14/12/2007 E.Kemp - Encontro CBPF - 05/07 1
The ANGRA
Neutrino ProjectErnesto Kemp
State University at Campinas - UNICAMP
“Gleb Wataghin” Physics Institute
Cosmic Rays and Chronology Department
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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…
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).
Control room at Savannah River reactor
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OutlineNeutrinos from Reactors: main features of the particle source
Production, Flux and SpectraPhysics with Reactor Neutrinos
Detection and DetectorsMeasurements and Applications
Oscillations (lepton mixing parameters)Control of released thermal powerNuclear fuel composition
The ANGRA Project: all of this in BrazilConclusions
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
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Reactor Neutrinos: main features
Source: copious β-decays from fission process
<Nν> = 6,7 antineutrinos / fission
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Reactor Neutrinos: main features
Pressurized Water Reactors (PWR - wider usage around the world)
The emission has 6 main contributionseν
n-capture in fission fragments
Σ on :
~ 6.7 / fissioneν>< νN
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Antineutrino Flux:
Where: Typical valuesD = distance from reactor core [50 m]Pth = delivered thermal power [4 GW]W = energy release per fission [203.87 MeV]
21-212
][][10241.6
4−
⋅×
><=Φ cms
MeVWGWP
DN th
πν
ν
2-112106.2 −×=Φ cmsν
Reactor Neutrinos: main features
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Spectra
Reactor Neutrinos: main features
ILL Measurements
Phys.Lett. B160, 325 (1985)
Obs.: 238U is only calculated
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Reactor Neutrinos:detection principles…actually we detect anti-neutrinos.
The νe interacts with a free proton (hydrogen) via inverse β-decay:
νe
e+
pn
W
Later the neutron captures giving a coincidence signal. Reines and Cowan used cadmium to enhance the neutron capture
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Just a personal remark:
Things have not been dramatically changed in the last years…
3500 BC
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Just a personal remark:
Things have not been dramatically changed in the last years…
Last week
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This is also true in the field ofReactor 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.
The first successful neutrino detector
1956 … 2006
KamLANDdesign
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Electronics Hut
Steel Sphere
Water Cherenkov outer detector 225 PMTs
1 kton liquid-scintillator
PMTs1325 17”554 20”34% coverage
1km Overburden
Big Detectors:KamLAND (running)
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TitoloSurrounding RockFe shield
Region III (VETO): 90 ton of standard scintillator, 48 PMTGeode: opaque vessel, structure for192 PMT of 8 “Region II (buffer): 17 ton of standard scintillatorRegion I (target): transparent plexiglass vesselfilled with 5 ton of Gd dopedscintillator (< 0.1 % of mass)
Big Detectors:
CHOOZ (France) 1995-1998
6 m
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Smaller ones:Palo Verde (AZ – E.U.A.)1998-1999
2 reactors @
1 @
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Smaller ones:Rovno (Ukraine)1988-1989
10 m
General view of Rovno NPP in Ukraine in 1983
Cores1 & 2
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νe
e+γ
γn
Acrylic volume (20 mm) filled with mineral oil
Thin acrylic walls (5 mm) volume containing scintillator doped with Gd(~0.5 g/l)
outer volume (540 l)
central volume (target, 510 l)
mirror light reflectors
light guides(pure mineral oil)
84 PMT
Smaller ones:Rovno (Ukraine)1988-1989
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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
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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.
