soo-bong kim dept. of physics & astronomy seoul national university april 15, 2009
DESCRIPTION
A Korean Project of Neutrino Oscillations. Soo-Bong Kim Dept. of Physics & Astronomy Seoul National University April 15, 2009. 14 C b decay. Physics in trouble with b decay. Energy & momentum are not conserved. F. A. Scott, Phys. Rev. 48 , 391 (1935). Predicted discrete spectra. - PowerPoint PPT PresentationTRANSCRIPT
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Soo-Bong Kim
Dept. of Physics & Astronomy Seoul National University
April 15, 2009
A Korean Project of Neutrino Oscillations
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Birth of NeutrinoBirth of Neutrino
Total spin is not conserved, either… 14C 14N + e–
spin 0 spin 1 spin 1/2
Bohr: Energy and momentum may not be conserved in decay ?…
F. A. Scott, Phys. Rev. 48, 391 (1935)Observed continuous spectra Predicted discrete spectra
14C decay
Physics in trouble with decay Energy & momentum are not conserved
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Wolfgang Pauli’s introduction of an imaginary particle (1931)
Wolfgang Pauli’s introduction of an imaginary particle (1931)
Neutrino : Undetectable massless neutral fermion (Weakly interacting)
Neutrino
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Neutrino: Elementary Particles
Elementary particles with almost no interactions
Almost massless: impossible to measure its mass
Universe full of neutrinos
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Tiny Neutrino Masses
E=mc2
mass
10-27kg10-30kg10-36kg
SM
GUT
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Mixing Angles
(12 , 23 , 13)
Unmeasured yet
Oscillating Neutrinos
Three flavors of neutrinos repeat transformation among them as time goes by.
Discovery of Neutrino Oscillations (1998)CKM Quark Mixing and CP Violation
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Properties of Neutrinos
Almost no interaction with matter (via weak interaction only)
Mass is too small to measure
Elementary particles with three flavors (e, , )
Transformation among the three flavors
Universe full of neutrinos (330 per 1cm3)
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Why is the neutrino physics so improtant?Why is the neutrino physics so improtant?
Neutrino Oscillation and Mass Window for New Physics !
Origin of Our Universe !!
Neutrinos are hot !
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1
2
Neutrino OscillationNeutrino Oscillation
1 2
m1 m2
Flavor states Mass states
• neutrino oscillations due to wave property of neutrino
1 1
2 2
cos sin
sin cos
m
m
im t p im t pt e e 2 21 2/ 4 / 4
1 2| , | cos ( ) | s in ( )
2
1
2-Neu
trin
o Osc
illat
ion
2-Neu
trin
o Osc
illat
ion
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Oscillation Probability Oscillation Probability
Neutrino energy
Neutrino trajectory
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Solar Neutrino(e) OscillationsSolar Neutrino(e) Oscillations
Nuclear fusion : 4p → 4He + 2e+ + 2e + thermal energy
Deficit of solar neutrinos → Evidence for oscillations
- Homestake (Cℓ, 1968~1993): first measurement
- Kamiokande (H2O, 1986~1993): energy/directionality
- SAGE & GALLEX/GNO (Ga, 1990~2001)
- Super-Kamiokande (H2O, 1996~ ): precision exp.
Discovery of Solar Neutrino Oscillations
- SNO (D2O, 2002): detect / (e → & )
Confirmation of Solar Neutrino Oscillations
- KamLAND (2002): reactor neutrino oscillation
12 측정 )
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Atmospheric Neutrino() OscillationsAtmospheric Neutrino() Oscillations
Cosmic ray (p, He, …) + Atmosphere → /K meson → → e +
Discovery of atmospheric neutrino oscillations ( → )
- Super-Kamiokande (1998)
- measurement of 23
Confirmation of atmospheric neutrino oscillations
- K2K (2004) : accelerator beam (250km)
- MINOS CNGS (2006) : ~700km
23 측정 )
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Summary of Neutrino Oscillation Parameters
23
12
13
m12
2 = 7.9(5% )10-5 eV2
m23
2 = 2.4(13% )10-3 eV2 ≈ m132 mass difference :
sin212
= 0.31(9%)
sin223
= 0.44(+20–11% )
sin213
< 0.17 (90% C.L.) mixing angles :
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Precision Measurementof Neutrino Oscillation Parameters
Ue3
(New field of particle physics open!)
U Ue1 Ue2 Ue 3
U1 U2 U 3
U1 U 2 U 3
1 0 0
0 cos23 sin23
0 sin23 cos23
cos13 0 e iCP sin13
0 1 0
e iCP sin13 0 cos13
cos12 sin12 0
sin12 cos12 0
0 0 1
1 0 0
0 e i / 2 0
0 0 e i / 2i
0reactor and accelerator
13 = ?
atmospheric SK, K2K
23 = ~ 45°Large and maximal mixing!
(atmospheric neutrinos & neutrino beams)
SNO, solar SK, KamLAND
12 ~ 32°
(Solar neutrinos& reactor neutrinos)
?
