neutrino physics and detectors - ihepindico.ihep.ac.cn/event/6387/session/13/... · sbnd ) nmo...
TRANSCRIPT
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Neutrino Physics and Detectors
Liangjian Wen
International Conference on Technology and Instrumentation in Particle Physics (TIPP), Beijing, May 21-26, 2017
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What we have learned?
2
𝑉𝑉 =1 0 00 𝑐𝑐23 𝑠𝑠230 −𝑠𝑠23 𝑐𝑐23
𝑐𝑐13 0 𝑠𝑠13𝑒𝑒−𝑖𝑖𝛿𝛿0 1 0
−𝑠𝑠13𝑒𝑒𝑖𝑖𝛿𝛿 0 𝑐𝑐13
𝑐𝑐12 𝑠𝑠12 0−𝑠𝑠12 𝑐𝑐12 0
0 0 1
𝑒𝑒𝑖𝑖𝜌𝜌 0 00 𝑒𝑒𝑖𝑖𝜎𝜎 00 0 1
Standard Parametrization of the PMNS Matrix
𝜽𝜽𝟐𝟐𝟐𝟐 ~ 𝟒𝟒𝟒𝟒∘
Atmospheric,LBL accelerator
𝜽𝜽𝟏𝟏𝟐𝟐 ~ 𝟗𝟗∘
Reactor,LBL accelerator
𝜽𝜽𝟏𝟏𝟐𝟐 ~ 𝟐𝟐𝟒𝟒∘
Solar,KamLAND
0ν2β, LNV?
Quarks vs. Leptons: A big puzzle of fermion flavor mixings
|𝑈𝑈| = |𝑉𝑉| =
CKM PMNS
Hierarchy! Approximate μ-τ symmetry?
|𝚫𝚫𝒎𝒎𝟐𝟐𝟐𝟐𝟐𝟐 | ~ 𝟐𝟐.𝟒𝟒 × 𝟏𝟏𝟏𝟏−𝟐𝟐 eV𝟐𝟐 𝜹𝜹 ~ ? 𝚫𝚫𝒎𝒎𝟐𝟐𝟏𝟏
𝟐𝟐 ~ 𝟖𝟖 × 𝟏𝟏𝟏𝟏−𝟒𝟒 eV𝟐𝟐
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Future Neutrino Puzzles
3
Fritzsch-Xing Plot
∆m231>0 ?
δCP ?ν=ν ?
UPMNSU+PMNS = I ?
νs exists ?…
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Neutrino physics:problems and methods
Mass GeologyAstronomyDirac/Majorana
Oscillation/sterile neutrinos
Magnetic moments Cosmology
Reactor EarthSolarAtmos-phericAcceleratorRadioactive
sourcesAstro-objects
Relic-neutrino
Liquid scintillator
Semiconductor/crystals/gaseous/scintillator
EmulsionNuclear chemistry
Water Cerenkov
Samplingdetector
Liquid Argon
Y.F. Wang @ TIPP2011
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Apologies for incompleteness, bias and mis-handling
Selected Topics• Neutrino oscillations (running & future)
– Reactor neutrinos: Daya Bay, Double Chooz, RENO, JUNO, RENO-50, …– Accelerator neutrinos: T2K, NoVA, LBNF/DUNE– Atmospheric neutrinos: ORCA, Hyper-K, PINGU, INO, …– Solar neutrinos: SuperK, SNO, Borexino, …– Sterile neutrinos
• NLDBD searches– KamLAND-Zen, EXO, Gerda, Majorana, CUORE/CUPID, SNO+, NEXT,
SuperNEMO, PandaX-III, AMoRE, CANDLES, COBRA, …
• Neutrino astronomy– Supernova in combination with solar/atmospheric/reactor neutrino
detectors– Geo-neutrinos in combination with solar/reactor neutrinos– High energy neutrinos (not covered in this talk)
5
Precision Measurements
ν=ν ?δCP=?
∆m31>0?
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Reactor Experiments
6
Daya Bay Double Chooz
RENO
• Daya Bay– Δ(sin22θ13) ~ 0.003 ~3%– Δ(Δm2
ee) ~ 0.07 ~ 3%– operation till 2020
• RENO: ~5%.– operation funding secured until
Feb. 2019
• Double Chooz: ~10%– secured to Jan. 2018 (may change)
by J. Zhao
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Sterile ν exists?
