The ANGRA Neutrino Project

Transcription

1 The ANGRA Neutrino Project Ernesto Kemp State University at Campinas - UNICAMP Gleb Wataghin Physics Institute Cosmic Rays and Chronology Department 14/12/2007 E.Kemp - Encontro CBPF - 05/07 1

2 Doing Physics with Neutrinos from Reactors The neutrino history is closely related to nuclear reactors. The original neutrino discovery experiment, by Reines and Cowan, used reactor neutrinos Control room at Savannah River reactor Original papers on neutrino first detection: "Detection of the Free Neutrino: A Confirmation", C. L. Cowan, Jr., F. Reines, F. B. Harrison, H. W. Kruse and A. D. McGuire, Science 124, 103 (1956). "The Neutrino", Frederick Reines and Clyde L. Cowan, Jr., Nature 178, 446 (1956). 14/12/2007 E.Kemp - Encontro CBPF - 05/07 2

3 Outline Neutrinos from Reactors: main features of the particle source Production, Flux and Spectra Physics with Reactor Neutrinos Detection and Detectors Measurements and Applications Oscillations (lepton mixing parameters) Control of released thermal power Nuclear fuel composition The ANGRA Project: all of this in Brazil Conclusions Special thanks for the people that directly (or not ) has contributed with material for this talk: J. Dos Anjos, D.Reyna, M.Goodman, T.Lasserre, J.Conrad, V.Sinev, A.Barbosa, H.Lima Jr., M.Albuquerque, H.Nunokawa, O.L.G.Peres, A.Bernstein, M.Apollonio 14/12/2007 E.Kemp - Encontro CBPF - 05/07 3

4 Reactor Neutrinos: main features Source: copious β-decays from fission process <N ν > = 6,7 antineutrinos / fission 14/12/2007 E.Kemp - Encontro CBPF - 05/07 4

5 Reactor Neutrinos: main features Pressurized Water Reactors (PWR - wider usage around the world) The ν e emission has 6 main contributions Σ on : < N ν > ~ 6.7 ν e / fission n-capture in fission fragments 14/12/2007 E.Kemp - Encontro CBPF - 05/07 5

6 Reactor Neutrinos: main features Antineutrino Flux: Φ ν = < Nν > 2 4πD Pth[ GW ] W[ MeV ] s -1 cm 2 Where: Typical values D = distance from reactor core [50 m] P th = delivered thermal power [4 GW] W = energy release per fission [ MeV] Φ ν = s -1 cm 2 14/12/2007 E.Kemp - Encontro CBPF - 05/07 6

7 Reactor Neutrinos: main features Spectra ILL Measurements Phys.Lett. B160, 325 (1985) Obs.: 238 U is only calculated 14/12/2007 E.Kemp - Encontro CBPF - 05/07 7

8 Reactor Neutrinos: detection principles actually we detect anti-neutrinos. The ν e interacts with a free proton (hydrogen) via inverse β-decay: ν e W e + p n Later the neutron captures giving a coincidence signal. Reines and Cowan used cadmium to enhance the neutron capture 14/12/2007 E.Kemp - Encontro CBPF - 05/07 8

9 Just a personal remark: Things have not been dramatically changed in the last years 3500 BC 14/12/2007 E.Kemp - Encontro CBPF - 05/07 9

10 Just a personal remark: Things have not been dramatically changed in the last years Last week 14/12/2007 E.Kemp - Encontro CBPF - 05/07 10

11 This is also true in the field of Reactor Neutrinos detection... Few modifications has been introduced if one consider the main guidelines and detection principles successfully applied in the experimental design of Reines and Cowan : A large liquid scintillator volume viewed by PMTs. KamLAND design The first successful neutrino detector 14/12/2007 E.Kemp - Encontro CBPF - 05/07 11

12 Big Detectors: KamLAND (running) 1km Overburden Electronics Hut Steel Sphere PMTs % coverage 1 kton liquidscintillator Water Cherenkov outer detector 225 PMTs 14/12/2007 E.Kemp - Encontro CBPF - 05/07 12

