Bertin, V.

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Antares: A Deep-Sea 0.1 km2 Neutrino TelescopeV. BertinTo cite this version:V. Bertin. Antares: A Deep-Sea 0.1 km2 Neutrino Telescope. Moriond Workshop Very HighEnergy Phenomena in the Universe 21, Jan 2001, Les Arcs, France. pp.1-13, 2001. <in2p3-00012819>HAL Id: in2p3-00012819http://hal.in2p3.fr/in2p3-00012819Submitted on 27 May 2003HAL is a multi-disciplinary open accessarchive for the deposit and dissemination of sci-entific research documents, whether they are pub-lished or not. The documents may come fromteaching and research institutions in France orabroad, or from public or private research centers.L’archive ouverte pluridisciplinaire HAL, estdestine´e au de´poˆt et a` la diffusion de documentsscientifiques de niveau recherche, publie´s ou non,e´manant des e´tablissements d’enseignement et derecherche franc¸ais ou e´trangers, des laboratoirespublics ou prive´s.V.Bertin CPPM / ANTARES Coll. -Moriond 20011ANTARES :A deep-sea 0.1 km² neutrino telescopeVincent Bertin - CPPM-Marseilleon behalf of the Antares CollaborationVery High Energy Phenomena in the Universe - Rencontres de Moriond  - January 2001V.Bertin CPPM / ANTARES Coll. -Moriond 20012The ANTARES Collaboration? University of Oxford? University of Sheffield? ITEP, Moscow? CPPM, Marseille (IN2P3)? DSM/DAPNIA, Saclay (CEA)? IReS, Strasbourg? Univ. of H.-A., Mulhouse? C.O.M. Marseille? IFREMER, Marseille/Brest? IGRAP (INSU), Provence? University of Bari ? University of Bologna ? University of Catania ? LNS  – Catania? University of Rome ? University of Genova ? IFIC, Valencia? NIKHEF, Amsterdam V.Bertin CPPM / ANTARES Coll. -Moriond 20013neutrinomuonCherenkovlight coneANTARESDetectorinteractionLattice of Photomultipliers : “Optical Modules”Muon track direction from  arrival time of lightNeutrino direction: ∆ (θν −θµ ) ≈ 0.7o / E0.6(TeV)Muon energy from energy loss and rangeDetection PrincipleA 1km3 detector should record 200 to 2000 high energy cosmic neutrinosper year (Eν > 10-100 TeV).V.Bertin CPPM / ANTARES Coll. -Moriond 20014Phase I : Water properties measurements? Perform precise measurements of crucial environmental parameters :? In situ measurements on Antares site(2400 m depth off French Mediterranean coast)? Long term measurements of opticalbackground (40K decays, bioluminescence)and biofouling of Optical Modules? Measurement of water transparency @ 466 nm :λabs ~ 55-65 m ;λscat > 100 mat large anglesAverage ~ 40 kHz on a 8” PMT ~ 60 kHz on a 10” PMTV.Bertin CPPM / ANTARES Coll. -Moriond 20015ANTARES Phase I : Demonstrator? First line of 350m high equipped with 16 pairs of Optical Modules? Summer 98 : successful deployment test at 2300m depth performed with Dynamical Positioning ship? December 99-June 00 : demonstrator equipped with 7 PMTs + acoustic positioning system linked to shore station by electro-optical cable? December 98 : successful undersea electrical connection test of detector anchor performed at 2400m depth by IFREMER submarine vehicle NautileV.Bertin CPPM / ANTARES Coll. -Moriond 200160 10 20 30 40 50 60 70 80 90133.8133.85133.9133.95134134.05134.1temps (min)YD3 (m)mesures       inte rpola tionTime (min)5cmAcoustic positioning system~ 1 cmInter-transponder≤ 3 cmRang.-Transpond.~ 1 cm         Inter-rangemeterAccuracy (σ)DevicesTriangulation allows  ≤ 5 cm accuracy4 transponders 3 rangemetersY coord. Range 3 (m)V.Bertin CPPM / ANTARES Coll. -Moriond 20017Reconstruction of Atmospheric Muons  ct (m)          z (m)           z ( m)           ct (m)          Fit with hyperbola(noise K40)Point measured? More than 5× 104 coincidences  in all 7 PMTs have been recorded.? Polar angle of down-going muons deduced from depth vs. time pattern.? Hyperbolic fit (including multimuons).? 40K filtered out by the reconstruction software (see boxed hit in example).V.Bertin CPPM / ANTARES Coll. -Moriond 20018Reconstruction of Atmospheric MuonsOver 50k 7-fold coincidences recordedmore than 1350 reconstructed events per dayAngular DistributionDataSimulationTrack angle  (o)Preliminary comparisonwith simulation ofsingle and multiple muons ∆(fit-point) in nsResidual (ns)     V.Bertin CPPM / ANTARES Coll. -Moriond 20019ANTARES Phase II : 0.1 km² Detector2500m300mactiveElectro-opticsubmarine cable~ 40kmJunction boxReadout cablesShore stationanchorfloatElectronics containers~60mAcoustic beacon~100m10 strings : 900 PMTs in totalDetector to be deployed at ANTARES site by 2002 - 2004Local electronicOptical ModuletripletHydrophoneTime calibrationLED BeaconTo be deployed in Spring 2001V.Bertin CPPM / ANTARES Coll. -Moriond 2001100.1 km² Detector : Expected performanceAngular resolution Energy resolution? Including effects of reconstruction and selection, PMT TTS, positioning, timing calibration accuracy and scattering.? Below ~10 TeV angular error is dominated by ν-µ physical angle.? Above ~10 TeV angular accuracy is better than 0.4° (reconstruction error).?σE /E ≈ 3 (E  >1 TeV)? Below E ~ 100 GeV energy estimation via muon range measurement.V.Bertin CPPM / ANTARES Coll. -Moriond 200111ANTARES 0.1 km² Detector Site? 40 km SE of Toulon, Southern France  (42º 50’ N,   6º 10’ E)? Shore base at La Seyne-sur-Mer (excellent infrastructure) ? 2400 m below sea level? 3.5π sr of the sky is covered     ? 0.5π sr overlap with Amanda? Galactic Centre surveyedV.Bertin CPPM / ANTARES Coll. -Moriond 200112Scientific Programme? Search for neutralinos via their self-annihilation to products containing neutrinos at the centre of the Earth, Sun and Galaxy? Neutrino oscillations via the modification in the energy spectrum due to observation of the first oscillation minimumLow energy             Medium Energy High energy? Observation of neutrinos from (extra-)galactic sourcessuch as GRB, AGN, Supernovae remnants, molecular clouds, etc.χχχχχχχχχχχχχχχχχχχχχχχV.Bertin CPPM / ANTARES Coll. -Moriond 200113ConclusionsANTARES has made excellent progress over the past 4 years :? Site environmental characterisation OK? Tests of marine technologies under control? Deployment and operation of Demonstrator String? First down-going muons reconstructed? Expanding CollaborationANTARES is well engaged in Phase II of its programmeby the design, the installation and the running of a 10-strings 0.1 km² detector in 2002-2004Major step forward towards a km-scaleneutrino telescope in the Mediterranean Sea

Antares: A Deep-Sea 0.1 km2 Neutrino Telescope

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