MINOS Result. The ND analysis predicts: events in the Far Detector 54 observed, 0.7σ excess. 49.1±7.0(stat.)±2.7(syst.

MINOS Result The ND analysis predicts: 49.1±7.0(stat.)±2.7(syst.) events in the Far Detector 54 observed, 0.7σ excess 26

MINOS Result The ND analysis predicts: 49.1±7.0(stat.)±2.7(syst.) events in the Far Detector 54 observed, 0.7σ excess Normal hierarchy Inverted hierarchy 26

MINOS Result The ND analysis predicts: 49.1±7.0(stat.)±2.7(syst.) events in the Far Detector 54 observed, 0.7σ excess Normal hierarchy The 90% C.L. limits are: sin 2 (2θ13) < 0.12 (normal) sin 2 (2θ13) < 0.20 (inverse) for sin 2 (2θ23) = 1, δcp = 0, Δm 2 31 = 2.43 x 10-3 ev 2 Inverted hierarchy 26

3-flavor Analyses 27

3-flavor Analyses SuperK - atmospheric Excluded by CHOOZ at 90% C.L. 99% C.L. 90% C.L. 68% C.L. best Excluded by CHOOZ at 90% C.L. 99% C.L. 90% C.L. 68% C.L. best 27

3-flavor Analyses SuperK - atmospheric Global solar - SNO analysis Excluded by CHOOZ at 90% C.L. 99% C.L. 90% C.L. 68% C.L. best Excluded by CHOOZ at 90% C.L. 99% C.L. 90% C.L. 68% C.L. best Similar results obtained by SuperK Collaboration 27

Summary (Mixed) Oscillation analysis sin 2 θ13 (value) sin 2 θ13 (90% CL) SuperK (atmospheric,norm) 0.006+.030 -.006 <0.066 SuperK (atmospheric,inv) SuperK (solar,global) 0.044 +.041 -.032 <0.122 sin 2 θ13 (95% CL) 0.025 +.018 -.016 <0.059 sin 2 θ13 0 0.02 0.04 0.06 SNO (solar,global) 0.020 +.021 -.016 <0.057 MINOS (normal) at δcp=0 MINOS (inverted) at δcp=0 0.007 +.014 -.007 <0.03 0.015 +.021 -.013 <0.05 CHOOZ <0.037 CHOOZ limit 28

Global 3-flavor fit 29

Global 3-flavor fit Several 3-flavor fits have been made to all data 29

Global 3-flavor fit Several 3-flavor fits have been made to all data We quote results (updated 2/10/2010) from: T.Schwetz, M.Tortola, J.W.F. Valle in arxiv 0808.2016.v3 29

Global 3-flavor fit Several 3-flavor fits have been made to all data We quote results (updated 2/10/2010) from: T.Schwetz, M.Tortola, J.W.F. Valle in arxiv 0808.2016.v3 Parameter best fit 2σ 3σ Δm 2 21 [10-5 ev 2 ] 7.59 +0.23-0.18 7.22-8.03 7.03-8.27 Δm 2 31 [10-3 ev 2 ] 2.40 +0.12-0.11 2.18-2.64 2.07-2.75 sin 2 θ12 0.318 +0.019-0.016 0.29-0.36 0.27-0.38 sin 2 θ23 0.50 +0.07-0.06 0.39-0.63 0.36-0.67 sin 2 θ13 0.013 +0.013-0.009 <0.039 <0.053 29

Quark/Lepton Comparison 30

Quark/Lepton Comparison Mixing Angles 30

Quark/Lepton Comparison Mixing Angles CKM Matrix, graphically 30

Quark/Lepton Comparison Mixing Angles < CKM Matrix, graphically PMNS Matrix, graphically 30

Quark/Lepton Comparison log m (MeV) Mixing Angles < 6 5 4 3 2 t c b s τ μ CKM Matrix, graphically PMNS Matrix, graphically 1 0 u d e -1 Masses, graphically 30

