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The High Energy Neutrino Sky as seen by Antares

The High Energy Neutrino Sky as seen by Antares. Dorothea Samtleben NIKHEF, Amsterdam. Astrophysics Neutrinos are valuable cosmic messengers coming undeflected from cosmic sources Multimessenger approach exploited together with

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The High Energy Neutrino Sky as seen by Antares

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  1. The High Energy Neutrino Sky as seen by Antares Dorothea Samtleben NIKHEF, Amsterdam

  2. Astrophysics Neutrinos arevaluablecosmicmessengers comingundeflectedfromcosmicsources Multimessenger approachexploitedtogetherwith withdetectorsforelectromagneticradiationandgravitationalwaves Extraterrestrial Neutrinos Cosmic Neutrino Background ParticlePhysics Dark Matter WIMPs accumulate in massive objects (Sun, Earth) => possiblyannihilationsignals observable, Atmosphereactsas ‘beam dump‘ for cosmicrays => Studies for - Prompt production (highenergies) - Neutrino oscillations (lowenergies) Halzen, F. & Klein,S.R. Review of Scientific Instruments 81, 081101, 2010

  3. Artist‘sview Artist‘sview Neutrino sources SN1006 Optical, radio, X-rays Gamma Ray Bursts Supernova remnants Microquasars Highlyenergeticparticleaccelerationneededtoexplainobservedcosmicrayenergyspectrum - g from inverse Compton scattering - gfromsynchrotronradiationofelectrons - gfrompiondecay Neutrino fluxescanbederivedfromgemissionbyassumingpiondecayasoriginofg gg

  4. 2p downward sensitivity assumed Mediterranean Field of View > 25% > 75%

  5. ANTARES Collaboration NIKHEF, Amsterdam Utrecht KVI Groningen NIOZ Texel • University of Erlangen • Bamberg Observatory ITEP,Moscow MoscowStateUniv ISS, Bucarest IFIC, Valencia UPV, Valencia UPC, Barcelona 7 countries 31 institutes ~150 scientists+engineers CPPM, Marseille DSM/IRFU/CEA, Saclay APC, Paris LPC, Clermont-Ferrand IPHC, Strasbourg Univ. de H.-A., Mulhouse IFREMER, Toulon/Brest C.O.M. Marseille LAM, Marseille GeoAzurVillefranche INSU-DivisionTechnique 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

  6. 3D PMTarray Cherenkov light from m 42° Sea floor m nm interaction p, a nm p m nm nm Cosmicraysinteractwithatmosphere => Showers, muons, neutrinos Neutrinos arrivefromastrophysicalsources Neutrino interaction in Earth => Muonpassesdetector

  7. 12 lines mounted on the sea floor (2475m deep) • 25 storeys / line • 3 Photomultipliers / storey ANTARES detector PMT PMT 40 km to shore

  8. Track reconstruction ~105atmosphericmuons per day ~5 atmosphericneutrinos per day Quality importanttoeliminatemisreconstructedmuontracks Track resolution 0.43 0.10 deg in PS analysis

  9. 2007/8 analysispublished (ApJ743 L14 2011) Update 2007-2010 data (813 days): 3048 neutrinocandidates Neutrino skyseenby Antares(galacticcoordinates) Most significantcluster, 9 eventswithin 3 degrees (2.2s) Selected potential neutrinosources in red

  10. Fluxlimit Study for 51 potential neutrinosources: Nosignificantexcess => upperlimits Best limitsford<-30 5s 90% discovery potential in comparisontoIceCube 40 forvarious different declinations => Sensitivityto different energyranges

  11. Diffuse neutrinoflux Distribution of R in data in comparisonto MC expectations Simulation ofenergyestimator R Data 2007-2009, corresponding to 335 active days Distinctionof diffuse fluxfromatmosphericneutrinosbyenergy (harderspectrumexpectedfromsources) Energyestimator R based on hitmultiplicity on Photomultipliers Prompt neutrinos (RPQM) E-2 flux at limit

