Neutrinos: Yesterday, Today and Tomorrow. Stanley Wojcicki SLAC Summer Institute 2010 August 13, 2010

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1 Neutrinos: Yesterday, Today and Tomorrow August 13,

2 My Marching Orders 2

3 My Marching Orders...the summary talk should be visionary, rather than a dedicated summary of the SSI program. 2

4 My Marching Orders...the summary talk should be visionary, rather than a dedicated summary of the SSI program. He s a visionary 2

5 Neutrinos are Ubiquitous 3

6 Neutrinos are Ubiquitous They are made by nature: In the Big Bang By the elements in the earth, air, and water By the sun and other stars In the explosion of supernovae By the cosmic rays 3

7 Neutrinos are Ubiquitous They are made by nature: In the Big Bang By the elements in the earth, air, and water By the sun and other stars In the explosion of supernovae By the cosmic rays And they are made by humans: In power plants (reactors) In decays of artificially produced isotopes In the accelerators In nuclear bombs 3

8 Neutrinos are Ubiquitous They are made by nature: In the Big Bang By the elements in the earth, air, and water By the sun and other stars In the explosion of supernovae By the cosmic rays And they are made by humans: In power plants (reactors) In decays of artificially produced isotopes In the accelerators In nuclear bombs 3

9 Energy spectra T.Montaruli SSI2010 4

10 Energy spectra Accelerators T.Montaruli SSI2010 4

11 Outline 5

12 Outline Historical Background 5

13 Outline Historical Background The ν Standard Model Experimental Evidence Potential Problems 5

14 Outline Historical Background The ν Standard Model Experimental Evidence Potential Problems The Issue of ν Mass 5

15 Outline Historical Background The ν Standard Model Experimental Evidence Potential Problems The Issue of ν Mass Double β Decay 5

16 Outline Historical Background The ν Standard Model Experimental Evidence Potential Problems The Issue of ν Mass Double β Decay ν s in Cosmology and Astrophysics 5

17 Outline Historical Background The ν Standard Model Experimental Evidence Potential Problems The Issue of ν Mass Double β Decay ν s in Cosmology and Astrophysics LHC and Neutrinos 5

18 Outline Historical Background The ν Standard Model Experimental Evidence Potential Problems The Issue of ν Mass Double β Decay ν s in Cosmology and Astrophysics LHC and Neutrinos Practical Applications? 5

19 Outline Historical Background The ν Standard Model Experimental Evidence Potential Problems The Issue of ν Mass Double β Decay ν s in Cosmology and Astrophysics LHC and Neutrinos Practical Applications? Key Outstanding Questions, Future 5

20 Evolution of ν Studies 6

21 Evolution of ν Studies I. The Beginnings The Key Experiments 6

22 Evolution of ν Studies I. The Beginnings The Key Experiments II. Neutrinos as a Probe The Structure Functions Establishing the Standard Model 6

23 Evolution of ν Studies I. The Beginnings The Key Experiments II. Neutrinos as a Probe The Structure Functions Establishing the Standard Model III. Nature of Neutrinos and Probe The Intrinsic Properties The Oscillation Parameters Studies of Cosmos and the Earth 6

24 Pauli Conjecture 7

25 Pauli Conjecture I have hit upon a desperate remedy to save the "exchange theorem" of statistics and the law of conservation of energy. Namely, the possibility that in the nuclei there could exist electrically neutral particles, which I will call neutrons, that have spin 1/2 and obey the exclusion principle and that further differ from light quanta in that they do not travel with the velocity of light. Zurich, December 4,

26 Pauli Conjecture I have hit upon a desperate remedy to save the "exchange theorem" of statistics and the law of conservation of energy. Namely, the possibility that in the nuclei there could exist electrically neutral particles, which I will call neutrons, that have spin 1/2 and obey the exclusion principle and that further differ from light quanta in that they do not travel with the velocity of light. Zurich, December 4, 1930 Iʼve done a terrible thing today, something which no theoretical physicist should ever do. I have suggested something that can never be verified experimentally...". Pauli in a letter to Baade 7

27 Pauli Conjecture I have hit upon a desperate remedy to save the "exchange theorem" of statistics and the law of conservation of energy. Namely, the possibility that in the nuclei there could exist electrically neutral particles, which I will call neutrons, that have spin 1/2 and obey the exclusion principle and that further differ from light quanta in that they do not travel with the velocity of light. Zurich, December 4, 1930 Iʼve done a terrible thing today, something which no theoretical physicist should ever do. I have suggested something that can never be verified experimentally...". Pauli in a letter to Baade Is this the situation today with the leptogenesis? 7