Positron energy spectrum implies the neutrino spectrum
In undoped scintillator the neutron will capture on hydrogen
More likely the scintillator will be doped with gadolinium to enhance capture
capturennepe
+→ν
Eν = Evis + 1.8 MeV – 2me
n +H → D* → D + γ (2.2 MeV)
n+ mGd → m+1Gd* →Gd + γ’s (Σ = 8 MeV)
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Physics:Flavor Oscillation (the basics)
νe = ν1 cosθ + ν2 sinθ ν(t)=e−ιΕtν(0)νµ = −ν1 sinθ + ν2 cosθ
P(νe→νµ) = <νµ (t)|νe (0)> = sin2θcos2θ|e-ιE2t-e-ιE1t|2
= sin2(2θ) sin2(1.27 ∆m2L/E)
νµ
νe
ν2
ν1 θ
Mass BasisFlavor basis
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Mixing Matrix (quark sector)
CKM Matrix
0.2~ where1
11
bsd
VVVVVVVVV
b's'd'
23
2
3
tbtstd
cbcscd
ubusud
λλλ
λλλλ
≈
=
For quarks: flavor basis ≈ mass basis
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Mixing Matrix : Neutrinos
=
3
2
1
τ3τ2τ1
µ3µ2µ1
e3e2e1
τ
µ
e
ννν
UUUUUUUUU
ννν
≈−
−
22
21
21
22
21
21
22
22 0
15.0Ue3 <
For neutrinos: flavor basis ≠ mass basis
•PMNS Matrix
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Why Ue3 ?
Ue3 is 100% sensitive to the mixing angle θ13Any observation of CP violation in leptons
requires a non-zero value of θ13
=
3
2
1
τ3τ2τ1
µ3µ2µ1
e3e2e1
τ
µ
e
ννν
UUUUUUUUU
ννν
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Oscillation Probability
P = sin2(2θ) sin2(1.27 ∆m2L/E)∆m2= |m1
2-m22| (eV2)
sin2(2θ) is the strength of the mixing; sin2(2θ)=0 is “no oscillations”E is the neutrino energy (GeV) (∝log(Ep) at accelerator)L is the distance from the source to the detector (km)P is the probability of oscillation. On a parameter space plot, (sin2(2θ) vs. ∆m2), a limit or signal curve corresponds to constant P. The level of sensitivity depends on the statistics.
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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 θ12)
Seen by Super-K and confirmed by Soudan II and K2K. (θ23)
Unconfirmed observation by LSND, currently being investigated by MiniBooNE. Possibly implies the existence of sterile neutrinos or CPT violation.
Current Status
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Open questions:Neutrino Mass Differences
Only 2 independent mass differences
Mass hierarchy unknown
223
212
213 mmm ∆+∆=∆
(∆m2solar~ 5 x 10-5 eV)
(∆m2atm~ 3 x 10-3 eV)
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Open questions:Mixing Parameters
θ13 : the last unknown parameter
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Physics motivations to do accurate measurements of θ13 :
The discovery of neutrino oscillations imply thatneutrinos are massive and that the Standard Model is incomplete. The minimal extension of the SM requires 3 masseigenstates, ν1, ν2, ν3 and a unitary mixing matrixU which relates the neutrino mass basis to theflavor basis. These observations may have profoundastrophysical consequences. CP violation in thelepton sector may hold the key of matter-antimatterasymmetry in the universe.
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3 ν Oscillation Probability Equations
Based on θ12, θ13, θ23
P(νe→νµ) = sin2(2 θ13)sin2(θ23)sin2(∆m2L/4E)P(νe→ντ) = sin2(2 θ13)cos2(θ23)sin2(∆m2L/4E)P(νµ→ντ) = sin2(2 θ23)cos4(θ13)sin2(∆m2L/4E)P(νµ→νe) = sin2(2 θ13)sin2(θ23)sin2(∆m2L/4E)
Ignoring the small ∆m2 scale, CP violation and matter effects.
