1. P. Sapienza, NOW 2010 The KM3NeT project  Introduction & Main objectives  The KM3NeT Technical Design Report  Telescope physics performance  New developments  Summary 1

2. P. Sapienza, NOW 2010 Motivation for the high energy neutrino detection 2 Neutrino will provide unique pieces of information on High Energy Universe Physics case Astrophysical high energy neutrino sources (SNR, microquasars, AGN, GRB) Origin of cosmic rays Unknown neutrino sources Indirect search of Dark Matter

3. P. Sapienza, NOW 2010 Detection principle – TeV-PeV => Optical Cherenkov 3 Upward-going neutrinos interact in rock or ice or sea/lake water. Emerging charged particles (in particular muons) produce Cherenkov light in water/ice Detection by array of photomultipliers Muon direction reconstructed from photon arrival times and PMT positions Estimates indicate that a detector size of the order of km3 is needed for astronomy

4. P. Sapienza, NOW 2010 High energy neutrino telescope world map 4 AMANDA IceCube ANTARES, NEMO, NESTOR KM3NeT Baikal Pylos La Seyne Capo Passero

5. P. Sapienza, NOW 2010 KM3NeT: towards a km 3 -scale telescope in the Mediterranean Sea  KM3NeT consortium consists of 40 European institutes including those in Antares, Nemo and Nestor  KM3NeT Design Study defined telescope design and outlined main technological options  Approved under the 6° FP (funded by EU for the period 2006-2009)  Conceptual Design Report published in 2008 http://www.km3net.org/public.phphttp://www.km3net.org/public.php  Technical Design Report (TDR) outlines technologies for the construction, deployment and maintenance of a deep sea neutrino telescope http://www.km3net.org/public.php (TDR contents frozen in November 2009) http://www.km3net.org/public.php  KM3NeT Preparatory Phase define legal, governance and funding aspects. Production planes for the detector elements, infrastructure features and prototype validation will be also defined  Approved under the 7° FP (funded by EU for the period 2008-2012) 5

6. P. Sapienza, NOW 2010 KM3NeT main objectives 6  Energy range and main physics goals  Investigate neutrino “point sources”  optimisation in the energy regime 1-100 TeV with a coverage of most of the sky including the Galactic Centre  Implementation requirements  Construction time ≤5 years  Operation over at least 10 years without “major maintenance”  Cabled platform for deep-sea research (marine sciences)

7. P. Sapienza, NOW 2010 Sky view of a Mediterranean Sea telescope 7 >75% >25%  KM3NeT complements the IceCube field of view  KM3NeT observes a large part of the sky (~3.5  ) Sensitivity for up-going neutrinos considered From Mediterranean 24h per day visibility up to about  =-50°

8. P. Sapienza, NOW 2010 KM3NeT: an artistic view 8 Primary Junction box Secondary Junction boxes Detection Units Electro-optical cable

9. P. Sapienza, NOW 2010 Technical Challenges and Telescope Design  Technical design Objective: Build 3D-array of photodetectors and connect them to shore (data, power, slow control)  Optical modules  Data acquisition, information technology and electronics  Mechanical structures  Deep-sea infrastructure  Deployment  Calibration 9 Design rationale: Cost-effective Reliable Producable Easy to deploy Design rationale: Cost-effective Reliable Producable Easy to deploy Builds on the experience gained with ANTARES, NEMO and NESTOR

10. P. Sapienza, NOW 2010 Other issues addressed in the Design Study 10  Site characteristics  Measure site characteristics (optical properties and optical background, currents, sedimentation, …)  Simulations  Determine detector sensitivity, optimise detector parameters  Earth and Sea science requirements  Define the infrastructure needed to implement multidisciplinary science nodes

11. P. Sapienza, NOW 2010 Single PMT Optical Module 11  8” PMT with 35% quantum efficiency inside a 13” glass sphere  good timing  evolution from pilot projects => well known technology

12. P. Sapienza, NOW 2010 Multi-PMT Optical Module 12  31 3” PMTs inside a 17” glass sphere with 31 bases (total ~140 mW)  Cooling shield and stem  First full prototype end of 2010  Single vs multi photon hit separation  Larger photocade area per OM

13. P. Sapienza, NOW 2010 TDR - Detection Unit concepts 13 Flexible tower with horizontal bars equipped with single-PMTs or multi-PMT OMs Triangular arrangements of OMs with single-PMTs or multi-PMT Evolution of the ANTARES storey Slender string Vertical sequence of multi-PMTs OMs Simulations indicate that local 3D OM arrangement resolve ambiguities in the reconstruction of the muon azimuthal angle DUs are the mechanical structures that hold OMs, enviromental sensors, electronics,…

14. P. Sapienza, NOW 2010 Deployment strategy 14  Compact package & Self unfurling => easy logistics that speeds up and eases deployment  Connection to seabed network by Remotely Operated Vehicle Spherical deployment structure for string with multi-PMT OM The packed flexible tower Successful deployment test in February 2010 Successful deployment test in December 2009

15. P. Sapienza, NOW 2010 KM3NeT performance 15 ☐ Quality Cuts applied (0.2°@30TeV) Quality Cuts optimized for sensitivity Up-going neutrino Effective Area Detector resolution Median of   rec    

16. P. Sapienza, NOW 2010 TDR- KM3NeT Sensitivity & Discovery potential 16 KM3NeT sensitivity 90%CL KM3NeT discovery 5  50% IceCube sensitivity 90%CL IceCube discovery 5  50% 2.5÷3.5 above sensitivity flux. (extrapolation from IceCube 40 string configuration) binned method unbinned method | Observed Galactic TeV-g sources (SNR, unidentified, microquazars) F. Aharonian et al. Rep. Prog. Phys. (2008) Abdo et al., MILAGRO, Astrophys. J. 658 L33-L36 (2007)  Galactic Centre Sensitivity and discovery fluxes for point like sources with a E -2 spectrum for 1 year of observation time (full detector 154 DUx2) Observation of RXJ1713 at 5  within about 5 years Sensitivity and discovery potential will improve with unbinned analysis

17. P. Sapienza, NOW 2010 Developments after the TDR  Major effort towards the construction and validation of pre-production model of the DU underway  Bar with horizontal extent  Optimised design and plan for extensive deployment tests defined  Multi-PMT Optical Module  Development plan for validation of technology and validation procedure defined  Optimization of simulation of the detector performance ongoing  Deployment of first prototype DU planned end 2011  Hkhk  Gjgjgj  Gjgjg  hjkhjhj 17

18. P. Sapienza, NOW 2010 Packaging of a tower with 20 storey for compact deployment 18 6 m 1.1 m 2.6 m

19. P. Sapienza, NOW 2010 Concluding remarks 19  The KM3NeT TDR is a major milestone for KM3NeT  Km3NeT detector volume will be about 5 km 3  KM3NeT activities, together with the success of the pilot projects, puts the project on a firm ground  KM3NeT will cover a large fraction (87%) of the sky with a sensitivity and discover potential that will be better than any other neutrino telescope

20. P. Sapienza, NOW 2010 Concluding remarks 20  Major impact also on the deep-sea sciences  Technological solutions developed by KM3NeT modified the state-of- the-art for deep-sea sciences  Strong synergies with the EMSO project  Collaboration with INGV and IFREMER already active at the Catania and Toulonsites  Significant acceleration of the convergence process towards a unique technical solution  Final prototyping process will be coordinated within the Preparatory Phase