13 Big Detectors: Titolo CHOOZ (France) Surrounding Rock Fe shield 6 m Region III (VETO): 90 ton of standard scintillator, 48 PMT Geode: opaque vessel, structure for 192 PMT of 8 Region II (buffer): 17 ton of standard scintillator Region I (target): transparent plexiglass vessel filled with 5 ton of Gd doped scintillator (< 0.1 % of mass) 14/12/2007 E.Kemp - Encontro CBPF - 05/07 13

14 Smaller ones: Palo Verde (AZ E.U.A.) /12/2007 E.Kemp - Encontro CBPF - 05/07 14

15 Smaller ones: Rovno (Ukraine) General view of Rovno NPP in Ukraine in 1983 Cores 1 & 2 10 m 14/12/2007 E.Kemp - Encontro CBPF - 05/07 15

16 Smaller ones: Rovno (Ukraine) ν e γ e + γ outer volume (540 l) n Acrylic volume (20 mm) filled with mineral oil Thin acrylic walls (5 mm) volume containing scintillator doped with Gd (~0.5 g/l) central volume (target, 510 l) 84 PMT light guides (pure mineral oil) mirror light reflectors 14/12/2007 E.Kemp - Encontro CBPF - 05/07 16

17 Smaller ones: San Onofre (CA E.U.A.) 2004-running Currently operational: 4 cells with 640 kg of Gd doped scintillator; quasi-hermetic muon veto; hermetic water shield 14/12/2007 E.Kemp - Encontro CBPF - 05/07 17

18 Reactor Neutrino Event Signature The main reaction process is inverse β-decay followed by neutron capture Two part coincidence signal is crucial for background reduction. + ν e p e n n capture Positron energy spectrum implies the neutrino spectrum E ν = E vis MeV 2m e In undoped scintillator the neutron will capture on hydrogen n +H D * D + γ (2.2 MeV) More likely the scintillator will be doped with gadolinium to enhance capture n+ m Gd m+1 Gd * Gd + γ s (Σ = 8 MeV) 14/12/2007 E.Kemp - Encontro CBPF - 05/07 18

19 Physics: Flavor Oscillation (the basics) Flavor basis ν µ Mass Basis ν 2 ν e ν e = ν 1 cosθ + ν 2 sinθ ν µ = ν 1 sinθ + ν 2 cosθ ν 1 θ ν(t)=e ιεt ν(0) P(ν e ν µ ) = <ν µ (t) ν e (0)> = sin 2 θcos 2 θ e -ιe 2 t -e -ιe 1 t 2 = sin 2 (2θ) sin 2 (1.27 m 2 L/E) 14/12/2007 E.Kemp - Encontro CBPF - 05/07 19

20 Mixing Matrix (quark sector) CKM Matrix d' s' b' V = V V 1 λ 3 λ ud cd td λ V V 1 2 λ V us cs ts V V V 3 λ 2 λ 1 ub cb tb d s b where λ ~ 0.2 For quarks: flavor basis mass basis 14/12/2007 E.Kemp - Encontro CBPF - 05/07 20

21 14/12/2007 E.Kemp - Encontro CBPF - 05/07 21 Mixing Matrix : Neutrinos = τ3 τ2 τ1 µ3 µ2 µ1 e3 e2 e1 τ µ e ν ν ν U U U U U U U U U ν ν ν U e3 < 0.15 For neutrinos: flavor basis mass basis PMNS Matrix

22 Why U e3? ν ν ν e µ τ U = U U e1 µ1 τ1 U U U e2 µ2 τ2 U U U e3 µ3 τ3 ν ν ν U e3 is 100% sensitive to the mixing angle θ 13 Any observation of CP violation in leptons requires a non-zero value of θ 13 14/12/2007 E.Kemp - Encontro CBPF - 05/07 22

23 Oscillation Probability P = sin 2 (2θ) sin 2 (1.27 m 2 L/E) m 2 = m 12 -m 22 (ev 2 ) sin 2 (2θ) is the strength of the mixing; sin 2 (2θ)=0 is no oscillations E is the neutrino energy (GeV) ( log(e p ) at accelerator) L is the distance from the source to the detector (km) P is the probability of oscillation. On a parameter space plot, (sin 2 (2θ) vs. m 2 ), a limit or signal curve corresponds to constant P. The level of sensitivity depends on the statistics. 14/12/2007 E.Kemp - Encontro CBPF - 05/07 23

