•10 −3 eV cm -2 s -1 sensitivity. 24 This implies that if the conversion ν µ → µ has a probability of 10 -4 , as much as it results at ≃ 10 13 eV, than the signal (∼ 30 eV cm -2 s -1 sr -1 ) would be at detection threshold 3 • 10 −3 eV cm -2 s -1 sr -1 .…”
Section: Muons Decay In Flight Feeding the Unique Neutrino Induced Te...mentioning
open a new wonderful passe-partout keyhole for neutrino, been seen along the Moon. The lunar solid angle is small and the muon or tau expected rate is rare, but future largest tau radio array as GRAND one might well discover such neutrino imprint.
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