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LAGUNA and Neutrino Physics

LAGUNA and Neutrino Physics. NOW 2008 Lothar Oberauer TU München, Germany. LAGUNA Physics. L arge A pparatus for G rand U nification and N eutrino A strophysics Proton Decay Neutrinos as probes Supernova neutrinos Solar neutrinos Geoneutrinos Neutrino properties.

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LAGUNA and Neutrino Physics

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  1. LAGUNA and Neutrino Physics NOW 2008 Lothar Oberauer TU München, Germany

  2. LAGUNA Physics • Large Apparatus for Grand Unification and Neutrino Astrophysics • Proton Decay • Neutrinos as probes Supernova neutrinos Solar neutrinos Geoneutrinos • Neutrino properties

  3. LAGUNA Physics • Detecting proton decay implies de facto discovery of Grand Unification (GU) • GU: new symmetry between quarks and leptons • GU: guide of fermion masses and mixing • GU: one motivation for SUSY => LSP is Dark Matter candidate • GU: motivation for See-Saw => small n masses

  4. LAGUNA Physics • Galactic Supernova neutrino burst understanding of gravitational collapse neutrino properties: Q13 and mass hierarchy mass effects on flavor transitions within the supernova and when passing through the Earth early alert for astronomers Black Hole formation? • Diffuse Supernova neutrinos link to supernova rates => star formation rate; probing models of gravitational collapse

  5. LAGUNA Physics • Solar neutrinos Search for small flux variations in time Precise measurements of thermo nuclear fusion reactions measurement of inner solar metallicity (CNO neutrinos at high statistics) • Neutrino beams Search for Q13 Search for leptonic CP-violation (if Q13is not to small)

  6. LAGUNA Physics • Complementary to LHC and planned ILC goals LHC: Higgs mechanism, SUSY, Rare decays LAGUNA: Proton decay, neutrino astronomy, CP violation in leptons

  7. LAGUNA • European ApPEC roadmap recommendation: We recommend that anew large European infrastructureis put forward, as a futureinternational multi-purpose facility on the 105-106 ton scalefor improved studies of proton decayand of low-energy neutrinos from astrophysical origin

  8. LAGUNA structure and aims • Proposed and accepted in the ApPEC meeting at Munich in November 2005 • Investigate common R&D requirements • Coherent work on common problems • Take advantage of acquired technological know-how in Europe • Kick-off meeting at ETH Zurich 3-4 July 07 • Mature design and proposals should emerge in 2010

  9. LAGUNA financial situation • Design Study for future European observatory • Volume of proposal 5 M€ • Approved as a whole by the European Commission (EC) • Funding: 1.7 M€ • Focus on the part of the programme which cannot be performed on a national (regional) basis • Underground Sites infrastructure studies • 2008 until 2010

  10. LAGUNA Collaboration - Italy

  11. LAGUNA Collaboration Consortium composed of 21 beneficiaries 9 university entities (ETHZ, U-Bern, U-Jyväskylä, U-OULU, TUM, UAM, UDUR, USFD, UA) 8 research organizations (CEA, IN2P3, MPG, IPJ PAN, KGHM CUPRUM, GSMiE PAN, LSC, IFIN-HH) 4 SMEs (Rockplan, Technodyne, AGT, Lombardi) Additional university participants (IPJ Warsaw, U-Silesia, U-Wroclaw, U-Granada)

  12. LAGUNA Detector types • Mt Water Cherencov MEMPHIS • 100kt Liquid Argon GLACIER • 50kt liquid Scintillator LENA

  13. MEMPHYS TRE MEMPHIS 1 shaft = 215 kt water target Possible location: extension of Frejus laboratory Ongoing R&D for single photo detection Synergy with HK (Japan) and UNO (USA)

  14. MEMPHIS • PROS “Simple” Detector Large and useful experiences (SuperK) • CHALLENGES Huge amount of photo-sensors (>100,000) Very large underground cavities Costs? Imaging with SuperK water Cherenkov detector

  15. GLACIER: Liquid argon scintillation and electron TPC φ≈70 m h =20 m Max drift length Passive perlite insulation

  16. GLACIER • Liquid Argon TPC • -> 10 to 100 kt target mass • Pioneering work in ICARUS R&D program • Two independent programs: GLACIER in Europe and LARTPC in USA

  17. GLACIER • PROS Brilliant energy and track resolution Particle ID and separation Basically background free for many applications • CHALLENGES “complicated” detector technology Huge number of channels (depending on position resolution) Large span of the cavity

