Neutrinos in Astrophysics and Cosmology - INFN Sezione di Ferrara

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Portion of the Hubble Ultra Deep Field Dark Energy 73% (Cosmological Constant) Normal Matter 4% (of this about 10% luminous) Dark Matter 23% Neutrinos 0.1−2% 0.1 2% Georg Raffelt, Raffelt, Max-Planck-Institut für für Physik, München, Germany IDAPP 2d Meeting, 12-13 May 2006, Ferrara, Italy
Formation of Structure Smooth Structured Structure forms by gravitational instability of primordial density fluctuations A fraction of hot dark matter suppresses small-scale small scale structure Georg Raffelt, Max-Planck-Institut für Physik, München, Germany IDAPP 2d Meeting, 12-13 May 2006, Ferrara, Italy
Page 1 and 2: Fermion Mass Spectrum IDAPP 2d Meet
Page 3 and 4: ⎛ ν ⎜ ⎜ ν ⎜ ⎝ ν 3 2 1
Page 5 and 6: Georg Raffelt, Max-Planck-Institut
Page 7 and 8: Stellar Collapse and Supernova Expl
Page 9 and 10: Neutrino Signal of Supernova 1987A
Page 11 and 12: Large Detectors for Supernova Neutr
Page 13 and 14: The Future: A Megatonne Detector? M
Page 15 and 16: IceCube as a Supernova Neutrino Det
Page 17 and 18: Level-Crossing Level Crossing Diagr
Page 19 and 20: SN statistics in external galaxies
Page 21 and 22: Experimental Limits on Relic Supern
Page 23: DSNB Measurement with Neutron Taggi
Page 27 and 28: Neutrino Free Streaming - Transfer
Page 29 and 30: Sensitivity Forecasts for Future LS
Page 31 and 32: Extending the Mass Bound to Other L
Page 33 and 34: Mass Limits on Hot Dark Matter Axio
Page 35 and 36: Dirac masses from coupling to stand
Page 37 and 38: Leptogenesis by Majorana Neutrino D
Page 39 and 40: Leptogenesis by Majorana Neutrino D
Page 41 and 42: Portion of the Hubble Ultra Deep Fi

Neutrinos in Astrophysics and Cosmology - INFN Sezione di Ferrara

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