1. High energy neutrino astronomy with Cherenkov telescopes L. Moscoso CEA/Irfu/SPP & APC – Paris Rive Gauche XI ICATPP Conference Villa Olmo, Como, Italy, 5-9/10/2009

2. 5-9 Oct. 2009 L. Moscoso, ICATPP, Villa Olmo, Como, Italy2 The history of the sky survey The light since the origins Extension to the non visible since tens of years (Radio, IR, UV, X and gamma) Satellites  tens of GeV Large arrays  tens of TeV Multi-wavelenth astronomy

3. 5-9 Oct. 2009 L. Moscoso, ICATPP, Villa Olmo, Como, Italy3 Cosmic ray spectrum 50 J

4. 5-9 Oct. 2009 L. Moscoso, ICATPP, Villa Olmo, Como, Italy4 The GZK effect Interaction with IR, CMBR, Radio  absorption of HE photons and degradation of the proton energy Region above 100Mpc cannot be explored with photons above 10TeVProtons:Usefulabove 10 20 eV only. Galaxy Local cluster

5. 5-9 Oct. 2009 L. Moscoso, ICATPP, Villa Olmo, Como, Italy5 High energy neutrinos The neutrino as an alternative solution Multi-wavelength and multi-messenger studies Multi-wavelength and multi-messenger studies Exploration of the most remote regions of the Universe Exploration of the most remote regions of the Universe –Not absorbed (weak cross section) –Electrically neutral: not deflected by magnetic fields But at least a km 3 is necessary!

6. 5-9 Oct. 2009 L. Moscoso, ICATPP, Villa Olmo, Como, Italy6 Synchrotron radiation followed by inverse Compton The mechanism The mechanism HE electron LE  HE electron HE 

7. 5-9 Oct. 2009 L. Moscoso, ICATPP, Villa Olmo, Como, Italy7 Synchrotron radiation followed by  photo-production The mechanism The mechanism HE electron LE  HE proton HE  ° HE nucleon HE 

8. 5-9 Oct. 2009 L. Moscoso, ICATPP, Villa Olmo, Como, Italy8 Synchrotron radiation followed by  ± photo-production The mechanism The mechanism L CR  L   L HE electron LE  HE proton HE  ± HE nucleon HE muon HE  HE electron HE   HE e

9. 5-9 Oct. 2009 L. Moscoso, ICATPP, Villa Olmo, Como, Italy9 Scientific issues Particle physics and Cosmology –DM indirect search –Neutrino oscillations Astrophysics –Quasars –Gamma ray bursts (GRB) –Microquasars –Pulsars –SNR –Topological defects + other exotics

10. 5-9 Oct. 2009 L. Moscoso, ICATPP, Villa Olmo, Como, Italy10 Difficult detection Very weak cross section  Huge detector Very weak cross section  Huge detector km 3 Very high cosmic ray flux  shielded detector Very high cosmic ray flux  shielded detector Underground or submarine

11. 5-9 Oct. 2009 L. Moscoso, ICATPP, Villa Olmo, Como, Italy11 Detection techniques HE induced muon produced in the surrounding medium by HE neutrino HE induced muon produced in the surrounding medium by HE neutrino –Upward-going neutrinos only (2  ) –Mass = R  S (R   2.5 km we @ 1 TeV; 10 km @10 TeV) HE muons produced inside the detector by HE neutrino interactions (4  ) HE muons produced inside the detector by HE neutrino interactions (4  ) –Requires a very large detector (IceCube or KM3NeT) VHE e interaction inside the detector (4  ) VHE e interaction inside the detector (4  ) –Detection of cascades

12. 5-9 Oct. 2009 L. Moscoso, ICATPP, Villa Olmo, Como, Italy12 Induced muons  detector The cherenkov light is detected by the PMTs The neutrinos interact With the surrounding matter The muon generates the Cherenkov light p   c =43° Correlation time-position  direction of the muon Precision on the position: 10cm Precision on time: 1ns

13. 5-9 Oct. 2009 L. Moscoso, ICATPP, Villa Olmo, Como, Italy13 The advantages Target mass  R  increases with the neutrino energy Target mass  R  increases with the neutrino energy Interaction cross section increases with the neutrino energy Interaction cross section increases with the neutrino energy Detection efficiency increases with the muon energy and therefore with the neutrino energy Detection efficiency increases with the muon energy and therefore with the neutrino energy  Enrichment of the high energy neutrinos

