non-accelerator-based neutrino experiments yifang wang institute of high energy physics beijing,...
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Non-accelerator-based neutrino experiments
Yifang Wang
Institute of High Energy Physics
Beijing, 100039
Recent results on • Neutrino oscillations
– Atmospheric neutrinos: m223 and sin2223
– Solar neutrinos: m212 and sin2212
– 13 and CP phase: sin2213 and
• Neutrino masses– Absolute neutrino masses– Neutrinoless decays
• Neutrino magnetic moments
Neutrino oscillations:
Pontecorvo-Maki-Nakagawa-Sakata Matrix
Majorana phasesOnly appear in 0 decays
cij=cosij, sij=sinij
Atmospheric SolarCP phase
Mass eigenstates
Weak eigenstates
Sub-dominant 13 oscillations
A total of 6 parameters: 2 m2, 3 angles, 1 phases
+ 2 Majorana phases
Evidence of Neutrino Oscillations
Unconfirmed:LSND:m2 ~ 0.1-10 eV2
Confirmed:Atmospheric:m2 ~ 210-3 eV2
Solar:m2 ~ 8 10-5 eV2
Psin22sin2(1.27m2L/E)2 flavor oscillation in vacuum:
Atmospheric neutrinos --- SuperKamiokande
L ~ 20 km
L ~ 104 km
Earth
E ~ 300 MeV - 2 GeV
Super-K
p, He
e
P(l l )1 sin2 (2 )sin2 m 2L
4E
Oscillation probability:SK-I: 1996-2001
SK-II:2003-2005
e/ 1/2
e
e
Full analysis of SK-I ---- Zenith angle distributions
~15km ~13000km ~500km
2-flavor oscillations
Null oscillation Best fit
Saji’s talk
sin22=1.0, m2=2.1x10-3 eV2
2 = 175.2/177 dof
90% C.L. region:
sin22> 0.92,
1.5 < m2 < 3.4x10-3 eV2
L/E Oscillation result
m2=2.4x10-3,sin22=1.00
2min=37.9/40 d.o.f
(sin22=1.02, 2min=37.7/40 d.o.f)
1.9x10-3 < m2 < 3.0x10-3 eV2
0.90 < sin22 @ 90% C.L.
Strong constraint on m2
standard zenith angleanalysis(90%C.L.)
Best fit expectation
w/ systematic errors
Mostly upwardMostly downward
3-Flavor Analysis result
no
rmal
inve
rted
Bestfit: m2 = 2.7x10-
3ev2, sin223 = 0.5, sin213 = 0.0
no evidence for non zero 13
m3
m2
m1
m3
m2
m1
sin223
sin
2 1
3
m2
sin213
m2
sin
2 1
3
(preliminary)
Standard Solar model: BP04
pp (1010 cm-2 s -1)
pep (108 cm-2 s -1)
hep (103 cm-2 s -1)
7Be (109 cm-2 s -1)
8B (106 cm-2 s -1)13N (108 cm-2 s -1)15O (108 cm-2 s -1)17F (106 cm-2 s –1)
5.94 (1%)
1.40 (2%)
7.88 (16%)
4.86 (12%)
5.82 (23%)
5.71 (36%)
5.03 (41%)
5.91 (44%)
Cl SNU
Ga SNU
10-36 atom-1 s –1
8.5 1.8
131 11
Bahcall, Pinsonneault, PRL2004
Solar neutrino experiments ----- Super-K, SNO, KamLAND
Z
mantle
core
SK Day
z
SK: Un-bined day/night analysis of SKIEnergy and zenith angle dependence of event rate variatoin.
