Neutrino Mass and Neutrino Mass and MixingMixing

David SinclairDavid Sinclair

Carleton UniversityCarleton University

PIC2004PIC2004

OutlineOutline

History of neutrino mass and History of neutrino mass and mixingmixing

Recent results and current statusRecent results and current status Future ProspectsFuture Prospects

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

Mass MeasurementsMass Measurements

Electron Energy

M=0

M>0

Decay

Neutrino Mass from Tritium Neutrino Mass from Tritium DecayDecay

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

Neutrino Vacuum Neutrino Vacuum OscillationOscillation

)4/(sin2sin1 222 ELmPe

MSW EffectMSW Effect

Electron Density

e

Mass

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

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

ijijijij

ii

i

τττ

μμμ

eee

li

sandcwhere

e

e

cs

sc

iδecs

sccs

sc

UUU

UUU

UUU

U

sin,cos

00

00

001

0

010

0

00

010

001

0

0

001

100

0

0

2/

2/

1313

1313

2323

23231212

1212

321

321

321

3

2

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

Recent ResultsRecent Results

Neutrino mass from cosmologyNeutrino mass from cosmologyWMAP, 2DF WMAP, 2DF

mm11+m+m22+m+m33< 1 eV< 1 eV

Evidence for Neutrino Evidence for Neutrino Oscillation - Oscillation - AtmosphericAtmospheric

Definitive Data from Definitive Data from SKSK

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

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

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

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

Salt – Pure DSalt – Pure D22OO ConstrainedConstrained

Not Constrained

Pure D2O Salt

Neutrino parameters Neutrino parameters fromfromSolar experiments (Solar experiments (ee))

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

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

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

Mass of NeutrinosMass of Neutrinos

Normal Inverted

Double-beta effective mass constrained by oscillation data

NEMOXavier Sarazin for the NEMO-3 Collaboration Neutrino 2004 Paris 14-19 June 2004

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)

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

Experimental approach - CUORE Experimental approach - CUORE

Source = detector (calorimetric)

Incident particle

absorber crystal

e-

e-

Thermal detectors

heat bath

Thermal sensor

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

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

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