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2005-2010 : Neutrino physics in underground labs

2005-2010 : Neutrino physics in underground labs. ~. Carlos Pena Garay IAS. The Neutrino Matrix :SM + n mass. 3 s ranges :. 1 s ranges :. Solar + KamLAND Atmospheric + K2K CHOOZ. thanks to Gonzalez-Garcia, Maltoni. LSND vs KARMEN. LSND : L=30 m, 20<E<60 MeV

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2005-2010 : Neutrino physics in underground labs

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  1. 2005-2010 : Neutrino physics in underground labs ~ Carlos Pena Garay IAS UAM-IFT, Madrid

  2. The Neutrino Matrix :SM + n mass 3 s ranges: 1 s ranges: Solar + KamLANDAtmospheric + K2K CHOOZ thanks to Gonzalez-Garcia, Maltoni

  3. LSND vs KARMEN LSND : L=30 m, 20<E<60 MeV 3.5 to 7 s appearance signal depending on analysis 67 signal events in 1030 signal+background KARMEN : L=17.5 m, 20<E<60 MeV 15 events observed 15.8 background expected Church et al, hep-ex/0203023 Discussion : S. Pascoli, M. Sorel

  4. Known knows

  5. Known knows

  6. 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 Valle’s talk, Halzen’s talk

  7. Known Unknows NH ? or IH ? q13 ?, d ? 4q23=p ? m? Majorana mass ?

  8. Hierarchy By matter effects in the 13 sector in atmospheric neutrinos, long baseline experiments, similar to matter effects determination in solar neutrinosq13 non zero break q13 – hierarchy degeneracyBy vacuum oscillations with d(Dm231)<Dm221valid even if q13=0 break q13 – hierarchy degeneracyBy high statistics short baseline reactor neutrino experimentsq13 not too smallBy matter effects in SupernovaBy neutrinoless double beta decay … Raffelt’s talk Discussion

  9. 4q23=p By solar osc. in atmospheric neutrinos, sub-GeV valid even if q13 =0 discrimination of octantBy atmospheric neutrinos, multi-GeVq13 nonzero discrimination of octantAccelerator neutrinos, MINOS : Non –maximal 3s detection if q23 is outsidethe ATM+K2K 90%CL (sin2q23<0.4) thanks to Gonzalez-Garcia, Maltoni, Winter

  10. 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

  11. 2010 null hypothesis: Preliminary! 3 s ranges: 1 s ranges: 1s determination of small parameters relevant in CP violation observables Solar + 2xKamLAND2xAtmospheric + K2K CHOOZMINOSDoble-CHOOZ thanks to Gonzalez-Garcia, Maltoni, Winter

  12. Mass scale Direct mass detection : KATRIN CosmologyNeutrinoless double beta decay Raffelt’s talk, Verde’s Discussion

  13. Majorana mass observed searching If observed : Neutrinos are MajoranaCan we learn anything more ?

  14. 0nbb 214Bi 214Bi ? Positive signal ? Klapdor et al (part of HM) 28.8 (6.9)->3-4s Bckg ~ 60 ev.

  15. Present Limits : Candidate Detector Present <m> (eV) nucleus type (kg yr) T1/20νββ (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 - 2.6 136Xe Xe scint ~10 >1.2*1024 (90%CL) <2.9 150Nd >1.2*1021 (90%CL) 160Gd >1.3*1021 (90%CL)

  16. Projected/proposed

  17. 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

  18. From Osc. Data :

  19. 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 don’t today)<0.01 eV sensitivity

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