(Δm2 = 6.3×10-5 eV2, tan2θ = 0.55)
L e iBi S
i 1
N bin
1
ni
Bi U i c mi S p c , E z c , E
#B.G. in eachenergy bin
#SignalEvents
Event“Time"
BackgroundShape
Solar signalshape
ADN 0.018 0.016 0.0120.013
cf. old method 0.02 0.021 0.0120.013
j j
i
MC
MC
Ishihara’s talk
Average of SK-I
Period '96-'01 accident '03-'05#PMTs 11,146 5,182Photo Coverage 40 % 19 %Light yield ~6 p.e./MeV ~2.8 p.e/MeV Energy threshold 5.0 MeV 8.0 MeV
SKII works well
The Sudbury Neutrino Observatory
• 2092 meters deep underground• 1000 tons of ultrapure D2O in a 12 meter diameter acrylic vessel
• 7000 tons of ultrapure H2O as shield • 9500 PMTs • 40 helium proportional counters with total length of 398 m
CC:e + d e- + p + p
NCx + d x + n + p
ESx + e- x + e-
e
x= e+
x= e+()/6
Three neutron detection methods
energy
Isotropyradius
direction
Signal extraction in salt phaseDeng’s talk
Neutrino flux: > 0
)sys()stat(21.2Φ 10.010.0-
+0.310.26-ES
+=
)sys()stat(76.1Φ 09.009.0-
+0.060.05-CC
+=
)sys()stat(39.2Φ 12.012.0-
+0.240.23-ES
+=
)sys()stat(09.5Φ 46.043.0-
+0.440.43-NC
+=
)sys()stat(59.1Φ 06.008.0-
+0.080.07-CC
+=
)sys()stat(21.5Φ 38.038.0-
+0.270.27-NC
+=
D2O phase salt phase(unit 106/cm2/s)
SSM8
meas8 )(0.23(th))exp)(04.088.0()( BB
First salt results
KamLAND
Sources: reactor neutrinos
• 200 MeV/fission
• 6 e/fission
6 1020 e/s/3GWth
Flux and spectrum of reactor neutrino are known within 3%
Null Oscillation Probability
Disappearance 99.995%Shape Distortion 99.9%Combined 99.99996%
Hypothesis test
Scaled no oscillation
excluded at 99.9% C.L.
Shimizu’s talkShimizu’s talk
Combined solar Combined solar νν – KamLAND 2-flavor analysis – KamLAND 2-flavor analysis
Includes (small) matter effectsIncludes (small) matter effects
07.009.040.0tan
105.06.02.8
122
25212
eVm
A new background just found:
preliminary
13C(, n)16O ~ 10 event
Accidental 2.69 ± 0.028He/9Li 4.8 ± 0.9 induced n < 0.89
Previously estimated backgrounds
An incomplete list of “exotic” explanations• Atmospheric neutrinos (m2
23)– Atmospheric neutrino production model:
K2K– e, s
– CHOOZ, SK Fit, Tau appearance
– Decoherence: SK, KamLAND
– neutrino decays: SK, KamLAND
• Solar neutrinos (m212)
– Standard Solar Neutrino(SSN) model– Solar density profile– SNO( appearance), KamLAND
– SMA, QVO-VO, LOW solutions: KamLAND– Spin-Flip, non-standard interactions, …
– KamLAND
– Decoherence: SK, KamLAND
– neutrino decays: SK, KamLAND
Neutrino oscillations established
SuperK KamLAND
Decay* excluded at 95% CL
Decoherence† excluded at 94% CL
*V.Barger et al. Phys. Rev. Lett. 82 (1999) 2640
†E.Lisi et al., Phys. Rev. Lett. 85 (2000) 1166
A total of six mixing parameters :Known : | m2
32|, sin2232 --Super-K
m221, sin2221 --SNO,KamLAND
Unknown : sin22 , , sign of m232
at reactors:
Pee 1 sin22sin2 (1.27m2L/E)
cos4sin22sin2 (1.27m2L/E)
at LBL accelerators:
Pe ≈ sin2sin22sin2(1.27m2L/E) +
cos2sin22sin2(1.27m212L/E)
A()cos213sinsin()