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How to Measure θ13
Option 1: Accelerator based neutrino beamsP(νµ→ντ) = sin2(2 θ23)cos4(θ13)sin2(∆m2L/4E)
P(νµ→νe) = sin2(2 θ13)sin2(θ23)sin2(∆m2L/4E)
Ignoring matter effects, the small ∆m2 scale and CP violation
~1.0
<0.05
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The θθ2323 Degeneracy ProblemAtmospheric neutrino measurements are sensitive to sin22θ23
But the leading order term in offaxis νµ→νe oscillations is
If the atmospheric oscillation is not exactly maximal (sin22θ23<1.0) then sin2θ23 has a twofold degeneracy
∆=→
νµ νν
ELmP x
2232
232 27.1sinθ2sin)(
∆=→
νµ νν
ELmP e
2132
132
232 27.1sinθ2sinθsin)(
45º 90º2θ 2θθθ
sin2 sinsin2222θθ2323
sinsin22θθ2323
Super-K Measures
Offaxis θ13 Measures
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sin2 2θ 13
δ
~sinδ
~cosδ
There are 2 Observables•P(νµ→νe)•P(νµ → νe)
Interpretation in terms of sin22θ13, δ and sign of ∆m223 depends on the value of these parameters and on the conditions of the experiment: L and E
Minakata and Nunokawa, hep-ph/0108085
Degeneracies in appearance experiments (beam-like)
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Resolving Degeneracies
Experiments at different baselines (affects both L/E and matter)Experiments at different energiesData with neutrinos and anti-neutrinosBetter parameter measurements (θ23)Accelerator experiments cost >U$ 200M and take >10 years to build
But, If θ13 = 0, degeneracies collapse anyway.
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How to Measure θ13
Option 2: Reactor neutrinosP(νe→νe) = 1 - sin2 2θ13 sin2(∆m2
atm L/4E)
P
L/E(km/MeV)
Ignoring small ∆m2
Look for νe disappearance at small distance (L/E)
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Reactor Neutrinos
Eν ~ 4 MeVToo low for CP violation to occur
L ~ 1-4KmToo short for matter effects to begin
No Degeneracy Problems
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(syst) %7.2±
MC (no oscillations assumption) vs data
e+ spectrum
R=data/MC compatible with 1→ non oscillation
CHOOZ results
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MC (no oscillations assumption) vs data
Compatible with no oscillations
Palo Verderesults
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Chooz and Palo Verde Reactor Experiments
•• sin22θ13< 0.18 at 90% CL (at ∆m2=2.0×10-3)
• Future experiments should try to improve on these limits by at leastan order of magnitude.
Down to sin22θ13< 0.01
•• Neither experiments found evidence for νe oscillation.
• This null result eliminated νµ→ νe as the primary mechanism for the Super-K atmospheric deficit.
Chooz Systematic Uncertainties
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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 compositionPrecise determination of fuel refreshment (fuel cycles)Safeguards tool on non-proliferation
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Thermal power measurements using neutrino detection
∫
σf =
Nν = 1
4πR2
Wth
Ef · 1,602×10-19Np ε σf
Σ
ρ(E) σ(E) R(E,T) dE dT
Ethr
Emax
∫T
ρ(E) = αi ρi (E) Ef = αi EiΣi = 5,9,8,1
Σi = 5,9,8,1 i = 5,9,8,1
αi σi
σf =
αi = 1Σ
Change duringreactoroperational cycle
constant
σf, Ef
235U 6.39 201.9239Pu 4.18 210.0238U 8.89 205.5241Pu 5.76 213.6
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Thermal power measurements using neutrino detection
Nν = constant · Wth · Ef
σf
E5
σ5· (1 + k)
Nν = γ · (1 + k) · Wth
Account of fuel composition
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Date2/23/05 2/27/05 3/3/05 3/7/05 3/11/05 3/15/05 3/19/05
Rea
ctor
Pow
er(%
)
-20
0
20
40
60
80
100
Date2/23/05 2/27/05 3/3/05 3/7/05 3/11/05 3/15/05 3/19/05
Ant
ineu
trino
cou
nts
per d
ay0
100
200
300
400
500
600
Predicted count rate using reported reactor powerObserved count rate, 24 hour averageReported reactor power
Checking reactor activity:
Rovno (Ukraine) San Onofre (USA)
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Dependence of the detector rate from reactor power
nν ~ γW
Reactor power in % from nominal value (1375 MW)
Rat
e pe
r 105
sec 174000
events
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Measuring of power production by neutrino method
0 100 200 3000
100
200
300
400
0.9
1.0
1.1
N ν [x103]
ε ν[ G
W⋅ d
ay]
εν/ εT
δεT ~ δWth ·t
δεν ~ 1/(Nν)1/2
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Fuel composition:The Burn-up effect
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Observing the Fuel Burn-up
Calculated cross-section evolution
Observed counting rate evolution : ~ 6%
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Ratio of spectra: time evolution
1 2 3 4 5 6 7visible energy, MeV
1.001.011.021.031.041.051.061.071.081.091.101.111.121.131.141.15
S /Si b
20406080
120
160
200
240280
305S(t)/S(t=0)
time (days) after reactor starts
For standard cycle of PWR at Rovno Nuclear Station, Wth=1375 MW
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Spectra
Reactor Neutrinos: main features – just to remember
Other isotopes than 235U become dominant in higher energies
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2 3 4 5 6 7 8 9
0.00
0.02
0.04
0.06
0.08
0.10
0.12
Eν (MeV)
ρ en d
/ρbe
g–
1
Ratio of neutrino spectra at the beginning and end of reactor campaign
Expected fromILL spectra
Rovno 1988-1990
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Nuclear Reactors Around the World
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How Does The IAEA Monitor Fissile Material Now ?