24 Current Status Unconfirmed observation by LSND, currently being investigated by MiniBooNE. Possibly implies the existence of sterile neutrinos or CPT violation. Seen by Super-K and confirmed by Soudan II and K2K. (θ 23 ) First observed by Ray Davis and descendents. Precise measurements by Super-K, SNO and KamLAND. Presumed to be dominated by mixing between states 1and 2 (or θ 12 ) 14/12/2007 E.Kemp - Encontro CBPF - 05/07 24

25 Open questions: Neutrino Mass Differences Only 2 independent mass differences 2 12 Mass hierarchy unknown 2 m = m + m ( m 2 solar~ 5 x 10-5 ev) ( m 2 atm~ 3 x 10-3 ev) 14/12/2007 E.Kemp - Encontro CBPF - 05/07 25

26 Open questions: Mixing Parameters θ 13 : the last unknown parameter 14/12/2007 E.Kemp - Encontro CBPF - 05/07 26

27 Physics motivations to do accurate measurements of θ 13 : The discovery of neutrino oscillations imply that neutrinos are massive and that the Standard Model is incomplete. The minimal extension of the SM requires 3 mass eigenstates, ν 1, ν 2, ν 3 and a unitary mixing matrix U which relates the neutrino mass basis to the flavor basis. These observations may have profound astrophysical consequences. CP violation in the lepton sector may hold the key of matter-antimatter asymmetry in the universe. 14/12/2007 E.Kemp - Encontro CBPF - 05/07 27

28 3 ν Oscillation Probability Equations Based on θ 12, θ 13, θ 23 P(ν e ν µ ) = sin 2 (2 θ 13 )sin 2 (θ 23 )sin 2 ( m 2 L/4E) P(ν e ν τ ) = sin 2 (2 θ 13 )cos 2 (θ 23 )sin 2 ( m 2 L/4E) P(ν µ ν τ ) = sin 2 (2 θ 23 )cos 4 (θ 13 )sin 2 ( m 2 L/4E) P(ν µ ν e ) = sin 2 (2 θ 13 )sin 2 (θ 23 )sin 2 ( m 2 L/4E) Ignoring the small m 2 scale, CP violation and matter effects. 14/12/2007 E.Kemp - Encontro CBPF - 05/07 28

29 How to Measure θ 13 Option 1: Accelerator based neutrino beams P(ν µ ν τ ) = sin 2 (2 θ 23 )cos 4 (θ 13 )sin 2 ( m 2 L/4E) ~1.0 P(ν µ ν e ) = sin 2 (2 θ 13 )sin 2 (θ 23 )sin 2 ( m 2 L/4E) <0.05 Ignoring matter effects, the small m 2 scale and CP violation 14/12/2007 E.Kemp - Encontro CBPF - 05/07 29

30 The θ 23 Degeneracy Problem Atmospheric neutrino measurements are sensitive to sin 2 2θ m P( ν µ ν x ) = sin 2 2θ 23 sin 27 Eν But the leading order term in offaxis ν µ ν e oscillations is Super-K Measures 2 23 L m P( ν µ ν e) = sin 2 θ23 sin 2θ13 sin 27 Eν If the atmospheric oscillation is not exactly maximal (sin 2 2θ 23 <1.0) then sin 2 θ 23 has a twofold degeneracy Offaxis θ 13 Measures 2 13 L sin 2 sin 2 2θ 23 sin 2 θ 23 θ θ 2θ 45º 90º 2θ 14/12/2007 E.Kemp - Encontro CBPF - 05/07 30

31 Degeneracies in appearance experiments (beam-like) ~cosδ Minakata and Nunokawa, hep-ph/ ~sinδ δ There are 2 Observables P(ν µ ν e ) P(ν µ ν e ) sin 2 2θ 13 Interpretation in terms of sin 2 2θ 13, δ and sign of m 2 23 depends on the value of these parameters and on the conditions of the experiment: L and E 14/12/2007 E.Kemp - Encontro CBPF - 05/07 31

32 Resolving Degeneracies Experiments at different baselines (affects both L/E and matter) Experiments at different energies Data with neutrinos and anti-neutrinos Better parameter measurements (θ 23 ) Accelerator experiments cost >U$ 200M and take >10 years to build But, If θ 13 = 0, degeneracies collapse anyway. 14/12/2007 E.Kemp - Encontro CBPF - 05/07 32