  18. LENA: Liquid scintillator

  19. LENA • Low Energy Neutrino Astronomy • -> 50 kt target mass • R&D on liquid scintillators • BOREXINO successful in measuring solar neutrinos (7Be, 8B) • DOUBLE-CHOOZ in France • Hanohano project (10 kt at Hawai) in USA

  20. LENA • PROS Mature technology Good energy and position resolution Cavity, PMs electronics standard (size like SuperK, also number of PMs) • CHALLENGES Keep purity like BOREXINO but for 50 kt (relevant for solar neutrino detection in the sub-MeV range)

  21. Sensitivities on Proton Decay • p -> p0e+ Water Cherenkov MEMPHIS ca. 1035 y (5000 kt y exposure) Limit SK-I and II: t > 8.4 x1033y • p -> K+n Liquid Argon GLACIER ca. 1035 y (1000 kt y exposure) Liquid Scintillator LENA ca. 5 x 1034 y (500 kt y exposure) Limit SK-I: t > 2.3 x1032y

  22. Sensitivity on Supernova n MEMPHIS mainly sensitive on ne Approx. rate for 1 Mt: ~ 40 events @ 1 Mpc Prop. < 10% per year ~ 4 events @ 3.3 Mpc Prop. ~ 15% per year ~ 0.4 events @ 10 Mpc Prop. ~ 80% per year

  23. Sensitivity on Supernova n Sensitive on ne ! Important for neutronisation phase Sensitive on oscillation parameter and mass hierarchy

  24. Sensitivity on Supernova n

  25. DSNB Detection via inverse beta decay • Free protons as target Delayed signal (~200 ms) • Threshold 1.8 MeV • En ~ Ee - Q (n spectroscopy) • suppress background via delayed coincidence method • n + p -> D + g(2.2 MeV) • position reconstruction => fiducial volume (suppress external background) Prompt signal

  26. OutlineDSNB BackgroundEvent Rates Spectroscopy dependent on SN model(assumed fSN=2.5) LL: 113KRJ: 100TBP: 60 dependent on SNR fSN=0.7 17fSN=2.5 100fSN=4.2 220 TU München LENA at Pyhäsalmi(Finland) DSN event rate in 10yrsinside the energy window from 9.7 to 25 MeV ~25% of events are due to v’soriginating from SN @ z>1! background events: 13

  27. Solar Neutrinos • 8B neutrinos: MEMPHIS, GLACIER, LENA • CNO and pep: LENA (~ 300 / d) • 7Be: LENA (~ 6000/ d) • Precise measurement of LMA prediction • Accurate measurement of inner solar metallicity • Search for small flux variations

  28. GEO Neutrinos • LENA rate between 3 x 102 and 3 x 103per year (at Pyhäsalmi, Finland) Background ~ 240 per year in [1.8 MeV – 3.2 MeV] from reactor neutrinos < 30 per year due to 210Po alpha-n reaction on 13C (Borexino purity assumed) ~ 1 per year due to cosmogenic background (9Li - beta-neutron cascade) Can be statistically subtracted

  29. Long baseline oscillations Q13 dCPsign(DM2) nm -> nene-> nm New neutrino source. “Betabeams, nu-factory” Time scale ~ 2020 (?) High Intensity conventional neutrino source. “Superbeams” Time scale > 2014 (?)

  30. LNGS SUNLAB Polkowice-Sieroszowice, Poland L=2300 L=950 IUS LSC Laboratoire Souterrain de Modane, France Institute of Underground Science in Boulby mine, UK Laboratorio Subterraneo de Canfranc, Spain Laboratori Nazionali del Gran Sasso, Italy L=1050 km L=630 km L=732 km L=130 km

  31. Long baseline oscillations Study J-Parc -> Okinoshima Distance 653 km Power 1.66 MW Measurement 5 years (arXiv:0804.2111) Similar results for ~ 300 kt Water Cherenkov (fiducial mass)

  32. LENA and Reactor neutrinos • At Frejus ~ 17,000 events per year • High precision on solar oscillation parameter: • Dm212~ 1% • Q12 ~ 10% S.T. Petcov, T. Schwetz, Phys. Lett. B 642, (2006), 487 J. Kopp et al., JHEP 01 (2007), 053

  33. LENA and indirect Dark Matter search • Light Wimp mass between 10 and 100 MeV • Annihilation under neutrino emission in the Sun • Monoenergetic electron-antineutrino detection in LENA S. Palomares-Ruiz, S. Pascoli, Phys. Rev. D 77, 025025 (2008)

  34. Conclusions • LAGUNA started July 2008 • Physics program aims on GUT (p-decay), LE n astrophysics, n oscillations • High discovery potential • Site studies for 7 candidates until 2010 • LAGUNA is European but open for world wide cooperation

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