1. Dorothea Samtleben Leiden University / NIKHEF, Amsterdam

2. Particle Physics Atmosphere acts as ‘beam dump‘ for cosmic rays => Studies for - Prompt production (high energies) - Neutrino oscillations (low energies) Dark Matter WIMPs accumulate in massive objects (Sun, Earth) => possibly annihilation signals observable, Astrophysics Neutrinos are valuable cosmic messengers coming undeflected from cosmic sources Multimessenger approach exploited together with detectors for electromagnetic radiation and gravitational waves

3. Microquasars Highly energetic particle acceleration needed to explain observed cosmic ray energy spectrum -  from inverse Compton scattering -  from synchrotron radiation of electrons -  from pion decay Neutrino fluxes can be derived from  emission by assuming pion decay as origin of   SN1006 Optical, radio, X-rays Artist‘s view Supernova remnants Gamma Ray Bursts - Atmospheric neutrino flux ~ E -3 - Neutrino flux from cosmic sources ~ E -2

4. > 75% > 25% 2  downward sensitivity assumed

5. 5 CPPM, Marseille DSM/IRFU/CEA, Saclay APC, Paris LPC, Clermont-Ferrand IPHC, Strasbourg Univ. de H.-A., Mulhouse LAM, Marseille COM, Marseille GeoAzur Villefranche INSU-Division Technique Univ./INFN of Bari Univ./INFN of Bologna Univ./INFN of Catania LNS-Catania Univ. Napoli Univ./INFN of Pisa Univ./INFN of Rome Univ./INFN of Genova  IFIC, Valencia  UPV, Valencia  UPC, Barcelona  NIKHEF,  Amsterdam  Leiden  Utrecht  KVI Groningen  NIOZ Texel  ITEP,Moscow  Moscow State Univ  University of Erlangen Bamberg Observatory Univ. of Wurzeburg  ISS, Bucarest 8 countries 34 institutes ~150 scientists+engineers  LPRM, Oujda The ANTARES Collaboration

6.  42° interaction Sea floor Cherenkov light from  3D PMT array   p    p,  Cosmic rays interact with atmosphere => showers, muons, neutrinos Neutrinos arrive from cosmic sources Muon neutrino interaction in Earth => Muon passes detector Also showers reconstructable => sensitive also to e  

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

8. Quality of track fit can be used to decrease misreconstruction => Use likelihood value and angular error estimate ~10 5 atmospheric muons per day ~5 atmospheric neutrinos per day Maximum likelihood fit using hit positions and times (nanosecond resolution)

9. Track resolution degrees In point source analysis

10. Analysis 2007-2010 data (813 days), 4 10 8 events, 3058 neutrino candidates Skymap of p-values in equatorial coordinates Most significant cluster, p-value=0.026 (α, δ) = (−46.5 ◦, −65.0 ◦ ) 5(9) events are within 1(3) degrees s (2.2  ) Ap J 760:53 (2012)

11. Study for 51 potential neutrino sources: No significant excess => upper limits Best limits for  <-30

12. Data 2007-2009, corresponding to 335 active days Distinction of diffuse flux from atmospheric neutrinos by energy (harder spectrum expected from sources) Energy estimator R based on hit multiplicity on Photomultipliers Simulation of energy estimator R Distribution of R in data in comparison to MC expectations E -2 flux at limit Prompt neutrinos (RPQM)

13. E 2  (E) 90% = 5.3 10 -8 GeV cm -2 s -1 sr -1 20 TeV<E<2.5 PeV 90% upper limit assuming E -2 flux spectrum Physics Letters B 696 (2011) 16

14. PRELIMINARY E 2  (E) 90% = 3.2 10 -8 GeV cm -2 s -1 sr -1 45 TeV<E<6.3 PeV 90% upper limit assuming E -2 flux spectrum 2008-2011 data used Two different energy estimators: - dE/dx as evaluated from charge collected in the detector - Combined likelihood for hit/no-hit for all OMs L: length  : efficiency Atmospheric energy spectrum by unfolding measured spectrum New diffuse limit using dE/dx estimator

15. 15 Fermi Bubbles: Excess of ɣ-rays seen in Fermi data in extended distinct regions (each ~ 25000 light-years) Homogenous intensity Sharp edges Flat E -2 spectrum (between 1 and 100 GeV) Background estimated from average of 3 equivalent regions Event selection optimized for best model rejection factor Galactic coordinates Good visibility for ANTARES

16. 16 Data 2008-2011 Fermi Bubbles zone: N obs = 16 Excluding Bubbles zone: = 11 = (9+12+12)/3 No significant excess → set upper limits 50 TeV cutoff 100 TeV cutoff 500 TeV cutoff No cutoff Solid: 90% CL limits Dotted: model prediction ANTARES preliminary Upper limits with respect to different models PRELIMINARY Dotted: different models

17. Dark Matter WIMPs accumulate in heavy objects (Sun, Galactic Center, Earth) Capture/Annihilation in equilibrium at the Sun core Annihilation e.g. in bb/  /WW -> +.. Model-independent event simulation using WIMPSIM Interactions in the Sun and flavor oscillation, regeneration of  in the Sun taken into account    

18.     Neutrino candidates in the direction towards the sun (angular distance  ) kinematics  2 based track reconstruction efficient for low energies Different detector configurations Angular resolution (median)

19. Spin-independent cross-section limit for ANTARES 2007-2008 in CMSSM For CMSSM: Branching ratios = 1 (for WW, bb, ττ) (Large variation of branching ratios over parameter space) PRELIMINARY

20. Spin-dependent cross-section limit for ANTARES 2007-2008 in CMSSM For CMSSM: Branching ratios = 1 (for WW, bb, ττ) (Large variation of branching ratios over parameter space) PRELIMINARY

21. Low energy atmospheric neutrinos important Baseline L from zenith angle  Energy estimate from track length Different track reconstruction using multi-line and single-line events (only zenith reconstructed) Single Line Multi Line Dashed: with oscillation Simulation of reconstructed neutrinos

22. Data Best Fit No oscillations Antares, K2K, Minos, SuperK For maximal mixing  m 2 =(3.1±0.9) 10 -3 eV 2 PhysLettB 714, 224 (2012)

23. First Funding already available to allow start of construction 2013-15 Building/Deployment of first batch of detectors 2015++ Completion of Detector 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

24. 860m Track resolution 0.1deg @ TeV New detector concept: Sphere with 31 PMTs - good directionality - single photon counting Multiple building blocks 640 strings (in total) 20 storeys/string => 12800 DOMs 1 building block 800 m

25. 860m Track resolution 0.1deg @ TeV New detector concept: Sphere with 31 PMTs - good directionality - single photon counting Multiple building blocks 640 strings (in total) 20 storeys/string => 12800 DOMs First light of sphere with 31 PMTs in Antares Rate histogram for multiplicity of coincidences -> seeing first muons!

26. Neutrino telescope in seawater successfully established with high angular resolution Variety of physics analyses underway, first results published Large several cubic kilometer array Km3NeT planned in the Mediterranean Sea Construction of first KM3NeT detection units underway First light with new optical module in Antares! => NEW WINDOW TO THE UNIVERSE BECOMES AVAILABLE