1 / 16

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

montanezj
Download Presentation

NOY TAZA

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript


  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

More Related