Future prospects of neutrino oscillation study Osamu Yasuda Tokyo Metropolitan University April 27, IPMU

Size: px

Start display at page:

Download "Future prospects of neutrino oscillation study Osamu Yasuda Tokyo Metropolitan University April 27, IPMU"

Rebecca Logan
5 years ago
Views:

1 Future prospects of neutrino oscillation study Osamu Yasuda Tokyo Metropolitan University April 7, IPMU 1/68

2 1. Introduction. New Physics probed by experiments 3. Conclusions /68

3 1. Introduction Framework of 3 flavor oscillation Mixing matrix Functions of mixing angles 1, 3, 13, and CP phase e 1 1 solar +KamLAND (reactor) U U U e1 3 mixing angles & m jk U U U e U U U e3 3 3 θ 1 3 have been measured: π 6 5 1, m1 810 ev atm +KK,MINOS(accelerators) π 3 D-CHOOZ+Daya Bay+RENO (reactors), TK+MINOS+NOvA etc θ 3, m ev θ 13 4 Both hierarchy patterns are allowed Normal Hierarchy Inverted Hierarchy / 0 3/68

4 δm m 1 Lisi@BSM in Okinawa 016 4/68

5 Oscillation vs non-oscillation experiments neutrino oscillation m jk =m j -m k neutrinoless double beta decay m ee = (U ej ) m j exp(i j ) direct measurement m =( U ej m j) 1/ cosmology Majorana phases m j 5/68

6 neutrinoless double beta decay m ee = (U ej ) m j exp(i j ) m ee Biller@NuPhys015 ) min(m j Strumia-Vissani: hep-ph/ /68

7 direct measurement m =( U ej m j) 1/ m β Strumia-Vissani: hep-ph/ min(m j ) 7/68

8 Cosmology NUPHYS015 8/68

9 U U e1 U μ1 U τ1 U e U μ U τ U e3 U μ3 U τ3 c1 s / 1 s / 1 s1 c / 1 c / ε / / Next task is to measure sign(m 31 ), /4-3 and sign(m 31 ) : mass hierarchy /4-3 : octant : CP phase These quantities are expected to be determined in future experiments with huge detectors. Both mass hierarchies are allowed 3 1 normal hierarchy 1 3 inverted hierarchy m 0 m /68

10 (1) Determination of sgn(δm 31) ~ ΔE31 ΔE31L P(νμ ν e) s3sin θ13 ~ sin ΔE 31 ΔE ~ ΔE ΔE cosθ A ΔE sinθ Δm /E, A 13 sgn(δm 31 ) G F N e 31 can be deduced 13 1/000km 1/ 0 To identify sgn(δm ) 31, a longer baseline (L>1000km) will be necessary, because AL~ O(1) is necessary. 10/68

11 Future exp. vs Mass Hierarchy Significance () of MH Now PINGU Juno INO -atm DUNE HKatm THK Noa SKatm Year 11/68

12 () Measurement of sin θ Contribution of always comes with sin 13 Measurement of is difficult U c iδ c s s c s c s eiδ 0 c s e c s 1/68

13 Sensitivity to at TK & Noa Huber et al., arxiv: v1 90%CL 13/68

14 Proposed experiments (----) (----) (----) (----) + e THK (JP, JPARCHK) L=95km, E~0.6GeV DUNE (US, FNALHomestake, SD), E ~ GeV, L ~ 1300km 14/68

15 Future plan: THK Extension of TK (large #(events)) 1.66MW beam Hyperkamiokande (300 times KK) (0 times SK) Main purpose: Measurement of CP phase Hyper-kamiokande 15/68

16 Hyperkamiokande (H O:0.5Mt=SKx10, 05(?)-) Precision measurement of oscillation Further search for nucleon decays Precision measurement of supernova (if any) 16/68

17 Atmospheric w/s, MIAPP, Feb /68

18 Nu Frontier W/S, Dec /68

19 Future plan: DUNE.3MW 40-kt Liquid Argon Sanford Underground RF E ~ GeV, L ~ 1300km 19/68

20 CIPANP 015 0/68

21 Sensitivity to at Future LBL experiments THK DUNE Hyper- Kamiokande LOI, arxiv: v 1 [hep-ex] Svoboda@01 1/68

22 In the mean time, TK found e appearance TK Collaboration, Phys.Rev. D91 (015) 7, (Received 6 February 015) /68

23 Result of global analysis in Okinawa 016 3/68

24 We even already have a hint on the value of : = -/ seems to be favored Things are moving faster than we expected! In addition to the standard oscillation scenario, research on New Physics is important to give further motivations for future long baseline experiments. 4/68