14. 5-9 Oct. 2009 L. Moscoso, ICATPP, Villa Olmo, Como, Italy14 Physics background Atm. muons Atm. 10 6 d  /d  cm -2 s -1 sr -1 cos  2400 m depth, E > 1 TeV Atmospheric showers atmospheric muons   10 9 events/year Atmospheric neutrinos   3000/year

15. 5-9 Oct. 2009 L. Moscoso, ICATPP, Villa Olmo, Como, Italy15 The neutrino telescopes NESTOR : Pylos, Greece ANTARES La-Seyne-sur-Mer, France BAIKAL: Baikal lake, Siberia DUMAND, Hawaii (cancelled 1995) AMANDA, IceCube South Pole NEMO Catania, Italy

16. 5-9 Oct. 2009 L. Moscoso, ICATPP, Villa Olmo, Como, Italy16 The Mini Tower for NEMO Phase-1 Optical modules Floor control module Mechanical stresses are applied only to the tensioning ropes Tower Base Module Floor 1 Floor 2 Floor 3 Floor 4 Backbone e.o. cable Tensioning ropes e.o. Jumper cable Tower base - JB Break-out

17. 5-9 Oct. 2009 L. Moscoso, ICATPP, Villa Olmo, Como, Italy17 Nemo Phase 1 Shore station 2.5 km e.o. Cable with double steel shield 21 km e.o. Cable with single steel shield JBU J J 5 km e.o. cable Geoseismic station SN-1 (INGV) 5 km e.o. cable  10 optical fibres standard ITU- T G-652  6 electrical conductors  4 mm 2

18. 5-9 Oct. 2009 L. Moscoso, ICATPP, Villa Olmo, Como, Italy18 The Antares station Submarine cable -2475m La Seyne sur Mer Michel Pacha institute On shore station

19. 5-9 Oct. 2009 L. Moscoso, ICATPP, Villa Olmo, Como, Italy19 The ANTARES detector vincenzo flaminio ~ 60 m 100 m 350 m 14.5 m Link cable Junction Box Cable to shore 2500m depth Storey 45°

20. 5-9 Oct. 2009 L. Moscoso, ICATPP, Villa Olmo, Como, Italy20 Number of Triggers CABLE REPAIR 5 lines (2007) 19.10 6 μ 10 or more lines (2008) 65.10 6 μ Total : 240 days = 80% of calendar Selected :167d = 70% of total Total : 243 days = 83% of calendar Selected :173d = 71% of total

21. 5-9 Oct. 2009 L. Moscoso, ICATPP, Villa Olmo, Como, Italy21 Zenith angular distribution neutrinos June 2007 – Dec 2008 5+10+12 lines 341 active days 1062 upward neutrino candidates upgoingdowngoing Good agreement with “standard” neutrino oscillations : sin 2 2θ = 1; Δm 2 = 2.4 · 10 -3 eV 2

22. 5-9 Oct. 2009 L. Moscoso, ICATPP, Villa Olmo, Como, Italy22 Search for point-like sources Upper limits obtained with 2007 data (5 lines, 140 day lifetime), compared with 1 year of complete detector (12 lines) and other experiments Analysis of 12-line data is ongoing For further information see talks given by M. Vecchi (INFN-Roma1) & U. Fritsh (ECAP Univ. Erlangen)

23. 5-9 Oct. 2009 L. Moscoso, ICATPP, Villa Olmo, Como, Italy23 5 lines (2007): Depth vs. Intensity Preliminary Work on reducing systematics is ongoing 2,5km 6km

24. 5-9 Oct. 2009 L. Moscoso, ICATPP, Villa Olmo, Como, Italy24 Transients with ANTARES Triggered searches (alerts from satellites: Integral, Swift, Fermi)Triggered searches (alerts from satellites: Integral, Swift, Fermi) Low backgrounds due to direction and time coincidencesLow backgrounds due to direction and time coincidences Dump all L0 data in 2min window around trigger (i.e. no trigger losses)Dump all L0 data in 2min window around trigger (i.e. no trigger losses) Special track reconstruction using known directionSpecial track reconstruction using known direction Neutrino multiplets in time optical follow-up (Tarot in France and at La Silla)Neutrino multiplets in time optical follow-up (Tarot in France and at La Silla) Full sky 24h/24 searchFull sky 24h/24 search Sliding time window around eventsSliding time window around events Fast online reconstruction  optical follow up to identify sourceFast online reconstruction  optical follow up to identify source Gravitational waves and neutrinos (Virgo + Ligo + Antares)Gravitational waves and neutrinos (Virgo + Ligo + Antares) Drafting a MoU in progressDrafting a MoU in progress