7
Parameter space allowed by LSND and MiniBooNE is excluded by the combination of MINOS(+), Daya Bay and Bugey-3
Next generation sterile experiments are almost ready(SOX, PROSPECT, SoLid, Chandler, NEOS, Neurino4, DANSS, nuLat, …)
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NOvA Far Detector(on surface)Ash River, MN810 km
NuMI beam and NOvA Near detector Fermilab
14 mrad
Accelerator Experiments
8
T2K
MINOS
OPERA
NOν A
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Hits on δCP
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Future Neutrino Detectors for neutrino mass ordering and δCP
RENO-50
INO
( protoDUNE,MicroBooNE, ICARUS-T600,
SBND )
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NMO determination at JUNO
• Physics– NMO determination: 3-4σ in 2026– Precision measurement of 3/6 mixing parameters – Rich physics: supernova-ν, geo-ν, atmospheric-ν, solar-ν, exotics, etc
• Key: get max. photons in a 20 kton LS detector– High QE PMT, high coverage– High transparent LS (> 20m A.L @430nm)– Low radioactivity (< 10-15 g/g (U, Th)) 11
JUNORENO-50
reactor ν expts.
Independent on CP phase and θ23 (Acc. & Atm. do). Energy Resolution is the key
J. Phys. G43:030401 (2016)
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Central detector
Water Cherenkov
Top Tracker
Calibration
Pool
Dep
th: 4
4m
Pool ID:43.5m
AS: ID35.4m
SSLS: ID40.1m
AS: Acrylic sphere; SSLS: stainless steel latticed shell
Filling +Overflow
Acrylic sphere(20Kt LS in it)
~18000 20” PMT+~25000 3’’ PMT
~2000 20’’ PMT
SS latticed shell
Electronics
Acrylic Sphere: ID: 35.4mThickness:120mm
SSLS:ID: 40.1mOD: 41.1m
Water poolID: 43.5mHeight: 44mWater Depth: 43.5m
JUNO Detectors
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Success: 20” MCP-PMT
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MCP Principle
Project Team
• Advantages:– Higher QE: transmissive
photocathode at top + reflective photocathode at bottom
– High CE: less shadowing effect– Easy for production: less manual
operation and steps
5”(8”) Prototype
20” Prototype
Design Production
2009 2010~2013 2013~2015 2016~2019
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MCP-PMT Performance
14Min:24.5%; Max:29%
Average:26.5%
QE & uniformity Dark rate
After pulse
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PMT Purchasing of JUNO
15
15k MCP-PMT (75%) from NNVT5k Dynode(25%) from Hamamatzu
Dec.16, 2015Characteristics unit MCP-PMT
(NNVC)R12860
(Hamamatsu)Detection Efficiency
(QE*CE*area) % 27%, >24% 27%, >24%
P/V of SPE 3.5, > 2.8 3, > 2.5TTS on the top point ns ~12, < 15 2.7, < 3.5Rise time/ Fall time ns R~2, F~12 R~5,F~9 Anode Dark Count Hz 20K, < 30K 10K, < 50K
After Pulse Rate % 1, <2 10, < 15
Radioactivity of glass ppb238U:50232Th:5040K: 20
238U:400232Th:40040K: 40
By Scaling PMT Spec for LS quantity to reach 3σ@ 6year
Decision based on risk, price, performance merit for physics
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Challenge: LS Purification• Extremely clean LS in Borexino,
relatively mature technology• Technologies
– Al2O3 column, distillation, gas striping, water extraction
16
LS pilot plant in Daya Bay LS hall.
A new batch of purified LS was produced and filled into DYB-AD1. evaluate radioactivity optimize LS recipe
Borexino, N. Rossi @ Neutrino2016
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Accelerator ν
NMO & δCP determination via Matter Effects
17
νμ νe
Atmospheric ν
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Hyper Kamiokande
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SuperK50 kt, PMT coverage: ~40%
Threshold: ~4 MeVLight yield: 6 PE/MeV
HyperK(2 tanks in stages)
20x larger,same photo-coverage
better PMTs
• Technical issues– PMTs protection under pressure (60 m)– Water circulation system– High eff. PMT
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ORCA
19Optical module
31 x 3” PMTs
Shower like (ν NC, νe CC)
Track like (νμ CC)
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Indian Neutrino Observatory: INO
20
• 50kt magnetized Iron CALorimeterdetector (ICAL) interleaved by RPC for detecting atmospheric neutrinos– Neutrino mass ordering– Octant and precision of |Δm2
31| and θ23– New physics– Magnetic monopole search
• Features: – Muons fully contained up to 20 GeV– Good charge resolution, B=1.5 T– Good tracking/Energy/time resolution Copper coils, B=1.5 T
4 cm air gap5.6 cm thick ion plate
3 modules, 151 layers
One module:16 m x 16 m x 14.5 m
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EGADS and SK-Gd
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• Gd in water: – GdCl3 highly soluble in water– Improve low energy detection