Quark/Lepton Comparison Mixing Angles 4 3 2 1 CKM Matrix, graphically PMNS Matrix, graphically 0 Normal hierarchy - similar pattern of masses Inverted hierarchy - different mass pattern < log m (MeV) 6 5 t b c τ s μ d u e -1 Masses, graphically 30

LSND Effect R. Van de Water Nu2010 31

LSND Effect Apparent ν μ -> νe transition R. Van de Water Nu2010 31

LSND Effect Apparent ν μ -> νe transition Oscillation interpretation R. Van de Water Nu2010 31

LSND Effect Apparent ν μ -> νe transition Oscillation interpretation If effect is due to oscillations, there must be a 4th, sterile, neutrino R. Van de Water Nu2010 31

MiniBooNE 32

MiniBooNE MiniBooNE was designed to test the LSND result L/E is similar to that in LSND but L and E are roughly an order of magnitude larger; different systematics 32

MiniBooNE MiniBooNE was designed to test the LSND result L/E is similar to that in LSND but L and E are roughly an order of magnitude larger; different systematics target and horn decay region absorber dirt detector Booster K + π + ν µ ν e??? primary beam secondary beam tertiary beam (protons) (mesons) (neutrinos) 32

MiniBooNE Results R. Van de Water Nu2010 33

MiniBooNE Results Neutrinos - 6.5E20 POT LSND Region Neutrinos: Excess of electrons (γʼs?) below 475 MeV No excess in the LSND region R. Van de Water Nu2010 33

MiniBooNE Results Neutrinos - 6.5E20 POT Antineutrinos - 5.66E20 POT LSND Region LSND Region Neutrinos: Excess of electrons (γʼs?) below 475 MeV No excess in the LSND region Antineutrinos: Small excess below 475 MeV Excess of events (>2σ) in LSND region R. Van de Water Nu2010 33

MINOS ν Result P.Vahle Neutrino2010 34

MINOS ν Result MINOS took 1.7E20 protons on target in ν μ mode P.Vahle Neutrino2010 34

MINOS ν Result MINOS took 1.7E20 protons on target in ν μ mode Δm 2 = 3.36 +0.45 0.40 10 3 ev 2 sin 2 (2θ) = 0.86 ± 0.11 P.Vahle Neutrino2010 34

MINOS ν Result MINOS took 1.7E20 protons on target in ν μ mode Δm 2 = 3.36 +0.45 0.40 10 3 ev 2 sin 2 (2θ) = 0.86 ± 0.11 There is a request to increase the data set to 4E20 POT P.Vahle Neutrino2010 34

ν/ν in the Solar Sector 35

ν/ν in the Solar Sector Solar includes all solar experiments (3 phases of SNO, SuperKamiokande, Chlorine, Gallium and Borexino) 35

ν/ν in the Solar Sector Solar includes all solar experiments (3 phases of SNO, SuperKamiokande, Chlorine, Gallium and Borexino) ν ν 2ν model 35

ν/ν in the Solar Sector Solar includes all solar experiments (3 phases of SNO, SuperKamiokande, Chlorine, Gallium and Borexino) ν ν 2ν model 3ν model 35

Neutrino Masses ν 36

2 Questions re ν Mass 37

2 Questions re ν Mass The question of neutrino masses focuses on 2 related questions: 37

2 Questions re ν Mass The question of neutrino masses focuses on 2 related questions: What is the absolute scale of neutrino masses, ie what is the mass of the lowest lying neutrino 37

2 Questions re ν Mass The question of neutrino masses focuses on 2 related questions: What is the absolute scale of neutrino masses, ie what is the mass of the lowest lying neutrino What is the mass hierarchy, ie is m1 or m3 the lightest neutrino 37

Methods There are three general ways of determining neutrino mass scale: β decay, 0ν2β decay, cosmology They all measure different combination of miʼs Kinematics in β decay: Rate of no-ν double β decay: Cosmology: m cos = m j j m β = U eju ej m 2 j j m ββ = 1/2 U 2 m ej j j 38

