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LSND vs KARMEN LSND : L=30 m, 20
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May 19, 2005 UAM-IFT, Madrid
2005-2010 : Neutrino physics in underground 2005-2010 : Neutrino physics in underground labslabs
Carlos Pena GarayIAS
~
The Neutrino Matrix :SM + The Neutrino Matrix :SM + massmass
)9.7( 9.8eV10
0.7 25
2m
Δ
)2.2( 6.3eV10
M6.1 23
2
Δ 3 ranges
81.056.073.043.054.020.082.058.072.042.053.020.020.000.064.049.087.076.0
||||||||||||||||||
||
321
321
321
τττ
μμμ
eee
i
UUUUUUUUU
U
(0.45) 68.0tan0.31 122
(1.0) 1.2tan0.51 232
(0.005) 041.0sin 132
)1(2
1)cos1(21)cos1(
21
)1(2
1)cos1(21)cos1(
21
)1(2
1)1(2
1
~||
iU 04.021.0 06.000.0
12.01cos1
1 ranges
thanks to Gonzalez-Garcia, Maltoni
Solar + KamLANDAtmospheric + K2K CHOOZ
LSND vs KARMENLSND vs KARMEN
LSND : L=30 m, 20<E<60 MeV3.5 to 7 appearance signal depending on analysis 67 signal events in 1030 signal+background
KARMEN : L=17.5 m, 20<E<60 MeV15 events observed15.8 background expected
310 )8.06.2()( eνP Church et al, hep-ex/0203023
Discussion : S. Pascoli, M. Sorel
Known knowsKnown knows
Known knowsKnown knows
Where we are ?Where we are ?Test matter effects in solar neutrinos : - From vacuum averaged oscillations to adiabatic transitions- Daynight effect
Test atmospheric oscillations : robustness of m232
Improve precision
Tests beyond SM physics
Neutrinos as astrophysical probes
Valle’s talk, Halzen’s talk
NH ? or IH ?
13 ??
m?
423= ?
Known UnknowsKnown Unknows
Majorana mass ?
HierarchyHierarchyBy matter effects in the 13 sector in atmospheric neutrinos, long baseline experiments, similar to matter effects determination in solar neutrinos 13 non zero break 13 – hierarchy degeneracyBy vacuum oscillations with m2
31)<m221
valid even if 13=0
break 13 – hierarchy degeneracyBy high statistics short baseline reactor neutrino experiments 13 not too smallBy matter effects in SupernovaBy neutrinoless double beta decay
Raffelt’s talk
… )sin(2sinsin ~ ,132
232 LP mme
Discussion
2323==
By solar osc. in atmospheric neutrinos, sub-GeV valid even if 13 =0 discrimination of octant
By atmospheric neutrinos, multi-GeV 13 nonzero discrimination of octant
Accelerator neutrinos, MINOS : Non –maximal 3 detection if 23 is outside the ATM+K2K 90%CL (sin223<0.4)thanks to Gonzalez-Garcia, Maltoni, Winter
1)-sin(r P ~ 232
12e
e FF
1)-sin(r P ~ 232
13e
e FF
1313 smallness smallness
Solar + 2xKamLAND2xAtmospheric + K2K CHOOZMINOSDouble-CHOOZ 03.0sinat 6
01.0sinat 3
014.0sin 041.0sin
132
132
132
132
All probes are sensitive to 13 (at different scales, with different sensitivities)
2005-2010 hits : 1. MINOS more precise determination of the atmospheric splitting2. Double-CHOOZ sets the most stringent limit, unless atmospheric splitting is lower than expected.Discussion
2010 null hypothesis: Preliminary! 2010 null hypothesis: Preliminary!