(1-1.5 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 Declarations2 Verify with Bulk
Accountancy:
(months to years)
Operators Report Fuel Burnup and Power HistoryNo Direct Pu Inventory Measurement is Made Until the Fuel is Reprocessed
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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+SanOnofre) are fully consistent with A
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Where should we go?The present geopolitics of reactor experiments
Angra
Daya Bay
KASKARENO
Double Chooz?
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All of this in BrazilAngra dos Reis Reactor Experiment:The ANGRA Neutrino Project
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The ANGRA collaboration
•17 Researchers14 physicists2 ingeneerings1 Pos-Doc
• 2 Students1 PhD1 Undergraduate
Applying:2 Pos-Docs + 1 MsC students
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Frontier Physics in BrazilVery 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
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Angra dos Reis RJ – Brazil
Angra-IAngra-II
Angra-III
SP
MG
RJ
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Angra dos Reis nuclear plant features
3 Reactors: 2 in operation + 1 planned
--4.0Angra-IIIplanned > 2010
~1.3 years90 %4.0
~ 1.2 x 1020 f/sAngra-II(2000)
~1.5 years80 %1.8Angra-I(1985)
Fuel CycleAverage Uptime
Thermal Power (GW)
Reactor(starting date)
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Institutional Responsibilities
Experimental Group ELETRONUCLEAR
CNEN
construction
operation
regulatorysubmission
approval
All communication channels established !!
Support from brazilian nuclear authorities:ELETRONUCLEAR (Operating Company) CNEN (National Commission for Nuclear Energy)
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Current ConfigurationNear (reference) detector:
50 ton detector (7.2 m dia)300 m from core250 m.w.e.
Far (oscillation) detector:500 tons (12.5 m dia)1500 m from core2000 m.w.e. (under “Frade” peak )
Very Near detector:1 ton prototype project~ 50m of reactor core
Detector ConstructionStandard 3 volume design
reactors
“Morro do Frade”
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Sites
Near Site
Far Site
Very Near Detector(power monitor and safeguards)
Detectors for Neutrino OscilationMeasurements
Reactor
tunnel
500 m
Angra III
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Morro do Frade Zoom Out
Far Site
Near Site
Entrance L = 1500 m
depth = 100 m
Angra-I
View of the Experimental Layout
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Civil Construction Design
25 m
15 m20 m
8 m 1250 m
10 m15 m
10 m
8 m
~100 m
ExperimentalHall
Ground Level
Far Near
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101 102 103 10410-7
10-6
1x10-5
1x10-4
10-3
10-2
10-1
100
Angra
Kaska
Gran Sasso
D-Chooz / Braidwood
Daya Bay
Kamioka
Palo VerdeBugey
µ
vert
ical
inte
nsity
(cm
-2s-1
str-1
)
Far Detector Depth (m.w.e.)
