Neutrino Oscillation Physics
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1 Experimental Neutrino Oscillation Physics XL International Meeting on Fundamental Physics Pau Novella CIEMAT 1
2 Overview Neutrino Oscillation physics Measuring the oscillation The first generation The precision generation The latest mixing angle What's next? All in all... 2
3 Neutrino Oscillation Physics 3
4 In the beginning Pauli postulates 1956: reactor neutrinos detected 1990's: neutrino oscillations... Physics Beyond the Standard Model... Today Reactors play a major role again! 4
5 Neutrino mixing νe m1 νµ m2 ντ m3 Oscillation physics Atmospheric sector θ23 interference sector θ13, δ Solar sector θ12 5
6 Neutrino Oscillations If neutrinos are massive and have different masses... Oscillation parameters: ( 12, 13, 3), ( m221, m231), If θ13 small and m221 << m232 : amplitude P αβ =sin 2 2θ sin 2 frequency ( Δm2 L 4 E ν Posc ) 6
7 Measuring The Oscillation 7
8 Neutrino Sources matm, atm msol, sol Δmij2 mi2-mj2 8
9 Neutrino Energies 9
10 Hunting neutrinos Radiochemical experiments: Homestake, Gallex,... MINOS Cherenkov: SuperKamiokande, MiniBooNE,... Scintillator calorimeters: KamLAND, Double Chooz.. Tracking calorimeters: MINOS, NOvA, LAr TPCs: ICARUS, MicroBooNE Emulsions: OPERA KamLAND SuperK ICARUS 10
11 Setting up the experiment Comparison with no-oscillation expectation Known flux before oscillation (Or prediction) FD ND 2 P αβ =sin 2θ sin 2 ( Δm2 L 4 E ν ) 11
12 The first Generation 12
13 The Solar Sector Solar experiments: Radiochemical experiments: Homestake, Gallex,... Water cherenkov: SuperKamiokande Heavy water: SNO Liquid scintillator: Borexino 33-50% lower flux than the theoretical predictions since 1968 Reactor experiment: KamLAND oscillation confirmed Oscillarion parameters measured 13
14 The Atmospheric Sector Atmospheric neutrinos Atmospheric experiments: SuperKamiokande Accelerator experiments: K2K, MINOS E~GeV, L ~100km 14
15 Interference sector: SBL Reactor experiments Past reactor experiments... Phys. Rev. Lett. 90, (2003) Gratta et Al. Rev. Mod. Phys, 74, 2002 solar Measurement of reactor flux From CHOOZ: sin2(2 13) <
16 Summary of the 1st Generation 16
17 Global Analysis in 2008 m2atm atm) Minos and Super K Phys. Rev. Lett. 101:131802,2008 Experimental results: m2~2.4x10 3 ev2 ~ 45º Phys. Rev. Lett. 100:221803, 2008 m2sol sol) Kamland and solar data m2~7.6 x10 5 ev2 ~ 33º sin ) < 0.15 Chooz 17
18 3 Global Analysis in 2010 Global fit for 3 flavour scenario Preference for 13 0 First hint of 13 : sin2( 13) ~ G.L. Fogli et Al, hep/ph v2 18
19 Three flavor scenario? 19
20 LSND Liquid scintillator detector Search for e appearance ν µ νe L= 30 m E~40 MeV Excess of e (3.8 ): m2 =.3 to 3 ev2 Can be fitted withing 3-flavor scenario 20
21 Reactor neutrino anomaly New reference Reactor Neutrino Spectra PRC & PRC84, (2011) Re-analysis 19 short Baseline Experiments Results PRD83, (2011) Th. Lasserre, Town meeting, CERN 2012 R=0.927±0.023: 3.0 σ deviation with respect to R=1 (rate only) 21
22 Gallium Neutrino Anomaly 1 MCi Calibration runs of GALLEX and SAGE detectors Gallex: 51Cr source (750 kev) SAGE: 51Cr and 37Ar (810 kev) Observed/Expected Event Ratio: R=0.86±0.05 Phys. Rev. D 82, (2010); arxiv: No-oscillation hypothesis disfavored at about 2.7σ 22
23 Th. Lasserre, Town meeting, CERN 2012 Reactor/Gallium anomalies But not consistent with LSND Phys.Rev. D85 (2012)
24 So after the first round of experiments... 24
25 After 1st round of experiments... Oscillation measured: massive neutrinos but need for precision Still several questions Mass hierarchy? 13 0? 23 maximal? CP violation in the leptonic sector? Sterile neutrinos? Let's go for a 2nd (and 3rd) round 25
26 The Precision Generation 26
27 Second Generation Accelerators MINOS T2K MiniBooNe Nova (2013) OPERA & ICARUS Reactors: Appearance Atm Sector θ13, Double Chooz Daya Bay RENO Sterile Solar/Atmospheric: SuperKamiokande Borexino INO (design) Solar/Atm Sectors θ13, Sterile Supporting experiments flux and energy spectrum: SHINE (NA61) -N cross-sections: SciBooNE, MINERVA, T2K,... 27
28 2 nd Generation: Accelerator experiments 28
