Mohamad-Ziad Charif - Antares

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"The most exciting phrase to hear in science, the one that heraldsnew discoveries, is not ‘Eureka‘ but ‘That’s funny...‘ "- Isaac Asimov(1920 - 1992)
Contents1 Introduction 42 Dark Matter 62.1 Indirect evidence . . . . . . . . . . . . . . . . . . . . . . . . . . 62.1.1 Galactic rotation curves . . . . . . . . . . . . . . . . . . 62.1.2 Galaxy clusters . . . . . . . . . . . . . . . . . . . . . . . 72.1.3 Gravitational lensing . . . . . . . . . . . . . . . . . . . . 72.1.4 Velocity Dispersions of galaxies & Mass to light ratio . . . 82.1.5 Cosmic microwave background . . . . . . . . . . . . . . 92.1.6 ΛCDM model . . . . . . . . . . . . . . . . . . . . . . . . 92.1.6.1 Dark matter in ΛCDM . . . . . . . . . . . . . . 112.2 WIMPs . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 132.2.1 Standard Scenario . . . . . . . . . . . . . . . . . . . . . 132.2.2 WIMPs in Supersymmetry . . . . . . . . . . . . . . . . . 142.2.2.1 MSSM . . . . . . . . . . . . . . . . . . . . . . 162.3 Methods of detection . . . . . . . . . . . . . . . . . . . . . . . . 192.3.1 Direct detection . . . . . . . . . . . . . . . . . . . . . . . 192.3.2 Indirect detection . . . . . . . . . . . . . . . . . . . . . . 202.4 Dark matter in the Sun . . . . . . . . . . . . . . . . . . . . . . . 233 The ANTARES Neutrino Telescope 333.1 Neutrino interaction with matter . . . . . . . . . . . . . . . . . . 333.1.1 Bremsstrahlung radiation . . . . . . . . . . . . . . . . . . 343.1.2 Medium ionization . . . . . . . . . . . . . . . . . . . . . 353.1.3 Pair production . . . . . . . . . . . . . . . . . . . . . . . 363.1.4 Cherenkov radiation . . . . . . . . . . . . . . . . . . . . 363.2 Neutrino telescopes . . . . . . . . . . . . . . . . . . . . . . . . . 383.2.1 ANTARES . . . . . . . . . . . . . . . . . . . . . . . . . 393.2.1.1 Detector layout . . . . . . . . . . . . . . . . . 443.2.1.2 Calibration . . . . . . . . . . . . . . . . . . . . 483.2.1.3 Status of the detector . . . . . . . . . . . . . . 591
Page 4 and 5: 3.2.1.4 Performance and characteris
Page 6 and 7: Chapter 1IntroductionThe early hist
Page 8 and 9: Chapter 2Dark MatterIn this chapter
Page 10 and 11: Figure 2.2: Comparison of the measu
Page 12 and 13: Figure 2.4: CMB anisotropy observed
Page 14 and 15: Figure 2.5: Combination of the WMAP
Page 17: Figure 2.6: Temporal evolution of t
Page 20 and 21: Figure 2.9: Parameter space of m 1/
Page 22 and 23: Figure 2.10: Limits on spin-indepen
Page 26 and 27: Figure 2.14: Detected gamma ray flu
Page 28 and 29: 600km/s. If we assume the worst cas
Page 30 and 31: Figure 2.17: Conversion factor from
Page 32 and 33: The eigenstate mixing can be writte
Page 34 and 35: Figure 2.19: Flux of ν µ / ¯ν
Page 36 and 37: Figure 3.1: The neutral current (NC
Page 38 and 39: Muon Energy (GeV )1p| dEdx | (GeV.c
Page 40 and 41: Figure 3.4: Energy loss of per dist
Page 42 and 43: Figure 3.6: Effective muon range as
Page 44 and 45: Figure 3.8: Differential flux of at
Page 46 and 47: 3.2.1.1 Detector layoutOptical Modu
Page 48 and 49: • The LED (light emitting diode)
Page 50 and 51: Anchor & BuoyEach line is anchored
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Figure 3.17: Distribution of azimut
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Figure 3.20: Height and radial disp
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Figure 3.22: Distribution of sea cu
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Figure 3.24: Time offset among OMs
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Figure 3.26: Distribution of time d
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Line number Connection Date Mainten
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Figure 3.29: Comparison between sky
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Figure 3.31: The effective area for
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Figure 4.1: Median counting rate of
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Figure 4.4: Average neutrino events
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2. All hits on the same floor are m
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4.2.1 Neutrino simulationFigure 4.6
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• Multiplicity range of the muon
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Chapter 5Dark Matter search in the
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Figure 5.2: Annihilation spectrum f
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Livetime(days) 5 Lines 9 Lines 10 L
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Figure 5.4: Monte Carlo Truth distr
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Figure 5.7: Tchi2 distribution for
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Figure 5.9: Tchi2 distribution for
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Figure 5.11: Sun’s position taken
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Figure 5.13: Comparison between the
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Figure 5.15: Estimation of the back
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Figure 5.16: Mean angle between the
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Figure 5.18: A comparison of the di
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a look at figure 5.22 we find a cle
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The resulting optimized sensitiviti
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Figure 5.26: A comparison plot of t
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dΦ µdE ν= dΦ νdE νP earth ρN
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Figure 5.31: Limits on the muon flu
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Chapter 6Dark Matter search in the
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Figure 6.1: . True Position of the
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Figure 6.3: Comparison of the three
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For BBFit all variables mentioned i
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Figure 6.6: The distribution of χ
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annihilation channel W + W − the
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lowering the total contribution of
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6.4.2 BBFit Single-line analysisThe
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Figure 6.15: Comparison between the
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Figure 6.17: Comparison of Nhit dis
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Figure 6.19: The estimation of the
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Figure 6.21: Comparison of the opti
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Figure 6.23: Comparison of sensitiv
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Figure 6.25: Estimation of our back
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Figure 6.28: Comparison of the mult
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Figure 6.29: Comparison of the Λ d
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Figure 6.31: Comparison of the cos(
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Figure 6.34: Comparison of the esti
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The optimal Λ cut for all dark mat
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Figure 6.40: Sensitivity to neutrin
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6.7 Comparison with 2007-2008 analy
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mass of 200 GeV and a cross-section
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Chapter 7ConclusionsThe limits pres
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Bibliography[1] Volders, L. M. J. S
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[22] S. Burles et al., “Big bang
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[46] G. Debrassi, S. Heinemeyer, W.
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[74] C. Hettlage, K. Mannheim, and
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[102] D. Heck and J. Knapp, “Fors
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Mohamad-Ziad Charif - Antares

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