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Daya Bay Reactor Neutrino Oscillation Experiment Jen-Chieh Peng - - PowerPoint PPT Presentation
Daya Bay Reactor Neutrino Oscillation Experiment Jen-Chieh Peng - - PowerPoint PPT Presentation
Daya Bay Reactor Neutrino Oscillation Experiment Jen-Chieh Peng University of Illinois at Urbana-Champaign (on behalf of the Daya Bay Collaboration) International Workshop on Double Beta Decay and Neutrinos Osaka, Japan, June 11-13,
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Outline
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Physics case for a precise measurement The proposed Daya Bay neutrino oscillation experiment Schedule and expected sensitivity of the Daya Bay experiment θ
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What we have learned from neutrino
- scillation experiments
2 2 2 5 2 21 2 1 2 2 2 3 2 32 3 2 e 12 13 12 13 13 12 23 12 2
(7.9 0.7) 10 ev (90%c.l.) | | | | (2.4 0.6) 10 1) Neutrinos are massive 2) Neutrinos do mix with each ot ev (90% ) e c.l. h r
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m m m m m m c c s c s e s c c s
δ µ τ
ν ν ν
− − −
∆ = − = ± × ∆ = − = ± × = − −
1 3 13 12 23 12 23 13 23 13 2 12 23 12 23 13 12 23 12 23 13 23 13 3 12 23 3 3 1 1 12 2 3
( cos , sin ) 13 , 2. 34 , 45 , 13 for the l 2 , epton MNSP Matrix
i i i i ij ij ij ij
s e c c s s s e s c s s c c s e c s s c s e c c c s
δ δ δ δ
θ θ θ ν ν ν θ θ θ θ θ − − − − = ≤ =
- 3) Neutrino masses and mixings have provided clear evidence for
physic .22 for the quark C s beyond the Stand KM Matrix ard Model
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What we do not know about the neutrinos
- Dirac or Majorana neutrinos?
- Mass hierachy and values of the masses?
- Existence of sterile neutrinos?
- Value of the θ13 mixing angle?
- Values of CP-violation phases?
- Origins of the neutrino masses?
- Other unknown unknowns …..
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What we know and do not know about the neutrinos
e 12 13 12 13 1 12 23 12 23 12 23 12 23 23 13 2 12 23 12 23 12 23 13 13 12 23 23 1 3 3 1 13 13 3 i i i i i
s e s e s e s c c s c s c c s c c s s s c s s c c c s e s c c e s c
µ δ δ δ δ δ τ
ν ν ν ν ν ν
−
= − − − − − −
- What is the νe fraction of ν3?
(proportional to sin2θ13)
- Contributions from the CP-phase
δ to the flavor compositions of neutrino mass eigenstates depend
- n sin2θ13)
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Why measuring θ13?
A measurement of sin22θ13 at the sensitivity level of 0.01 can rule out at least half of the models!
- Models based on the
Grand Unified Theories in general give relatively large θ13
- Models based on
leptonic symmetries predict small θ13
A recent tabulation of predictions of 63 neutrino mass models on sin2θ13 (hep-ph/0608137)
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Why measuring θ13?
A measurement of sin22θ13 AND the mass hierarchy can rule out even more models!
A recent tabulation of predictions of 63 neutrino mass models on sin2θ13 (hep-ph/0608137)
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Why measuring θ13?
Leptonic CP violation
2 12 12 13 13 23 23 2 2 2 13 23 12
( ) ( ) 16 sin sin sin sin 4 4 4
e e
P P s c s c s c m m m L L L E E E
µ µ
ν ν ν ν δ → − → = − ∆ ∆ ∆ If sin22θ13 > 0.02-0.03, then NOvA+T2K will have good coverage on CP δ. Size of sin22θ13 sets the scale for future leptonic CP violation studies
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Current Knowledge of θ13
- ∆
× −
θ13
- !
- θ
θ θ θ
"#$%#∆
&× −
θ θ θ θ
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decay pipe horn absorber target p detector
π+ π+ µ+
'())*+ '(,)*+
- µ ≈ θ θ ∆
- .
&* ν +
- ≈ − θ ∆
- .
&* ν + )& θ θ ∆
- .
&* ν
/ ν → 0 )+ / 12345##)1%6 / $6) / νµ → ν )+ / ++)θ / 12345##) / +$
Some Methods For Determining θ13
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Detectingν : Inverse β Decay
ν + → 7 7 35 → 7→ 8 7γ3'5365 → 79 → 9: → 9 7γ;3!'5365 / < 6 %1)4%$ / *6#ν $16( *ν ≈ <7 7< 73 577≈ <7 7!'
&4
/ <)$β
β β β)6 =9>%
)(
Eν (MeV) 2 3 4 5 6 7 8 9 10
Arbitrary
F l u x Cross Section Observable ν Spectrum
From Bemporad, Gratta and Vogel
1 1
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Measuring θ13 with Reactor Neutrinos
Search for θ13 in new oscillation experiment
~1-1.8 km > 0.1 km
2 4 2 2 21 13 2 2 2 31 13 12
cos sin 2 sin 2 si sin 4 1 n 4
ee
m L E m P L E
ν ν
θ θ θ ∆ ∆ − ≈ −
θ θ θ θ13
0.3 0.4 0.5 0.6 0.7 0.8 0.9 1 1.1 0.1 1 10 100
Nosc/Nno_osc Baseline (km) Large-amplitude
- scillation due to θ12
Small-amplitude oscillation due to θ13 integrated over E
∆ ∆ ∆ ∆m2
13≈
≈ ≈ ≈ ∆ ∆ ∆ ∆m2
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detector 1 detector 2
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Results from Chooz
=9>%) )ν7→ 7 7 .4 8
- !&9?
