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

Transcription

1 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

2 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

3 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

4 3-flavor Analyses 27

5 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

6 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

7 Summary (Mixed) Oscillation analysis sin 2 θ13 (value) sin 2 θ13 (90% CL) SuperK (atmospheric,norm) <0.066 SuperK (atmospheric,inv) SuperK (solar,global) <0.122 sin 2 θ13 (95% CL) <0.059 sin 2 θ SNO (solar,global) <0.057 MINOS (normal) at δcp=0 MINOS (inverted) at δcp= < <0.05 CHOOZ <0.037 CHOOZ limit 28

8 Global 3-flavor fit 29

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

10 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 v3 29

11 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 v3 Parameter best fit 2σ 3σ Δm 2 21 [10-5 ev 2 ] Δm 2 31 [10-3 ev 2 ] sin 2 θ sin 2 θ sin 2 θ <0.039 <

12 Quark/Lepton Comparison 30

13 Quark/Lepton Comparison Mixing Angles 30

14 Quark/Lepton Comparison Mixing Angles CKM Matrix, graphically 30

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

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

17 Quark/Lepton Comparison Mixing Angles 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

18 LSND Effect R. Van de Water Nu

19 LSND Effect Apparent ν μ -> νe transition R. Van de Water Nu

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

21 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 Nu

22 MiniBooNE 32

23 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

24 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

25 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) Both neutrino and antineutrino exposures were obtained Antineutrino run tests the LSND directly 32

26 MiniBooNE Results R. Van de Water Nu

27 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 Nu

28 MiniBooNE Results Neutrinos - 6.5E20 POT Antineutrinos E20 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 Nu

29 MiniBooNE Results Neutrinos - 6.5E20 POT Antineutrinos E20 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 10E20 POT in ν mode requested to resolve the issue R. Van de Water Nu

30 MINOS ν Result P.Vahle Neutrino

31 MINOS ν Result MINOS took 1.7E20 protons on target in ν μ mode P.Vahle Neutrino

32 MINOS ν Result MINOS took 1.7E20 protons on target in ν μ mode Δm 2 = ev 2 sin 2 (2θ) = 0.86 ± 0.11 P.Vahle Neutrino

33 MINOS ν Result MINOS took 1.7E20 protons on target in ν μ mode Δm 2 = ev 2 sin 2 (2θ) = 0.86 ± 0.11 P.Vahle Neutrino

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

35 ν/ν in the Solar Sector 35

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

37 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

38 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

39 Neutrino Masses ν 36

40 2 Questions re ν Mass 37

41 2 Questions re ν Mass The question of neutrino masses focuses on 2 related questions: 37

42 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

43 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

44 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

45 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

46 Mass from β Decay 39

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

48 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 KeV, T1/ yrs Current mass limit - 39

49 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 KeV, T1/ yrs Current mass limit - Experimental challenges: Statistics Resolution Control of Systematics 39

50 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 KeV, T1/ yrs Current mass limit - Experimental challenges: Statistics Resolution Control of Systematics 39

51 KATRIN - The Last Hurrah 40

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

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

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

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

56 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: (2009). Uniform B field Low pressure T2 gas. B field Antenna array for cyclotron radiation detection. T 2 gas J.Formaggio, Neutrino

57 Comparison with other ways from S.Parke Nu

58 Comparison with other ways Kinematics of Decay from S.Parke Nu

59 Comparison with other ways Kinematics of Decay Cosmology from S.Parke Nu

60 Comparison with other ways Kinematics of Decay Cosmology Double Beta Decay from S.Parke Nu

61 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 Nu

62 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 The measured mass parameter is different for the three different classes of experiments from S.Parke Nu

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

64 2ν Double Beta Decay 44

65 2ν Double Beta Decay M(Z,A) -> M(Z+2,A) + 2e - + 2νe 44

66 2ν Double Beta Decay M(Z,A) -> M(Z+2,A) + 2e - + 2νe Can occur in few tens of nuclei 44

67 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

68 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

69 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

70 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 x yrs 150 Nd x yrs 82 Se x yrs 96 Zr x yrs 116 Cd x yrs 48 Ca x yrs 130 Te x yrs 76 Ge x yrs 44

71 0ν Double Beta Decay 45

72 0ν Double Beta Decay M(Z,A) -> M(Z+2,A) + 2e - Can only occur if ν s are Majorana 45

73 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

74 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

75 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 2ν mode 0ν mode 45

76 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 2ν mode 0ν mode 2ν/0ν ~ (for mββ = 50 mev) 45

77 Comparison of Isotopes M.Pavan and F.Simkovic, Nu

78 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, Nu

79 Current Status 47

80 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

81 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 ~ ev 47

82 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 ~ ev Cuoricino - mββ ~.3-.7 ev 47

83 Goals for Next Phase 48

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

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

86 Goals for Next Phase One wants to reach mββ ~10meV ~30 lower than the current best limit, ie value of τ1/ times higher Current targets ~ 10kg Currently (finite background), τ1/2 ~ N 1/2 = M 1/2 48

87 Goals for Next Phase One wants to reach mββ ~10meV ~30 lower than the current best limit, ie value of τ1/ 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

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

89 Neutrino Mass 50

90 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

91 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

92 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

93 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

94 Current Mass Status Y.Wong Neutrino

95 Current Mass Status!"#$#%&'$&(&)$*** +,-!.'/%01' 2/3(&$)'#&'(0*'4565 JFK'L*M*')NN#"'0;3;&''''''''''''''''''' +,-!.78(0(91':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 Neutrino

96 Supernovas 52

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

98 Supernovas Supernovas are spectacular events in which neutrinos play an important role: Some important characteristics: Peak luminosity ~ luminosity of whole galaxy Total energy ~ 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

99 Supernovas Supernovas are spectacular events in which neutrinos play an important role: Some important characteristics: Peak luminosity ~ luminosity of whole galaxy Total energy ~ 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 One recent visible supernova, SN1987a, 51.4 kpsec away 52

100 Supernovas Supernovas are spectacular events in which neutrinos play an important role: Some important characteristics: Peak luminosity ~ luminosity of whole galaxy Total energy ~ 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 One recent visible supernova, SN1987a, 51.4 kpsec away Expect ~10,000 evts in SuperK, wealth of information re νʻs 52