33 How to Measure θ 13 Option 2: Reactor neutrinos P(ν e ν e ) = 1 - sin 2 2θ 13 sin 2 ( m 2 atm L/4E) Ignoring small m 2 P L/E(km/MeV) Look for ν e disappearance at small distance (L/E) 14/12/2007 E.Kemp - Encontro CBPF - 05/07 33

34 Reactor Neutrinos E ν ~ 4 MeV Too low for CP violation to occur L ~ 1-4Km Too short for matter effects to begin No Degeneracy Problems 14/12/2007 E.Kemp - Encontro CBPF - 05/07 34

35 CHOOZ results MC (no oscillations assumption) vs data e + spectrum ± 2.7% (syst) R=data/MC compatible with 1 non oscillation 14/12/2007 E.Kemp - Encontro CBPF - 05/07 35

36 Palo Verde results MC (no oscillations assumption) vs data Compatible with no oscillations 14/12/2007 E.Kemp - Encontro CBPF - 05/07 36

37 Chooz and Palo Verde Reactor Experiments Neither experiments found evidence for ν e sin 2 2θ 13 < 0.18 at 90% CL (at m 2 = ) Future experiments should try to improve on these limits by at least an order of magnitude. Down to sin 2 2θ 13 <0.01 oscillation. This null result eliminated ν µ ν e as the primary mechanism for the Super-K atmospheric deficit. Chooz Systematic Uncertainties 14/12/2007 E.Kemp - Encontro CBPF - 05/07 37

38 Applications of Reactor Neutrinos Instantaneous Measurements of: Released thermal power In principle, a precise control of the RTP leads to improvement on the efficiency of heat transfer Nuclear fuel composition Precise determination of fuel refreshment (fuel cycles) Safeguards tool on non-proliferation 14/12/2007 E.Kemp - Encontro CBPF - 05/07 38

39 Thermal power measurements using neutrino detection constant 1 N ν = 4πR 2 σ f = E max W th E f 1, N p εσ f ρ(e) σ(e) R(E,T) de dt Change during reactor operational cycle T E thr σ f, E f 235 U Pu U Pu ρ(e) = Σ α i ρ i (E) E f = α i E i Σ α i = 1 i = 5,9,8,1 Σ σ f = Σ α i σ i i = 5,9,8,1 i = 5,9,8,1 14/12/2007 E.Kemp - Encontro CBPF - 05/07 39

40 Thermal power measurements using neutrino detection N ν = constant W th σ f E f σ 5 (1 + k) E 5 N ν = γ (1 + k) W th Account of fuel composition 14/12/2007 E.Kemp - Encontro CBPF - 05/07 40

41 Checking reactor activity: Antineutrino counts per day /23/05 2/27/05 3/3/05 3/7/05 3/11/05 3/15/05 3/19/05 Date Predicted count rate using reported reactor power Observed count rate, 24 hour average Reported reactor power Reactor Power (%) Rovno (Ukraine) San Onofre (USA) 14/12/2007 E.Kemp - Encontro CBPF - 05/07 41

42 Dependence of the detector rate from reactor power Rate per 10 5 sec events n ν ~ γw Reactor power in % from nominal value (1375 MW) 14/12/2007 E.Kemp - Encontro CBPF - 05/07 42

43 Measuring of power production by neutrino method 400 ε ν / ε T 1.1 ε ν [GW day] δε T ~ δw th t δε ν ~ 1/(N ν ) 1/ N ν [x10 3 ] /12/2007 E.Kemp - Encontro CBPF - 05/07 43

44 Fuel composition: The Burn-up effect 14/12/2007 E.Kemp - Encontro CBPF - 05/07 44

45 Observing the Fuel Burn-up Calculated cross-section evolution Observed counting rate evolution : ~ 6% 14/12/2007 E.Kemp - Encontro CBPF - 05/07 45

46 Ratio of spectra: time evolution S /S S(t)/S(t=0) i b For standard cycle of PWR at Rovno Nuclear Station, W th =1375 MW time (days) after reactor starts visible energy, MeV 14/12/2007 E.Kemp - Encontro CBPF - 05/07 46

