Neutrino Mass and Mixing
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Neutrino Mass and Neutrino Mass and MixingMixing
David SinclairDavid Sinclair
Carleton UniversityCarleton University
PIC2004PIC2004
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OutlineOutline
History of neutrino mass and History of neutrino mass and mixingmixing
Recent results and current statusRecent results and current status Future ProspectsFuture Prospects
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HistoryHistory
Original proposal by Pauli, FermiOriginal proposal by Pauli, Fermi– Neutrino mass must be smallNeutrino mass must be small– Only 1 neutrino proposed so no Only 1 neutrino proposed so no
mixingmixing
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Mass MeasurementsMass Measurements
Electron Energy
M=0
M>0
Decay
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Neutrino Mass from Tritium Neutrino Mass from Tritium DecayDecay
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Neutrino MixingNeutrino Mixing
Pontecorvo suggested (late 50’s) Pontecorvo suggested (late 50’s) that neutrinos would oscillate by that neutrinos would oscillate by analogy with Kanalogy with K00
When Davis showed deficit of When Davis showed deficit of solar neutrinos, oscillation again solar neutrinos, oscillation again raised as a possible solutionraised as a possible solution
This solution not popular until This solution not popular until MSWMSW
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Neutrino Vacuum Neutrino Vacuum OscillationOscillation
)4/(sin2sin1 222 ELmPe
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MSW EffectMSW Effect
Electron Density
e
Mass
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Implications of Implications of neutrino oscillationsneutrino oscillations ee are not mass eigenstates are not mass eigenstates
Mass states are Mass states are and and Lepton number not conservedLepton number not conserved
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Theoretical BiasesTheoretical Biases
Mixings would be small Mixings would be small (comparable to Cabibbo (comparable to Cabibbo mixing)mixing)
SeeSaw model suggests SeeSaw model suggests
2MqM
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ijijijij
ii
i
τττ
μμμ
eee
li
sandcwhere
e
e
cs
sc
iδecs
sccs
sc
UUU
UUU
UUU
U
sin,cos
00
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2/
2/
1313
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2323
23231212
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ilil U If neutrinos have mass:
For three neutrinos:
Solar Atmospheric
Using the oscillation framework:
CP Violating Phase Reactor... Majorana Phases
Maki-Nakagawa-Sakata-Pontecorvo matrix
(Double Decay)
Full neutrino mixing matrix
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Recent ResultsRecent Results
Neutrino mass from cosmologyNeutrino mass from cosmologyWMAP, 2DF WMAP, 2DF
mm11+m+m22+m+m33< 1 eV< 1 eV
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Evidence for Neutrino Evidence for Neutrino Oscillation - Oscillation - AtmosphericAtmospheric
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Definitive Data from Definitive Data from SKSK
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Evidence for Evidence for OscillationsOscillationsSolarSolar Chlorine experiment sees ¼ SSM Chlorine experiment sees ¼ SSM
fluxflux Gallium experiments see ½ SSM Gallium experiments see ½ SSM
fluxflux Kamiokande sees ½ SSM fluxKamiokande sees ½ SSM flux
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Definitive data - SNODefinitive data - SNO
Heavy water Cerenkov detectorHeavy water Cerenkov detector Measure Measure ee flux with CC reaction flux with CC reaction Measure total Measure total flux with NC reaction flux with NC reaction
CC
NC
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SNOSNO
1000 Tonnes of D1000 Tonnes of D22OO 12 M Acrylic vessel12 M Acrylic vessel 10,000 phototubes10,000 phototubes 8000 Tonnes of pure 8000 Tonnes of pure
light waterlight water 2000 m deep in Mine2000 m deep in Mine World’s largest deep World’s largest deep
caverncavern All materials very pureAll materials very pure
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3 Phases of SNO3 Phases of SNO