,( @$63#%5 )% &146
@ν ) 3)%=145 6
A6)%)
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- Increase statistics:
– Use more powerful nuclear reactors – Utilize larger target mass, hence larger detectors
- Suppress background:
– Go deeper underground to gain overburden for reducing cosmogenic background
- Reduce systematic uncertainties:
– Reactor-related:
- Optimize baseline for best sensitivity and smaller reactor-related errors
- Near and far detectors to minimize reactor-related errors
– Detector-related:
- Use “Identical” pairs of detectors to do relative measurement
- Comprehensive program in calibration/monitoring of detectors
- Interchange near and far detectors (optional)
How to Reach a Precision of 0.01 in sin22θ13?
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World of Proposed Reactor Neutrino Experiments
Angra, Brazil Diablo Canyon, USA Braidwood, USA Chooz, France Krasnoyasrk, Russia Kashiwazaki, Japan RENO, Korea Daya Bay, China
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Location of Daya Bay
/ &4# AB / 4# CD
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!!"##$ × × × × % &'(() "##$ × × × × % (*("##$ × × × × %
9? × νe )
The Daya Bay Nuclear Power Complex
/ #% 3 9?5 / ##%163& 9?5 / E)%6 )%)%) %%1%##) $1%%))6
18 ( *( "## "## ) "## +'
,-.( )($%% %))% /' )(1 %%$B%
<(@
0-
1
- 2
- ( *("
#86 "6 2$1%(F! " @#. 2$1%( / #. F!#86 2$1%(
- /
3' !#. #86 2$1%(!
+ +
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Conceptual design of the tunnel and the Site investigation including bore holes completed
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Tunnel construction
- The tunnel length is about 3000m
- Local railway construction company has a lot of experience
(similar cross section)
- Cost estimate by professionals, ~ 3K $/m
- Construction time is ~ 15-24 months
- A similar tunnel on site as a reference
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Antineutrino Detectors
- Three-zone cylindrical detector design
– Target zone, gamma catcher zone (liquid scintillator), buffer zone (mineral oil) – Gamma catcher detects gamma rays that leak out
- 0.1% Gd-loaded liquid scintillator as
target material
– Short capture time and high released energy from capture, good for suppressing background
- Eight ‘identical’ detector modules, each with 20 ton
target mass
– ‘Identical’ modules help to reduce detector-related systematic uncertainties – Modules can cross check the performance of each other when they are brought to the same location
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- !"#
$%&'()*!+#,-# )$!./0 *$$1)-#
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Detector Prototype at IHEP
- 0.5 ton prototype
(currently unloaded liquid scintillator)
- 45 8” EMI 9350 PMTs:
14% effective photocathode coverage with top/bottom reflectors
- ~240 photoelectron
per MeV : 9%/√E(MeV)
prototype detector at IHEP
Energy Resolution
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Background Sources
- 1. Natural Radioactivity: PMT glass, steel, rock,
radon in the air, etc
- 2. Slow and fast neutrons produced in rock &
shield by cosmic muons
- 3. Muon-induced cosmogenic isotopes: 8He/9Li
which can β β β β-n decay
- Cross section measured at CERN (Hagner et. al.)
- Can be measured in-situ, even for near detectors
with muon rate ~ 10 Hz
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- F!
- !
Cosmic-ray Muon
/ G#9 B #))6#%+%#) / 6'GAHI%#% 6J6
138 97 60 55 Mean Energy (GeV) 0.041 0.17 0.73 1.16 Muon intensity (Hz/m2) 355 208 112 98 Overburden (m) Far Mid Ling Ao DY B
( *( / 3'
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Muon System
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Water Shield
- Pool around the central detectors - 2.5m water in all directions.
- Side, bottom & AD surfaces are reflective (Tyvek or equivalent)
- Outer shield is optically separated 1m of water abutting sides and bottom
- f pool
– PMT coverage ~1/6m2 on bottom and on two surfaces of side sections
- Inner shield has ≥1.5m water buffer for AD’s in all directions but up,
there the shield is 2.5m thick
– 8” PMTs 1 per 4m2 along sides and bottom - 0.8% coverage
Far Hall
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Muon System Active Components
- Inner water shield
–
415 8” PMTs
- Outer water shield
– 548 8” PMTs
- RPCs
– 756 2m × 2m chambers in 189 modules – 6048 readout strips
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Summary of Systematic Uncertainties
0.32% (Daya Bay near) 0.22% (Ling Ao near) 0.22% (far) Backgrounds 0.2% Signal statistics 0.38% (baseline) 0.18% (goal) Detector (per module) 0.087% (4 cores) 0.13% (6 cores) Reactors Uncertainty sources
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