47 Reactor Neutrinos: main features just to remember Spectra Other isotopes than 235U become dominant in higher energies 14/12/2007 E.Kemp - Encontro CBPF - 05/07 47

48 Ratio of neutrino spectra at the beginning and end of reactor campaign ρ end /ρ beg Rovno Expected from ILL spectra E ν (MeV) 14/12/2007 E.Kemp - Encontro CBPF - 05/07 48

49 Nuclear Reactors Around the World 14/12/2007 E.Kemp - Encontro CBPF - 05/07 49

50 How Does The IAEA Monitor Fissile Material Now? (1-1.5 years) (months to years) (months) (forever) 1. Check Input and Output Declarations 2. Verify with Item Accountancy 3.Containment and Surveillance 1 Gross Defect Detection 2 Continue Item Accountancy 3. Containment and Surveillance 1 Check Declarations 2 Verify with Bulk Accountancy: Operators Report Fuel Burnup and Power History No Direct Pu Inventory Measurement is Made Until the Fuel is Reprocessed 14/12/2007 E.Kemp - Encontro CBPF - 05/07 50

51 Antineutrino Detectors Advantages as Safeguards Tool A. Measure fissile content directly B. Measure thermal power, which constraints fissile content C. Operate continuously, non-intrusively, and remotely experimental works has already demonstrated B and C with a simple detector, and data (Rovno+San Onofre) are fully consistent with A 14/12/2007 E.Kemp - Encontro CBPF - 05/07 51

52 Where should we go? The present geopolitics of reactor experiments Double Chooz RENO? KASKA Daya Bay Angra 14/12/2007 E.Kemp - Encontro CBPF - 05/07 52

53 All of this in Brazil Angra dos Reis Reactor Experiment: The ANGRA Neutrino Project 14/12/2007 E.Kemp - Encontro CBPF - 05/07 53

54 The ANGRA collaboration 17 Researchers 14 physicists 2 ingeneerings 1 Pos-Doc 2 Students 1 PhD 1 Undergraduate Applying: 2 Pos-Docs + 1 MsC students 14/12/2007 E.Kemp - Encontro CBPF - 05/07 54

55 Frontier Physics in Brazil Very interesting for the Brazilian science: Possibility to do frontier experimental physics profiting from an already existing facility (Angra-I and II reactors). (Angra-III?) Relative low cost investments compared with ANGRA (I + II + III) reactors cost. Possibility to use the future facility for other experiments and purposes: R&D for new neutrino detection techniques gravitational antenna: GRAVITON project 14/12/2007 E.Kemp - Encontro CBPF - 05/07 55

56 Angra dos Reis RJ Brazil MG SP RJ Angra-II Angra-I Angra-III 14/12/2007 E.Kemp - Encontro CBPF - 05/07 56

57 Angra dos Reis nuclear plant features 3 Reactors: 2 in operation + 1 planned Reactor (starting date) Thermal Power (GW) Average Uptime Fuel Cycle Angra-I (1985) % ~1.5 years Angra-II (2000) 4.0 ~ 1.2 x f/s 90 % ~1.3 years Angra-III planned > /12/2007 E.Kemp - Encontro CBPF - 05/07 57

58 Institutional Responsibilities Experimental Group construction operation ELETRONUCLEAR All communication channels established!! approval CNEN regulatory submission Support from brazilian nuclear authorities: ELETRONUCLEAR (Operating Company) CNEN (National Commission for Nuclear Energy) 14/12/2007 E.Kemp - Encontro CBPF - 05/07 58

59 Current Configuration Morro do Frade reactors Near (reference) detector: 50 ton detector (7.2 m dia) 300 m from core 250 m.w.e. Far (oscillation) detector: 500 tons (12.5 m dia) 1500 m from core 2000 m.w.e. (under Frade peak ) Very Near detector: 1 ton prototype project ~ 50m of reactor core Detector Construction Standard 3 volume design 14/12/2007 E.Kemp - Encontro CBPF - 05/07 59

60 Far Site tunnel Sites Detectors for Neutrino Oscilation Measurements Near Site Angra III 500 m Reactor Very Near Detector (power monitor and safeguards) 14/12/2007 E.Kemp - Encontro CBPF - 05/07 60

