NEUTRINOS II The Sequel

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1 NEUTRINOS II The Sequel More About Neutrinos Ed Kearns Boston University NEPPSR V August 18, 2006 Ed Kearns Boston University NEPPSR

2 There is something unusual about this neutrino talk compared to many other neutrino talks you may have seen. Can you discern it? August 18, 2006 Ed Kearns Boston University NEPPSR

3 The Number of Neutrinos is Three August 18, 2006 Ed Kearns Boston University NEPPSR

4 (L in km, E in GeV) or (L in m, E in MeV) August 18, 2006 Ed Kearns Boston University NEPPSR

5 The Sun Flavor Produced ν e Baseline m Energy MeV Flavor Detected ν e, NC SNO, Super-K, others Reactor ν e km 0.3 GeV ν e KamLAND, Chooz ν e km 0.3 GeV ν e Double Chooz, Daya Bay Cosmic rays Accelerator Stopped π Beta Beam ν Factory ( ν + ν ),( ν + ν ) ν µ ν µ µ µ ν, ν ν, ν ν µ µ µ µ µ ν, ν e e ( ν + ν ),( ν + ν ) µ e e µ e e km 250, 735 km 295, 810 km 540 m km 50 m???? subgev TeV GeV 0.7, 2.2 GeV 500 MeV 0.5 GeV 50 MeV GeV? 20 GeV? ( ν + ν ),( ν + ν ) ν ν µ µ µ, e ν, ν e ν ν µ, e ν, ν e ν, ν e e e ν, ν, ν, ν e e µ µ ( ν + ν ),( ν + ν ) e e e µ µ e e Super-K, others K2K, MINOS T2K, NOνA MiniBooNE T2KK LSND, KARMEN?????? August 18, 2006 Ed Kearns Boston University NEPPSR

The first hints of neutrino mixing, and the first convincing results came from natural sources Solar Neutrinos Atmospheric Neutrinos Φ ( ν ) < Φ ( ν + ν + ν ) Φ(SSM) e e µ τ

6 The first hints of neutrino mixing, and the first convincing results came from natural sources Solar Neutrinos Atmospheric Neutrinos Φ ( ν ) < Φ ( ν + ν + ν ) Φ(SSM) e e µ τ Also important: Super-K, Kamiokande, SAGE, Gallex/GNO, Homestake Confirmed by MACRO, Soudan 2 Started by Kamiokande and IMB August 18, 2006 Ed Kearns Boston University NEPPSR

7 But we must keep in mind an important negative result Chooz reactor experiment No evidence for electron neutrino disappearance over ~ 1 km sin 2θ < 0.2 (at m ~ 2 10 ev ) Also Palo Verde Reactor experiment August 18, 2006 Ed Kearns Boston University NEPPSR

8 Atmospheric Neutrinos Pretty! August 18, 2006 Ed Kearns Boston University NEPPSR

9 Flux Atmospheric Neutrinos Cross Section 2:1 flavor ratio Up-down symmetric Angular Pointing e/µ Pretty technical! August 18, 2006 Ed Kearns Boston University NEPPSR

10 Atmospheric Neutrinos August 18, 2006 Ed Kearns Boston University NEPPSR

11 Super-Kamiokande III (newly rebuilt, filling in May 2006) August 18, 2006 Ed Kearns Boston University NEPPSR

12 August 18, 2006 Ed Kearns Boston University NEPPSR

13 August 18, 2006 Ed Kearns Boston University NEPPSR

14 How we bin and fit the data at SK 380 bins (SK-I+SK-II) + 70 systematic terms August 18, 2006 Ed Kearns Boston University NEPPSR

15 Muon Neutrino Tau Neutrino Mixing 380 bins (SK-I + SK-II) ν ν fit 2 χ = / 755 DOF µ τ sin 2θ > 0.95, m = ev (68% CL) August 18, 2006 Ed Kearns Boston University NEPPSR

16 August 18, 2006 Ed Kearns Boston University NEPPSR

17 What about electron neutrinos? August 18, 2006 Ed Kearns Boston University NEPPSR

18 What about tau neutrinos? E ν > 3.5 GeV August 18, 2006 Ed Kearns Boston University NEPPSR

19 Neural Network Analysis of Tau Appearance August 18, 2006 Ed Kearns Boston University NEPPSR

Neural Network Analysis of Tau Appearance 134 ± 48 events in excess + 16 27 cf.

