Mohamad-Ziad Charif - Antares

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The optimal Λ cut for all dark matter models is Λ > −5.6 (with the exceptionof 50 GeV b + b − with Λ > −5.9). For Nhit max the range of this is from 50 (lighterWIMPS) to 90 (heavier WIMPs). The β cuts can be seen in figure 6.37. Not alot of variation can be seen in the value of β cuts, most dark matter models havea cut of β < 0.8 ◦ &β < 0.6 ◦ . However, the cut behaves as predicted, larger cutsbelong to lighter WIMPs and softer spectra while tighter cuts belong to heavierWIMPs and harder spectra. On a side note, 50 GeV b + b − does not converge on acut for β (value larger than 70 ◦ ). As for the ∆(Ψ) optimal cuts we present themFigure 6.37: Optimal β [ ◦ ] cuts as a function of WIMP mass and annihilationchannel.in figure 6.38, again we see larger ∆(Ψ) cuts for lighter WIMPs (3.5 ◦ ∼ 4.5 ◦ ) andtighter cuts for heavier WIMPs (1.6 ◦ ∼ 2.4 ◦ ). When these values are comparedto those who obtained with BBFit Multi-lines analysis in figure 6.11 we see thatfor the cuts obtained here are between 1 ◦ and 2 ◦ tighter. This is due to the factthat the AAFit angular resolution is better than BBFit’s angular resolution. Thisdifference can be clearly seen in figure 6.39. This result should be obvious forus, as AAFit’s reconstruction strategy is supposed to be more accurate than BBFit(better treatment of the detector and its geometry).Finally figure 6.40 shows the expected sensitivities to dark matter annihilatingin the Sun using AAFit reconstruction strategy. The values presented here areat the same order of magnitude of those obtained with BBFit combined analysis.However, a more detailed comparison will be presented in the following section.144
Figure 6.38: Optimal ∆(Ψ) [ ◦ ] cuts as a function of WIMP mass and annihilationchannel.Figure 6.39: Comparison of the mean angle between the neutrino direction andthe reconstructed muon direction as a function of neutrino energy.BBFit: χ 2 < 1.6, AAFit: Λ > −5.6, β < 0.8 ◦ .145
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"The most exciting phrase to hear i
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3.2.1.4 Performance and characteris
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Chapter 1IntroductionThe early hist
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Chapter 2Dark MatterIn this chapter
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Figure 2.2: Comparison of the measu
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Figure 2.4: CMB anisotropy observed
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Figure 2.5: Combination of the WMAP
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Figure 2.6: Temporal evolution of t
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Figure 2.9: Parameter space of m 1/
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Figure 2.10: Limits on spin-indepen
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Figure 2.14: Detected gamma ray flu
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600km/s. If we assume the worst cas
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Figure 2.17: Conversion factor from
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The eigenstate mixing can be writte
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Figure 2.19: Flux of ν µ / ¯ν
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Figure 3.1: The neutral current (NC
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Muon Energy (GeV )1p| dEdx | (GeV.c
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Figure 3.4: Energy loss of per dist
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Figure 3.6: Effective muon range as
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Figure 3.8: Differential flux of at
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3.2.1.1 Detector layoutOptical Modu
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• The LED (light emitting diode)
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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
Page 96 and 97: Figure 5.16: Mean angle between the
Page 98 and 99: Figure 5.18: A comparison of the di
Page 100 and 101: a look at figure 5.22 we find a cle
Page 102 and 103: The resulting optimized sensitiviti
Page 104 and 105: Figure 5.26: A comparison plot of t
Page 106 and 107: dΦ µdE ν= dΦ νdE νP earth ρN
Page 108 and 109: Figure 5.31: Limits on the muon flu
Page 110 and 111: Chapter 6Dark Matter search in the
Page 112 and 113: Figure 6.1: . True Position of the
Page 114 and 115: Figure 6.3: Comparison of the three
Page 116 and 117: For BBFit all variables mentioned i
Page 118 and 119: Figure 6.6: The distribution of χ
Page 120 and 121: annihilation channel W + W − the
Page 122 and 123: lowering the total contribution of
Page 124 and 125: 6.4.2 BBFit Single-line analysisThe
Page 126 and 127: Figure 6.15: Comparison between the
Page 128 and 129: Figure 6.17: Comparison of Nhit dis
Page 130 and 131: Figure 6.19: The estimation of the
Page 132 and 133: Figure 6.21: Comparison of the opti
Page 134 and 135: Figure 6.23: Comparison of sensitiv
Page 136 and 137: Figure 6.25: Estimation of our back
Page 138 and 139: Figure 6.28: Comparison of the mult
Page 140 and 141: Figure 6.29: Comparison of the Λ d
Page 142 and 143: Figure 6.31: Comparison of the cos(
Page 144 and 145: Figure 6.34: Comparison of the esti
Page 148 and 149: Figure 6.40: Sensitivity to neutrin
Page 150 and 151: 6.7 Comparison with 2007-2008 analy
Page 152 and 153: mass of 200 GeV and a cross-section
Page 154 and 155: Chapter 7ConclusionsThe limits pres
Page 156 and 157: Bibliography[1] Volders, L. M. J. S
Page 158 and 159: [22] S. Burles et al., “Big bang
Page 160 and 161: [46] G. Debrassi, S. Heinemeyer, W.
Page 162 and 163: [74] C. Hettlage, K. Mannheim, and
Page 164: [102] D. Heck and J. Knapp, “Fors
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Mohamad-Ziad Charif - Antares

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