25. 5-9 Oct. 2009 L. Moscoso, ICATPP, Villa Olmo, Como, Italy25IceCube Full project: 80 60-floors detector Full project: 80 60-floors detector First analysis results on 22 strings First analysis results on 22 strings 40 strings now installed: will allow a 4  survey 40 strings now installed: will allow a 4  survey Installation of a deep dense core (7 strings) foreseen Installation of a deep dense core (7 strings) foreseen

26. 5-9 Oct. 2009 L. Moscoso, ICATPP, Villa Olmo, Como, Italy26

27. 5-9 Oct. 2009 L. Moscoso, ICATPP, Villa Olmo, Como, Italy27 Flux upper limits vs declination 2009.09.26Chad Finley27

28. 5-9 Oct. 2009 L. Moscoso, ICATPP, Villa Olmo, Como, Italy28 See T. Montaruli, ICRC09

29. 5-9 Oct. 2009 L. Moscoso, ICATPP, Villa Olmo, Como, Italy29 Solar wimp limits Phys.Rev.Lett.102:201302,2009, C. Rott, ICRC 09

30. 5-9 Oct. 2009 L. Moscoso, ICATPP, Villa Olmo, Como, Italy30KM3NeT ++ +… A research facility in the Mediterranean Sea  A next generation neutrino telescope (at the km-scale)  Cabled observatory for Earth and Marine sciences 38 institutes from 10 European countries

31. 5-9 Oct. 2009 L. Moscoso, ICATPP, Villa Olmo, Como, Italy31 Design goals  Substantially competitive with IceCube  Volume > 1 km 3  Optimized for energy range 1 TeV – 1 PeV  Angular resolution < 0.1 o  Zenith angle:  Full acceptance for neutrinos originating from directions up to at least 10° above the horizon  For energies > 100 TeV angular acceptance limited only by the absorption of the Earth See the talk given by G. De Bonis (INFN-Pisa)

32. 5-9 Oct. 2009 L. Moscoso, ICATPP, Villa Olmo, Como, Italy32 KM3NeT Design Study Design study  funded by EU FP6 in February 2006 Development of a cost-effective design for a cubic km sized deep-sea infrastructure housing a neutrino telescope…. Conceptual Design Report released in April 2008 released in April 2008 (www.km3net.org) (www.km3net.org) Includes: Science case Site studies Design goals Technical implementation

33. 5-9 Oct. 2009 L. Moscoso, ICATPP, Villa Olmo, Como, Italy33 Km3Net Design Study

34. 5-9 Oct. 2009 L. Moscoso, ICATPP, Villa Olmo, Como, Italy34 Funded by the EU FP7 framework in March 2008 Primary objective  pave the path to political and scientific convergence on the legal, governance, financial engineering and siting aspects of the infrastructure….. Km3Net Preparatory Phase Km3net timeline

35. 5-9 Oct. 2009 L. Moscoso, ICATPP, Villa Olmo, Como, Italy35 Conclusions Since many years the neutrino has been considered as an alternative way to observe the Universe Since many years the neutrino has been considered as an alternative way to observe the Universe It was a long way to achieves some very large volume neutrino telescopes It was a long way to achieves some very large volume neutrino telescopes Now two devices are operating Now two devices are operating 50% of the km 3 detector at the South Pole is achieved and the full detector will be completed in 2011 50% of the km 3 detector at the South Pole is achieved and the full detector will be completed in 2011 The first neutrino telescope in the Mediterranean has been achieved too and is operating The first neutrino telescope in the Mediterranean has been achieved too and is operating The study for a km 3 detector in the Mediterranean is reaching the final phase (TDR editing). The construction will probably start at the end of the preparatory phase (2011) The study for a km 3 detector in the Mediterranean is reaching the final phase (TDR editing). The construction will probably start at the end of the preparatory phase (2011)