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NOY TAZA

NOY TAZA. Neutrino Observatory Project in TAZA A. Hoummada University HASSAN II CASABLANCA On behalf of the NOY collaboration D. Lebrun & F. Montanet LPSC - Grenoble. High energy messengers. CMB. Light absorbed. (  e :   :   ). neutrino (  e :2   ). Charged particles

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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 the NOY collaboration D. Lebrun & F. Montanet LPSC - Grenoble

  2. 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

  3. L. Moscoso - HE Tau_Nu - Beijing Scientific aims of ANTARES • 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 • annihilation of neutralinos in the Sun or Galactic Centre. • Magnetic Monopoles + other fields of research

  4. L. Moscoso - HE Tau_Nu - Beijing High energy emission (-ray): • inverse-compton (electronic)? Low energy emission (X-ray) : Synchrotron emission of e- in jet e-  e- p   • 0 decay (hadronic) ?     If hadronic origin  high energy neutrinos ee High energy gamma & neutrinos

  5. so we are here today something occurred over there one billion years ago L  B

  6. Quark mixing (CKM): θ12 ～13°→ θ23 ～2°→ θ13 ～0.2°→ δ～65° Lepton mixing (MNS): θ23 ～45°→ θ12 ～33°→ θ13<10°→ δ/ρ/σ Flavor Mixing and CP Violation

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