25 . New Physics probed by experiments Motivation for research on New Physics High precision measurements of oscillation in future experiments can be used to probe physics beyond SM by looking at deviation from SM+m (like at B factories). Research on New Physics is important. It would give further motivations for THK & DUNE. 5/68

26 Scenario 3 flavor unitarity Phenomenological constraints on the magnitude of the effects Light sterile O(10%) NSI at production / detection O(1%) NSI in propagation e- O(100%) Others: O(1%) Unitarity violation due to heavy particles O(0.1%) 6/68

27 .1 Light sterile neutrinos s.1.1 Motivation for s Sterile neutrinos have been phenomenologically motivated by the following: LSND anomaly Reactor anomaly Galium anomaly Some hint for s from cosmological observations Sterile is not necessarily required from theory 7/68

.1. LSND anomaly LNSD experiment (1993-1998@LANL) e E~50MeV, L~30m Region with N =3 oscillation Δm O(1)eV,

28 .1. LSND anomaly LNSD experiment e E~50MeV, L~30m Region with N =3 oscillation Δm O(1)eV, sin θ O(10 It cannot be explained by N =3 oscillation LEP data N =3 active light 4th must be sterile - )?? 8/68

E~1GeV, L~1km, (L/E) MB =(L/E) LSND Neutrino mode(007) (negative) Antineutrino

29 .1.3 MiniBooNE(00-, FNAL) Aim was to check LSND Karagiorgi, Djurcic, Conrad, Shaevitz, Sorel, Phys.Rev.D80:073001,009. E~1GeV, L~1km, (L/E) MB =(L/E) LSND Neutrino mode(007) (negative) Antineutrino mode(010) (Affirmative) e e e 1995 Is LSND true? 007 LSND was wrong! 010 LSND was true? Sterile neutrino oscillation!? 9/68

30 .1.4 Reactor anomaly Recent reevaluation of reactor flux suggests affirmative interpretation of oscillation (new flux)= (old flux) x 1.03 Bugey(reactor ): Negative w/ old flux : Mention et al, PRD83 (011) Bugey(reactor)+etc: Affirmative w/ new flux? : Allowed region@90%cl Allowed region@90%cl No oscillation for Δm41 O(1)eV oscillation may exist for Δm41 O(1)eV 30/68

.1.5 Galium anomaly SAGE, nucl-ex/051041 Calibration of Ga solar

90% 68% Giunti-Laveder, 1006.344v3 [hep-ph] Results of Ga solar exp.

31 .1.5 Galium anomaly SAGE, nucl-ex/ Calibration of Ga solar experiments Gallex/GNO 51 Cr SAGE 51 Cr, 37 Ar Gallex SAGE 99% 95% 90% 68% Giunti-Laveder, v3 [hep-ph] Results of Ga solar exp. can be interpreted as e disappearance due to active-sterile oscillation 31/68

32 .1.6 3/68

33 .1.7 Cosmological Observation (CMB+LSS) N >3? Before Planck 013 After Planck 013 There seems to be conflict between cosmological observations It may be premature to conclude N =3 (or N >3). Planck 013 results. XVI, Cosmological parameters, arxiv: v1 33/68

34 .1.7 Cosmological Observation(Planck013) Is s oscillation dead? sin θ 14 ( e ) e sin θ 4 ( μ) μ Mirizzi, Mangano, Saviano, Borriello, Giunti, Miele, Pisanti, arxiv: Even if the negative result of Planck013 is confirmed, it is still possible that s has never been in thermal equilibrium due to lepton asymmetry s oscillation is still possible 34/68

35 .1.8 Oscillation with N =4 schemes Because of the hierarchy: Δm sol Δm atm Δm LSND N =3 schemes can t explain LSND. Δm 1Δmsol,Δm3 Δmatm N =4 schemes may be able to explain all. LEP 4 th has to be sterile Δm 1Δmsol,Δm3 Δmatm,Δm43 ΔmLSND 35/68

36 Matter effects of neutrinos The term which is proportional to identity can be ignored 36/68

37 Matter effects of neutrinos e, s CC NC V A e A n N = framework A 0 n A e n e G A (1/ F ΔA ΔA N e )G A ΔA 0 e A s n F N n 37/68

38 (+)-scheme η η s s ν ν U atm U sol s1 : s1 : ν ν μ e U U s s ν ν s s 1 0 (100%) Strongly disfavored by SK atm data (100%) Strongly disfavored by SNO sol data Δχ Maltoni et al., hep-ph/ global solar + KamLAND η s atmospheric χ PG χ PC PC: parameter consistency test PG: parameter goodness-of-fit test For any value of U s1 + U s, fit to sol+atm data is bad. 38/68