29 Oscillation analysis in 3D ( 13, ): need to analyze oscillations in the 3-flavor scenario Oscillation parameter correlated Still unknown parameters Degeneracies Several Channels Different energies Different BL Matter effects 29
30 MINOS (II) Phys.Rev.Lett. 107 (2011) Appareance analysis: 13 from e 30
31 T2K Precision measurement of atm. sector and 13 Off-axis beam: 185 kw (2012) disapearance appearance Backgrounds: e in beam 0 in NC 31
32 T2K Results First results on disappearance with 1.4x1020 pot e appearance: 6 events over background of 1.5 (2.5 ) NH (δ=0) sin2(2θ13)=0.11 and 0.03<sin2(2θ13)<0.28 at 90% C.L. IH (δ=0) sin2(2θ13)=0.14 and 0.04<sin2(2θ13)<0.34 at 90% C.L. The 5σ appearance result is expected by June Published in Phys. Rev. Lett. 107, (2011) 32
33 Opera and Icarus OPERA: direct detection of (appearance) Emulsion Cloud Chambers (granularity!) + trackers e, µ LNGS ντ τ π, CERN <Eν > = 17 GeV νe ντν µ p,n,π,k... ICARUS: 1st large scale detector with LAr (600 tons) Milestone towards future Mton detectors Searches for statistically Atm/solar sectors, sterile,... 33
34 NO A 2013 LBL Off-axis experiment (NuMI, 700 kw) Searches for e and e LBL: matter effects! Mass hierarchy, Totally active tracking liq. Scint. FD: 15 kton ND: 220 ton 34
35 MiniBooNE Check LSND results (same L/E) and modes mode: E<475 MeV: 3 excess in e-like events MicroBooNE: LAr TPC E>475 MeV: inconsistent with 90% CL mode: E<475 MeV: 1.3 excess in e-like events E>475 MeV: 2 fit consistent with 99.4 CL Data taking is over 35
36 The Latest Mixing Angle: 13 Reactor experiments 36
37 13: Why reactor neutrinos? L ~ 1 km P( e x) In contrast to accelerator experiments... No parameter correlations Pure e beam Low energy No matter effects Cheap, as source exists High flux and large xsection 37
38 Detecting reactor neutrinos IBD: e + p e+ + n Th: 1.8 MeV. Disappearance! Target: scintillator + n catcher (Gd) Detector: PMTs Prompt signal (1 8 MeV) e- e+ e E spectrum p n Gd Delayed signal (30 s, 8 MeV) 38
39 Setting up the experiment Reactor neutrinos: <E > ~ 4 MeV Solar sector Systematics! Oscillation! ~ 1 km ~ 100 m 39
40 Expected oscillation signal Toy Monte Carlo 8 GWth 8x1029 free protons Detection efficiency 80% 1 km 3 years: ~ events expected Toy MC Only statistical error! Deficit! Energy dependent! P. Novella, Moriond
41 New Generation Experiments Multi detector setups! 41
42 The Double Chooz Experiment First Results Chooz-B nuclear power plant Ardennes, France 42
43 The Double Chooz Detector Far Detector operating since early
44 Double Chooz Results First results on 13 form reactor experiments 100 days of data, FD only, 2011 Rate + Shape analysis 44
45 Daya Bay Flux from 6 x 2.9 GWth reactors 6 detectors in 2 Near (~500m) and 1 Far (1648m) sites Phys.Rev.Lett. 108 (2012) Rate only analysis (55 days): 5.2 signal (2012) 45
46 RENO Flux from 6 x 2.8 Gwth reactors Two identical Near (409m) and far detectors (1444m) 16 ton Phys.Rev.Lett. 108 (2012) Rate only analysis: 4.9 signal (2012) 46
47 Summary on 7.7 But we are not done: shape analysis!!! T.Schwetz H. Minakata 47
48 What's next? 48
49 Open questions after 2nd round... Mass hierarchy? 23 = /4, 23 < /4 or 23 > /4? CP violation? To address these questions, Super-Beams, Beta-Beams and NF are being studied is now known... and it is large! Is there a fast/easy/cheap way to resolve the above questions? What can be achieved with the current facilities? Can they be upgraded? New kton detectors? Can we answer any of these questions within ~10 year Discussion ongoing to define the roadmap for neutrino physics NuTURN 2012 and Town meeting: European Strategy for Neutrino Oscillation physics Spanish community also planning about next steps 49
50 International efforts LAGUNA LAGUNA-LBNO Underground facility for physics and p decay 2008 Large Baseline experiment EuroNu MW-superbeam Beta Beam Neutrino Factory Fermilab program: LBNE, Project X KEK/JPARC: T2HK, 0.75 to 4 MW Combining results from current experiments: maybe MO and 23, but no CP Upgraded beams: more energy, power (>700 kw) and purity Detectors: more massive, more granularity and energy resolution Degeneracies: different energies, baselines, channels 50