Why at reactors• Clean signal, no cross talk with and matter
effects• Relatively cheap compare to accelerator based
experiments • Can be very quick• Provides the direction to the future of neutrino physics
0.3
0.4
0.5
0.6
0.7
0.8
0.9
1
1.1
0.1 1 10 100
Nos
c/Nn
o_os
c
Baseline (km)
Small-amplitude
oscillation due to 13
Large-amplitude
oscillation due to 12
Current Knowledge of 13
Maltoni etal., hep-ph/0405172
Sin2(213) < 0.09
Sin2(213) < 0.18
At m231 = 2103 eV2,
sin22 < 0.15
K.B.Luk’s talk
How to reach 1% precision ?• Three main types of errors: reactor
related(~2-3%), background related (~1-2%) and detector related(~1-2%)• far/near detector to cancel reactor errors• movable detectors, near far ?• optimum baseline • detector design threshold, fiducial volume, resolution, scintillator,
light transport, … • sufficient shielding • calibration• statistics
Typical precision: 3-6%
xperi
Proposed Reactor Neutrino Experiments
Angra, Brazil
Diablo Canyon, USA
Braidwood, USAChooz, France Krasnoyasrk, Russia
Kashiwazaki, Japan
Daya Bay, China
Currently Proposed sites/experiments
Site
(proposal)
Power
(GW)
Baseline
Near/Far (m)
Detector
Near/Far(t)
Overburden
Near/Far (MWE)
Sensitivity
(90%CL)
Angra dos Reis (Brazil)
4.1 300/1300 50/500 200/1700 0.007
Braidwood (US) 6.5 270/1800 25/50 450/450 0.01
Chooz-II (France) 8.4 150/1050 10/10 60/300 0.03
Daya Bay (China) 11.6 350/1800 20/40 250/1200 0.01
Diablo Canyon (US)
6.4 400/1800 25/50 100/700 0.01
Kashiwazaki (Japan)
24.3 350/1300 8.5/8.5 300/300 0.02
Krasnoyarsk (Russia)
3.2 115/1000 46/46 600/600 0.01
Sensitivities to Sin2213 @ 90%CL
Double Chooz
KASKA
BraidwoodDaya Bay
PowerBaselineDetectorOverburden
rock
watermodule with 10
t Gd-doped liquid scintillator
Two veto detectors: Water + RPC multiple detector modules for
Redundancy is important to achieve <1% precision
Daya Bay experiment
Absolute neutrino masses
• β-decay:
(m ve)eff =[Σi | Uei |2 m2 vi
]1/2
• Endpoint of decays
3H → 3He + e- + e
E0 = 18.574 KeV
• Currently the best limit:
m< 2.2 eV @ 95%CL
• Katrin expected: m
< 0.3 eV @ 95%CL
Neutrino mass from
Cosmology
Data mi
@95%CL)*References
2dFGRS < 1.8 eV Elgaroy et al. PRL 89, 2002
WMAP+2dF+… < 0.7 eV Spergel et al. APJS 148,2003
WMAP+2dF < 1.0 eV Hannestad, JCPA 0305, 2003
XLF+WMAP+2dF+…
0.56+0.30 -0.26 eV Allen et al. MNRAS346(2003)
SDSS+WMAP < 1.7 eV Tegmark et al. PRD 69,2004
WMAP+ACBAR+
2dF+SDSS+…
< 1.0 eV Crotty et al. PRD 69,2004
*With different assumptions, fitting constrains and datasets
A strong constraint to LSND and Heidelberg-Moscow decay results
Continuous spectrum Monochromatic spectrum
decays : <Mee> = | Σi (Uei )2 m vi
|
Resolution and backgrounds are critical
NEMO-03 first results
Ec1+Ec2 (keV)
DataMonte-CarloRadonMonte-CarloT1/2 = 3.5 1023
100Mo 6914 g
216.4 days4.10 kg.y
Ec1+Ec2 (keV)
100Mo: T1/2() > 3.5 1023 y (@90% C.L.) m < 0.7 – 1.2 eV82Se: T1/2() > 1.9 1023 y (@90% C.L.) m < 1.3 – 3.6 eV
3 m
4 mB (25 G)
20 sectorsLalanne’s talk
