juande zornoza (ific, valencia) on behalf of the antares collaboration
DESCRIPTION
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. - PowerPoint PPT PresentationTRANSCRIPT
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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
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*Scientific scope
MeV GeV TeV PeV EeV
Astrophysical neutrinosDark matter (neutralinos, KK)
Oscillations
Supernovae
GZK
Limitation at high energies:Fast decreasing fluxes E-2, E-3
Limitation at low energies:-Short muon range-Low light yield-40K (in water)
Detector density
Detector size
Origin of cosmic rays Hadronic vs. leptonic signatures Nature of dark matter
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*Detection of DM by NTs*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
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*Detection principle of optical Cherenkov detectors
The neutrino is detected by the Cherenkov light emitted by the muon produced in the CC interaction.
1.2 TeV muon traversing ANTARES
N X
W
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*Data*ANTARES was completed in 2008*During 2007, 5 lines were already operative*This analysis uses data of 2007 (5 lines) and 2008 (9-10-12 lines)*About 1000 up-going neutrino candidates in the selected sample*Binned search
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*Data vs MC: elevation
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*Data vs MC: fit quality
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*Background
All upward-going events from 2007-2008 data Example of Sun tracking in horizontal coordinates
• Background estimated from data (2007-2008 period, ~295 days)• Fast algorithm for muon track reconstruction (Astro. Phys. 34 (2011) 652-662)• Using the Sun visibility at the ANTARES location• Background from CR interactions in the Sun corona much lower (few percent of total)
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• 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... Earth
*Signal: WimpSim
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MWIMP = 350 GeV
*Main annihilation channels
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*Signal and cut optimization• 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:
Acceptance to be estimated for different sets (tchi2,cone)Average upper limit (Feldman-Cousins)
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Neutrino flux sensitivity for 2007-2008 dataPreliminary For CMSSM:
Branching ratios = 1(WW, bb, ττ)
For mUED: Theoretical branching ratios taken into account
Reason:High dependence of branching ratios over CMSSM parameter space
*Neutrino flux sensitivity
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Muon flux sensitivity for ANTARES 2007-2008Preliminary
Flux Φμ
Annihilation rate Γ
Capture rate C
Cross-section σSD
*Muon flux sensitivity
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PreliminarySpin-dependent cross-section flux sensitivity for
ANTARES 2007-2008
Compare SUSY predictions to
observables as sparticles masses,
collider observables, dark matter relic density, direct detection cross-
sections, …SuperBayes
(arXiv:1101.3296)
χ2
*CMSSM cross-section sensitivity
G. Lambard
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Spin-dependent cross-section flux sensitivity for ANTARES 2007-2008 Preliminary
1σ2σ
Compare mUED predictions to
observables as KK masses, collider
observables, relic density, direct
detection cross-sections, …
SuperBayes modified version
(Physical Review D 83, 036008 (2011))
*mUED cross-section sensitivity
G. Lambard
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*Summary• 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…
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* Neutrino candidate with 12-line detector
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18
De C. Hettlage et al., Astropart.Phys. 13 (2000) 45-50 Simple parameterization averaged on the oscillations
* Background in the Sun direction IICR and Solar atmosphere
It doesn’t represent more than 10-3 events per year in a 5 lines cofiguration (few events for a km3), 0.4% of the total atmospheric background…
νμ
• Interactions p-p give a production of neutrinos through the decay products