51 Detectors LAGUNA: proton decay, astrophysics and CP-violation in the lepton sector Detectors for Neutrino Factory: MIND: magnetized, MINOS-like TASD: magnetized NOVA-like Magnetized LAr MEMPHYS MIND 750kton water 51
52 SuperBeams Muon Neutrino beam from pion decay: beam power 1-4 MW E ~ 5 GeV, On/off axis detectors mass ~100 kton Long baseline: mass hierarchy Data taking: 10 years 52
53 Beta-Beams Electron Neutrino beam from beta decay: He 3 Li e ν e Ne Fe e 10 9 Pure e beam: smaller beam systematics and backgrounds Best detectors: water Cerenkov and LAr (LE) and iron calorimeter (HE) No disappearance: no measurement Technical challenges: ion production, acceleration, storage ring νe 53
54 Neutrino Factory Muon Neutrino beam from muon decay: Dectector able to measure charge Magnetized Iron calorimeters (MIND) muon production (MERIT), cooling (MICE), acceleration (EMMA) IDS-NF: 54
55 Comparing facilities Requirements: CPV: 2 complementary channels Degeneracies: different E/L P. Coloma et al, arxiv:1203:5651 Mass hierarchy: LBL Comparison: is measured (large!): Discovery potential not really useful Small CP asymmetries (systematics!) Better compare in terms of precision! 55
56 Projects for Next Generation CERN to Fréjus (SBL): LAGUNA-LBNO LAGUNA_LBNO SuperBeam (5GeV, 4MW) Water Cherenkov Upgrade: Beta-Beam CERN to Phyhäsalmi (LBL): SuperBeam (5GeV, 4MW) LAr+Mag. Iron, Liq. Scint. Upgrade: Neutrino Factory T2HK JPARC 4 MW, H2K LBNE Fermilab 2.3 MW beam, LAr All based on SuperBeams! CERN to Kamioka (arxiv: v1) SuperBeam (~5GeV, 4MW) Super-Kamiokande (8770 km) 56
57 Still one more question... Sterile neutrinos? Indications that three-flavor mixing might not be the sufficient: SBL reactor anti-neutrino measurements: reactor flux anomaly Radioactive source measurements: Gallium anomaly Accelerator-based experiments: LSND & MiniBooNE 57
58 Testing the Reactor Flux Anomaly Anti- detectors close to compact reactor cores (~10m) Saclay First experiment already at commissioning stage: Nucifer (Non Proliferation: Pth & Fuel Composition) 1m3 Gd-LS detector Osiris Site in Saclay (70 MW) Other projects: Stereo, SCRAMM, DANSS (building), NIST 58
59 Testing the Gallium anomaly Place source close/inside detectors Existing detectors (KamLAND, Borexino,...) Several options: 51 Cr: Borexino, SNO+, Baksan 144 Ce: Ce-LAND in KamLAND/Borexino,... arxiv:
60 Sterile neutrinos with accelerators Accelerator based short baseline proposals: LAr & Fermilab Requested features for a definitive experiment: L/E matching m2 ICARUS/NESSIE / run modes At least two detection locations e appearance and disappearance Fermilab: BooNE, LArLAr, SBL Nova CERN: ICARUS/NESSIE LAr (1kton) + Muon spectrometer (3kton) 60
61 Sterile neutrinos with accelerators Accelerator based short baseline proposals: LAr & Fermilab Requested features for a definitive experiment: L/E matching m2 ICARUS/NESSIE / run modes At least two detection locations e appearance and disappearance Fermilab: BooNE, LArLAr, SBL Nova CERN: ICARUS/NESSIE LAr (1kton) + Muon spectrometer (3kton) 61
62 Where we are... 62
63 Summary Atm/sol oscillation parameters have been measured Time for precision: mass hierarchy, 23? Interference sector is large: need to define the next step Search for CPV in leptonic sector ( ) Super-beams, beta-beams?, NF? Not everything understood in current results: Mass ordering, 23, CP? Sterile neutrinos?: SBL experiments Exciting times! 63
64 Thank you! 64
65 Solar Sector SNO Sensitive to all flavors: CC ES NC ν e + d p + p + e Φ CC = φe ν x + e ν x + e Φ ES = φe φµτ ν x + d p + n + ν x Φ NC = φe + φµτ In case of no oscillations: Φ CC = Φ NC = Φ ES 65
66 Solar Sector KamLAND Rector neutrino experiment (Kamioka) 1 KT liquid scintillator L = 180 Km, E ~ 3 MeV Disappearance of νe Solar sector: PRL 100, (2008) 66
67 Atmospheric Sector SuperKamiokande 50 kton water cherenkov detector Phys. Rev. D71 (2005) deficit: different energies and baselines 41.4 m 39.3 m 67
68 Atmospheric Sector K2K and MINOS K2K: first accelerator LBL experiment MINOS: precision accelerator LBL experiment Muon neutrino Fermilab Magnetized iron calorimeters Steel planes + scint. strips Near 1.04 km from target Far 735 km (Minnesota) 68
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