28 The Key Experiments (1) 8

29 The Key Experiments (1) I. The First Observation of Neutrinos C.L.Cowan,Jr., F.Reines, et al., Science 124, 103 (1956) Double coincidence method (reactor νʼs): ν + p e + + n, followed by n capture Free neutrinos exist! 8

30 The Key Experiments (1) I. The First Observation of Neutrinos C.L.Cowan,Jr., F.Reines, et al., Science 124, 103 (1956) Double coincidence method (reactor νʼs): ν + p e + + n, followed by n capture Free neutrinos exist! II. The Determination of Helicity of Neutrinos M.Goldhaber, L.Grodzins and A.Sunyar, Phys. Rev. 109, 1015 (1958) Neutrinos are lefthanded! Weak interactions are V-A, not S/T! 8

31 The Key Experiments (2) 9

32 The Key Experiments (2) III. The 2-Neutrino Experiment.Danby et al., Phys. Rev. Lett. 9, 36 (1962) Neutrinos from π decay do not produce electrons There are two neutrinos! 9

The Key Experiments (2) III. The 2-Neutrino Experiment.Danby et al., Phys. Rev. Lett. 9, 36 (1962) Neutrinos from π decay do not produce electrons There are two neutrinos!

33 The Key Experiments (2) III. The 2-Neutrino Experiment.Danby et al., Phys. Rev. Lett. 9, 36 (1962) Neutrinos from π decay do not produce electrons There are two neutrinos! IV. The Observation of Neutral Currents D.C.Cundy et al., Phys. Lett. 31B, 478 (1970) ν µ + e e + ν µ, Cannot proceed via W exchange Neutral Currents (Z 0 ) must exist! 9

34 Standard Model 10

35 Standard Model 3 of the 12 Fundamental Constituents of Matter 10

36 Anomalies: 80ʼs, early 90ʼs 11

37 Anomalies: 80ʼs, early 90ʼs Several anomalies in neutrino physics 11

38 Anomalies: 80ʼs, early 90ʼs Several anomalies in neutrino physics Solar neutrino puzzle Deficit (factor of ~3) in number of solar neutrinos observed in Davisʼs experiment 11

39 Anomalies: 80ʼs, early 90ʼs Several anomalies in neutrino physics Solar neutrino puzzle Deficit (factor of ~3) in number of solar neutrinos observed in Davisʼs experiment Atmospheric neutrino anomaly Deficit of ν μʻs in atmospheric neutrinos 11

40 Anomalies: 80ʼs, early 90ʼs Several anomalies in neutrino physics Solar neutrino puzzle Deficit (factor of ~3) in number of solar neutrinos observed in Davisʼs experiment Atmospheric neutrino anomaly Deficit of ν μʻs in atmospheric neutrinos LSND effect Suggestion of ν μ -> ν e transition 11

41 Anomalies: 80ʼs, early 90ʼs Several anomalies in neutrino physics Solar neutrino puzzle Deficit (factor of ~3) in number of solar neutrinos observed in Davisʼs experiment Atmospheric neutrino anomaly Deficit of ν μʻs in atmospheric neutrinos LSND effect Suggestion of ν μ -> ν e transition All suggest possibility of oscillation 11

42 Theoretical scepticism 12

43 Theoretical scepticism Theoretical views: The pattern of the charged lepton mass ratios is not very much different from that of the quark mass ratios... expect mixing angles to be somehow related to fermion masses. 12

44 Theoretical scepticism Theoretical views: 1000 lb Gorilla The pattern of the charged lepton mass ratios is not very much different from that of the quark mass ratios... expect mixing angles to be somehow related to fermion masses. CKM Matrix, graphically 12

45 Theoretical scepticism Theoretical views: 1000 lb Gorilla The pattern of the charged lepton mass ratios is not very much different from that of the quark mass ratios... expect mixing angles to be somehow related to fermion masses. AND CKM Matrix, graphically 12

46 Theoretical scepticism Theoretical views: 1000 lb Gorilla The pattern of the charged lepton mass ratios is not very much different from that of the quark mass ratios... expect mixing angles to be somehow related to fermion masses. AND Any unbiased observer who has not been brainwashed by speculations concerning supersymmetry, axions, or galaxy formation would conclude that the leading suspect in the dark matter puzzle must be the light neutrino at the relevant mass range of ev. CKM Matrix, graphically 12

