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