Mass from β Decay 39

Mass from β Decay Experimental result does not depend on: Nature of neutrino (Dirac or Majorana) 39

Mass from β Decay Experimental result does not depend on: Nature of neutrino (Dirac or Majorana) Optimal (so far) nucleus - H 3 End point energy - 18.58 KeV, T1/2-12.32 yrs Current mass limit - 39

Mass from β Decay Experimental result does not depend on: Nature of neutrino (Dirac or Majorana) Optimal (so far) nucleus - H 3 End point energy - 18.58 KeV, T1/2-12.32 yrs Current mass limit - Experimental challenges: Statistics Resolution Control of Systematics 39

KATRIN - The Last Hurrah 40

KATRIN - The Last Hurrah Projected Sensitivity: 200 mev Start of Data Taking: 2013 40

Another Way? The Concept Cyclotron Frequency ω(γ) = ω 0 γ = eb K + m e Coherent radiation emitted can be collected and used to measure the energy of the electron in a non-destructive manner. Radiative Power Emitted P tot (β, β) = 1 2e 2 ω0 2 4π 0 3c β 2 1 β 2 B. Monreal and J. Formaggio Published in Phys. Rev. D80:051301 (2009). Uniform B field Low pressure T2 gas. B field Antenna array for cyclotron radiation detection. T 2 gas J.Formaggio, Neutrino 2010 41

Comparison with other ways from S.Parke Nu2010 42

Comparison with other ways Kinematics of Decay from S.Parke Nu2010 42

Comparison with other ways Kinematics of Decay Cosmology from S.Parke Nu2010 42

Comparison with other ways Kinematics of Decay Cosmology Double Beta Decay from S.Parke Nu2010 42

Comparison with other ways Kinematics of Decay Cosmology Double Beta Decay Obviously, we should all hope for inverted hierarchy The goal is to reach a value which would either exclude inverted hierarchy or obtain a measurement from S.Parke Nu2010 42

Double Beta Decay e - ν-ν n n e - p p 43

2ν Double Beta Decay 44

2ν Double Beta Decay M(Z,A) -> M(Z+2,A) + 2e - + 2νe 44

2ν Double Beta Decay M(Z,A) -> M(Z+2,A) + 2e - + 2νe Can occur in few tens of nuclei 44

2ν Double Beta Decay M(Z,A) -> M(Z+2,A) + 2e - + 2νe Can occur in few tens of nuclei Process is second order in WI, hence strongly suppressed 44

2ν Double Beta Decay M(Z,A) -> M(Z+2,A) + 2e - + 2νe Can occur in few tens of nuclei Process is second order in WI, hence strongly suppressed NEMO-3 44

2ν Double Beta Decay M(Z,A) -> M(Z+2,A) + 2e - + 2νe Can occur in few tens of nuclei Process is second order in WI, hence strongly NEMO-3 suppressed Measured half-lives (τ1/2) 100 Mo - 7.2 x 10 18 yrs 150 Nd - 9.2 x 10 18 yrs 82 Se - 9.6 x 10 19 yrs 96 Zr - 2.35 x 10 19 yrs 116 Cd - 2.9 x 10 19 yrs 48 Ca - 4.4 x 10 19 yrs 130 Te - 7.0 x 10 20 yrs 76 Ge - 1.7 x 10 21 yrs 44

0ν Double Beta Decay 45

0ν Double Beta Decay M(Z,A) -> M(Z+2,A) + 2e - Can only occur if ν s are Majorana 45

0ν Double Beta Decay M(Z,A) -> M(Z+2,A) + 2e - Can only occur if ν s are Majorana 1/τ 1/2 = G(Q,Z) x M νν (Z,A) 2 x mββ 2 m ββ = Phase space Matrix element Effective mass U 2 m ej j j 45