CP : CP phase
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13 from Reactor and Accelerator Experiments
Pee 1 sin2 213 sin2 m312L
4E
cos4 13 sin2 212 sin2 m21
2L
4E
- Clean measurement of 13
- No matter effects
CP violation
mass hierarchy
matter
* Reactor
* Accelerator
- sin2213 is a missing key parameter for any measurement of CP
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Nuclear Power Plants
Reactor Neutrinos
영광
울진
Reactor Neutrinos
인체에 유해한 방사능 ( 중성자 , 알파선 , 베타선 , 감마선 ) 은 원자로 내부에서 차폐됨
핵붕괴시 방출되는 중성미자는 물질과 거의 반응을 하지 않으므로 인체에 무해하며 원자로를 빠져 나와서 사방으로 끊임없이 퍼져 나감 ( 매초당 ~1017/m2 방출 ) 영광발전소는 열생산 최대용량이
17GW 로서 세계 2 위의 강력한 중성미자 방출원임
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Energy Spectra of Reactor NeutrinosEnergy Spectra of Reactor Neutrinos
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Detection Method of Reactor Neutrinos(Reines & Cowan, 1957)
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(2) 5<Edelayed <11MeV
n capture energy
Detection of Reactor Neutrinos
p
νe
e+
e-
γ(0.511MeV)
γ(0.511MeV)
n
Gd
γ
γ γ
γ
E ~ 8MeV
30μs
prompt signal
Delayed signal(1) 0.7<Eprompot <9MeV
e+ energy
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Chooz: 13<130
RENO (13 )
KamLAND (12)
Reactor Neutrino ExperimentsReactor Neutrino Experiments
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New Reactor Neutrino Experiment (13)
Need identical detectors to reduce the systematic errors in 1% level
Detectors should be at underground to reduce the cosmic-ray backgrounds
Find disappearance of e fluxes due to neutrino oscillation as a function of energy using multiple, identical detectors
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Oscillation Parameters from Reactor Neutrinos
0
0.2
0.4
0.6
0.8
1
1.2
0.1 1 10 100 1000
L(km)
P(νe
->
νe)
sin2 13=0.1
L~50km: accurate sin2212
sin2213=0.1, E=4MeV
P e e 1 sin2 213sin2 m132 L
4E
P e e 1 sin2 212sin2 m122 L
4E
L~1.5km: pure sin2213 L~5km: m213
Scope of RENO Project
L~180kmKamLAND:accurate m2
12
moderate 12
3RENO
)1%(4.2~sin
sin
122
122
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Reduction of Reactor Neutrinos due to Oscillations
sin2213 > 0.01 with 10 t• 14GW• 3yr ~ 400 t•GW•yr (400 t•GW•yr: a 10(40) ton far detector and a 14(3.5) GW reactor in 3 years)
Dis
app
eara
nce
Reactor neutrino disappearance Prob. due to 13 with the allowed 2 range in m23
2
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Double-CHOOZ (France)
* Proposal (June 20, 2006) : hep-ex/0606025
Double-Chooz Collaboration: France, US, Germany, Italy, Japan, England, Brasil, Spain & Russia
* 2010 년 근거리 /원거리검출기 동시 가동
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Daya Bay (China)
* Proposal to DOE (Jan. 15, 2007): hep-ex/0701029
Daya Bay Collaboration: China, US, Czech Republic, Hong Kong, Russia & Taiwan
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Experiment Location
Thermal
Power
(GW)
Detector Locations
Near/Far
(m)
Depth
Near/Far
(mwe)
Target
Near/Far
(tons)
Double-CHOOZ France 8.7 280/1050 60/300 10/10
RENO Korea 17.3 290/1380 120/450 16/16
Daya Bay China 11.6 360(500)/1985(1613) 260/910 402/80
World Competition in the Reactor Neutrino Experiments
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Chonnam National University Dongshin University Gyeongsang National University Kyungpook National University Pusan National University Sejong University Seoul National University Sungkyunkwan University Institute of Nuclear Research RAS (Russia) Institute of Physical Chemistry and Electrochemistry RAS (Russia)
+++ http://neutrino.snu.ac.kr/RENO
RENO Collaboration
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RENO Experimental Setup
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Google Satellite View of YongGwang Site
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Schematic View of Underground FacilitySchematic View of Underground Facility
100m 300m
70m high
200m high
1,380m
290m Far Detector
Near Detector Reactor
s
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Schedule for RENO Construction
Activities
Detector Design& Specification
Geological Survey& Tunnel Design
DetectorConstruction
DetectorCommissioning
2006 2007 2008 20093 6 9 12 3 6 9 12 3 6 9 12 3 6 9 12
Detector construction
Tunnel excavation
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Rock sampling (DaeWoo Engineering Co.)
