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Juande Zornoza (IFIC, Valencia) on behalf of the ANTARES collaboration

Search for Dark Matter in the Sun with the ANTARES Neutrino Telescope in the CMSSM and mUED frameworks. Juande Zornoza (IFIC, Valencia) on behalf of the ANTARES collaboration. Origin of cosmic rays Hadronic vs. leptonic signatures Nature of dark matter. Detector size.

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Juande Zornoza (IFIC, Valencia) on behalf of the ANTARES collaboration

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  1. SearchforDarkMatter in theSunwiththe ANTARES Neutrino Telescope in the CMSSM and mUEDframeworks JuandeZornoza (IFIC, Valencia) onbehalf of the ANTARES collaboration

  2. Origin of cosmic rays • Hadronic vs. leptonicsignatures • Nature of dark matter Detector size Supernovae Limitation at high energies: Fast decreasing fluxes E-2, E-3 Oscillations Limitation at low energies: -Short muon range -Low light yield -40K (in water) Dark matter (neutralinos, KK) Astrophysical neutrinos Scientificscope GZK MeV GeV TeV PeV EeV Detector density

  3. WIMPs (neutralinos, KK particles) are among the most popular explanations for dark matter • They would accumulate in massive objects like the Sun, the Galactic Center, dwarf galaxies… • The products of such annihilations would yield “high energy” neutrinos, which can be detected by neutrino telescopes • In the Sun a signal would be very clean (compared with gammas from the GC, for instance) • Sun travel in the Galaxy makes it less sensitive to non-uniformities Detection of DM byNTs  

  4. nm m W N X   1.2 TeVmuon traversing ANTARES • The neutrino is detected by the Cherenkov light emitted by the muon produced in the CC interaction. Detection principle of optical Cherenkov detectors

  5. ANTARES wascompleted in 2008 • During 2007, 5 lineswerealreadyoperative • Thisanalysisuses data of 2007 (5 lines) and 2008 (9-10-12 lines) • About 1000 up-going neutrino candidates in theselectedsample • Binnedsearch Data

  6. Data vs MC: elevation

  7. Data vs MC: fit quality

  8. Background estimatedfrom data (2007-2008 period, ~295 days) • Fastalgorithm for muon track reconstruction (Astro. Phys. 34 (2011) 652-662) • Using the Sun visibilityat the ANTARES location • Background from CR interactions in the Sun corona muchlower (few percent of total) All upward-goingeventsfrom 2007-2008 data Example of Sun tracking in horizontal coordinates Background

  9. The WIMPSIM package (Blennow, Edsjö, Ohlsson, 03/2008) is used to generate events in the Sun in a model-independent way • Great statistics: with 3×106 WIMPs annihilations • Capture rate and annihilations in equilibrium at the Sun core • Annihilations in c,b and t quarks, leptons and direct channels • Interactions taken into account in the Sun medium • Three flavors oscillations, regeneration of leptons in the Sun medium (Bahcall et al.) • Available parameters: WIMPs mass, oscillations parameters... Signal: WimpSim Earth

  10. MWIMP = 350 GeV Main annihilation channels

  11. Neutrino flux at the earth, from the Dark Matter coannihilation, are convoluated with the efficiency of the detector for a cuts parameter space (track fit quality cut Q,cone) • Neutrino background from the scrambled data in the Sun direction is evaluated in the same space • Minimize this quantity: Average upper limit (Feldman-Cousins) Acceptance to be estimated for different sets (tchi2,cone) Signal and cut optimization

  12. Neutrino flux sensitivity Neutrino flux sensitivity for 2007-2008 data Preliminary For CMSSM: Branching ratios = 1 (WW, bb, ττ) For mUED: Theoreticalbranching ratios takenintoaccount Reason: High dependence of branching ratios over CMSSM parameterspace

  13. Muon flux sensitivity Muon flux sensitivity for ANTARES 2007-2008 Preliminary Flux Φμ Annihilation rate Γ Capture rate C Cross-section σSD

  14. CMSSM cross-sectionsensitivity Spin-dependent cross-section flux sensitivity for ANTARES 2007-2008 Preliminary χ2 Compare SUSY predictions to observables as sparticles masses, collider observables, darkmatterrelicdensity, direct detection cross-sections, … SuperBayes (arXiv:1101.3296) G. Lambard

  15. mUEDcross-sectionsensitivity Spin-dependent cross-section flux sensitivity for ANTARES 2007-2008 Preliminary Compare mUEDpredictions to observables as KK masses, collider observables, relicdensity, direct detection cross-sections, … SuperBayes modified version (Physical Review D 83, 036008 (2011)) 1σ 2σ G. Lambard

  16. Dark matter is a major goal for neutrino telescopes (and an important complement to direct detection experiments) • Computed the detector efficiency for two common dark matter models (CMSSM, mUED) • First analysis done by looking at Sun; other sources (GC, dwarf galaxies…) to be done • Sensitivities for the CMSSM and mUED, in muon flux and SD cross-section calculated: almost ready for unblinding 2007-2008 data • Analysis on 2007-2010 data in progress… Summary

  17. Neutrino candidate with 12-line detector

  18. Interactions p-pgive a production of neutrinos through the decayproducts De C. Hettlage et al., Astropart.Phys. 13 (2000) 45-50 Simple parameterization averaged on the oscillations νμ Background in the Sun direction IICR and Solaratmosphere It doesn’trepresent more than 10-3 events per yearin a 5 linescofiguration (few events for a km3), 0.4% of the total atmospheric background…

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