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LAGUNA

LAGUNA. L arge A pparatus for G rand U nification and N eutrino A stronomy Future Observatory for n -Astronomy at low energies Search for proton decay (GUT) Detector for “long-baseline” experiments. COLLABORATING INSTITUTES APC, Paris, France CEA, Saclay, France

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LAGUNA

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  1. LAGUNA • Large Apparatus for Grand Unification and Neutrino Astronomy • Future Observatory for n-Astronomy at low energies • Search for proton decay (GUT) • Detector for “long-baseline” experiments

  2. COLLABORATING INSTITUTES APC, Paris,France CEA, Saclay,France CPPM, IN2P3-CBRS, Marseille,France CUPP, Pyhäsalmi,Finland ETHZ, Zürich,Switzerland Institute for Nuclear Research, Moscow,Russia IPNO, Orsay,France LAL, IN2P3-CNRS, Orsay,France LPNHE, IN2P3-CNRS, Paris,France MPI-K Heidelberg,Germany Max Planck für Physik, München,Germany Technische Universität München,Germany Universidad de Granada, Spain Universität Hamburg,Germany University of Bern,Switzerland University of Helsinki,Finland University of Jyväskylä,Finland University of Oulu,Finland University of Silesia, Katowice,Poland University of Sheffield,UK LAGUNADETECTOR LOCATIONS Rrumania Institute of Physics and Nuclear Engineering, Bucharest IFIN-HH Romania

  3. Beneficiary for the design study 1. (Coordinator) Swiss Federal Institute of Technology Zurich ETH Zurich Switzerland 2. University of Bern U-Bern Switzerland 3. University of Jyväskylä U-Jyväskylä Finland 4. University of Oulu U-Oulu Finland 5. Kalliosuunnittelu Oy Rockplan Ltd Rockplan Finland 6.Commissariat àl’Energie Atomique /Direction des Sciencesde la Matière CEA France 7.Institut National de Physique Nucléaire et de Physique des Particules (CNRS/IN2P3) IN2P3 France 8.Max-Planck-Gesellschaft 9. Technische Universität München TUM Germany 10. H.Niewodniczanski Institute of Nuclear Physics of the Polish IFJ PAN Poland 11. Academy of Sciences, Krakow KGHM CUPRUM Ltd Research and Development Centre KGHM CUPRUM Poland 12. Mineral and Energy Economy Research Institute of the Polish Academy of SciencesIGSMiEPAN Poland 13. Laboratorio Subterraneo de Canfranc LSC Spain 14. Universidad Autonoma, Madrid UAM Spain 15. University of Granada UGR Spain 16. University of Durham UDUR United Kingdom 17. The University of Sheffield U-Sheffield United Kingdom 18. Technodyne International Ltd Technodyne United Kingdom 19. University of Aarhus U-Aarhus Denmark 20. AGT Ingegneria Srl, Perugia AGT Italy 21.Institute of Physics and Nuclear Engineering, Bucharest IFIN-HH Romania 22. Lombardi Engineering Limited Lombardi Switzerland

  4. FP 7 design study recommendations LAGUNA: Design of a pan-European Infrastructure for Large Apparatus studying Grand Unification and Neutrino Astrophysics Key questions in particle and astroparticle physics can be answered only by construction of new giant underground observatories to search for rare events and to study sources of terrestrial and extra-terrestrial neutrinos. In this context, the European Astroparticle Roadmap of 03/07, via ApPEC and ASPERA, states: ...recommend a new large European infrastructure, an international multi-purpose facility of 100-1000 kton scale for improved studies of proton decay and low-energy neutrinos. Water-Cherenkov, Liq. Scintillator & Liq. Argon should be evaluated as a common design study together with the underground infrastructure and eventual detection of accelerator neutrino beams. This study should take into account worldwide efforts and converge by 2010... Furthermore, the latest particle physics roadmap from CERN of 11/06 states: ...very important non-accelerator experiments takes place at the overlap of particle and astroparticle physics exploring otherwise inaccessible phenomena; Council will seek with ApPEC a coordinated strategy in these areas of mutual interest.

  5. LAGUNALarge Apparatus for Grand Unificationand Neutrino Astrophysics 100m 30m coordinated F&E “Design Study”European Collaboration,FP7 Proposal APPEC Roadmap LENAliquid scintillator13,500 PMs for 50 kt targetWater Čerenkov muon veto MEMPHYSWater Čerenkov500 kt target in 3 tanks,3x 81,000 PMs GLACIERliquid-Argon100 kt target, 20m driftlength,28,000 PMs foor Čerenkov- und szintillation

  6. Location of Phyasalmi in Finnland

  7. possible orientation of LENA tank Blue zones are regions with high mechanical stress due to horizontal rock pressure

  8. Cost estimate from rockplan predesign study Excavation + site investigation 55 M€ LAB construction + tank 60 M€ Detector: Scintillator+ electronics 190 M€ Engeneering 30 M€ Costs not including Tax and 20 % uncertainty

  9. Astrophysics • Details of a gravitational collapse (Supernova Neutrinos) • Studies of star formation in former epochs of the universe („Diffuse Supernovae Neutrinos Background“ DSNB) • High precision studies of thermo-nuclear fusion processes(Solar Neutrinos) • Test of geophysical models(“Geo-neutrinos”)

  10. Galactic Supernova in Lena

  11. EARTH Flavor conversion n emission Shock wave OBSERVING SN NEUTRINOS sensitive to SN dynamics -> matter induced oscillation Core Collapse Event rate spectra • f: from simulations of SN explosions • P : from n oscillations + simulations (density profile) • s : (well) known • e : under control

  12. Supernova neutrino luminosity (rough sketch) T. Janka, MPA Relative size of the different luminosities is not well known: it depends on uncertainties of the explosion mechanism and the equation of state of hot neutron star matter. Info on all neutrino flavors and energies desired!