Rock samples from boring
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Rock quality map
• Near detector site: - tunnel length : 110m
- overburden
height : 46.1m
• Far detector site: - tunnel length : 272m- overburden
height : 168.1m
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Stress analysis for tunnel design
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Mixing & Supplying Liquid Scintillators
Data Acquisition System
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Mockup Detector Event Display
Real time display: Online monitoring tool
Basic information on histograms
PMT hit display
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RENO Detector Design and Specification
RENO Detector
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Structure design completed (’08. 12)
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PMT test completed & under purchase
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Use SK new electronics
광센서의 신호를 초고속 처리하는 ASIC을 사용한 데이터 수집 장비
DAQ Electronics completed (’08. 11)
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Mixing for Liquid Scintillator :
Aromatic Solvent
Flour WLS Gd-compound
LAB PPO, BPO
Bis-MSB, POPOP
0.1% Gd+TMHA
(trimethylhexanoic acid)
0.1% Gd compounds with CBX (Carboxylic acids; R-COOH) 합성 연구 :
- CBX : TMHA (trimethylhexanoic acid), MVA (2-methylvaleric acid)
R&D of Gd Loaded Liquid Scintillator
LAB(Linear Alkyl Benzene) Properties :
CnH2n+1-C6H5 (n=10~14) Light yield measurement
PC100% LAB100% PC40% PC20% LAB100% PC20% N2 LAB60% LAB80% MO80%
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Synthesis of Gd-carboxylateprecipitation
Rinse with 18MΩ water
Dryer
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R&D with LAB
Light yield measurement
PC100% LAB100% PC40% PC20% LAB100% PC20% N2 LAB60% LAB80% MO80%
CnH2n+1-C6H5 (n=10~14)
• High Light Yield : not likely Mineral oil(MO)• replace MO and even Pseudocume(PC) probably• Good transparency (better than PC)• High Flash point : 147oC (PC : 48oC)• Environmentally friendly (PC : toxic)• Components well known (MO : not well known)• Domestically available: Isu Chemical Ltd. (
이수화학 )
PC 와 Mineral oil/Dodecane 대용으로 사용할 수 있는 LAB(Linear Alkylbenzene) 의 분자 구조식
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Measurement of LAB Components with GC-MS
C16H26 C17H28 C18H30 C19H32
7.17% 27.63% 34.97% 30.23%
LAB : (C6H5)CNH2N+1
# of H [m-3] = 0.631 x 1029
H/C = 1.66
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Raw/MCRaw/MCDataData
ProductionProductionModulesModules
ReconstructionReconstructionModulesModules
UserUserAnalysisAnalysisModulesModules
UserUserntuplesntuples
RACFrameWork
default modules data input and output, database access for run configuration and calibrationHas talk-to function for changing input parameters without recompilingAddition of modules by userModules can be set as filter module for selecting eventsEasy to use and build in RENO software environment
RRENO AAnalysisnalysis CControlontrol
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Inverse Beta DecayInverse Beta Decay
Cosmic MuonCosmic Muon
RENO Event Display
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target
buffer
-catcher
Reconstruction of Cosmic Muons
~140cm
~40cm
~120cm
A
B
C
D
Veto(OD)
Buffer(ID)
pulse height timeOD PMTs
ID PMTs
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Reconstructed vertex: ~8cm at the center of the detector
Reconstruction : vertex & energy
1 MeV (KE) e+
Energy response and resolution:
%)14.00(E
)%03.074.7(EE
visible energy
3.01.29
/MeV 9.08.208
PMT coverage, resolution
~210 photoelectrons per MeV
|y|
y (
mm
)
Evis (MeV)
y
4 MeV (KE) e+
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Calculation of Background Rates due to RadioactivityConcentration
40K (ppb) Concentration
232Th (ppb) Concentration
238U (ppb) 40K [Hz] 232Th [Hz] 238U [Hz]
Total [Hz]
Rock 4.33(ppm) 7.58(ppm) 2.32(ppm) 1.06 7.14 0.99 9.19
LS in Target 0.001 0.001 0.001 0.90 0.09 0.26 1.25
Target Contatiner 0.008 0.05 0.008 0.08 0.06 0.03 0.17
LS in Gamma Catcher 0.001 0.001 0.001 1.52 0.13 0.38 2.03
Gamma Catcher Container
0.008 0.05 0.008 0.07 0.04 0.03 0.14
LS in Buffer 0.001 0.001 0.001 0.08 ~ 0 0.03 0.11
Buffer Tank 0.06 0.9 0.9 0.03 0.10 0.20 0.33
PMT 13.6 208.5 49.4 2.50 5.23 2.99 10.72
Total ~24
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Systematic ErrorsSystematic Source CHOOZ (%) RENO (%)
Reactor related absolute
normalization
Reactor antineutrino flux and cross section
1.9 < 0.1
Reactor power 0.7 < 0.1
Energy released per fission
0.6 < 0.1
Number of protons in
target
H/C ratio 0.8 0.2
Target mass 0.3 < 0.1
Detector Efficiency
Positron energy 0.8 0.2
Positron geode distance 0.1 0.0
Neutron capture (H/Gd ratio)
1.0 < 0.1
Capture energy containment
0.4 0.1
Neutron geode distance 0.1 0.0
Neutron delay 0.4 0.1
Positron-neutron distance
0.3 0.0
Neutron multiplicity 0.5 0.05
combined 2.7 < 0.6
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RENO Expected Sensitivity
10x better sensitivity than current limit
New!! (full analysis)
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GLoBES group workshop@Heidelberg – Mention’s talk
SK m2