1. V. Bertin - CPPM - PONT Avignon - April'14 Indirect search for Dark Matter with the ANTARES Neutrino Telescope Vincent Bertin - CPPM-Marseille on behalf of the ANTARES Collaboration Progress on Old and New Themes in cosmology – Avignon – April 2014

2. V. Bertin - CPPM - PONT Avignon - April'14      Relic WIMPs captured in celestial bodies Indirect detection of WIMPs in a neutrino telescope  Potential  sources are Sun, Earth & Galactic Centre Signal less affected by astrophysical uncertainties than  -ray indirect detection  self-annihilations into c,b,t quarks,  leptons or W,Z,H bosons can produce significant high-energy neutrinos flux

3. V. Bertin - CPPM - PONT Avignon - April'14 Neutrino telescope: Detection principle   43° Sea floor p    p,   Reconstruction of  trajectory (~ ) from timing and position of PMT hits interaction Cherenkov light from  3D PMT array

4. V. Bertin - CPPM - PONT Avignon - April'14 14.5 m ~60-75 m Buoy 350 m 100 m Junction Box Main Electro- optic Cable (~40 km) Storey 12 lines 25 storeys / line 3 PMs / storey ~900 PMs Depth : 2500m The ANTARES detector Site Map Submarine links

5. V. Bertin - CPPM - PONT Avignon - April'14 The ANTARES site ANTARES site 2480 m depth

6. V. Bertin - CPPM - PONT Avignon - April'14 Region of Sky Observable by Neutrino Telescopes Mkn 501 Mkn 421 CRAB SS433 Mkn 501 RX J1713.7-39 GX339-4 SS433 CRAB VELA Galactic Centre IceCube (South Pole) (ice: ~0.6°) ANTARES (43° North) (water: ~0.3°) Angular resolution

7. V. Bertin - CPPM - PONT Avignon - April'14 Indirect search towards the Sun with ANTARES Detector building started in 2006, completed in May 2008 Analysis based on data collected between 2007 and 2012  > 7000 upgoing neutrino candidates (in ~1321 effective days) Reconstruction strategies: –BBFit (  2 based)  optimal for low energies/masses (<250 GeV) –Single line events : reconstruction of zenith angle only  very low energies –Multiline events: reconstruction of zenith & azimuth angles –AAFit (likelihood based)  high energies/masses (>250 GeV) –lambda (quality parameter, basically the likelihood value) –beta: angular error estimation Selection parameters: –tchi2: ~  2 (BBFit) –lambda: Quality reconstruction parameter ~ likelihood (AAFit) –beta: angular error estimate (AAFit) –Cone opening angle around the Sun (or zenith band for single line events)

8. Event selection : background rejection V. Bertin - CPPM - PONT Avignon - April'14  Selection of neutrinos and rejection of atmospheric muons by selecting up-going tracks and cutting on track fit quality  Rejection of atmospheric neutrinos by looking into a cone towards the Sun direction (or zenith band for single line events)  Remaining background estimated from scrambled data Track fit quality parameter Elevation angle MC atm.  MC atm.

9. Neutrino signal from WIMP annihilations V. Bertin - CPPM - PONT Avignon - April'14 WIMPSIM package (Blennow, Edsjö, Ohlsson, 03/2008) used to generate events in the Sun in a model independent way Annihilations into b quarks (soft spectrum) and   leptons, WW/ZZ bosons (hard spectrum) used as benchmarks Take into account interactions in the Sun medium, regeneration of  in the Sun and oscillations WIMPSIM package (Blennow, Edsjö, Ohlsson, 03/2008) used to generate events in the Sun in a model independent way Annihilations into b quarks (soft spectrum) and   leptons, WW/ZZ bosons (hard spectrum) used as benchmarks Take into account interactions in the Sun medium, regeneration of  in the Sun and oscillations

10. Selection optimization and observed events V. Bertin - CPPM - PONT Avignon - April'14 Neutrino fluxes at the Earth produced by Dark Matter coannihilation are convoluated with the detector efficiency for given selection parameter sets (track fit quality, cone size) Neutrino background given by scrambled data in the Sun direction is evaluated for the same selection set Optimization of sensitivity performed by minimizing Observed events in the Sun direction vs. scrambled data in 2007-2012 Optimal half-opening angle of the search cone around the Sun No observed excess

11. Limit on neutrino flux coming from the Sun V. Bertin - CPPM - PONT Avignon - April'14 Limits on neutrino flux assuming 100% Branching Ratio of WIMP annihilations into benchmark channel Effective area of signal as function of WIMP mass  low threshold at M WIMP ~ 50 GeV

12. Limits on Spin Dependent cross sections V. Bertin - CPPM - PONT Avignon - April'14 Conversion to limits on WIMP-proton Spin Dependent cross sections assuming equilibrium between capture and annihilation rates inside the Sun  much better sensitivity of neutrino telescopes on SD cross-section w.r.t. direct detection due to capture on Hydrogene inside the Sun Comparison to predictions of CMSSM and MSSM-7 models taking into account recent experimental constraints (Higgs mass,…) PRELIMINARY First limits with ANTARES 2007-2008 data published in JCAP11 (2013) 032

13. Search for Dark Matter towards the Galactic Centre V. Bertin - CPPM - PONT Avignon - April'14 WIMPs self-annihilate according to (halo model-dependent) Galactic Centre e, μ, τ Earth oscillations in the vacuum Sun position R sc ρ sc WIMPs can propagate with a minimum of astrophysical uncertainties where

