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 masses

4. LAGUNA Physics Galactic Supernova neutrino burst understanding of gravitational collapse neutrino properties:   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   Search for leptonic CP-violation (if    is 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 a new large European infrastructure is put forward, as a future international multi-purpose facility on the 10 5 -10 6 ton scale for improved studies of proton decay and 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. MEMPHIS TRE MEMPHYS 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  ≈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 ( 7 Be, 8 B) 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 ->    e + Water Cherenkov MEMPHIS ca. 10 35 y (5000 kt y exposure) Limit SK-I and II:  x     y p -> K + Liquid Argon GLACIER ca. 10 35 y (1000 kt y exposure) Liquid Scintillator LENA ca. 5 x 10 34 y (500 kt y exposure) Limit SK-I:  x     y

23. Sensitivity on Supernova MEMPHIS mainly sensitive on e 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

24. Sensitivity on Supernova Sensitive on e ! Important for neutronisation phase Sensitive on oscillation parameter and mass hierarchy

25. Sensitivity on Supernova

26. DSNB Detection via inverse beta decay Free protons as target Threshold 1.8 MeV E  ~ E e - Q ( spectroscopy) suppress background via delayed coincidence method n + p  D +  (2.2 MeV) position reconstruction => fiducial volume (suppress external background) Delayed signal (~200  s) Prompt signal

27. LENA at Pyhäsalmi (Finland) dependent on SN model (assumed f SN =2.5) LL:113 KRJ:100 TBP:60 dependent on SNR f SN =0.7 17 f SN =2.5 100 f SN =4.2 220 DSN event rate in 10yrs inside the energy window from 9.7 to 25 MeV background events: 13 ~25% of events are due to v’s originating from SN @ z>1! TU München Outline DSNB Background Event Rates Spectroscopy

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

29. GEO Neutrinos LENA rate between 3 x 10 2 and 3 x 10 3 per year (at Pyhäsalmi, Finland) Background ~ 240 per year in [1.8 MeV – 3.2 MeV] from reactor neutrinos < 30 per year due to 210 Po alpha-n reaction on 13 C (Borexino purity assumed) ~ 1 per year due to cosmogenic background ( 9 Li - beta-neutron cascade) Can be statistically subtracted

30. Long baseline oscillations    CP  sign(  M 2 )    e e   High Intensity conventional neutrino source. “Superbeams” Time scale > 2014 (?) New neutrino source. “Betabeams, nu-factory” Time scale ~ 2020 (?)

31. 31 Laboratorio Subterraneo de Canfranc, Spain LSC Laboratori Nazionali del Gran Sasso, Italy LNGS SUNLAB Polkowice-Sieroszowice, Poland Institute of Underground Science in Boulby mine, UK IUS Laboratoire Souterrain de Modane, France L=630 km L=130 km L=2300 L=950 L=732 km L=1050 km

32. 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)

33. LENA and Reactor neutrinos At Frejus ~ 17,000 events per year High precision on solar oscillation parameter:  m 2 12     S.T. Petcov, T. Schwetz, Phys. Lett. B 642, (2006), 487 J. Kopp et al., JHEP 01 (2007), 053

34. 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)

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