61 View of the Experimental Layout Morro do Frade Zoom Out Far Site L = 1500 m Entrance Angra-I Near Site depth = 100 m 14/12/2007 E.Kemp - Encontro CBPF - 05/07 61

62 Civil Construction Design Far Near Ground Level 8 m 8 m 1250 m ~100 m 25 m Experimental Hall 10 m 20 m 15 m 15 m 10 m 14/12/2007 E.Kemp - Encontro CBPF - 05/07 62

63 µ Intensity vs. Depth from LVD data: PHYS. REV. D, 58, (1998) 10 0 µ vertical intensity (cm -2 s -1 str -1 ) x10-4 1x Bugey Palo Verde D-Chooz / Braidwood Kaska Daya Bay Angra Kamioka Gran Sasso Far Detector Depth (m.w.e.) 14/12/2007 E.Kemp - Encontro CBPF - 05/07 63

64 VND Detector site: 50 m 100 m Selected Places for the VERY NEAR DETECTOR shaft ( < 15 m) 14/12/2007 E.Kemp - Encontro CBPF - 05/07 64

65 Expected Rates for Angra Very Near Near Far Signal (events/day) 1000 (66m) 2500 (300m) 1000 (1500m) Muon rate (Hz) 150 ~ Correlated background ( 9 Li) 44 < 20 ~ 2 (events/day) 14/12/2007 E.Kemp - Encontro CBPF - 05/07 65

66 Expected Signal & Background Cilindrical detector dimensions R= 1.40m; H=3.10m target=1ton Distance (m) Signal (day) Depth (mwe) Muons (Hz) /12/2007 E.Kemp - Encontro CBPF - 05/07 66

67 Costs: civil construction 14/12/2007 E.Kemp - Encontro CBPF - 05/07 67

68 Costs: detectors Acrylic (2 concentric spheres) Near Detector (scaling from SNO) Steel / Structural Support (outer sphere + PMT supports) Electronics ($100/channel + $1K/PMT) Mineral Oil ($553 / ton) Liquid Scintillator (w/o Gadolinium) ($1190 / ton) SubTotal Total / Detector (design, contingency, etc..ie. X 2) Near $3M $200K $1.2M (1054 Channels) $70K $100K $4.6M $9.2M Far $11.5M $600K $3.6M (3293 Channels) $232K $730K $16.7M $33.4M 14/12/2007 E.Kemp - Encontro CBPF - 05/07 68

69 ν Survival Probabilities: experimental overview 14/12/2007 E.Kemp - Encontro CBPF - 05/07 69

70 ν Survival Probabilities: Angra E th = 1.8 MeV (both detectors) ; P=95%@5MeV (far detector) P ( ν e ν e ) 1,0 0,9 0,8 0,7 0,6 0,5 0,4 0,3 0,2 0,1 Near Detector: 0.3 km Far Detector: 1.5 km E = 1.8 MeV E = 5.0 MeV E = 1.8 MeV 0,0 0, L/E [km/mev] 14/12/2007 E.Kemp - Encontro CBPF - 05/07 70

71 ANGRA s approach: Precise Shape measurement Ratio of energy spectra Challenge: uniformity in both detector responses 14/12/2007 E.Kemp - Encontro CBPF - 05/07 71

72 Shape vs. Rate A Luminosity Transition sin 2 2θ 13 Sensitivity 90%CL at m 2 = ev 2 From Huber, Lindner, Schwetz and Winter Spectral shape only Statistical error only σ cal bin-to-bin energy calibration error σ norm normalization error Exposure (GW ton years) 14/12/2007 E.Kemp - Encontro CBPF - 05/07 72

73 ANGRA Sensitivity studies conventions d/d: detectors b/b: bin (energy) capital: correlated small: uncorrelated DC expectations 500 ton (fiducial volume) 3 years 14/12/2007 E.Kemp - Encontro CBPF - 05/07 73

74 Sensitivity studies conventions d/d: detectors b/b: bin (energy) capital: correlated small: uncorrelated 14/12/2007 E.Kemp - Encontro CBPF - 05/07 74