µ Intensity vs. Depthfrom LVD data: PHYS. REV. D, 58, 092005 (1998)
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VND Detector site:
100 m
Selected Places for the
VERY NEAR DETECTOR
shaft ( < 15 m)
50 m
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Expected Rates for Angra
~ 2< 2044Correlated background (9Li)(events/day)
0.3~ 30150Muon rate (Hz)
1000(1500m)
2500(300m)
1000(66m)
Signal(events/day)
FarNear Very Near
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Expected Signal & Background
457100564907148093370
127060
Signal (day)Distance(m)
1108024550350404503075520
Muons (Hz)Depth(mwe)
Cilindrical detector dimensionsR= 1.40m; H=3.10m target=1ton
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Costs: civil construction
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Costs: detectors
Near Detector
$33.4M$9.2MTotal / Detector(design, contingency, etc…..ie. X 2)
$16.7M$4.6MSubTotal
$730K$100KLiquid Scintillator (w/o Gadolinium)($1190 / ton)
$232K$70KMineral Oil ($553 / ton)
$3.6M(3293
Channels)
$1.2M(1054
Channels)
Electronics ($100/channel + $1K/PMT)
$600K$200KSteel / Structural Support (outer sphere + PMT supports)
$11.5M$3MAcrylic (2 concentric spheres)(scaling from SNO)
FarNear
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ν Survival Probabilities: experimental overview
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ν Survival Probabilities: AngraEth= 1.8 MeV (both detectors) ; P=95%@5MeV (far detector)
0,1 1 10 1000,00,10,20,30,40,50,60,70,80,91,0
Far D
etec
tor:
1.5
km
E = 1.8 MeVE = 5.0 MeVE = 1.8 MeV
Nea
r Det
ecto
r: 0
.3 k
m
P (
ν e ν e)
L/E [km/MeV]
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ANGRA’s approach:Precise Shape measurement
Ratio ofenergyspectra
Challenge: uniformity in both detector responses
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90%CL at ∆m2 = 3×10-3 eV2
σcal → bin-to-bin energy calibration error
σnorm → normalization error
From Huber, Lindner, Schwetz and Winter
Statistical error only
Spectral shape only
Exposure (GW·ton·years)
sin2 2
θ 13
Sens
itivi
tyShape vs. Rate A Luminosity Transition
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ANGRA Sensitivity studies
conventions
•d/D: detectors
•b/B: bin (energy)
•capital: correlated
•small: uncorrelated
• 500 ton (fiducial volume)
• 3 years
DC expectations
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Sensitivity studies
conventions
•d/D: detectors
•b/B: bin (energy)
•capital: correlated
•small: uncorrelated
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Reactor ν experiment physics
18,000/yr0.82.00.03340(1)Late 09RENO
15,000/yr0.8 ×0.92.5
0.080.040.025
29(1)29(1+1)80(1+3)
Oct 07(far)
Oct 08(near)Double Chooz
70,000/yr110,000/yr(before/after 2010)
0.75×0.832.50.013700(3)08(fast)09(full)Daya Bay
350,000/yr0.8×0.92.5
0.00700.00600.0055
3900(1)9000(3)
15000(5)2013(full)ANGRA
Far event rate
Efficienciesfor ∆m2
(10-3eV2)Sin22θ sensitivity
GW-t-yr(yr)
Optimistic start dateReactor
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TheThe Neutrino Neutrino DetectorDetector
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)
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Very Near Detector: 3 volumes DesignA) 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
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TheThe Neutrino Neutrino DetectorDetector
PMTs coverage
6.91m
2.5m
2.2m
2.2m
Total area = Sside + Stop + Sbottom
≈ (17.28+3.8+3.8) ≈ 24.88m2
Photocathode area = 0.038m2
20% coverage ⇒ 4.98m2
# PMTs = 4.98/0.038 ≈ 131
0.43m
0,43m0.45m
0.45m
128 PMTs implemented
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Testing the Design: Detailed G4 simulation under construction
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TheThe VETO VETO systemsystem
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TheThe VETO VETO systemsystemX&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
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TheThe VETO VETO systemsystem
Scintillator + fiber setup, built at FNAL, likely to be used at the AMIGA Project under AUGER.