20 Neural Network Analysis of Tau Appearance 134 ± 48 events in excess cf. 78 ± 27 excess events expected ~2.4 σ effect August 18, 2006 Ed Kearns Boston University NEPPSR

21 What about the oscillation pattern? Expand Fiducial Volume Keep events with good L/E resolution August 18, 2006 Ed Kearns Boston University NEPPSR

22 August 18, 2006 Ed Kearns Boston University NEPPSR

23 Lorentz Invariance Violation? Weak Equivalence Principle, CPT Invariance Violation? 1 Best fit is at L/ E. 2 χ > 100 disfavored by > 10σ Sterile Neutrinos? ν ν χ 2 µ sterile = 2 µ τ = ν ν χ 2 = χ 2 = χ / / σ DOF DOF NC should disappear Red: µ τ Blue: µ-sterile Matter effect suppression P osc MaVans and ν oscillate in rock Cos(zenith) Low energy ν oscillate in air 2 = σ MaVaNs? August 18, 2006 Ed Kearns Boston University NEPPSR χ hep-ph/ Dark energy related scalar field causes ρ dependent m 2

24 August 18, 2006 Ed Kearns Boston University NEPPSR

25 We know a certain amount about the mixing angles, except θ 13 is only bounded. By B. Kayser August 18, 2006 Ed Kearns Boston University NEPPSR

26 Neutrino Mixing Matrix Parameterization times Majorana Phases (not shown) WHY?? August 18, 2006 Ed Kearns Boston University NEPPSR

A. de Gouvea We know the neutrino is much lighter than the quarks and leptons, and we have measured the mass splittings pretty well. The most massive must 2 have m > 0.05 ev ( m atm ).

27 A. de Gouvea We know the neutrino is much lighter than the quarks and leptons, and we have measured the mass splittings pretty well. The most massive must 2 have m > 0.05 ev ( m atm ). We know the heirarchy between 1 and 2. But we don t know: Degenerate Inverted hierarchy Normal hierarchy ev } ev 5 2 August 18, 2006 Ed Kearns Boston University NEPPSR

Three Active Neutrinos or CPT violation?? KamLAND won t allow it now. LSND : m ~ ev 2 2 Atmospheric : m ~2.

28 Three Active Neutrinos or CPT violation?? KamLAND won t allow it now. LSND : m ~ ev 2 2 Atmospheric : m ~ ev Solar : m ~ 8 10 ev Pick any two! or a sterile neutrino?? H. Murayama August 18, 2006 Ed Kearns Boston University NEPPSR

29 LSND +/- Weakly significant (3.8σ) + No known defect - Complementary experiment, KARMEN, sees no effect (+ but with less sensitivity) August 18, 2006 Ed Kearns Boston University NEPPSR

MiniBooNE L = 540 m (10 LSND) E = 500 MeV (10 LSND) ν not ν µ µ 950 kl of pure mineral oil Cherenkov+scintillation 1280 PMTs Blind Analysis 50 STATUS: 7.2x10 20 pot anti-ν since Jan.

30 MiniBooNE L = 540 m (10 LSND) E = 500 MeV (10 LSND) ν not ν µ µ 950 kl of pure mineral oil Cherenkov+scintillation 1280 PMTs Blind Analysis 50 STATUS: 7.2x10 20 pot anti-ν since Jan Expect result real soon now Important to be unambiguous and correct! Un-blind sample Osc ν e MisID ν µ ν e from µ + ν e from K EnuQE (GeV) ν e from K 0 ν e from π + August 18, 2006 Ed Kearns Boston University NEPPSR

Long Baseline Experiments ILLINOIS LAB WILL BOMBARD WISCONSIN WITH NEUTRINOS Wisconsin State Journal August 8, 2002 KEK - Kamioka (K2K) ~1 GeV neutrinos L=250 km 1999-2004 Fermilab Soudan

31 Long Baseline Experiments ILLINOIS LAB WILL BOMBARD WISCONSIN WITH NEUTRINOS Wisconsin State Journal August 8, 2002 KEK - Kamioka (K2K) ~1 GeV neutrinos L=250 km Fermilab Soudan (MINOS) ~3 GeV neutrinos L=735 km Started 2005 CERN Gran Sasso (Opera/ICARUS) ~17 GeV neutrinos (broadband) L=732 km Starts in 2006 August 18, 2006 Ed Kearns Boston University NEPPSR

MINOS Far Detector 120 GeV protons, 4x10 13 ppp, 1.

4 kton far detector 484 steel/scintillator planes 1.

32 MINOS Far Detector 120 GeV protons, 4x10 13 ppp, 1.87 s cycle 0.4 MW beam power 1 kton near detector 5.4 kton far detector 484 steel/scintillator planes 1.2 T solenoidal magnetic field 750 km baseline, peak energy ~ 3 GeV 92% ν µ, 1.5% ν e /ν e -bar νs to Soudan, MN Near Detector Main Injector August 18, 2006 Ed Kearns Boston University NEPPSR

Final results from K2K First results from MINOS N N OBS EXP = 112 = 158.1 + 9.2 8.