75 Reactor ν experiment physics Reactor Optimistic start date GW-t-yr (yr) Sin 2 2θ sensitivity for m 2 (10-3 ev 2 ) Efficiencies Far event rate ANGRA 2013(full) 3900(1) 9000(3) 15000(5) ,000/yr Daya Bay 08(fast) 09(full) 3700(3) ,000/yr 110,000/yr (before/after 2010) Double Chooz Oct 07(far) Oct 08(near) 29(1) 29(1+1) 80(1+3) ,000/yr RENO Late (1) ,000/yr 14/12/2007 E.Kemp - Encontro CBPF - 05/07 75

76 The Neutrino Detector Detector regions Active region [ 1m, h=1.3m] (Liquid Scintillator + 0.1% Gadolinium) Gama catcher [ 1.6m, h=1.9m] (Liquid Scintillator) Buffer [ 2.2m, h=2.5m] (Mineral oil) 14/12/2007 E.Kemp - Encontro CBPF - 05/07 76

77 Very Near Detector: 3 volumes Design A) Target (1 ton) Acrylic vessel + lqd scintillator(+gd) B) Gamma-Catcher Acrylic vessel + lqd scintillator C) Buffer Steel vessel + mineral oil D) Vertical Tiles of Veto System & E) X-Y Horizontal Tiles of Veto System Plastic scintillator padles above and under the external steel cylinder: muon tracking through the detector 15% of coverage 14/12/2007 E.Kemp - Encontro CBPF - 05/07 77

78 The Neutrino Detector PMTs coverage 2.2m 0.43m 0,43m 0.45m Total area = S side + S top + S bottom ( ) 24.88m 2 20% coverage 4.98m 2 2.5m Photocathode area = 0.038m m # PMTs = 4.98/ m 128 PMTs implemented 14/12/2007 E.Kemp - Encontro CBPF - 05/ m

79 Testing the Design: Detailed G4 simulation under construction 14/12/2007 E.Kemp - Encontro CBPF - 05/07 79

80 The VETO system 14/12/2007 E.Kemp - Encontro CBPF - 05/07 80

81 The VETO system X&Y and Barrel Scintillators X&Y 3m long, 1cm thick, 15cm wide Readout by: optical fiber + segmented PMT or small size PMTs. Assembled as a single piece Barrel 3m long, 1.5cm thick, 60-70cm wide Readout by: small size PMTs. Fixed on a barrel structure 14/12/2007 E.Kemp - Encontro CBPF - 05/07 81

82 The VETO system Scintillator + fiber setup, built at FNAL, likely to be used at the AMIGA Project under AUGER. Multianode photomultipliers (Ex: Hamamatsu R8520 series) 14/12/2007 E.Kemp - Encontro CBPF - 05/07 82

83 Electronics & DAQ Front-end electronics input buffer + amplifier/shaper To ADC: + line driver To Trigger system: + comparator Input Buffer Amplifier & Shaper Line Driver Comparator To ADC To Trigger Data Acquisition (DAQ) VME-based off-the-shelf high-performance devices (ADCs, FPGAs, FIFOs) two sub-systems: neutrino signal / VETO Neutrino: 120 input channels sampled at 250Msps / 10-bit resolution VETO: 110 LVDS signals to a large/fast FPGA (Stratix II) 14/12/2007 E.Kemp - Encontro CBPF - 05/07 83

84 Neutrino Detection electronics: Laboratory for Detection CBPF / BR front panel VME bus standard: VME 6U P1 P2 (16cm x 23cm) ADC FPGA BUFFER one module: 16 ADC input 250 MHz buffer size per channel = 524 µs 128 PMT channels => 8 modules required dedicated lines on P2 to receive VETO interrupt requests to indicate almost full condition control / status registers (e.g.: number of events in a buffer) 14/12/2007 E.Kemp - Encontro CBPF - 05/07 84

85 VETO electronics: Laboratory for Detection CBPF / BR front panel VME bus LVDS input channels LVDS receivers LVDS receivers FPGA P1 P2 Standard: VME 6U One module: 2 connectors on the front panel 68 LVDS input channels (total) LVDS receivers to reduce I/O pins in FPGA 110 scintillators 2 modules required 26 input channels free for new ideas (16cm x 23cm) 14/12/2007 E.Kemp - Encontro CBPF - 05/07 85

