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Dark Matter Search in the Galactic Center with ANTARES
Dark Ghosts – 1st GNN Workshop on Indirect Dark Matter Detection with Neutrino Telescopes Valencia, April 2014 Juan de Dios Zornoza (IFIC – Valencia) on behalf of the ANTARES Collaboration
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ν can propagate with a minimum of astrophysical uncertainties
Galactic Centre νe, νμ, ντ WIMPs ν oscillations in the vacuum ν can propagate with a minimum of astrophysical uncertainties Earth Galactic Center WIMPs self-annihilate according to <σAv> (halo model-dependent) ρsc where Sun position Rsc
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GC: scrambled data vs MC
blue: MC red: scrambled data black: average limit good agreement, but still, we use scrambled data
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GC: Simulation tools Spectrum simulation: Cirelli et al.
Halo: CLUMPY, to calculate the J-factor versus the opening angle arxiv: b bbar W+ W- tau+ tau- mu+ mu- nu nubar MWIMP = 360 GeV
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GC: effective area b bbar W+ W- tau+ tau- mu+ mu- nu nubar AAFit BBFit
12 line detector
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Galactic Centre Again, optimization based on flux limits b bbar W+ W-
tau+ tau- mu+ mu- nu nubar BBFit, singleline, tchi2<0.8 AAFit, lambda>-5.5 beta<0.5, costh>-0.1
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Galactic Centre J-factor DM density profile (NWF) For models like NFW, most of the dark matter is within the angular resolution of the detector
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GC: unblinding data BBFit-singleline, tchi2<1 AAFit, lambda>-5.6
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GC: limits on the flux b bbar W+ W- tau+ tau- mu+ mu- nu nubar
dash-dotted: BBFit-1L dasded: BBFit-ML solid: AAFit-ML
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GC: limits on <σv>
tau+ -tau- dash-dotted: BBFit-1L dasded: BBFit-ML solid: AAFit-ML
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GC: <σv> for different channels
b bbar W+ W- tau+ tau- mu+ mu- nu nubar dash-dotted: BBFit-1L dasded: BBFit-ML solid: AAFit-ML
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GC: Comparsion wrt other experiments
DMDMτ+τ- IC40 - GC PRELIMINARY IC79-Halo IC22-Halo IC IC59-dSphs IC59-Virgo ANTARES -NFW PAMELA PAMELA + FERMI + HESS Fermi-dSphs natural scale G. Lambard
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GC: other halo profiles
DMDMτ+τ- IC40 - GC PRELIMINARY IC79-Halo IC22-Halo IC IC59-dSphs IC59-Virgo ANTARES -NFW -Einasto -steep NFW* PAMELA PAMELA + FERMI + HESS Fermi-dSphs natural scale *(α,β,γ) = (1,3,1.3) and ρS = 0.3 GeV.cm-3, and RS = 21.7 kpc.
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