20052010 : Neutrino physics in underground labs

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2005-2010 Neutrino physics in underground labs

• Carlos Pena Garay
• IAS

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The Neutrino Matrix SM n mass

Solar KamLANDAtmospheric K2K CHOOZ
thanks to Gonzalez-Garcia, Maltoni
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LSND vs KARMEN

LSND L30 m, 20ltElt60 MeV 3.5 to 7 s appearance
signal depending on analysis 67 signal events in
1030 signalbackground KARMEN L17.5 m,
20ltElt60 MeV 15 events observed 15.8 background
expected
Church et al, hep-ex/0203023
Discussion S. Pascoli, M. Sorel
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Beyond standard picture

DL2 muon decay . Incompatible LSND with Karmen

Babu,Pakvasa, hep-ph/0204236
Disfavoured at 3.5s


Disfavoured at 3.2(5.8)s

Bilenki, Giunti, GG, Valle,

Baremboim et al, hep-ph/0212116
Disfavoured at 3.4s


Extra interactions. Incompatible LSND with atm.
SK
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Known knows

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Known knows

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Where we are ?

Test matter effects in solar neutrinos - From
vacuum averaged oscillations to adiabatic
transitions- Daynight effectTest atmospheric
oscillations robustness of Dm232Improve
precision Tests beyond SM physicsNeutrinos
as astrophysical probes
Valles talk, Halzens talk
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Known Unknows

NH ? or IH ?
q13 ?, d ?
4q23p ?
m ?
Majorana mass ?
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Hierarchy

By matter effects in the 13 sector in
atmospheric neutrinos, long baseline experiments,
similar to matter effects determination in solar
neutrinos q13 non zero break q13
hierarchy degeneracyBy vacuum oscillations with
d(Dm231)ltDm221 valid even if q130 break
q13 hierarchy degeneracyBy high statistics
short baseline reactor neutrino experiments
q13 not too smallBy matter effects in
SupernovaBy neutrinoless double beta decay

Raffelts talk
Discussion
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4q23p

By solar osc. in atmospheric neutrinos, sub-GeV
valid even if q13 0 discrimination of
octantBy atmospheric neutrinos, multi-GeV
q13 nonzero discrimination of
octantAccelerator neutrinos, MINOS Non
maximal 3s detection if q23 is outside the
ATMK2K 90CL (sin2q23lt0.4)
thanks to Gonzalez-Garcia, Maltoni, Winter
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q13 smallness

All probes are sensitive to q13 (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
Solar 2xKamLAND2xAtmospheric K2K
CHOOZMINOSDouble-CHOOZ
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2010 null hypothesis Preliminary!

Solar 2xKamLAND2xAtmospheric K2K
CHOOZMINOSDoble-CHOOZ
thanks to Gonzalez-Garcia, Maltoni, Winter
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Mass scale

Direct mass detection KATRIN CosmologyN
eutrinoless double beta decay
Raffelts talk, Verdes Discussion
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Neutrino mass Direct methods
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Majorana mass

searching
observed
If observed Neutrinos are MajoranaCan we
learn anything more ?
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Positive signal ?
Klapdor et al (part of HM) 28.8 (6.9) -gt
3-4s Bckg 60 ev.
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SN watch

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Present Limits

Candidate Detector Present
ltmgt (eV) nucleus type (kg
yr) T1/20?ßß (yr) 48Ca
gt9.51021 (76CL) 76Ge Ge
diode 30 gt1.91025 (90CL)
lt0.390.17-0.28 82Se
gt9.51021 (90CL) 100Mo
gt5.51022 (90CL) 116Cd
gt7.01022 (90CL) 128Te
TeO2 cryo 3 gt1.11023 (90CL) 130Te
TeO2 cryo 3 gt2.11023 (90CL)
lt1.1 - 2.6 136Xe Xe scint 10
gt1.21024 (90CL) lt2.9 150Nd
gt1.21021 (90CL) 160Gd
gt1.31021 (90CL)
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Projected/proposed

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nuclear matrix elements?

Nuclear Physics methods QRPA, SMTest QRPA
20 variationTest SM ? Test QRPA-SM ?If
positive signals Test of models, but no model
independent massCC n-nucleus interaction to
measure many virtual transition in neutrinoless
double beta
Faessler et al, 2005
Volpe, 2005
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From Osc. Data

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If no 0nbb

If IH is correct, we need a larger
atmospheric neutrino exp.or a longer baseline in
beam exp.Understanding of matrix elements(we
dont today)lt0.01 eV sensitivity