capabilities– flavor sensitive– Good for LBNE, supernova, reactor
and geo-neutrinos, …• A 200 ton-scale R&D project,
EGADS – is under construction at Kamioka
νe + p e+ + n
τ ≈ 28 µs(0.1% Gd)
n + p d + γ (2.2 MeV)n + Gd Gd* + γ (8 MeV)
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Liquid Ar TPC
22
• Idea first proposed in 1985– Dense target – ample Ionization & scintillation:
good energy resolution & Low threshold– Excellent tracking and PID capabilities
• Challenges– LAr purity (long-drift)– Readout wires or large electron multipliers– Cold electronics– Cryostat for multi-kiloton TPC
Wire [beam direction]
Tim
e [d
rift d
irect
ion]
MicroBooNE
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DUNE LArTPC R&D: Single-Phase
23
• APA/CPA assemblies• APA’s w/ “wrapped” induction wire planes• Scintillation detection: light guides
embedded in APA’s, SiPM readout
3.6 m
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DUNE LArTPC R&D: Dual-Phase• 12m max drift (vertical), LEM readout• S/N: ~100/1• Scintillation via PMT’s below cathode
24
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NLDBD experiments
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0νββ Decay
26
• Unique feasible way to determine the Majorana nature of ν. Possible to pin down mass ordering
• Lepton number violation process• If Majorana: a natural way to understand tiny ν masses (seesaw)• Set constraints on 2 Majorana-type CP-violating phases
Next generation
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0νββ Decay
27
Better
Bett
er
Different isotopes correspond to vastly different experimental techniques• Ultra-low external background• Good energy resolution• Large detector volume
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Technologies
28
CUPID (Zn82Se, Li2100MoO4, TeO2), AMoRE (100Mo), CANDLES (48Ca),
ZICOS (96Zr), AXEL (136Xe), DCBA (100Mo/ 150Nd), COBRA (CdZnTe), …
Feature: excellent energy resolutionChallenge: very large size; segmented
76Ge 130Te
Feature: Topological informationChallenge: very large size
82Se (130Te, 116Cd, 48Ca, 96Zr, 150Nd, 100Mo)
136Xe
Feature: existing large clean detector; self-shieldingChallenge: 2νββ background, internal purity
136Xe 130Te
Feature: homogeneous; decent energy resolution; 3D toponologyChallenge: 2νββ background, internal purity136Xe
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Sensitivity vs. Background and Exposure
29
Detector Exposure Detector efficiency
Isotope abundance
Background in ROI* For 90% C.L, α=1.64
For a none background-free experiment, the sensitivity (1st
order) of 0νββ decay half-life.
Chin.Phys.C 2017, 41(5): 53001-053001
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Fundamental Requirements• Enrichment of the source material
– 10 kg/100 kg scale ton scale
• Deep underground location to shield cosmogenic backgrounds
30
Several underground labsaround the world,next round of experiments1-2 km deep.
JUNO
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Fundamental Requirements• Ultra-low radioactive
contamination during detector construction
• New Techniques to discrimination signal from background
31
Materials used ≈<10-15 in U, Th(U, Th in the earth crust ~ ppm)
Non trivial for E ~ 1 MeVThis gets easier in larger detectors
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Future Concepts
32
B. Schwingenheuer @ CERN EP seminar, Jan 2017
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Future Concepts
33
~ 5000 kg
nEXO 130 cm
130cm
~ 150 kg
46 cm
EXO-200
A 5000 kg enriched LXe TPC, directly extrapolated from EXO-200
~EXO-200 size
~nEXO size
EXO-200 dataM. Marino @ Neutrino2014
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Future Concepts
34
Running “KamLAND-Zen 800” Future “KamLAND2-Zen” with 1000 kg enriched Xe. Assumptions:
winston cones: x 1.8Higher Q.E. PMTs: x 1.9LAB-based liquid scint.: x 1.4Overall: x 4.8
Expected resolution (2.6 MeV): 4% ~2%Target sensitivity 20 meV
0νββN-doped LS
Beyond JUNO: possible < 10 meV Chin.Phys.C 2017, 41(5): 53001-053001
Existing 1 kton LS
20 kton LS
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Summary• Few significant advances of neutrino physics. Hints on δCP
• Many technological progresses preparation for the next generation experiments– larger mass 10~20 times in general, comparing to the
previous generation– better resolution, precision, S/N ratio, etc
• New discoveries ahead of us, probably in 10 - 20 yrs– Neutrino mass ordering– Neutrino is Majorana?– δCP
35
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Thanks
Acknowledgements Many Information from relevant talks given at
Neutrino2016, ICHEP2016, NeuTel2017, NNN16, DBD16, etc.