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Qu’est-ce que la masse manquante de l’univers ? SUSY ! Neutralino ? Search for WIMP Weakly Interactive Massive Particle LHC FAAQ2006 Alain Bellerive 92
WIMP Interaction with Matter Spin independent interaction – scalar coupling M WIMP ~ 100 GeV heavy nuclei M Recoil < 100 keV Faint signals (heat, light, sound, electron) Clean and deap underground laboratory Low Energy Threshold Large Target Mass with Ultra-Low Background FAAQ2006 Alain Bellerive 93
Page 1 and 2:
Le neutrino, particule fantomatique
Page 3 and 4:
Les grandes questions du 21 ième s
Page 5 and 6:
The First Piece: - Fundamental Forc
Page 7 and 8:
Scope of Particle Physics FAAQ2006
Page 9 and 10:
History of the Neutrino • Disover
Page 11 and 12:
Elementary Particles electron & neu
Page 13 and 14:
Open Questions in Neutrino Physics
Page 15 and 16:
2) Underground laboratories: e.g. S
Page 17 and 18:
Electroweak Interactions L ( em NC)
Page 19 and 20:
• Define a quark mixing matrix wh
Page 21 and 22:
Evidence for Neutrino Oscillations
Page 23 and 24:
Macroscopic Properties of the Sun M
Page 25 and 26:
Neutrino Production in the Sun Ligh
Page 27 and 28:
Solar Neutrino Experiments • Revi
Page 29 and 30:
Chlorine Measurements: Homestake (U
Page 31 and 32:
Gallium Measurements: SAGE (on-goin
Page 33 and 34:
Water Detector: Super-Kamiokande (J
Page 35 and 36:
Solar ν Flux Measurement Results C
Page 37 and 38:
Solar Neutrino Problem • Historic
Page 39 and 40:
Neutrino Oscillations Neutrino Stat
Page 41 and 42: Solar Neutrino Oscillations P ee =
Page 43 and 44: Matter-Enhanced Neutrino Oscillatio
Page 45 and 46: Somewhere in the Depths of Canada..
Page 47 and 48: Underground laboratory in Sudbury S
Page 49 and 50: Subury Neutrino Observatory • Tim
Page 51 and 52: Purpose of SNO • If Solar Neutrin
Page 53 and 54: Neutrino detection in SNO • PMTs
Page 55 and 56: SNO observables - event by event PM
Page 57 and 58: Neutrino Reactions in SNO CC ν e d
Page 59 and 60: An Ultraclean Environment • Highl
Page 61 and 62: Three Ways to Catch Neutrons! (NC)
Page 63 and 64: Subury Neutrino Observatory D 2 O R
Page 65 and 66: Shape Constrained Neutrino Fluxes (
Page 67 and 68: SNO NC in D 2 O (April 2002) ~ 2/3
Page 69 and 70: Progress in 2002 on the Solar Neutr
Page 71 and 72: Neutrino Mixing (detail) As in the
Page 73 and 74: Subury Neutrino Observatory Salt Re
Page 75 and 76: Charged Current (CC=ν e ) Spectrum
Page 77 and 78: Day/Night Asymmetries A X = ( Φ (
Page 79 and 80: SNO: Results Phase II: neutrino osc
Page 81 and 82: NCD Deployment FAAQ2006 Alain Belle
Page 83 and 84: What SNO might tell us in the futur
Page 85 and 86: FAAQ2006 Alain Bellerive 85
Page 87 and 88: Summary • SNO provided direct evi
Page 89 and 90: Comment les particules acquièrent-
Page 91: Qu’est-ce que la masse manquante
Page 95 and 96: Pourquoi la matière domine-t-elle
Page 97 and 98: Conclusion • Plusieurs défis en
Page 99: FAAQ2006 Alain Bellerive 99
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