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Karsten Heeger, LBNL NDM03, June 11, 2003 Future Reactor Neutrino Experiments Novel Neutrino Oscillation Experiments for Measuring the Last Undetermined.

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Presentation on theme: "Karsten Heeger, LBNL NDM03, June 11, 2003 Future Reactor Neutrino Experiments Novel Neutrino Oscillation Experiments for Measuring the Last Undetermined."— Presentation transcript:

1 Karsten Heeger, LBNL NDM03, June 11, 2003 Future Reactor Neutrino Experiments Novel Neutrino Oscillation Experiments for Measuring the Last Undetermined Neutrino Mixing Angle  13 Karsten M. Heeger Lawrence Berkeley National Laboratory

2 Karsten Heeger, LBNL NDM03, June 11, 2003 Recent Discoveries in Neutrino Physics Non-accelerator experiments have changed our understanding of neutrinos Atmospheric+Solar (Super-K) Solar (SNO) Reactor (KamLAND) Neutrinos are not massless (mass is small: m e < 0.0000059 m e ) Evidence for neutrino flavor conversion e   Combination of experimental results show that neutrinos oscillate

3 Karsten Heeger, LBNL NDM03, June 11, 2003 U MNSP - Neutrino Mixing Matrix atmospheric present solar present Present and Future Measurements Dirac phase Majorana phases reactor and accelerator future 0  experiments future accelerator future solar future  12 = 30.3°  23 = ~ 45° Solar Atmospheric Chooz + SK tan 2  13 < 0.03 at 90% CL maximal large small … at best No good ‘ad hoc’ model to predict  13. If  13 < 10 -3  12, perhaps a symmetry? reactor  13 experiment

4 Karsten Heeger, LBNL NDM03, June 11, 2003 Neutrino Oscillation Parameters Beamstop Neutrinos   s  e Atmospheric, Reactor, Accelerator Neutrinos    Solar and Reactor Neutrinos e  ,  Except for LSND,  m ij 2 measured and confirmed.

5 Karsten Heeger, LBNL NDM03, June 11, 2003  13 and CP ? How large is U e3 ?  13 is key parameter for oscillation phenomenology since  12 and  23 are both large  13 determines whether CP violation is accessible CP proportional to  13  13 is key parameter for oscillation phenomenology since  12 and  23 are both large  13 determines whether CP violation is accessible CP proportional to  13 atmospheric present solar present reactor and accelerator future 0  experiments future

6 Karsten Heeger, LBNL NDM03, June 11, 2003 Why Are Neutrino Oscillation Measurements Important? Central Questions in Neutrino Oscillation Physics & The Role of  13 1. What is the e coupling of 3 ? How large is  13 ?  13 : an opportunity for discovery 2. What are  13,  m 2 31,  CP,  12,  m 2 21,  23,  m 2 32 ?  13 : breaks correlation, helps with determination of parameters 4. Is there CP ?  13 : defines the future of accelerator experiments Time 3. What is the mass pattern? Physics at high mass scales, physics of flavor, and unification: Why are neutrino masses so small? Why are the mixing angles large, maximal, and small? Is there CP violation, T violation, or CPT violation in the lepton sector?  13 The Mystery of the Matter-Antimatter Asymmetry Understanding the role of neutrinos in the early Universe ? Is there a connection between the lepton and the baryon sector?

7 Karsten Heeger, LBNL NDM03, June 11, 2003 Measuring  13 Method 1: Accelerator Experiments appearance experiment measurement of   e and   e yields  13,  CP baseline O(100 -1000 km), matter effects present Method 2: Reactor Neutrino Oscillation Experiment disappearance experiment but: observation of oscillation signature with 2 or multiple detectors look for deviations from 1/r 2 baseline O(1 km), no matter effects e e e decay pipe horn absorber target p detector ++ ++ ++

8 Karsten Heeger, LBNL NDM03, June 11, 2003  13 =? Reactor Neutrino Measurement of  13 - Basic Idea atmospheric frequency dominant last term negligible for and 1/r 2 P ee, (4 MeV) e flux

9 Karsten Heeger, LBNL NDM03, June 11, 2003 Concept of a Reactor Neutrino Measurement of  13 e e, ,  NEAR FAR 2-3 detectors, possibly with variable baseline O(km) No degeneracies No matter effects Practically no correlations Coincidence Signal: e + p  e + + n Prompt e + annihilation Delayed n capture,  s capture time E = E e + m n -m p E prompt = E kin + 2m e Comparison of near and far detectors  search for spectral distortions

10 Karsten Heeger, LBNL NDM03, June 11, 2003 Reactor Neutrino Measurement of  13 Present Reactor Experiments (a) (b) (c) Energy (MeV) (a) Flux at detector (b) cross-section (c) spectrum in detector detector 1 Future  13 Reactor Experiment detector 2 Ratio of Spectra Energy (MeV) independent of absolute reactor flux eliminate cross-section errors relative detector calibration rate and shape information Absolute Flux and Spectrum