1) Run with pure Heavy Water1) Run with pure Heavy Water 2) Add 0.2% NaCl to enhance NC 2) Add 0.2% NaCl to enhance NC
detectiondetection 3) Remove NaCl, add Neutral 3) Remove NaCl, add Neutral
Current Detectors (NCDs)Current Detectors (NCDs) Each phase is approx. 2 yearsEach phase is approx. 2 years
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Salt – Pure DSalt – Pure D22OO ConstrainedConstrained
Not Constrained
Pure D2O Salt
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Neutrino parameters Neutrino parameters fromfromSolar experiments (Solar experiments (ee))
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Evidence for Evidence for OscillationOscillationReactor NeutrinosReactor Neutrinos Short distance searches (CHOOZ, Short distance searches (CHOOZ,
Palo Verde etc) have been Palo Verde etc) have been negativenegative
Kamland provides definitive Kamland provides definitive demonstrationdemonstration
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Where are weWhere are we
36.2
02.12
101.2
05.082.02
106.02.8
132
232
23223
122
25212
Sin
Sin
eVm
Sin
eVm
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Neutrino-less double Neutrino-less double beta decaybeta decay Nice data on 2 neutrino decay Nice data on 2 neutrino decay
from NEMOfrom NEMO Nice cryogenic techniquesNice cryogenic techniques Tantalizing results from Tantalizing results from
GermaniumGermanium
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Mass of NeutrinosMass of Neutrinos
Normal Inverted
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Double-beta effective mass constrained by oscillation data
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NEMOXavier Sarazin for the NEMO-3 Collaboration Neutrino 2004 Paris 14-19 June 2004
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100Mo 6.914 kg Q= 3034 keV
decay isotopes in NEMO-3 detector
82Se 0.932 kg Q= 2995 keV
116Cd 405 g Q= 2805 keV
96Zr 9.4 g Q= 3350 keV
150Nd 37.0 g Q= 3367 keV
Cu 621 g
48Ca 7.0 g Q= 4272 keV
natTe 491 g
130Te 454 g Q= 2529 keV
measurement
External bkg measurement
search
Xavier Sarazin for the NEMO-3 Collaboration Neutrino 2004 Paris 14-19 June 2004
(All the enriched isotopes produced in Russia)
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Background subtracted
82Se T1/2 = 10.3 0.2 (stat) 1.0 (syst) 1019 y
116Cd if SSD T1/2 = 2.8 0.1 (stat) 0.3 (syst) 1019 y if HSD T1/2 = 3.05 0.1 (stat) 0.3 (syst) 1019 y
150Nd T1/2 = 9.7 0.7 (stat) 1.0 (syst) 1018 y
96Zr T1/2 = 2.0 0.3 (stat) 0.2 (syst) 1019 y
82Se
116Cd 150Nd
22 preliminary results for other nuclei
96Zr
• Data
simulation
Data
simulation
Data
simulation
Data
simulation
NEMO-3 932 g241.5 days
2385 eventsS/B = 3.3
NEMO-3 NEMO-3NEMO-3 5.3 g168.4 days72 eventsS/B = 0.9
37 g168.4 days449 events
S/B = 2.8
405 g168.4 days
1371 eventsS/B = 7.5
E1+E2 (keV)
E1+E2 (MeV) E1+E2 (MeV) E1+E2 (MeV)Xavier Sarazin for the NEMO-3 Collaboration Neutrino 2004 Paris 14-19 June 2004
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Experimental approach - CUORE Experimental approach - CUORE
Source = detector (calorimetric)
Incident particle
absorber crystal
e-
e-
Thermal detectors
heat bath
Thermal sensor
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Resolution of the 5x5x5 cmResolution of the 5x5x5 cm33 (~ (~ 760 g ) crystals760 g ) crystals
:0.8 keV FWHM @ 46 keV
1.4 keV FWHM @ 0.351 MeV
2.1 keV FWHM @ 0.911 MeV
2.6 keV FWHM @ 2.615 MeV
3.2 keV FWHM @ 5.407 MeV
(the best spectrometer ever realized)
Energy [keV]
Cou
nts
210Po line
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The FutureThe Future
Determine Determine 1313
– New Reactor experimentsNew Reactor experiments– Long baselineLong baseline
Are masses Majorana or DiracAre masses Majorana or Dirac– Double beta decayDouble beta decay
Is CP violatedIs CP violated– SuperbeamsSuperbeams
Sterile neutrinos?Sterile neutrinos?– MinibooneMiniboone
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The Future Looks Very The Future Looks Very ExcitingExciting Many new experiments taking Many new experiments taking
data or about to startdata or about to start Precision measurements of MNSP Precision measurements of MNSP
matrixmatrix Look for CP violationLook for CP violation Neutrino astrophysicsNeutrino astrophysics