1. neutrino physics, experiments I – Neutrino Mass João dos Anjos Centro Brasileiro de Pesquisas Físicas

2. Main Sources Recent Conferences presentations:Recent Conferences presentations: Neutrino 2008 – Christchurch, New Zealand. – 25 -31 Mai 2008Neutrino 2008 – Christchurch, New Zealand. – 25 -31 Mai 2008 Neutrino 2006 – Santa Fe, U.S.A. – 13-19 June 2006Neutrino 2006 – Santa Fe, U.S.A. – 13-19 June 2006 NuFact 08 – Valencia, Spain – 30 June – 4 July 2008NuFact 08 – Valencia, Spain – 30 June – 4 July 2008 NuFact 06 – Univ. Irvine, CA, U.S.A. – 24-30 August 2006NuFact 06 – Univ. Irvine, CA, U.S.A. – 24-30 August 2006 – Workshop on Neutrino Factories, Superbeams & Betabeam – Workshop on Neutrino Factories, Superbeams & Betabeam Absolute values of neutrino masses: status and prospectsAbsolute values of neutrino masses: status and prospects S.M.Bilenky et al; Physics Reports 379 (2003), 69-148 Neutrino masses and mixing: evidence and implicationsNeutrino masses and mixing: evidence and implications M.C. Gonzalez-Garcia – Rev. Modern Physics,75, 2003 CERN Summer Student School 2005CERN Summer Student School 2005 J.J. Gómez-Cadenas – IFIC/U. Valencia J.J. Gómez-Cadenas – IFIC/U. Valencia

3. Measuring the Neutrino Mass Direct neutrino mass measurements Double Beta Decay Astrophysical limits

4. Measuring the Neutrino Mass Oscillations tell us about neutrino mass differences, but what about the masses themselves? Three kinds of experiments: Precise experiments on the beta decay of tritium in order to measure directly the average neutrino mass. Neutrinoless double-beta decay experiments sensitive to other combination if neutrinos are their own antiparticle (Majorana particles) Precision studies of the distribution of the cosmic microwave background and large-scale structures of the universe revealed by clusters of galaxies

10. R. Wigmans

32. NEMO-3

39. A. Piepke

54. m 0.90 e V

55. m m m m 2.11 eV 1.8 eV 1.4 eV

58. M. Cirelli, Nufact 06

59. Evidences of DM Rotation curves of galaxies and clusters Weak modulation of strong lensing, Oort discrepancy, weak gravitational lensing, velocity dispersions of dwarf spheroidal galaxies and of spiral gallaxy satellites… Need non-luminous matter Black-holes, brown dwarfs, white dwarfs, giant planets, neutron stars …?

64. Neutrinos from WIMP annihilations Distance source-detector Branching ratio into annihilation channel i Neutrino spectrum from annihilation channel i

67. Conclusions Neutrino detectors can test DM properties Searches for neutrinos from DM annihilations/decays in celestial bodies could constitute powerful probes of DM properties Cherenkov neutrino detectors/telescopes are counting experiments and could only provide limited information Future neutrino detectors (MIND, TASD and LArTPC) will have very good energy resolution for 10’s GeV Reconstructing the neutrino spectra → information on DM mass, annihilation branching ratios and DM-proton cross section Due to small size, only suitable for large spin-dependent cross sections and neutrinos from annihilations in the Sun, but complementary to Neutrino Telescopes (with higher threshold) ‏ Neutrino detectors can set model-independent bounds on the DM annihilation cross section and on the DM lifetime

68. = 0.05 eV