1. Recent Developments in Neutrino Telescopy Spyros Tzamarias HEP2012: Recent Developments in High Energy Physics and Cosmology

2. 615 t of C 2 Cl 4 The Nobel Prize in Physics 2002 Masatoshi Koshiba Raymond Davis Jr. Riccardo Giacconi These discoveries of low (<100MeV) energy extraterrestrial neutrinos led us to various achievements on basic neutrino properties (oscillations) and stellar evolution. They also offer important possibilities to progress, e.g., with geoneutrinos and solar (CNO) neutrinos, and even more with supernova neutrinos.

3. Furthermore, the obtained knowledge and the increased confidence motivate us to continue, widening the scope and field of our investigation. The current experiments are monitoring a huge range of energies! Log(E/eV)

4. νμνμ μ- W-W- d As proposed by Markov in the late 50s, the neutrino-induced μ's offer the practical way to probe high energy neutrinos, whilst using the whole earth as an absorber of atmospheric muons. The size of such a detector is dictated by the muon’s range (due to EM interactions) i.e. the detector size for an efficient TeV-muon detection should be of the order of a km ln

5. Extraterrestrial High Energy Neutrino Sources Or What do we need these neutrinos for ? Cosmic-Hadron accelerators can produce VHE CR’s, γ-rays and neutrinos Electron acceleration is the main source of the non-thermal EM radiation, up to high energies (up to TeV). Many such e-accelerators have been identified. There is a connection between the (multi-TeV) γ and neutrino production Where are these Cosmic-Hadron accelerators? Cosmic-Hadron accelerators can produce VHE CR’s, γ-rays and neutrinos Electron acceleration is the main source of the non-thermal EM radiation, up to high energies (up to TeV). Many such e-accelerators have been identified. There is a connection between the (multi-TeV) γ and neutrino production Where are these Cosmic-Hadron accelerators?

7. W. Baade and F. Zwicky, Remarks on super-novae and cosmic rays, Phys. Rev. 46 (1934 ) 76 Galactic Sources ExtraGalactic Sources

8. Neutrinos (for all distances) and gammas point to the source of origin. However…

9. There many kinds of HE neutrino sources (perhaps as many as the Supersymmetric Scenaria)

14.  WIMP (neutralino) SUN earth Indirect Searches for Dark Matter

17. ICECUBEKM3NeT Full Sky Coverage

18. Why neutrinos from Galactic γ-ray (TeV) sources are important ? Observation of PeV (10 15 eV) γ-rays will point to hadron accelerators revealing the CR sources. However, a) PeV γ-rays do not survive large distances and b) the γ-ray spectra of the observed galactic sources exhibit energy cut-off Neutrino observation from RX J1713.7-3946 will prove unambiguously the hadronic production of γ-rays RX J1713.7-3946

19. REMINDER: there are not very reliable phenomenological models to predict precise upper bounds for the extragalactic neutrino fluxes A more efficient (larger effective area, better resolution) than ICECUBE detector is needed to discover galactic sources

20. NEMO

21. KM3NeT 21 International consortium involving more than 300 scientists from 10 EU countries One objective: build the most sensitive high energy neutrino telescope KM3NeT is one of the 44 pan-european research infrastructures on the ESFRI EU roadmap

22. An artists impression of KM3NeT (≈ 1/3) 22 Primary Junction box Secondary Junction boxes Detection Units Electro-optical cable

26. signal hits background hits pictorial representation of a ν charged current interaction inside the neutrino telescope Pattern Recognition and Track Reconstruction

27. Eν<10 TeV 10TeV<Eν<100 TeV 100TeV<Eν<1 PeV 1PeV<Eν Angle (ψ) between reconstructed muon track and parent neutrino (Degrees) z xy (θ m, φ m ) ψ (θ true, φ true ) Can we estimate accurately the tracking errors? Median of Ψ (degrees) vs the cosine of the zenith angle

28. Energy Estimation HOU Reconstruction & Simulation (HOURS): A complete simulation and reconstruction package for Very Large Volume underwater neutrino Telescopes, A. G. Tsirigotis et al., VLVNT2009 Reconstructed Energy (log of GeV) 0.5<cos(θ)<0.55

29. R.A Decl. RX J1713.7-3946

30. Comparison of the Discovery Potentials Number of events (N) – Angular profile (S) – Energy (E) years Discovery Potential in units of the reference flux RXJ1713

31. 5-σ DISCOVERY POTENTIAL years Discovery Potential in units of the reference flux 1,00

32. FOM (years of observation time) 5-σ DISCOVERY. 8.4y 7.6y 6.4y 6.0y 5.6y 1,00 KM3NeT with 608 strings at 100m (130m) apart will discover a neutrino source as the RXJ1713 after 5.6 (6) years of observation. The estimation error is less than 0.8y. PRELIMINARY: An extra 30% improvement ( i.e a discovery after 4 y of observation) can be achieved by taking into account the known source direction. A further improvement is expected by developing a more efficient method to reject low energy atmospheric neutrinos., see A. Tsirigotis talk

33. KM3NeT and EMSO E. Migneco KM3NeT-PP general meeting - Catania, february 22 2012 33 Real Time Environmental Monitoring Sinergy with the Earth and Sea Science Community Toulon, Sicily and Hellenic: sites of common interest for KM3NeT and EMSO Geophisics (geohazard): Seismic phenomena, low frequency passive acoustics, magnetic field variations,... Oceanography (water circulation, climate change): Current intensity and direction, Water temperature, Water salinity,... Biology (micro-biology, cetaceans,...): Passive acoustics, Biofouling, Bioluminescence, Water samples analysis,...

34. What after the Preparatory Phase? Need an organizational structure to manage the post- design and preparatory phase A Memorandum of Understanding is in preparation Goals – Complete the Physics Studies and the Optimization of the design – Validation of chosen technologies – Complete the final Technical Proposal – Central management – Definition of collaboration rules – Start of construction with engineering arrays in the potential “host” sites