1. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 High Energy Neutrino Astronomy Status and perspectives of the high energy neutrino observatories Paolo Piattelli, INFN Laboratori Nazionali del Sud Catania

2. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 Layout of the talk High Energy Neutrino Astronomy –Scientific motivations –Experimental techniques Status of the presently active neutrino detector projects –The currently active neutrino detectors: Baikal and Amanda –The ongoing projects: Antares, Nestor, Nemo What comes next –The km3 at the South Pole: IceCube –The km3 in the Mediterranean sea: KM3NeT Conclusions and outlook

3. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 Why neutrino astronomy? Neutrinos traverse space without being deflected or attenuated –They point back to their sources –They allow to view into dense environments –They allow to investigate the Universe over cosmological distances Neutrinos are produced in high energy hadronic processes –They can allow distinction between hadronic and leptonic acceleration mechanisms Neutrinos could be produced in Dark Matter annihilation

4. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 Particle propagation in the Universe Photons are absorbed on dust and radiation Protons are deviated by magnetic fields Extremely high energy protons interact with background radiation Only neutrinos are direct 1 parsec (pc) = 3.26 light years (ly) High energy particles > 10 17 eV gamma rays (0.01 - 1 Mpc) protons E>10 19 eV (10 Mpc) protons E<10 19 eV neutrinos Cosmic accelerator

5. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 Particle astrophysics with telescopes

6. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 Neutrino production in cosmic accelerators Proton acceleration Fermi mechanism proton spectrum dN p /dE ~E -2 Neutrino production Proton interactions p  p (SNR,X-Ray Binaries) p   (AGN, GRB, microQSO) decay of pions and muons Astrophysical jet Particle accelerator electrons are responsible for gamma fluxes (synchrotron, IC) F. Halzen

7. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 Principles of neutrino astronomy Neutrino telescopes search for muon tracks induced by neutrino interactions The downgoing atmospheric  flux overcomes by several orders of magnitude the expected  fluxes induced by interactions. On the other hand, muons cannot travel in rock or water more than  50 km at any energy Upgoing and horizontal muon tracks are neutrino signatures

8. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 Principles of neutrino astronomy neutrino muon Cherenkov light ~5000 PMT neutrino Flux estimate  need km3 scale detectors

9. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 The HE neutrino telescope world map 80’s:DUMAND R&D 90’s:BAIKAL, AMANDA, NESTOR 2k’s:ANTARES, NEMO R&D 2010:ICECUBE Mediterranean KM3 ? AMANDA ICECUBE Mediterranean km 3 BAIKAL DUMAND Pylos La Seyne Capo Passero

10. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 A closer look at the Mediterranean Sea ANTARES 3800:4000 m 2400 m 3400 m NEMO NESTOR

11. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 Baikal 192 OM arranged in 8 strings, 72 m height effective area >2000 m 2 (E  >1 TeV) 3600 m 1366 m Successfully running since 10 years Atmospheric neutrino flux measured Further upgrades planned, but km 3 hardly reachable

12. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 Amanda Optical Module AMANDA-II 19 strings 677 OMs Depth 1500-2000m Effective Area  10 4 m 2 (E  TeV) Angular resolution  2° above horizon: mostly fake events below horizon: mostly atmospheric 959 events The AMANDA sky map

13. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 The ANTARES neutrino telescope string based detector 12 lines 900 PMTs 2400 m deep ~70 m 350 m 100 m 14.5 m Submarine links Junction Box 40 km to shore Anchor/line socket a storey

14. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 ANTARES status and realization plan 2003: Deployment and operation of two prototype lines Several months of data taking Technical problems (broken fiber, water leak) no precise timing, no  reconstruction. Early 2005: 2 upgraded prototype lines Mid-2005: Line 1 2007: Detector completed

15. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 NESTOR Tower based detector Up- and downward looking PMTs 3800 m deep Dry connections First floor (reduced size) with 12 PMTs deployed and operated in 2003

16. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 NEMO The NEMO Collaboration has dedicated special efforts in: development of technologies for the km 3 (technical solutions chosen by small scale demostrators are not directly scalable to a km 3 ) search, characterization and monitoring of a deep sea site adequate for the installation of the Mediterranean km 3 (Capo Passero near Catania, depth 3400 m) Modular detector concept based on semi-rigid structures 16 storey towers with 4 OM per storey 20 m storey length 40 m spacing between storeys Underwater connections

17. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 NEMO Phase 1 project 2.330 m Double Armed Cable 20.595 m Single Armed Cable Drop cable 2 5.220 m Drop cable 1 5.000 m joint BU joint NEMO Phase 1 Lab Long term tests for: underwater connections, electronics, mechanical structures, optical and acoustic detectors. Multidisciplinary laboratory (will host an on-line underwater seismic station of the Istituto Nazionale di Geofisica e Vulcanologia) SN-1 Realization of a detector subsystem including all critical components Site infrastructures at 2000 m already realized 30 km offshore Catania Project completely funded by INFN and MIUR Completion foreseen in 2006

18. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 The Catania Test Site and ESONET The NEMO test site in Catania will also host SN-1 a deep sea station for on-line seismic and environmental monitoring by INGV. The NEMO test site will be the Italian site for ESONET (European Seafloor Observatory NETwork).

19. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 NEMO Phase 2 A deep water station at the Capo Passero site PROPOSED INFRASTRUCTURE -Shore station at Portopalo di Capo Passero to host the power system the data acquisition and detector integration facilities -100 km electro optical cable -Underwater infrastructures (main junction box) -Two intermediate connection stations in shallow and medium deep waters for interdisciplinary activities (agreement with INGV and SACLANTCen)

20. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 ICECUBE The technology for underice detectors is well established. The next step is the construction of the km3 detector ICECUBE. 80 strings (60 PMT each) 4800 10” PMT (only downward looking) 125 m inter string distance 16 m spacing along a string Instrumented volume: 1 km 3 (1 Gton) First string to be deployed in january 2005

21. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 Status of the IceCube project  many reviews – international and within the U.S. - strongly emphasize the exciting science which can be performed with IceCube  in Jan 2004, the U.S. Congress approved the NSF budget including the full IceCube MRE  significant funding approved also in Belgium, Germany and Sweden  in Feb 2004, NSF conducted a baseline review  “go ahead”  deployment over 6 years IceCube strings IceTop tanks 48Jan 2005 1632Jan 2006 3264Jan 2007 50100Jan 2008 68136Jan 2009 80160 Jan 2010 IceCube strings IceTop tanks 48Jan 2005 1632Jan 2006 3264Jan 2007 50100Jan 2008 68136Jan 2009 80160 Jan 2010 From O. Botner, Neutrino 2004

22. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 Do we need two km3 detectors? There are strong scientific motivations that suggest to install two neutrino telescopes in opposite hemispheres : Full sky coverage The Universe is not isotropic at z<<1, observation of transient phenomena Galactic Center only observable from Northern Hemisphere There are strong scientific motivations that suggest to install two neutrino telescopes in opposite hemispheres : Full sky coverage The Universe is not isotropic at z<<1, observation of transient phenomena Galactic Center only observable from Northern Hemisphere The most convenient location for the Northern km3 detector is the Mediterranean Sea: vicinity to infrastructures good water quality good weather conditions for sea operations The most convenient location for the Northern km3 detector is the Mediterranean Sea: vicinity to infrastructures good water quality good weather conditions for sea operations

23. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 Sky coverage TeV sources  QSO Galactic centre Galactic coordinates Mediterranean km 3 ICECUBE 1.5  sr common view per day

24. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 KM3NeT: a Design Study for the km3 Astroparticle PhysicsPhysics Analysis System and Product Engineering Information Technology Shore and deep-sea structure Sea surface infrastructure Risk Assessment Quality Assurance Resource ExplorationAssociated Science A Technical Design Report (including site selection) for a Cubic kilometre Detector in the Mediterranean WORK PACKAGES Collaboration of 8 Countries, 34 Institutions Aim to design a deep-sea km 3 -scale observatory for high energy neutrino astronomy and an associated platform for deep-sea science Request for funding for 3 years The experience and know how of the ANTARES, NESTOR and NEMO collaborations is merging in the KM3-NET activity

25. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 Objectives and scopes of the KM3NeT DS Critical review of current technical solutions Thorough tests of new developments Comparative studies of sites and recommendation on site choice Assessment of quality control and assurance Exploration of possible cooperation with industry Investigation of funding and governance models Establish path from current projects to the KM3 Expected outcome In three years a complete Technical Design Report for the KM3 will be produced

26. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 Exploitation model of the future KM3 facility Reconstructed data will be made available to the whole community Observation of specific objects with increased sensitivity will be offered Close relation to space and ground based observatories will be established (alerts for GRBs, Supernovae, etc…) “Plug-and-play solutions for detectors of associated science Goal: facility exploited in multi-user and interdisciplinary environment

27. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 Associated science Great interest in long term deep-sea measurements in many different scientific communities: –Marine biology –Ocenography –Environmental science –Geology and geophysics –… Substantial cross-links to ESONET (the European Sea Floor Observatory Network) Plan: include the associated science communities in the design phase to understand and react to their needs and make use of their expertise (e.g. site exploration)

28. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 Actions in the new I3 proposal Networking –A collaboration between the european projects (Antares, Nestor, Nemo) has been already established with KM3NeT) –Increase collaboration with other neutrino projects (Baikal, Amanda, IceCube) –Develop collaborations with gamma ray and space based observatories –Other common fields of interest may be: massive computer simulations, development of common databases and source catalogues, development of computing and analysis tools JRAs –Overlap with KM3NeT should be avoided –Development of new detection methods for future neutrino detectior projects (radio detection, acoustic detection, …) Transnational access –All the european existing projects can provide access for interdisciplinary studies as the future KM3NeT will do

29. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 Conclusions Baikal and Amanda have demonstrated the feasibility of the high energy neutrino detection Three projects in the Mediterranean are under way: –Antares and Nestor are currently under construction (first data taken) –NEMO is pursuing R&D for technical solutions for the km3 –All three collaborations together in a common effort towards the km3 To fully exploit neutrino astronomy we need 2 km3 scale detectors, one for each emisphere: –IceCube is starting construction soon and will be completed by 2010 –KM3NeT aims at producing a complete Technical Design Report in 2008

30. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 Remarks on EU applications The EU applies rather stringent and formal rules. These rules are not laws of nature - so physicists tend to ignore them! Writing proposals: –Take the evaluation criteria seriously: European added value Scientific and technological excellence Relevance of the objectives of the scheme Quality of the management –Read all available EU documentation and learn “EUish” Evaluation process –Well structured and transparent from inside … –… but completely opaque from the outside! –It helps a lot to take part in the EU evaluations Lessons learned with the successful KM3NeT experience (from Uli Katzt, KM3NeT coordinator)

31. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 End of presentation

32. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 Next slides are spares

33. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 ANTARES: first deep sea data Rate measurements: Strong fluctuation of bioluminescence background observed 10min Rate (kHz) time (s) Constant baseline rate from 40 K decays

34. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 ANTARES: long term measurements baseline rate (kHz) burst fraction time Also measured: current velocity and direction, line heading and shape, temperatures, humidities,... Important input for preparation & optimization of ANTARES operation. baseline rate = 15-minute average burst fraction = time fraction above 1.2 x baseline rate

35. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 NESTOR: reconstruction of muon tracks Track reconstruction using arrival times of light at PMs. Ambiguities resolved using signal amplitudes in up/down PM pairs. PM calibration

36. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 The HE neutrino telescope world map 80’s:DUMAND R&D 90’s:BAIKAL, AMANDA, NESTOR 2k’s:ANTARES, NEMO R&D 2010:ICECUBE Mediterranean KM3 ? AMANDA ICECUBE Mediterranean km 3 BAIKAL DUMAND Pylos La Seyne Capo Passero ANTARES 3800:4000 m 2400 m 3400 m NEMO NESTOR

37. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 Scientific goals Astronomy via high energy neutrino observation –Production of high energy neutrinos in the universe (acceleration mechanisms, top-down scenarios, …) –Investigation of the nature of astrophysical objects –Origin of high energy cosmic rays Indirect search for Dark Matter New discoveries Associated science

38. P. Piattelli, CRNT meeting, Paris 16-17 december 2004 NEMO Phase 1 project A step towards the km3 detector EO CABLE Length – 25 km 10 Optical Fibres ITU- T G-652 6 Electrical Conductors  4 mm 2 Realization of a detector subsystem including all critical components Site infrastructures at 2000 m already realized 30 km offshore Catania SHORE LABORATORY Project completely funded (jointly by INFN and MIUR) Completion foreseen in 2006 UNDERWATER LAB