NOY TAZA Neutrino Observatory Project in TAZA A. Hoummada University HASSAN II CASABLANCA On behalf of NOY collaboration D. Lebrun & F. Montanet LPSC - Grenoble - Neutrinos from galactic sources - Pulsars, Supernova Remnants - Microquasars - Intense activity in Galactic centre reported by TeV -ray telescopes - Neutrinos from extragalactic sources - Active Galactic Nuclei - Gamma Ray Bursts - Dark Matter, supersymetric particles (neutralinos, ) - Possible new Physics Beyond TeV Scale & new Neutrinos Hygh Energy Physics Scientific Objectives Of NOY - Cosmic Rays & Neutrino Astronomy - Neutrinos Oscillations Scheme - NOY : Detector & Site - Simulation results - Conclusion & Progress Outline 3 today so we are here 23-26/04/2006L. Moscoso - HE Tau_Nu - Beijing 4 High energy messengers neutrino ( e :2 ) Light absorbed Charged particles scattered by magnetic field ( e : : ) Neutrinos Protons Photons Log E (GeV) TeV PeVEeV ZeV CMB Abdeslam Hoummada CASABLANCA 14 November 2011 Neutrino Astronomy Ultrahigh-energy (UHE) cosmic rays All particle energy spectrum UHE neutrinos Cosmogenic Neutrinos: - progenitors are pions - pion decay 1 x e-type, 2 x -type - Oscillation: 2 x -type 1 x -type + 1 x -type e e If hadronic origin high energy neutrinos p 0 decay (hadronic) ? 7 23 45 12 33 13