)9.7( 6.8eV10
2.7 25
2m
Δ
)2.2( 8.2eV10
M6.1 23
2
Δ 3 ranges(0.45) 60.0tan0.37 12
2
(1.0) 5.1tan0.60 232
410.0sin 132
)1(2
1)cos1(21)cos1(
21
)1(2
1)cos1(21)cos1(
21
)1(2
1)1(2
1
~||
iU 03.021.0 04.000.0
07.01cos1
1 ranges
thanks to Gonzalez-Garcia, Maltoni, Winter
Solar + 2xKamLAND2xAtmospheric + K2K CHOOZMINOSDoble-CHOOZ
004.0036.0 Mm
050.0sin
2
2
132
1 determination of small parameters relevant in CP violation observables
Mass scaleMass scale
Direct mass detection : KATRIN
Cosmology
Neutrinoless double beta decay
eV 35.0at detection 5
eV 2.0 95%CL @ eV 2.2
|| 222
m
mm
mUm iei
(90%CL) eV 1.1 - 0.2
)(3 eV 44.0|| 14.020.0
2
ii
ei meUm i
95%CL @ eV 42.0 ic mm Raffelt’s talk, Verde’s Discussion
Majorana massMajorana mass
searchingobserved
2
02
00
2/1
2||
GTV
AfN
N
e
ii
ei
Mgg
MGF
FTm
m
meUm i
If observed : Neutrinos are Majorana
Can we learn anything more ?
Positive signal ?Positive signal ?
214Bi 214Bi
?
Klapdor et al (part of HM)28.8 (6.9) 3-4Bckg ~ 60 ev.
Present Limits :Present Limits :Candidate Detector Present <m> (eV) nucleus type (kg yr) T1/2
0νββ (yr)
48Ca >9.5*1021 (76%CL)76Ge Ge diode ~30 >1.9*1025 (90%CL) <0.39+0.17
-0.28
82Se >9.5*1021 (90%CL) 100Mo >5.5*1022 (90%CL)116Cd >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 - 2.6136Xe Xe scint ~10 >1.2*1024 (90%CL) <2.9150Nd >1.2*1021 (90%CL)160Gd >1.3*1021 (90%CL)
Projected/proposedProjected/proposedExperiment
Nucleus Detector T0ν (y) < mν > eV
CUORE 130Te .77 t of TeO2 bolometers
(nat)7 x 1026 .014-.091
EXO 136Xe 10 t Xe TPC + Ba tagging
1 x 1028 .013-.037
Gertha 76Ge 1 t Ge diodes in LN 1 x 1028 .013-.050Majorana 76Ge 1 t Ge diodes 4 x 1027 .021-.070MOON 100Mo 34 t nat.Mo
sheets/plastic sc.1 x 1027 .014-.057
DCBA 150Nd 20 kg Nd-tracking 2 x 1025 .035-.055CAMEO 116Cd 1 t CdWO4
in liquid scintillator
> 1026 .053-.24
COBRA 116Cd ,
130Te10 kg of CdTe semiconductors
1 x 1024 .5-2.
Candles 48Ca Tons of CaF2 in liq. scint. 1 x 1026 .15-.26
GSO 116Cd 2 t Gd2SiO5:Ce scint in liq scint
2 x 1026 .038-.172
Xmass 136Xe 1 t of liquid Xe 3 x 1026 .086-.252
nuclear matrix elements? nuclear matrix elements?
Nuclear Physics methods :
QRPA, SM
Test QRPA : 20% variation
Test SM ? Test QRPA-SM ?
If positive signals : Test of models, but no model independent mass
CC -nucleus interaction to measure many virtual transition in neutrinoless double beta
Faessler et al, 2005
Volpe, 2005
From Osc. Data :From Osc. Data :
212
122 sin2sin1 m
212
1222
31 sin2sin1 m
3213
2232
1222
21
sin
sin
iem
m
If no 0If no 0
If IH is correct, we need :a larger atmospheric neutrino exp.or a longer baseline in beam exp.
Understanding of matrix elements(we don’t today)
<0.01 eV sensitivity