47 Theoretical scepticism Theoretical views: 1000 lb Gorilla The pattern of the charged lepton mass ratios is not very much different from that of the quark mass ratios... expect mixing angles to be somehow related to fermion masses. AND Any unbiased observer who has not been brainwashed by speculations concerning supersymmetry, axions, or galaxy formation would conclude that the leading suspect in the dark matter puzzle must be the light neutrino at the relevant mass range of ev. CKM Matrix, graphically Most likely the solar neutrino problem has nothing whatsover to do with particle physics. It is a great triumph that astrophysicists are able to predict the number of B 8 neutrinos coming from the sun... within a factor of 2 or 3. 12

48 The Phase Transition 13

49 The Phase Transition une 5, 1998 Takayama 13

50 The Phase Transition une 5, 1998 Takayama 13

51 The Phase Transition une 5, 1998 Takayama 13

52 The ν Standard Model 14

53 The Formalism 15

54 The Formalism The neutrino mass states and flavor states are related by: 15

55 The Formalism The neutrino mass states and flavor states are related by: Atmospheric Subdominant Solar Double β Decay L/E ~ 500 km/gev L/E ~ 15 km/mev Δm 2 31 Δm

56 The Formalism The neutrino mass states and flavor states are related by: Atmospheric Subdominant Solar Double β Decay L/E ~ 500 km/gev L/E ~ 15 km/mev Δm 2 31 Δm flavor approximation is often adequate 15

57 SNO Experiment 16

58 SNO Experiment 1000 tons of D2O in a nickel mine 2092 m underground 16

59 SNO Experiment 1000 tons of D2O in a nickel mine 2092 m underground Separation is done on a statistical basis 16

60 SNO Experiment Φe Φµτ + Φe.154Φµτ+Φe 1000 tons of D2O in a nickel mine 2092 m underground Separation is done on a statistical basis Three measurements (CC, NC, ES) of two quantities (Φe,Φµτ) 16

61 KamLAND 17

62 KamLAND 1 kton liquid scintillator 30% photocathode coverage at 2700 m.w.e. depth 17

63 KamLAND It takes advantage of the former Kamioka cavern that is surrounded by reactors, typically ~180 km away 1 kton liquid scintillator 30% photocathode coverage at 2700 m.w.e. depth 17

64 KamLAND It takes advantage of the former Kamioka cavern that is surrounded by reactors, typically ~180 km away 1 kton liquid scintillator 30% photocathode coverage at 2700 m.w.e. depth 17

65 KamLAND/Solar 18

66 KamLAND/Solar Solar includes all solar experiments (3 phases of SNO, SuperKamiokande, Chlorine, Gallium and Borexino) 18

67 KamLAND/Solar Solar includes all solar experiments (3 phases of SNO, SuperKamiokande, Chlorine, Gallium and Borexino) 2ν model Some tension between 2 results in 2-flavor approximation 18

68 KamLAND/Solar Solar includes all solar experiments (3 phases of SNO, SuperKamiokande, Chlorine, Gallium and Borexino) 2ν model 3ν model Some tension between 2 results in 2-flavor approximation Inclusion of θ13 increases contours, gives small non-zero value of θ13 18

69 MINOS E ν Spectrum 19

70 MINOS E ν Spectrum Neutrino beam produced at Fermilab Near Detector - 1 km from the target Far Detector km away and 710 m underground 19

71 MINOS E ν Spectrum Neutrino beam produced at Fermilab Near Detector - 1 km from the target Far Detector km away and 710 m underground The flux is measured in the Near Detector and then extrapolated to obtain prediction in the Far Detector 19

72 MINOS E ν Spectrum Neutrino beam produced at Fermilab Near Detector - 1 km from the target Far Detector km away and 710 m underground The flux is measured in the Near Detector and then extrapolated to obtain prediction in the Far Detector 19

MINOS E ν Spectrum Neutrino beam produced at Fermilab Near Detector - 1 km from the target Far Detector - 735 km away and

73 MINOS E ν Spectrum Neutrino beam produced at Fermilab Near Detector - 1 km from the target Far Detector km away and 710 m underground The flux is measured in the Near Detector and then extrapolated to obtain prediction in the Far Detector 19

74 SuperKamiokande 20

75 SuperKamiokande 50 kt of water 42m high, 40 m diam 40% PMT coverage 1000m underground 20

76 SuperKamiokande electron fuzzy edges 50 kt of water 42m high, 40 m diam 40% PMT coverage 1000m underground muon sharp edges 20

