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The ANTARES detector status and results

The ANTARES detector status and results. A.Margiotta Dipartimento di Fisica and INFN Bologna on behalf of the ANTARES Coll. TeV  rays ( p+X   0  ) at the centre of our galaxy from supernova remnant RX J1713.7-39 . expected : p+X    .

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The ANTARES detector status and results

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  1. The ANTARES detector status and results A.Margiotta DipartimentodiFisica and INFN Bologna on behalf of the ANTARES Coll.

  2. TeV  rays (p+X 0) at the centre of our galaxy from supernova remnant RX J1713.7-39. expected: p+X   ANTARES the largestNorthern neutrino telescope HESS • Neutrino astronomy: • origin and acceleration of cosmic rays • dark matter • exotics • Cosmic sources of neutrinos • extragalactic: Active Galactic Nuclei, GRBs • galactic: micro quasars, supernova remnants … • diffuse flux of neutrinos • A. Kouchner’s talk thisafternoon ECRS10, Turku - Finland

  3. CRAB CRAB VELA SS433 SS433 Mkn 421 Mkn 501 Mkn 501 RX J1713.7-39 GX339-4 Galactic Centre sky view (galactic coordinates) AMANDA / IceCube (South Pole) ANTARES (43o N) acceptance visible sky 0.5sristantaneouscommonview 1.5srcommonviewover a day ECRS10, Turku - Finland

  4. Detection principle HE  from  CC-interaction Energy threshold ~ 10 GeV Array of PMTs Cherenkov photons (42° in water) neutrino muon µ µ W Reconstruction of mtrajectory(~ n)from timing and position of PMT hits N neutrino X ECRS10, Turku - Finland

  5. The ANTARES site Toulon La Seyne-sur-Mer control room Electro-optical Cable of 40 km 2500 m under s.l.

  6. 7 COUNTRIES 28 INSTITUTES ~ 150 SCIENTISTS AND ENGINEERS The ANTARES Collaboration • University of Erlangen • Bamberg Observatory • University/INFN of Bari • University/INFN of Bologna • University/INFN of Catania • LNS – Catania • University/INFN of Pisa • University/INFN of Rome • University/INFN of Genova • NIKHEF (Amsterdam) • KVI (Groningen) • NIOZ Texel • ITEP, Moscow • Moscow State Univ • CPPM, Marseille • DSM/IRFU/CEA, Saclay • APC, Paris • LPC, Clermont-Ferrand • IPHC (IReS), Strasbourg • Univ. de H.-A., Mulhouse • IFREMER, Toulon/Brest • C.O.M. Marseille • LAM, Marseille • GeoAzur Villefranche IFIC, Valencia UPV, Valencia UPC, Barcelona ISS, Bucarest 6 ECRS10, Turku - Finland

  7. 2006–2008: deployments of the detector lines ECRS10, Turku - Finland Line1, 2: 2006 Line3, 4, 5:January 2007 Line6, 7, 8, 9, 10:December 2007 Line 11, 12:May 2008

  8. 14.5 m ~60 m The telescopesetup • 12 lines of 75 PMTs • 1 line for Earth and Marine sciences (IL07) • 25 storeys / line • 3 PMTs / storey • 885 PMTs Storey 350 m 40 km to shore Junction Box Submarine links ECRS10, Turku - Finland

  9. titanium frame: support structure (2m) Optical Beaconwith blue LEDs: timing calibration Optical Module:10” Hamamatsu PMT in 17” glass sphere (sTTS 1.3 ns) photon detection Hydrophone: acoustic positioning Local Control Module(in Ti cylinder): Front-end ASIC, DAQ/SC, DWDM, Clock, tilt/compass, power distribution… The storey ECRS10, Turku - Finland

  10. Background Optical Background: bioluminescence (bacteria) and 40K decay (sea environment) ~70 kHz + bursts from macro-organisms few MHz, strongly affected by sea currents Physics Background : cosmic rays (atmospheric mand n). dense-water formation (coldwinter) and localseacurrentinstabilitiescausedsinkingoflargeamountsofbioluminescent material (crustacea, zooplankton….) In press in Ocean Science MILOM & L1 MILOMOnly 10 Lines & IL07 5 Lines Full ANTARES L1 & L2 • MILOM • L1F1 • L1F25 • IL07 Cable Fault ECRS10, Turku - Finland

  11. Position calibration • 1emitter/receiver at the bottomofeachline • 5receiversalongeachline • 4autonomoustranspondersaround the apparatus • Sound velocimetersinstalled at variousdepths • Tiltmeter and compass at eachstorey • Measurementsperformedevery2minutes Position of hydrophone relative to line base location 20 days Reconstructionoflineshape resolutionbetterthan 10 cm ECRS10, Turku - Finland

  12. Timecalibrations Time difference between the LED OB and an OM 3 OMs • Electronics + calibration ~ 0.5 ns • - TTS in photomultipliers ~ 1.3 ns • Light scattering + dispersion in sea water  ~ 1.5 ns at 40 m  = 0.4 ns Angular resolution  0.3o (for E > 10 TeV ) Optical LED beacon ECRS10, Turku - Finland

