1 / 35

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.

rafe
Download Presentation

LAGUNA and Neutrino Physics

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  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

More Related