0ν Double Beta Decay M(Z,A) -> M(Z+2,A) + 2e - Can only occur if ν s are Majorana 1/τ 1/2 = G(Q,Z) x M νν (Z,A) 2 x mββ 2 m ββ = Phase space Matrix element Effective mass U 2 m ej j j Main experimental challenges: Separation of 0ν signal from 2ν Background from radioactivity 45

Comparison of Isotopes M.Pavan and F.Simkovic, Nu2010 46

Comparison of Isotopes Want both of these to be high Want this to be high Want this to be low M.Pavan and F.Simkovic, Nu2010 46

Current Status 47

Current Status Claim for a signal in 76 Ge by a subset of Heidelberg-Moscow Collaboration giving mββ ~.2-.6 ev. Improved analysis now: >6σ, (MPLA 21,1547(2006)). Very controversial. 47

Current Status Claim for a signal in 76 Ge by a subset of Heidelberg-Moscow Collaboration giving mββ ~.2-.6 ev. Improved analysis now: >6σ, (MPLA 21,1547(2006)). Very controversial. NEMO-3 - mββ ~.6-1.4 ev 47

Goals for Next Phase 48

Goals for Next Phase One wants to reach mββ ~10meV 48

Goals for Next Phase One wants to reach mββ ~10meV ~30 lower than the current best limit, ie value of τ1/2 1000 times higher Current targets ~ 10kg 48

Goals for Next Phase One wants to reach mββ ~10meV ~30 lower than the current best limit, ie value of τ1/2 1000 times higher Current targets ~ 10kg Currently (finite background), τ1/2 ~ N 1/2 = M 1/2 a) Better calorimetry Must find ways to reduce background. Need: b) Better tracking c) Identification of daughter d) less radioactivity 48

νʻs in Cosmology and Astrophysics Prediction from cosmology (D.Schramm, 1977): N ν < 5 49

Neutrino Mass 50

Neutrino Mass Neutrino mass affects development of cosmic structures Hence most of the relevant experiments measure matter power spectrum and from it extract limits on m ν 50

Neutrino Mass Neutrino mass affects development of cosmic structures Hence most of the relevant experiments measure matter power spectrum and from it extract limits on m ν Various probes 50

Neutrino Mass Neutrino mass affects development of cosmic structures Hence most of the relevant experiments measure matter power spectrum and from it extract limits on m ν Various probes Galaxy Surveys Weak Lensing Surveys Lyman-α forest measurements Cluster surveys 21cm measurements 50

Neutrino Mass Neutrino mass affects development of cosmic structures Hence most of the relevant experiments measure matter power spectrum and from it extract limits on m ν Various probes CMB (Y.Wong Nu2010) Galaxy Surveys Weak Lensing Surveys Lyman-α forest measurements Cluster surveys 21cm measurements 50

Current Mass Status Y.Wong Neutrino2010 51

Current Mass Status!"#$#%&'$&(&)$*** +,-!.'/%01' 2/3(&$)'#&'(0*'4565 JFK'L*M*')NN#"'0;3;&''''''''''''''''''' +,-!.78(0(91':0)$&#";%< =(%%#$&(>?',;";@@;?'A(BB#0& C'DE+'4565 +,-!F78(0(91' 7GH7=GI A#;>'#&'(0*'455J S#9&#%>#>'3/>#0$T +,-!F7+#(O'0#%$;%< I#"#%/'#&'(0*'455P' Q:R;O;'#&'(0*'455P!! Y.Wong Neutrino2010 51

Supernovas 52

Supernovas Supernovas are spectacular events in which neutrinos play an important role: 52

Supernovas Supernovas are spectacular events in which neutrinos play an important role: Some important characteristics: Peak luminosity ~ luminosity of whole galaxy Total energy ~ 10 56 ergs 99% of energy in neutrinos Neutrino burst lasts ~10 sec Neutrinos come about 3 hrs before visible Expect ~2-3 supernovas/century in our galaxy Details depend on properties of neutrinos 52