100Mo 6.914 kg
Q= 3034 keV
82Se 0.932 kg
Q= 2995 keV
Current 0 resultsNucleus Detector (kg yr) Present T1/2
0 (yr) <m> (eV)
48Ca >9.5*1021 (76%CL)76Ge† Ge diode ~30 >1.9*1025 (90%CL) < 0.39+0.17
-0.28
82Se Foils 0.5 >1.9*1023 (90%CL) <1.3-3.6100Mo foils 4.1 >3.5*1023 (90%CL) <0.7-1.2116Cd >7.0*1022 (90%CL)128Te TeO2
cryo~3 >1.1*1023 (90%CL)
130Te TeO2 cryo
~3 >2.1*1023 (90%CL) < 1.1 - 2.6
136Xe Xe TPC ~10 >1.2*1024 (90%CL) < 2.9150Nd >1.2*1021 (90%CL)160Gd >1.3*1021 (90%CL)
† Controversial claim of positive 0signal with m = .39 eV c.f. Klapdor-Kleingrothaus Mod. Phys Lett. A27 (2001) 2409
EXO – a novel technology to remove backgrounds
• 136Xe 136Ba++ + 2e-
identified using optical spectroscopy
2P1/2
4D3/2
2S1/2
493nm
650nm
metastable 47s
30%
8 ns
850 m
Hz/bin
• Ions observed in .01 torr xenon
• Indefinite gas lifetime
• Trap dynamics dominate
• to be demonstrated in liquid or high
pressure gas environment
SNR ~100:1
S.Waldman’s talk
200 kg prototype underway
Strategy of the XMASS project
Dedicated detector forDouble beta decay search
~1 ton detector(FV 100kg)Dark matter search
~20 ton detector(FV 10ton)Solar neutrinosDark matter search
Prototype detector (FV 3kg) R&D
~2.5m~1m~30cm
NOW
Confirmation of feasibilities of the ~1 ton detectorAnalysis techniquesSelf shielding performanceLow background propertiesPurification techniques
Takeuchi’s talk
Future -decay experiments
Isotopes enrichment Mass
(t)
Sensitivity
(eV) (90%CL)
CUORE 130Te no 0.75 ~ 0.03
GENIUS 76Ge yes 0.1-1.0 ~ 0.01
Majorara 76Ge yes 0.42 ~ 0.02
MOON 100Mo yes 3.0 ~ 0.01
Super-NEMO 82Se yes 0.1 ~ 0.03
EXO 136Xe yes 10.0 ~ 0.01
A few of them will be realized
Direct searches of Neutrino magnetic moments
Finite mass Finite (e), SM: ~ 10-19 B
Enhanced by new physics
Signature: 1/T excess due to
-e scattering via channel
Sources: Kuo-Sheng reactor in Taiwan
Detector: 1Kg HPGe
No excess for ON/OFF
Limit:
e) < 1.3 10-10 B (90% CL)
Texono, Jin Li’s talk
22
11)(2
ETmedT
de
Current experimental limitsExperiments Up Limits @ 90% CL References
Texono e ) < 1.3 10-10 B PRL 90, 2003
MUNU e ) < 1.0 10-10 B PLB564, 2003
SK+all data + KamLAND ) < 1.1 10-10 B PRL93, 2004
Borexino ) <5.5 10-10 B PLB 563,2003
LSND e ) < 1.1 10-9 B
) < 6.8 10-10 B
PRD 63, 2001
DONUT ) < 3.9 10-7 B PLB 513, 2001
Future experimentsExperiments Sensitivity @ 90% CL Status
GEMMA e ) 3 10-11 B 2004
MAMONT e ) 2 10-12B R&D
Texono(ULEGe) e ) 2 10-11B R&D
Summary• Neutrino oscillations established
– Solar: m212 = (8.2+0.6
-0.5)10-3 eV2
tan212 = 0.40 +0.09-0.07 large but not maximal
– Atmospheric: m223 = (2.40.4)10-3 eV2
sin2223 > 0.92 @ 90%CL maximal – From global fit: sin2213 < 0.09 @ 90%CL
• Our next goal:– Absolute neutrino masses -decay experiments
– Dirac or majorana ? 0-decay experiments
– 13, CP and Mass hierarchy Reactor, Long baseline accelerator based experiments
A great success in the past A long way to go in the future