11 Karsten Heeger, LBNL NDM03, June 11, 2003 I. Undistorted vs Distorted Spectrum Optimize FAR detector with respect to NEAR NEAR - FAR 0.1 km (fixed) 1.7 km Ref: Huber et al. hep-ph/0303232 Baseline Optimization for Detector Placement II. Maximize Relative Distortions of Spectra Optimize both detector locations FAR - FAR 1 km ~2.5-3 km Based on shape analysis only Distance FOM L near < 1 km L far > 2.5 km

12 Karsten Heeger, LBNL NDM03, June 11, 2003 Baseline Optimization for Detector Placement (II) Advantages of FAR-FAR Configuration Oscillation signature in ratio of spectra. Avoid power plant boundaries at ~ 1km. Baseline Sensitivity to  m atm 2 Detector baselines sensitive to  m atm 2. Need option to adjust baseline once we have precision measurement  m atm 2. Region of interest for current  m atm 2 region: L far =~1.5 - 3 km. Measure  m atm 2.  m atm 2

13 Karsten Heeger, LBNL NDM03, June 11, 2003 Ref: Marteyamov et al, hep-ex/0211070 Reactor Detector locations determined by infrastructure Unique Feature - underground reactor - existing infrastructure ~20000 ev/year ~1.5 x 10 6 ev/year Kr2Det: Reactor  13 Experiment at Krasnoyarsk

14 Karsten Heeger, LBNL NDM03, June 11, 2003 Kr2Det: Reactor  13 Experiment at Krasnoyarsk L near = 115 m, L far =1000 m, N far = 16000/yr Ratio of Spectra Ref: Marteyamov et al., hep-ex/0211070. Energy (MeV)

15 Karsten Heeger, LBNL NDM03, June 11, 2003 Kashiwazaki: Proposal for Reactor  13 Experiment in Japan Kashiwazaki - 7 nuclear power stations, World’s most powerful reactors - requires construction of underground shaft for detectors near far Kashiwazaki-Kariwa Nuclear Power Station

16 Karsten Heeger, LBNL NDM03, June 11, 2003 near far 70 m 200-300 m 6 m shaft hole, 200-300 m depth Kashiwazaki: Proposal for Reactor  13 Experiment in Japan

17 Karsten Heeger, LBNL NDM03, June 11, 2003 A  13 Reactor Experiment in the US ? Site Criteria powerful reactor overburden (> 300 mwe) underground tunnels or detector halls controlled access to site  Variable/flexible baseline for optimization to  m 2 atm and to demonstrate subdominant oscillation effect  Optimization of experiment specific to site. Site selection critical

18 Karsten Heeger, LBNL NDM03, June 11, 2003 Diablo Canyon - An Ideal Site?

19 Karsten Heeger, LBNL NDM03, June 11, 2003 Powerful: Two reactors (3.1+ 3.1 GW E th ) on the California coast Overburden: Horizontal tunnel could give 800 mwe shielding! Infrastructure: Construction roads. Controlled access. Diablo Canyon - An Ideal Site 1500 ft nuclear reactor 2 underground detectors

20 Karsten Heeger, LBNL NDM03, June 11, 2003 Tunnel excavation required FAR : distance 1.5-2.5 km NEAR: distance 0.5-1 km Reactor separation: ~100 m An Ideal Oscillation Experiment with Variable Baseline? Possible layout of 2 or 3 detectors at Diablo Canyon Diablo Canyon plant boundary FAR: ~ 600-800 mwe NEAR: ~ 300-400 mwe Overburden

21 Karsten Heeger, LBNL NDM03, June 11, 2003 Tunnel excavation required FAR : distance 1.5-2.5 km NEAR: distance 0.5-1 km Reactor separation: ~100 m An Ideal Oscillation Experiment with Variable Baseline? Possible layout of 2 or 3 detectors at Diablo Canyon Diablo Canyon plant boundary FAR: ~ 600-800 mwe NEAR: ~ 300-400 mwe Overburden

22 Karsten Heeger, LBNL NDM03, June 11, 2003 Neutrino Detectors at Diablo Canyon - NEAR ~1 km ~0.5 km reactor Space constrained by hills and plant infrastructure Best overburden to the North East of power plant

23 Karsten Heeger, LBNL NDM03, June 11, 2003 Neutrino Detectors at Diablo Canyon - FAR Possible location Crowbar Canyon Parallel to Diablo Canyon Existing road access Possibility for good overburden Tunnels in radial direction from reactor 2 neutrino detectors, railroad-car size in tunnels at (variable) distance of NEAR/FAR I: 0.5-1 km FAR II:1.5-3 km Crowbar Canyon parallel to Diablo Canyon