77 SuperKamiokande electron fuzzy edges 50 kt of water 42m high, 40 m diam 40% PMT coverage 1000m underground muon sharp edges Zenith angle and L/E distributions are used to extract oscillation parameters 20

78 SuperKamiokande Example distributions electron fuzzy edges Upward Downward 50 kt of water 42m high, 40 m diam 40% PMT coverage 1000m underground muon sharp edges Zenith angle and L/E distributions are used to extract oscillation parameters Upward Downward -1 cosθzenith +1 20

79 SuperK/MINOS Y.Takeuchi Neutrino

80 SuperK/MINOS 2 flavor analysis All SK data (I, II, and III) are used Y.Takeuchi Neutrino

81 SuperK/MINOS 2 flavor analysis All SK data (I, II, and III) are used MINOS does better on Δm 2 determination Y.Takeuchi Neutrino

82 SuperK/MINOS 2 flavor analysis All SK data (I, II, and III) are used MINOS does better on Δm 2 determination SuperK does better on the mixing angle Y.Takeuchi Neutrino

83 OPERA 22

84 OPERA First candidate νμ -> ντ τ - -> π - + π 0 22

85 Sterile ν, MINOS 23

86 Sterile ν, MINOS Spectrum of NC events in FD P.Vahle Neutrino

87 Sterile ν, MINOS Spectrum of NC events in FD Expect (no νe): 757 events Observe: 802 events No depletion seen P.Vahle Neutrino

88 Sterile ν, MINOS Spectrum of NC events in FD Expect (no νe): 757 events Observe: 802 events No depletion seen Limit on fraction, fs, of oscillated ν μ converting to ν s assuming no νe or νe at CHOOZ limit: f s P ν µ ν s 1 P νµ ν µ < 0.22 (0.40) at 90% C.L. P.Vahle Neutrino

89 Mixed (Subdominant) Sector 24

90 Mixed (Subdominant) Sector 3 distinct approaches can be used 24

91 Mixed (Subdominant) Sector 3 distinct approaches can be used Reactor experiments (disappearance): Simple analysis - only θ13 dependence But subtract two large numbers; systematics 24

92 Mixed (Subdominant) Sector 3 distinct approaches can be used Reactor experiments (disappearance): Simple analysis - only θ13 dependence But subtract two large numbers; systematics Accelerator experiments (appearance): Dependance also on θ23, mass hierarchy, δcp 24

Mixed (Subdominant) Sector 3 distinct approaches can be used Reactor experiments (disappearance): Simple analysis - only θ13 dependence But subtract two large numbers;

93 Mixed (Subdominant) Sector 3 distinct approaches can be used Reactor experiments (disappearance): Simple analysis - only θ13 dependence But subtract two large numbers; systematics Accelerator experiments (appearance): Dependance also on θ23, mass hierarchy, δcp Atmospheric and solar experiments: Look for small effects in 3-flavor analyses 24

94 Reactors - CHOOZ limit 25

95 Reactors - CHOOZ limit Previous reactor experiments showed no depletion of neutrino flux, signature of oscillations 25

96 Reactors - CHOOZ limit Previous reactor experiments showed no depletion of neutrino flux, signature of oscillations Previous experiments Atmospheric sector optimum distance KamLAND Solar sector oscillation curve 25

97 Reactors - CHOOZ limit Previous reactor experiments showed no depletion of neutrino flux, signature of oscillations Previous experiments CHOOZ Spectra Atmospheric sector optimum distance KamLAND Solar sector oscillation curve 25

98 Reactors - CHOOZ limit Previous reactor experiments showed no depletion of neutrino flux, signature of oscillations Previous experiments CHOOZ Spectra CHOOZ Limits Atmospheric sector optimum distance KamLAND Solar sector oscillation curve MINOS Δm 2 value 25

99 Reactors - CHOOZ limit Previous reactor experiments showed no depletion of neutrino flux, signature of oscillations Previous experiments CHOOZ Spectra CHOOZ Limits Atmospheric sector optimum distance KamLAND Solar sector oscillation curve MINOS Δm 2 value CHOOZ limit: sin 2( 2θ13)<0.15 (90% C.L.) (at Δm 2 31 = 2.3 x 10-3 ev 2 ) 25

100 MINOS Result 26

Neutrino Experiments: Lecture 2 M. Shaevitz Columbia University

Neutrino Experiments: Lecture 2 M. Shaevitz Columbia University 1 Outline 2 Lecture 1: Experimental Neutrino Physics Neutrino Physics and Interactions Neutrino Mass Experiments Neutrino Sources/Beams and