Recent Developments in Neutrino Telescopy

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

2. 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. The Nobel Prize in Physics 2002 Raymond Davis Jr. Masatoshi Koshiba Riccardo Giacconi 615t of C2Cl4

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

4. νμ d W- μ- 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) ln i.e. the detector size for an efficient TeV-muon detection should be of the order of a km

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?

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

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 SupersymmetricScenaria)

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

17. Full Sky Coverage ICECUBE KM3NeT

18. Why neutrinos from Galactic γ-ray (TeV) sources are important ? Observation of PeV (1015eV)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 RX J1713.7-3946 Neutrino observation from RX J1713.7-3946will prove unambiguously the hadronic production of γ-rays

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 International consortiuminvolving more than 300 scientistsfrom 10 EU countries Oneobjective: build the most sensitive high energy neutrino telescope KM3NeT isoneof the 44pan-europeanresearchinfrastructures on the ESFRI EU roadmap

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

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

27. Can we estimate accurately the tracking errors? Median of Ψ (degrees) vs the cosine of the zenith angle (θtrue, φtrue) z (θm, φm) ψ x y Eν<10 TeV 100TeV<Eν<1 PeV 10TeV<Eν<100 TeV 1PeV<Eν Angle (ψ) between reconstructed muon track and parent neutrino (Degrees)

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

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

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

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

32. FOM (years of observation time) 5-σ DISCOVERY. 8.4y 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 7.6y 6.4y 1,00 6.0y 5.6y KM3NeT with 608 strings at 100m (130m) apart will discovera neutrino source as the RXJ1713 after 5.6 (6) years of observation. The estimation error is less than 0.8y.

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

34. Whatafter the PreparatoryPhase? • Needanorganizationalstructuretomanage the post-design and preparatoryphase • A Memorandum ofUnderstandingis in preparation • Goals • Complete the PhysicsStudies and the Optimizationof the design • Validationofchosentechnologies • Complete the finalTechnicalProposal • Central management • Definitionofcollaborationrules • Start ofconstructionwithengineeringarrays in the potential “host” sites