2016
DOI: 10.48550/arxiv.1610.05151
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Contributions of the Cherenkov Telescope Array (CTA) to the 6th International Symposium on High-Energy Gamma-Ray Astronomy (Gamma 2016)

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“…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
confidence: 99%
“…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
confidence: 99%