STATUS AND PHYSICS GOALS OF KM3NET Paolo Piattelli P. Piattelli, ICHEP14 Valencia INFN – LNS, Catania (Italy)

Physics with high-energy neutrinos P. Piattelli, ICHEP14 Valencia  VHE gamma-rays are absorbed by dust and radiation and do not disentangle between leptonic and hadronic mechanisms  Directions of charged cosmic rays scrambled by magnetic fields  Neutrinos can provide unperturbed information on the sources gamma rays protons E>10 19 eV (100 Mpc) protons E<10 19 эВ neutrino Particle accelerator

The KM3NeT sky P. Piattelli, ICHEP14 Valencia th Sensitivity for up-going neutrinos From Mediterranean 24h per day visibility up to about δ = -50°  KM3NeT complements the IceCube field of view  KM3NeT observes a large part of the sky (~3.5  )

The KM3NeT design P. Piattelli, ICHEP14 Valencia  Detection unit (DU) – vertical slender string with multi-PMT digital optical modules (DOMs)  Each DU 18 multi-PMT DOMs supported by two parallel ropes  Power and data distributed by a single backbone cable with breakouts at DOMs  Vertical distances between DOMs = 36 m  Lowest DOM at 100 m above the seabed  Total height of the DU ~700 m  Six building blocks of 115 DUs each, allow for a distributed detector

KM3NeT multi-site concept P. Piattelli, ICHEP14 Valencia detectors, each ~2km 3 in 3 sites KM3NeT-France: Toulon (depth ~ 2500m) KM3NeT-Italy: Capo Passero (depth ~ 3500m) KM3NeT-Greece: Pylos (depth ~ 4500m) Same technical design at all sites Common hardware, data handling and operation control Centrally managed Node for marine science at each installation site

The Digital Optical Module  31 3” PMTs with reflectors in 17-inch glass sphere (cathode area ~3x10” PMTs)  19 in lower, 12 in upper hemisphere  Suspended by support structure  31 PMT bases (total ~140 mW)  Aluminum cooling shield and stem  Piezo, Nano-beacon (LED), compass, tiltmeter  FPGA readout  2mm optical gel (ANTARES-type) 6 P. Piattelli, ICHEP14 Valencia

The Detection Unit P. Piattelli, ICHEP14 Valencia ~ 600 m Optical module 31 x 3” PMTs low-power HV LED & piezo inside FPGA readout White Rabbit DWDM 7 17” Launcher vehicle ‒ rapid deployment ‒ autonomous unfurling ‒ recoverable

DOM prototype P. Piattelli, ICHEP14 Valencia April

DOM prototype results P. Piattelli, ICHEP14 Valencia Multiplicity Rate [Hz] PMT orientation [deg.] atmospheric muons K40 random coincidences + data photon counting directionality atmospheric muons + data (M ≥ 7) shadowing Rate [a.u.]

Detection Unit prototype P. Piattelli, ICHEP14 Valencia DOMs with ETEL D783FLA PMTs 1 DOM with Hamamatsu R PMTs Deployed at the KM3NeT-It site at 3500m depth Operational since May 2014

DU prototype integration and deployment P. Piattelli, ICHEP14 Valencia Integrated at Nikhef (Amsterdam) and CPPM (Marseille) Deployed at 3500 m depth in the site of Capo Passero (Italy) in May 2014

First prototype DU data P. Piattelli, ICHEP14 Valencia Rate [Hz] Multiplicity number of events  t [  s] Time difference between optical modules KM3NeT preliminary

KM3NeT Phase-1 P. Piattelli, ICHEP14 Valencia Proof of feasibility of network of neutrino detectors  Started in January 2014  Funded with 31 million Euro  31 detection units will be deployed in  Sites: KM3NeT-It (24 DUs), KM3NeT-Fr (7 DUs)

KM3NeT Phase 1.5 P. Piattelli, ICHEP14 Valencia Measurement from the Northern Hemisphere of the neutrino signal reported by IceCube  Two building blocks of 115 detection units each  Cascade analysis – cut & count  Online data filter: ≥ 5 coincidences between PMTs in the same optical module, Δ t=10ns  Event filter: number of hits ≥ 2000  Atmospheric muon veto: (pseudo) vertex cut  Energy cut: total time-over-threshold ≥ 15 μ s  MRF/MDP cut: 2D cut based on Boosted Decision Tree & energy estimate

Atmospheric muon data P. Piattelli, ICHEP14 Valencia cosmic neutrinosatmospheric muons R 2 [10 3 m 2 ] vertex cut detector volume

Signal / noise P. Piattelli, ICHEP14 Valencia Boosted Decision Tree – multivariate algorithm, using topological/reconstruction quality related parameters BDT>0.35 – strong rejection of remaining atmospheric muons BDT atmospheric muons atmospheric neutrinos (tracks) atmospheric neutrinos (showers) cosmic neutrinos (tracks) cosmic neutrinos (showers)  events / 6 months

Phase 1.5 sensitivity P. Piattelli, ICHEP14 Valencia years significance [  ] muon tracks cascades Flux of high energy cosmic neutrino reported by IceCube will be measured already after 1 year phase-1.5 detector operation! 18 signal and 4 background events expected to be detected

KM3NeT Phase-2 P. Piattelli, ICHEP14 Valencia RXJ1713 ¶ Vela X § years significance [  ] Vela X (binned analysis) ¶ S.R. Kelner, et al., Phys. Rev. D 74 (2006) § F.L. Villante and F. Vissani, Phys. Rev. D 78 (2008) Neutrino astronomy 6 building blocks of 115 detection units each Galactic sources of cosmic rays (?) RXJ

KM3NeT outlook P. Piattelli, ICHEP14 Valencia Proof of feasibility of network of neutrino detectors Largest HE-neutrino telescope in the Northern Hemisphere Neutrino astronomy Phase-1 31 M€ (committed) Phase  170 M€ Phase  60 M€ For additional details on KM3NeT technology see the poster by T. Chiarusi (#16) For the low energy option (ORCA), not trated in this talk, see the poster by J. Hofenstädt (#168) Measure of the IceCube signal from the Northern Hemisphere Indication at 3 sigma level on galactic sources