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NOY TAZA

NOY TAZA. Neutrino Observatory Project in TAZA A. Hoummada University HASSAN II CASABLANCA On behalf of NOY collaboration D. Lebrun & F. Montanet LPSC - Grenoble. Outline.

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NOY TAZA

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  1. NOY TAZA Neutrino Observatory Project in TAZA A. Hoummada University HASSAN II CASABLANCA On behalf of NOY collaboration D. Lebrun & F. Montanet LPSC - Grenoble

  2. Outline - Cosmic Rays & Neutrino Astronomy - Neutrinos Oscillations Scheme- NOY : Detector & Site- Simulation results - Conclusion & Progress Scientific Objectives Of NOY - 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

  3. so we are here today

  4. L. Moscoso - HE Tau_Nu - Beijing High energy messengers CMB Light absorbed (e::) neutrino (e:2) Charged particles scattered by magnetic field Neutrinos Protons Photons PeV EeV TeV ZeV Log E (GeV) 1 2 3 4 5 6 7 8 9 10 11 12 13 Abdeslam Hoummada CASABLANCA 14 November 2011

  5. Neutrino Astronomy

  6. p  • 0 decay (hadronic) ?     If hadronic origin  high energy neutrinos ee All particle energy spectrum Ultrahigh-energy (UHE) cosmic rays Cosmogenic Neutrinos: - progenitors are pions - pion decay  1 x e-type, 2 x -type - Oscillation: 2 x -type  1 x -type + 1 x -type UHE neutrinos

  7. θ23 ～45°→ θ12 ～33°→ θ13<10°→ δ/ρ/σ Flavor Mixing

  8. NOY : Detector and Site 100 m

  9. NOY : Detector and Site RIF Mountain 750 m asl ATLAS Mountain 3000 m asl Valley 400 m asl Width from 6 to 15 km 2 Km from TAZA

  10. Neutrino Sensitivity for different neutrino enrgies : from 100 MeV to 100 GeV

  11. Conclusion • UHECR experiments will allow an exciting physics program complementary to UHE astronomy : - One can learn about high enregy process in QCD - One may be able to test new physics ideas in neutrino interactions - One may find dark matter - One may have indication on new Physics beyond the TeV scale - Outreach and Education Progress - September 2011 : Construction of the Cabane - February 2012 : Installation and Commissionning of the first prototype - Summer 2012 : Installation of the 5 stations and Data taking

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