39 .1.8. (3+1)-scheme Bugey (reactor): negative sin θ Bugey 4 U e4 (1 U e4 ) CDHSW (accelerator): negative 4 U e4 sin θ CDHSW 4 U 4 (1 U 4 ) 4 U 4 LSND (accelerator): affirmaive : sinθ LSND 4U e4 U 4 must be satisfied but there is no overlap between the left side of Bugey+CDHSW and the inside of LSND (Okada-OY Int.J.Mod.Phys.A1:3669,1997) 39/68

40 Palazzo, July /68

41 (3+)-scheme: With kinds sterile, fit improves a little, but not much. Kopp-Maltoni-Schwetz, arxiv: v [hep-ph] LSND LSND atm solar (3+)-scheme is consistent w/ all the 97%CL; other scenarios fit even worse) 41/68

42 MLF 4/68

43 MLF Spokesperson: Takasumi Maruyama 43/68

44 .1.9 Deficit due to s oscillations In flavor s oscillation framework i d dx ν E 0 μ ν U U ν s 0 E 0 An νs μ A (1/ n )G F N n If N n =const. ~ tanθ P( ν μ ν ~ ΔE n ΔE sinθ ΔEcosθ A n s ) sin ~ θ sin (ΔE cosθ A ) (ΔE sinθ) 1/ ~ ΔEL For m ~10eV, θ ~ =/4 at E ~ 10TeV 44/68

45 flavor s oscillation framework Nicolaidis, Tsirigoti, Hansson, hepph/ /68

46 (+)-scheme OY, hep-ph/ /68

47 (+)-scheme & (3+1)-scheme Nunokawa, Peres, Zukanovich-Funchal, hep-ph/ /68

48 ICECUBE 48/68

49 . Nonstandard scenarios () Motivation for Non Standard Interactions Theoretical motivation is phenomenological, but its discovery would give a clue to physics beyond Standard Model. There seems to be slight tension between the solar and KamLAND ; another tension between recent measurement of 13 of D-CHOOZ & Daya Bay + RENO. it may be a hint for either NSI in propagation (production/detection) or s Some models exist: NSI due exchange by light (MeV scale mass) mediators with small couplings allow to avoid existing bounds Farzan, Shoemaker, arxiv: /68

50 ..1 New Physics at source and detector Possible processes with charged current Grossman, Phys. Lett. B359, 141 (1995) NSI at production f Effective eigenstate f U s NSI at detection SM: U NP: U s U Effective eigenstate U d SM: U NP: U d U 50/68

51 Direct bounds on prod/det NSI From decays and zero distance oscillations l P u P d ud G L F L, R G F e P P e L L ud e Bounds ~O(10 - ) C. Biggio, M. Blennow and EFM E. NSI workshop at UAM /68

52 Moriond016 This may be a hint for NSI in production / detection or s 5/68

53 .. New Physics in propagation (matter effect) f f SM potential due to W exchange is modified by NP SM NP 53/68

54 Constraints on for experiments on Earth Davidson et al., JHEP 0303:011,003; Berezhiani, Rossi, PLB535 ( 0) 07; Barranco et al., PRD73 ( 06) ; Barranco et al., arxiv: Biggio et al., JHEP 0908, 090 (009) w/o 1-loop arguments Constraints are weak ee, e, ~O(1) are consistent with accelerator experiments data 54/68

55 Probability for solar P(ν e ν ) e Probability for solar is expressed in terms of the initial and final mixing angles, and depends on E through the initial mixing angle. ~ cos (0) ΔE Δm /E A G F n e (x) Mixing angle at production point (t=0) Matter potential at production point (t=0, i.e., in the center on the Sun) 55/68

56 up-turn of solar Due to no observation of MSW up-turn of solar Gonzalez-Garcia, Maltoni, arxiv: v1 [hep-ph] This may be a hint for NSI in propagation 56/68

57 up-turn of solar Better fit with sterile Maltoni, Smirnov, arxiv: v [hep-ph] This may be a hint for s 57/68

58 Constraints on NSI from high energy behavior of atm data Oki-OY PRD8 ( 10) Standard case with N = Standard case with N =3 = Deviation of 1-P( ) due to NSI contradicts with data c 1 c High energy atm data is well described by standard scheme constraints on NSI: c 0 1, c /68

59 with NSI c c c 0 1 e <<1, <<1, <<1 <<1: Shown by Fornengo et al. PRD65, , 0; Gonzalez-Garcia&Maltoni, PRD70, , 04; Mitsuka@nufact08 <<1: Shown from other expts. by Davidson et al. JHEP 0303:011, 03 e <<1: Shown by Oki-OY PRD8 ( 10) e c ee Shown by Friedland-Lunardini, PRD7:053009, 05 59/68

60 Summary of the constraints on To a good approximation, we are left with 3 independent variables ee, e, arg( e ): Furthermore, atm data implies tan e /(1+ ee ) Friedland-Lunardini, PRD7:053009, 05 Allowed region in ee, e 60/68

Constraint by SK atm on ee, e Best fit std Fukasawa-OY (arxiv:1503.08056) The standard case ( =0) is not best fit point (1.4).