  13. SELECTED RESULTS Atmosphericmuonflux Atmosphericneutrinos Point sources Diffuse nmflux ECRS10, Turku - Finland

  14. Atmosphericmuons Zenith distribution and flux of atmospheric m measured with the 5-line ANTARES detector , arXiv:1007.1777v1, in press in APP (DoI: 10.1016/j.astropartphys.2010.07.001) • Fordetails on: • NSU model : E. V. Bugaevet al., Phys. Rev. D58 (1998) 05401. • Polygonatomodel: J. Horandel, Astropart. Phys. 19 (2003) 193. • MUPAGE : G. Carminatiet al., Comput. Phys. Commun. 179 (2008) 915. 5-line detector • Mainsourcesofsystematicuncertainties: • environmentalparameters (absorption and scatteringlength) • detector parameters (OM efficiency) • Shadowed band: systematic uncertainty w.r.t. the black line (± 40 %) . • physics: • hadronicinteractionmodels • modelsofcosmicraycomposition • within systematic uncertainties data are reproduced by MC  good understanding of the detector and its environment • work in progress to reduce uncertainties blackpoints : data 5-line detector (2007) : MUPAGE Monte Carlo [Com. Phys. Comm. 179(2009)915] : CORSIKA + QGSJET + NSU param for primary CRs : CORSIKA + QGSJET + “poly-gonato” param for primary CRs : CORSIKA + SIBYLL + NSU param for primary CRs. ECRS10, Turku - Finland

  15. 2 km 4km MuonDepth-Intensity relation MUPAGE parameterization Parameterizationfrom E. V. Bugaevet al., PRD58 (1998) 05401 ECRS10, Turku - Finland

  16. Atmosphericneutrinos Scrambled ANTARES sky map May 2007 - December 2008 341 days detector live time Upgoing: 1062 neutrino candidates: 3.1 ν/day Monte Carlo: atmospheric neutrinos: 916 (30% syst. error) bad reco atmospheric m: 40 (50% syst.error) ECRS10, Turku - Finland

  17. Point sources–5lines searchforclustersofneutrinos 25 potential sources (stringent cuts to reduce background) analysis optimization based on simulations 5-line data unblinding 140 days of detector livetime no excess found 12 lines analysis in progress ECRS10, Turku - Finland

  18. Diffuse fluxanalysis • Selection of high energy neutrino events  Background rejection • High energy events high probability to have more than 1 hit on each PMT. • direct photons + mscattered photons + light from EM showers • Ri= numberofhits on i-th PMT • R = ΣRi/ number of all PMTs contributing to the event R> 1.31 • analysisoptimizedusing MC todefine the best R cut : • Model Rejection Factor technique [APP 19 (2003)393] Atmosphericmuons : qualitycuts on trackreconstruction Atmosphericneutrinos : low energyeventsremovedusinganenergyestimator ECRS10, Turku - Finland

  19. Diffuse fluxanalysis R< 1.31 Bartol(conventional n) 104.9 Max “prompt” model 2.1 Data 120 R1.31 Atmospheric n 10.5 2 Data 9 E2F(E)90%= 4.8×10-8 GeV cm-2 s-1 sr-1 20 TeV<E<2.5 PeV ECRS10, Turku - Finland

  20. Earth and Sea Science with the InstrumentationLine • Bioluminescence • EnvironmentalMonitoring • Seismology • Oceanography(Med Sea Circulation) The deepestInfra-red camera in the sea Next future: deploymentof a secondary JB forScientific and technologicalapplications IFREMER/CNRS ECRS10, Turku - Finland Seismo Meter

  21. AMADEUS 0o -60o 90o -90o 120o R&Dactivityforacoustic neutrino detection System ofhydrophones on the IL07 and line 12 Studyofenvironmental background Direction recostruction ECRS10, Turku - Finland

  22. Ongoingcombinedsearches • Receive GRB alertsfromsatellites(Fermi, Swift...) • searchforcoincidentneutrinoswithintimewindow (~100 seconds) • Send neutrino cluster alertforoptical follow-up • Trigger: multiple / HE single neutrino event; Reconstruction “on-line” (<10ms) • AlertmessagetoTarotTelescope in La Silla (Chile) • Tarottakes6imagesof3minutesimmediately and after1, 3, 9 and 27 dayssendingalertsto the ROTSE system (4telescopes) since3months • Correlationwith AUGER source distribution investigate directionalcorrelationofneutrinos and UHE particles • Correlationwith VIRGO-LIGO signals investigate correlationofneutrinos and gravitationalwaves ECRS10, Turku - Finland

  23. Conclusions • ANTARES detector completed in May 2008 • detector operation and calibration under control • maintenance capability demonstrated • Exciting physics program ahead • over two thousand neutrinos already reconstructed • astronomical sources, multi-messenger approach, other analyses in progress • Real-time readout and in-situ power capabilities facilitates • a large program of synergetic multi-disciplinary activities: biology, oceanography…… • A multidisciplinary deep-sea research infrastructure • A major step towards the KM3NeT (E. de Wolf’s talk – tomorrow afternoon - 3P_PA2) ECRS10, Turku - Finland

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