86 GEANT (Madrid ES) Latin American Advanced Networks CLARA 622Mbps Network Infra-structure for the USA 400Mbps 1Gbps Brazilian National Education and Research Network RNP Angra Neutrino Detector Rio Angra Extension of CBPF LAN s. Angra PoP Telecom Infra-strucutre USA 155Mbps 1Gbps Rede-Rio PSTN Data Storage (Mirror) 100 Mbps /16 CBPF Ethernet LAN. Router Firewall VoIP Private Line Minimum 512Kbps Optimum: 1 Mbps Data Storage Radio or Optical Fiber Link VoIP Ethernet Switch /24 2 Steps: 1 Infra-structure investment: router, switch, radio (fiber). 2 permanent private connection (CBPF-Angra) DAQ - Data Acquisition System 14/12/2007 E.Kemp - Encontro CBPF - 05/07 86

87 Alternatives: Single Ended Readout? Mineral Oil Buffer Gamma Catcher Target Could Reduce footprint by meters Reduce height by cm. Significant reduction in number of PMTs Problem: Long path lengths for reflected light 14/12/2007 E.Kemp - Encontro CBPF - 05/07 87

88 Non-proliferation effort in ANGRA ABACC: The Common System of Accounting and Control of Nuclear Materials is a mechanism created in order to verify if Argentine and Brazil utilize their nuclear materials exclusively for pacific purposes. 14/12/2007 E.Kemp - Encontro CBPF - 05/07 88

89 ABACC + ANGRA Project ASSESSMENT of the TECHNICQUE + IAEA! 14/12/2007 E.Kemp - Encontro CBPF - 05/07 89

90 ANGRA itens just under project Front-end Electronics DAQ Data transfer & Communications : Nuclear Complex << = >> Research Institutions On work: Construction Ingeneering Simulations Customized FPGA boards Deployment and operations strategies 14/12/2007 E.Kemp - Encontro CBPF - 05/07 90

91 Angra Project: Present Status Meeting September 05, 2006 with Eletronuclear representatives to define next step. Authorization to place a container next to the reactor building. Detailed project under way to be presented to the Minister of Science and Technology and to FAPESP. 14/12/2007 E.Kemp - Encontro CBPF - 05/07 91

92 Deploiment Streategy: Phase I: Setup infrastructure at the Angra site: - 20 container near the reactor building - Measurement of local muon flux: Cerenkov detector (Auger test tank) - Muon telescope (4 Minos type scintillator planes) 14/12/2007 E.Kemp - Encontro CBPF - 05/07 92

93 Deploiment Strategy Phase I: Setup infrastructure at CBPF & UNICAMP: Start to test components at CBPF and UNICAMP: - 8 phototubes - VME electronics Measurement of radioactive background (rocks and sand) 14/12/2007 E.Kemp - Encontro CBPF - 05/07 93

94 Phase II: Deploy LVD tank - 1 ton gadolinium dopped liquid scintillator tank - test signal+background - Tests with Californium source - Final site selection for underground laboratory PMT ISNP, 23/09/05 Test on the doped Tank 252 Ca Capture on H vs Gd <T> capture [t]: 200 µs vs ~30 µs efficiency [ε( E th )]: 60% vs ~70% Eγ emitted in the n- capture 8 MeV MeV ms Assunta di Vacri 18 14/12/2007 E.Kemp - Encontro CBPF - 05/07 94

95 Phase III: Construction of the underground laboratory. Construction of three volume detector and muon veto. Deployment of detector parts, integration and commissioning. 14/12/2007 E.Kemp - Encontro CBPF - 05/07 95

96 Conclusions Reactor neutrino experiments: faster and cheaper measurement of θ 13 Complementarity with accelerator experiments Short baseline Neutrino Oscillations : High precision experiment in Brazil around 2013 (possibility of a previous collaboration with Double Chooz) Previous experiments demonstrate a good capability of using Antineutrinos for Nuclear reactor distant monitoring. Applications: High precision thermal power and fuel composition measurement can be acchieved. Good opportunity develop experimental neutrino physics in Brazil and to contribute to new safeguards techniques. 14/12/2007 E.Kemp - Encontro CBPF - 05/07 96

97 Why not work here? Collaborators are welcomed Thank you! ANGRA III preview 14/12/2007 E.Kemp - Encontro CBPF - 05/07 97