  13. Event rates in LENA

  14. Separation of SN models ? • Yes, independent from oscillation model ! neutral current reactions in LENA e.g. TBP KRJ LL 12C: 700 950 2100 n p: 1500 2150 5750 Lawrence, Livermore Berkeley,Arizona Garching, Munich for 8 solar mass progenitor and 10 kpc distance

  15. Neutrinos from remnanant Supernovae Early star formation rate

  16. LENA: Diffuse SN Background • ne + p -> e+ + n • Delayed coincidence • Spectral information • Event rate depends on • Supernova type II rates • Supernova model • Range: 20 to 220 / 10 y • Background: ~ 1 per year M. Wurm et al., Phys. Rev D 75 (2007) 023007

  17. Neutrino Energy in MeV Solare Neutrinos Since May 07 BOREXINO Direct observation SuperK, SNO Gallium integral

  18. BOREXINO 1st result (astro-ph 0708.2251v2) • Scattering rate of 7Be solar non electrons 7Be n Rate: 47 ± 7STAT ± 12SYS c/d/100 t

  19. Expected from Borexino using new data: Be7 neutrino flux with high precission (< 10%) B 8 neutrino spectrum to low energy - shape information for oscillations New limit on neutrino magnetic moment CNO flux measurement

  20. gianni fiorentini, ferrara univ. @ n2004 Heat flow Neutrino flow Geo-Neutrinos : a new probe of Earth’s interior Antineutrino detection with inverse ß-decay reaction • Determine the radiogenic contribution to terrestrial heat flow, only half of the energy emission from the earth is understood • Test a fundamental geochemical paradigm about Earh’s origin: the Bulk Sylicate Earth • Test un-orthodox / heretical models of Earth’s interior (K in the core, Herndon giant reactor) • A new era of applied neutrino physics ?

  21. The crust (and the upper mantle only) are directly accessible to geochemical analysis. U, K and Th are “lithofile”, so they accumulate in the (continental) crust. U In the crust is: Mc(U) » (0.3-0.4)1017Kg. The » 30 Km crust should contains roughly as much as the » 3000 km deep mantle. Concerning other elements: Th/U »4* and 40K/U »1 For the lower mantle essentially no direct information: one relies on data from meteorites through geo-(cosmo)-chemical (BSE) model… According to geochemistry, no U, Th and K should be present in the core. crust Where are U, Th and K? U. M. L. M. Core

  22. Proton Decay and LENA • p K n • This decay mode is favoured in SUSY theories • The primary decay particle K is invisible in Water Cherenkov detectors • It and the K-decay particles are visible in scintillation detectors • Better energy solution further reduces background

  23. P -> K+ nevent structure: T (K+) = 105 MeV t (K+) = 12.8 nsec K+-> m+ n (63.5 %) K+-> p+ p0 (21.2 %) T (m+) = 152 MeV T (p+) = 108 MeV electromagnetic shower E = 135 MeV m+ -> e+n n (t = 2.2 ms) p+ -> m+ n(T = 4 MeV) m+ -> e+n n (t = 2.2 ms)

  24. 3 - fold coincidence ! • the first 2 events are monoenergetic ! • use time- and position correlation ! • How good can one separate the • first two events ? • ....results of a first Monte-Carlo calculation

  25. P decay into K and n m m K K time (nsec) Signal in LENA

  26. Background • Rejection: • monoenergetic K- and m-signal! • position correlation • pulse-shape analysis • (after correction on • reconstructed position)

  27. In LENA, we expect a background of ~ 5 / y without PSD discrimination • and after PSD-analysis this could be suppressed in LENA to • ~ 0.25 / y ! (efficiency~ 70% ) • A 30 kt detector (~ 1034 protons as target) would have a sensitivity of t < a few 1034years for the K-decayafter ~10 years measuring time • The minimal SUSYSU(5) model predicts the K-decay mode to be dominantwith a partial lifetime varying from 1029y to 1035 y ! • actual best limit from SK: t > 6.7 x 1032 y (90% cl)

  28. Results on fundamental physics from borexino counting test facility 1/100 of Brexino Target mass • electron decay Back et al.,Phys Lett.B 525 (2002) 29-40 • nucleon decay into invisible. channels. Back et al.,Phys Lett.B 563 (2003) 23-34 • νmagnetic moment Back et al.,Phys Lett.B 563 (2003) 35-47 • Heavy νmixing Back et al.,JETP Lett. Vol.78 N.5 (2003) 261-266 • Pauli exclusion principle Eur.Phys.Journ. C (2004) Lena= 10000 * CTF

  29. Conclusions • Low Energy Neutrino Astrophysics is very successful (Borexino direct observation of sub-MeV neutrinos) • Strong impact on questions in particle- and astrophysics • New technologies (photo-sensors, extremely low level background…) • Strong European groups

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