24 Karsten Heeger, LBNL NDM03, June 11, 2003 liquid scintillator detector + active muon veto V fiducial ~ 80-100 t Movable Detector Concept for Diablo Canyon  13 Project Modular, movable detectors Volume scalable smaller  faster larger  more sensitive

25 Karsten Heeger, LBNL NDM03, June 11, 2003 Detector and Shielding Concept Active muon tracker + passive shielding + movable, inner liquid scintillator detector liquid scintillator passive shielding 3-layer muon tracker and active veto  rock  movable scintillator detector n N= S + B cor + B acc

26 Karsten Heeger, LBNL NDM03, June 11, 2003 Detector and Shielding Concept liquid scintillator passive shielding 3-layer muon tracker and active veto  rock  movable scintillator detector n Movable Detector? Variable baseline to control systematics and demonstrate oscillation effect (if  13 found to be > 0) Non-trivial for medium-size (~100 t), low-background detector Engineering Study fixed muon veto + movable inner detector

27 Karsten Heeger, LBNL NDM03, June 11, 2003 Dominant Experimental Systematics Reactor Flux near/far ratio, choice of detector location Consider best experiment to date: CHOOZ relative ≤ 1% Target Volume & no fiducial volume cut Backgrounds external active and passive shielding for correlated backgrounds Detector Efficiency built near and far detector of same design calibrate relative detector efficiency  variable baseline may be necessary Ref: Apollonio et al., hep-ex/0301017 Total  syst ~ 1-1.5%  rel eff ≤ 1%  target ~ 0.3%  n bkgd < 1%  flux < 0.2%  acc < 0.5% Note: list not comprehensive relative fiducial vol. ~ 0.3%

28 Karsten Heeger, LBNL NDM03, June 11, 2003 Flux Systematics with Multiple Reactor Cores Neutrino flux at detector I from reactors A and B Diablo Canyon, CA Indivual reactor flux contributions and systematics cancel exactly if Condition I: 1/r 2 fall-off of reactor flux the same for all detectors. Condition 2: Survival probabilities are approximately the same Systematic effect due to baseline difference  baseline  0.2% Relative Error Between Detector 1 and 2 rate shape Relative flux error (1%)< 0.6%< 0.01% Reactor core separation (100 m)< 0.14%< 0.1% Finite detector length (10 m)< 0.2%< 0.1%  Shape analysis largely insensitive to flux systematics.  Distortions are robust signature of oscillations.  Approximate flux cancellation possible at other locations

29 Karsten Heeger, LBNL NDM03, June 11, 2003 Sensitivity to sin 2 2  13 at 90% CL Reactor-I: limit depends on  norm (flux normalization) Reactor-II: limit essentially independent of  norm statistical error only fit to spectral shape  cal relative near/far energy calibration  norm relative near/far flux normalization Reactor I 12 t, 7 GW th, 5 yrs Reactor II 250 t, 7 GW th, 5 yrs Chooz 5 t, 8.4 GW th, 1.5 yrs Ref: Huber et al., hep-ph/0303232

30 Karsten Heeger, LBNL NDM03, June 11, 2003 Sensitivity and Complementarity of  13 Experiments Sensitivity to sin 2 2  13 Ref: Huber et al., hep-ph/0303232 sin 2 2  13 < 0.01-0.02 @ 90 C.L. within reach of reactor  13 experiments 10 -1 10 -2 10 -3 Reactor Neutrino Measurement of  13 No matter effect Correlations are small, no degeneracies Insensitive to solar parameters  12,  m 21 2

31 Karsten Heeger, LBNL NDM03, June 11, 2003 Past and Present Reactor Neutrino Experiments

32 Karsten Heeger, LBNL NDM03, June 11, 2003 Future Diablo Canyon Experiment

33 Karsten Heeger, LBNL NDM03, June 11, 2003 50 Years of Scientific Discoveries at Reactors Next Step Understanding the role of neutrinos in the early Universe. Why is there matter and not antimatter? 2002 Discovery of massive neutrinos and oscillations KamLAND, Japan Diablo Canyon? 1995 Nobel Prize to Fred Reines at UC Irvine 1956 Discovery of neutrinos in the US: First detection of reactor neutrinos 1990’s Reactor neutrino flux measure- ments in US and Europe 50 years of discoveries

34 Karsten Heeger, LBNL NDM03, June 11, 2003 Summary: Reactor Measurement of  13 Reactor neutrino oscillation experiment is promising option to measure  13. Novel reactor oscillation experiment gives clean measurement of sin 2 2  13, no degeneracies, no matter effects. 2 or 3 detectors variable baseline largely independent of absolute reactor flux and systematics Sensitivity of sin 2 2  13 ~ 0.01 comparable to next-generation accelerator experiments. Complementary to long-baseline program. Allows combined analysis of reactor and superbeam experiments. Negotiations with US power plants underway. Diablo Canyon is an attractive possibility. http://theta13.lbl.gov/

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