Multianode photomultipliers(Ex: Hamamatsu R8520 series)
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Electronics & DAQ
Input Buffer
Amplifier&
ShaperComparator
LineDriver
To ADC
To Trigger
• Front-end electronicsinput buffer + amplifier/shaper
To ADC: + line driver
To Trigger system: + comparator
•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)
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Neutrino Detection electronics:Laboratory for Detection Systems @ CBPF / BR
• standard: VME 6U
• one module:16 ADC input channels @ 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)ADC FPGA BUFFER
(16cm x 23cm)
front panel
P1
P2
VME bus
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VETO electronics:Laboratory for Detection Systems @ CBPF / BR
FPGA
(16cm x 23cm)
front panel
P1
P2
LVD
S in
putc
hann
els • 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
LVDSreceivers
LVDSreceivers
VME bus
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GEANT(Madrid – ES)
RNPRNP
BrazilianNational Education
and Research Network
CLARA
Latin American Advanced Networks
1Gbps
1Gbps
622MbpsUSA
400Mbps
Rede-Rio100 Mbps
USA
155Mbps
NetworkNetwork InfraInfra--structurestructure for for thetheAngra Neutrino DetectorAngra Neutrino Detector
152.
84.0
.0/1
6
RouterFirewall
CBPFCBPF
...Ethe
rnet
LA
NMinimum 512Kbps
Optimum: 1 Mbps
TelecomInfra-strucutre
Angra PoP
Private Line
152.84.55.0/24
Ethernet Switch
DAQ - DataAcquisition
System
Radio orOptical Fiber Link
2 Steps:1 – Infra-structure investment: router, switch, radio (fiber).2 – permanent private connection (CBPF-Angra)
2 Steps:1 – Infra-structure investment: router, switch, radio (fiber).2 – permanent private connection (CBPF-Angra)
VoIP
VoIP
PSTN
Extension of CBPF LAN´s.RioRio AngraAngra
Data Storage (Mirror) Data
Storage
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Alternatives:Single Ended Readout?
Could Reduce footprint by 1.5 – 2 metersReduce height by 60-90 cm.Significant reduction in number of PMTsProblem: Long path lengths for reflected light
Target
GammaCatcher
Mineral OilBuffer
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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.
Non-proliferation effort in ANGRA
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ABACC + ANGRA Project
ASSESSMENT
of the
TECHNICQUE
+ IAEA !
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ANGRA itens just under project
Front-end ElectronicsDAQData transfer & Communications : Nuclear Complex << = >> Research Institutions
On work:Construction IngeneeringSimulations
Deployment and operations strategies
Customized FPGA boards
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Angra Project:Present Status
Meeting September 05, 2006 with Eletronuclearrepresentatives to define next step.
Authorization to place a container next to thereactor building.
Detailed project under way to be presented to the Minister of Science and Technology and to FAPESP.
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Deploiment Streategy:Phase I: Setup infrastructure at the Angra site:
- 20’ container near the reactorbuilding
- Measurement of local muonflux: Cerenkov detector (Auger test tank)
- Muon telescope (4 Minos typescintillator planes)
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Deploiment StrategyPhase I:Setup infrastructure at CBPF & UNICAMP:
Start to test componentsat CBPF and UNICAMP:- 8” phototubes- VME electronics
Measurement of radioactivebackground (rocks and
sand)
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Phase II: Deploy LVD tank
ISNP, 23/09/05ISNP, 23/09/05 Assunta di VacriAssunta di Vacri 1818
252252CaCa
PMTPMT
Capture on H vs Gd
• <T> capture [t]: 200 µs vs ~30 µs• efficiency [ε(≥Eth)]: 60% vs ~70%
Test on the Test on the dopeddoped TankTank
∑Eγ emitted in the n-capture ・ 8 MeV
MeV
ms
- 1 ton gadolinium doppedliquid scintillator tank
- test signal+background
- Tests with Californiumsource
- Final site selection forunderground laboratory
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Phase III:Construction of the underground laboratory.
Construction of three volume detector and muon veto.
Deployment of detector parts, integration and commissioning.
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ConclusionsReactor neutrino experiments: faster and cheapermeasurement of θ13
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.
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Why not work here ?Collaborators are welcomed…Thank you !
ANGRA III “preview”