14. Search for Dark Matter towards the Galactic Centre V. Bertin - CPPM - PONT Avignon - April'14 Spectra from Dark Matter annihilations in vacuum including EW corrections for 5 main benchmark channels from M. Cirelli et al., JCAP 1103 (2011) 051 (www.marcocirelli.net/PPPC4DMID.html) ANTARES visibility of the Galactic Centre M WIMP = 1 TeV Effective area for Aafit analysis

15. ANTARES observation of the Galactic Centre with 2007-2012 data V. Bertin - CPPM - PONT Avignon - April'14 BBFit-single line, tchi2<1 AAFit, lambda>-5.6 No observed excess Optimum cone opening angles

16. Limits on neutrino flux from Galactic Centre V. Bertin - CPPM - PONT Avignon - April'14 b bbar W+ W-    bar dash-dotted: BBFit-1L dasded: BBFit-ML solid: AAFit-ML PRELIMINARY

17. Limits on from Galactic Centre V. Bertin - CPPM - PONT Avignon - April'14 PRELIMINARY J factor for DM profiles computed using CLUMPY version 2011.09_corr2 A. Chardonnier et al., Comp. Phys. Comm. 183, 656 (2012 ) (http://lpsc.in2p3.fr/clumpy) Diff. J-factor NFW profile Integ. J-factor NFW profile NFW profile: Navarro, Frenk, White ApJ 490 (1997) 493.

18. Comparison to other experiments V. Bertin - CPPM - PONT Avignon - April'14 IC79 2010- 2011 ANTARES NFW Einasto steep NFW* IC40 - GC IC59-dSphs IC59-Virgo IC79-Halo IC22-Halo PAMELA + FERMI + HESS Fermi-dSphs natural scale PRELIMINARY DM DM      *(α,β,γ) = (1,3,1.3) and ρ S = 0.3 GeV.cm -3, and R S = 21.7 kpc.

19. Search for DM towards Dwarf Galaxies: sensitivity V. Bertin - CPPM - PONT Avignon - April'14 PRELIMINARY Stacking analysis of visible Dwarfs in progress…

20. Indirect Search for Dark Matter in the Earth V. Bertin - CPPM - PONT Avignon - April'14 Capture rate of WIMPs in the Earth dominated by SI cross-section Resonnant enhancement on dominant nuclei (Fe, Ni, Si,…) Angular distribution of neutrinos Energy distribution of neutrinos M WIMP = 100 GeV from M. Blennow, J. Edsjo and T. Ohlsson, arXiv:0709.389

21. Sensitivity to DM annihilations in the Earth V. Bertin - CPPM - PONT Avignon - April'14 PRELIMINARY Dark Matter density usually not at equilibirum due to low capture rates by the Earth Assume annihilation rate = 3 10 -26 cm 3 s -1

22. Summary and Outlook Indirect search for Dark Matter is a major goal for neutrino telescopes (important complementarity to direct detection experiments) Indirect search towards the Sun performed by ANTARES with data recorded in 2007-2012  competitve limits derived especially for low DM masses First ANTARES limits towards the Galactic Centre  best current limits using neutrinos  important complementary constraints on leptophilic Dark Matter models Study of other potential signal sources (Earth, dwarf galaxies, galaxy clusters…) are in progress V. Bertin - CPPM - PONT Avignon - April'14 Stay tuned for the BIG DARK DISCOVERY !!

23. V. Bertin - CPPM - PONT Avignon - April'14 Expected performance (MC Studies) Angular resolution better than 0.3° above a few TeV, limited by:  Light scattering + chromatic dispersion in sea water:  ~ 1.0 ns  TTS in photomultipliers:  ~ 1.3 ns  Electronics + time calibration:  < 0.5 ns  OM position reconstruction:  < 10 cm (↔  < 0.5 ns) Effective area for [m 2 ] increases with energy Earth shadowing above 100 TeV dominated by reconstruction   rec −  true  rec − dominated by kinematics

24. Background in the Sun direction V. Bertin - CPPM - PONT Avignon - April'14 Background estimated from data scrambled in time and  Using the Sun visibility at the ANTARES location Background due to neutrinos coming from CR interactions in the Sun corona negligeable (<1% of atmospheric neutrinos) All up-going events from 2007-2008 data Example of Sun tracking in horizontal coordinates

25. Current improvements of analysis sensitivity V. Bertin - CPPM - PONT Avignon - April'14 Include more statistics : > 7000 neutrinos collected in 2007-2012 data Use energy estimator for better selection of DM neutrinos with respect to atmospheric neutrino background Use alternative reconstruction algorithms with better performances for low energy events Include single line events : integrate on azimuth band for zenith direction of the Sun B Bbar spectrum 2007-2010 data WIMP Mass  major improvement of sensitivity for low energy events (M WIMP < 120 GeV)

26. Limits on SD and SI cross sections V. Bertin - CPPM - PONT Avignon - April'14 Conversion to limits on WIMP-proton SD/SI cross sections assuming equilibrium between capture and annihilation rates inside the Sun  much better sensitivity of neutrino telescopes on SD cross-section w.r.t. direct detection due to capture on Hydrogene inside the Sun Comparison to predictions of CMSSM models taking into account recent exp. constraints (Higgs mass,…)  Competitive limits obtained with ANTARES 2007-2008 arXiv:1302.6516

27. Limits on SD and SI cross-sections V. Bertin - CPPM - PONT Avignon - April'14 Comparison to predictions of MSSM-7 phenomenological models taking into account recent experimental constraints (Higgs mass,…)  Much weaker correlations of SD and SI cross sections than for CMSSM  Complementarity of constraints between direct and indirect detection arXiv:1302.6516