61 Constraint by SK atm on ee, e Best fit std Fukasawa-OY (arxiv: ) The standard case ( =0) is not best fit point (1.4). This may be because we have been unable to reproduce SK MC results completely. The.5 excluded region (tan<0.8) improves the old one (tan<1.5) by Friedland-Lunardini in /68

62 Fukasawa-OY (arxiv: ) Best fit std 6/68

63 Sensitivity of HK atm to ee, e (1) Rate analysis Fukasawa-OY arxiv #(events) HK = 0 x #(events) SK std=best fit The region e >1.5 is excluded. The.5 excluded region is tan < /68

Fukasawa-OY arxiv.1503.08056 The case of IH has a much larger allowed region.

64 Fukasawa-OY arxiv The case of IH has a much larger allowed region. This may be because the resonance occurs for the channel which has less #(events) than 64/68

Sensitivity of HK atm () Spectrum analysis Fukasawa-OY arxiv.1503.

65 Sensitivity of HK atm () Spectrum analysis Fukasawa-OY arxiv With the information of the energy spectrum, the allowed region becomes much smaller (Note the difference in scale). The.5 excluded region is tan < /68

66 Sensitivity of HK atm (3) Spectrum analysis in the presence of NSI Fukasawa-OY arxiv Relatively good sensitivity to NSI for ee < 66/68

67 Sensitivity of HK atm (4) Implication to solar If the deviation of the up-turn behavior of the solar is due to NSI in propagation, there is a chance to see it in atmospheric observation at HK with great significance. Fukasawa-OY work in progress 67/68

68 6. Summary (1) From various oscillation experiments, 3 mixing angles and mass squared difference have been determined. Undetermined parameters are & sign(m 31). Future experiments are planned to determine & sign(m 31). Just like the B factories, we can probe physics beyond SM by looking at deviation from SM+m 68/68

69 6. Summary () New physics beyond SM includes sterile, NSI, unitarity violation. At present there are a few anomalies: (i) LSND-MiniBooNE-reactor-Gallium anomaly (ii) Tension between solar & KamLAND (iii) Tension between D-CHOOZ &DB+RENO These anomalies can be tested in the future experiments. 69/68

70 Backup slides 70/68

71 in Okinawa /68

72 in Okinawa 016 NOvA analysis LID: a likelihoodbased selector LEM: Library Event Matching 7/68

73 Nova appearance: POT 6 events observed Nova Collaboration, Phys.Rev.Lett. 116 (016) LID: a likelihood-based selector LEM: Library Event Matching 73/68

74 Nova appearance: POT 6 events observed Nova Collaboration, Phys.Rev.Lett. 116 (016) 74/68

75 A likelihood-based selector (LID): compares the longitudinal and transverse energy deposition in the primary shower to template histograms for various simulated particles The likelihood differences among different particle hypotheses and other topological variables are used as input to an articial neural network to construct the primary classier. The energy range of events selected with this primary method is further restricted to 1.5 to.7 GeV to remove additional backgrounds from cosmic radiation. Library Event Matching (LEM): compares an input event from either data or simulation to a large and independent library of simulated events. The properties of the library events that are most similar to the input event provide information about the most likely identity of the neutrino interaction. This and additional identifying information from the best matches in the library is fed into an ensemble decision tree that gives the nal classier for this technique. 75/68

76 Nova disappearance: POT Nova Collaboration, Phys. Rev. D 93, (R) (016) 76/68

77 Nova disappearance: POT Nova Collaboration, Phys. Rev. D 93, (R) (016) 77/68

78 TK disappearance: POT 34 fully contained -like events TK Collaboration, arxiv: v1 [hep-ex] 78/68

79 TK appearance/disappearance: POT TK Collaboration, Phys. Rev. D 91, (015) 79/68

Searching for non-standard interactions at the future long baseline experiments

Searching for non-standard interactions at the future long baseline experiments Osamu Yasuda Tokyo Metropolitan University Dec. 18 @Miami 015 1/34 1. Introduction. New Physics in propagation 3. Sensitivity