  12. Diffuse neutrinoflux E2F(E)90%= 5.3 10-8GeV cm-2 s-1 sr-1 20 TeV<E<2.5 PeV 90% upper limit assuming E-2 flux spectrum

  13. c rc <sv> Searchfor Dark Matter n m Dark Matter WIMPs accumulate in heavy objects (Sun) Capture/Annihilation in equilibrium at the Sun core Annihilation e.g. in bb/tt/WW -> n+.. Model-independent event simulation using WIMPSIM Interactions in the Sun and flavor oscillation, regeneration of t in the Sun taken into account Background estimate from scrambled data Distancetosun

  14. Spin-independent cross-section limit for ANTARES 2007-2008 in CMSSM Dark Matter limitsfromthesun For CMSSM: Branchingratios = 1 (for WW, bb, ττ) (Large variationof branchingratiosover parameterspace) Compare SUSY predictions to observables as sparticles masses, collider observables, darkmatterrelicdensity, direct detection cross-sections, … SuperBayes(arXiv:1101.3296)

  15. Spin-dependentcross-section limit for ANTARES 2007-2008 in CMSSM Dark Matter limitsfromthesun For CMSSM: Branchingratios = 1 (for WW, bb, ττ) (Large variationof branchingratiosover parameterspace) Compare SUSY predictions to observables as sparticles masses, collider observables, darkmatterrelicdensity, direct detection cross-sections, … SuperBayes(arXiv:1101.3296)

  16. Spin-dependent cross-section limit for ANTARES 2007-2008 in mUED Dark Matter limitsfromthesun Extra dimension: Dark Matter as Kaluza Klein particles FormUED TheoreticalBranchingratiostakenintoaccount (no large variationoverphasespace) Compare mUEDpredictions to observables as KK masses, collider observables, relicdensity, direct detection cross-sections, … SuperBayesmodified version (Physical Review D 83, 036008 (2011))

  17. Monopole withmasses <1014GeVcanbeacceleratedtorelativisticspeedsanddespiteenergyloss in Earth still leavevisiblesignatures in neutrinotelescopes Light from Cerenkov radiationandbelow Cerenkov threshold via delectrons Significantlymorelightyieldthanfrommuons Limits for 0.625<b<0.995 Magnetic Monopole Search Upper Limits on theFlux Photon yield Cerenkov From MM • from • electrons • for MM Cerenkov fromm

  18. Neutrino oscillation Simulation of reconstructedneutrinos Single Line • Low energyatmosphericneutrinosimportant • Baseline L fromzenith angle q • Energyestimatefromtracklength • Different trackreconstructionusing multi-lineandsingle-lineevents (onlyzenithreconstructed) Multi Line Dashed: withoscillation

  19. Data Best Fit No oscillations For maximal mixing m2=(3.1±0.9) 10-3 eV2 Antares, K2K, Minos, SuperK Measurement contours 1,2,3 

  20. First Funding already available to allow start of construction 2012 Finalizing Design 2013-15 Building/Deployment of first batch of detectors 2015`++ Completion of Detector Objective: Deep Sea Research Infrastructure in the Mediterranean Sea hosting a multi cubic kilometer neutrino telescope Locations of the three pilot projects: ANTARES: Toulon NEMO: Capo Passero NESTOR: Pylos KM3NeT

  21. TDR ,180 m distances • optimized for E-2 source • spectrum • Average 180 m distances • IceCube • Average 130 m distances • Irregular pattern • Energy threshold lower • More optimised for Galactic sources Configuration New detectorconcept: Spherewith 31 PMTs 2400m 860m 1750m Track resolution 0.1deg @ TeV 5sdiscovery in 5 yearsofgalacticsourcesfeasible

  22. Technology ofunderwaterneutrinotelescope in seawatersuccessfullyprovenwithexcellent angular resolution Varietyofphysicsanalysesunderway, firstresultspublished Large severalcubickilometerarray Km3NeT planned in theMediterraneanSea, productionofdetectorsissoongettingstarted => NEW WINDOW TO THE UNIVERSE AVAILABLE

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