33 Final results from K2K First results from MINOS N N OBS EXP = 112 = > 4σ confirmation of atmospheric neutrino mixing m = ev 2 sin θ 23 > 0.87 (68% CL) August 18, 2006 Ed Kearns Boston University NEPPSR

34 θ13 Gateway Parameter CP violating phase + terms in matter effect August 18, 2006 Ed Kearns Boston University NEPPSR

35 Precision Reactor Experiments only depends on θ 13, not δ or hierarchy Survival Probability Requires careful control of systematics > 1% Require multiple detectors Require overburden to reduce background Can reach sin 2 2θ ~ km 100 km August 18, 2006 Ed Kearns Boston University NEPPSR

Double Chooz (France): 2 x 4 GW reactor cores 50-300 mwe overburden 0.3/1 km baseline Existing infrastructure early start? (above) 2x10 ton modules fixed Goal of 0.6% systematics Reach sin 2 2θ ~ 0.

36 Double Chooz (France): 2 x 4 GW reactor cores mwe overburden 0.3/1 km baseline Existing infrastructure early start? (above) 2x10 ton modules fixed Goal of 0.6% systematics Reach sin 2 2θ ~ 0.03 Daya Bay (Hong Kong): 6 reactor cores, 17 GW total mwe overburden 0.3/ km baseline Construct tunnels and labs (above) 8x20 ton modules moveable Goal of 0.36% systematics Reach sin 2 2θ ~ 0.01 August 18, 2006 Ed Kearns Boston University NEPPSR

37 Neutrino flux is roughly proportional to proton beam power. Neutrino beams power 2.00E E E E E E E E E E E+00 power (kw) BNL AGS Main Ring nu expts CERN WANF LSND KARMEN (ISIS) NuTev MiniBoone K2K NuMI (average) NuMI (peak power) NuMI (design) NuMI MI stacking NuMI RR stacking NuMI Accum. stacking NuMI Proton Driver CNGS J-PARC - T2K -19 Power[W]=(protons/pulse) (energy[ev]) (repetition rate[hz]) ( [C/proton]) or if available: Power[W]=(beam current[a]) (beam energy[ev]) August 18, 2006 Ed Kearns Boston University NEPPSR

38 Off-Axis Technique August 18, 2006 Ed Kearns Boston University NEPPSR

39 Physics Goals Discover ν e appearance (first such result barring LSND/MiniBooNE), measuring non-zero θ 13 Resolve if θ 23 is non-maximal More precisely measure m 23 August 18, 2006 Ed Kearns Boston University NEPPSR

40 T2K August 18, 2006 Ed Kearns Boston University NEPPSR

41 One is signal, one is background ν e + n e + p 0 ν + p ν + p+ π µ µ August 18, 2006 Ed Kearns Boston University NEPPSR

42 To 1 APD pixel NOνA L typical charged particle path 30 (25) kton totally active detector W D Planes of liquid scintillator (mineral oil) read by WLS fiber and APD Surface detector with small overburden (right) August 18, 2006 Ed Kearns Boston University NEPPSR

43 One is signal, one is background + ν e + p e + p+ π 0 ν + N ν + p+ π µ µ August 18, 2006 Ed Kearns Boston University NEPPSR

44 Resolving the Mass Hierarchy Matter effect enhances ν e appearance for normal hierarchy Effect is reversed (enhanced anti-ν e ) for inverted hierarchy T2K 10% ν 10% e νe NOνA bigger 600 MeV 290 km δm 2 23 =2.5x10-3 ev 2 sin 2 2θ 23 =1.0 δm 2 12 =7.1x10-5 ev 2 sin 2 2θ 12 =0.81 sin 2 2θ 13 = GeV 820 km August 18, 2006 Ed Kearns Boston University NEPPSR

45 Beyond T2K and NOνA August 18, 2006 Ed Kearns Boston University NEPPSR

46 P( ν ν ) P( ν ν ) µ e µ e ~1000 km eg. T2K-K A.K.A. CP Violation CP Asymmetry stronger at 2 nd maximum August 18, 2006 Ed Kearns Boston University NEPPSR

47 To do list: Real soon- 2006?! August 18, 2006 Ed Kearns Boston University NEPPSR

48 There was something unusual about this neutrino talk compared to many other neutrino talks you may have seen. Did you discern it? No contours! This is not because contours (confidence intervals) are bad. They are generally a very appropriate way to present a final result, and a very good way of comparing results (i.e by overlaying them). But contours are fully digested final answers there is no way to evaluate the character or quality of the data. As was mentioned: when reading a paper or proposal, try to find the important plot that characterizes the result, not simply states it. I recently seem to see many talks that seem to show only the contours. It s like seeing a talk that reports only the final numbers (with ±errors), and no other details. I imagine 90% of all neutrino physicists can sketch the Chooz contour for sin 2 θ 23, but many fewer can sketch the data and fit that produced it. So as an exercise for myself, I made this lecture without contours. Caveat: one set snuck in- can you find it? August 18, 2006 Ed Kearns Boston University NEPPSR

Accelerator Neutrino Experiments News from Neutrino 2010 Athens

Accelerator Neutrino Experiments News from Neutrino 2010 Athens Ed Kearns Boston University Outline Quick overview New result 1: OPERA tau appearance New result 2: MINOS nu- e appearance Looking forward