Mohamad-Ziad Charif - Antares

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Figure 6.21: Comparison of the optimized ∆(θ ◦ ) cut as a function of the WIMPmass and the annihilation channel .Figure 6.22: Sensitivity to neutrino flux coming from dark matter annihilationinside the Sun as a function of WIMP mass and the annihilation channel for theBBFit single-line analysis.130
6.4.3 Single & Multi line combined analysisIn this section we will discuss the comparison of the single and multi line analyzesand their combination method.6.4.3.1 Single Vs Multi line comparisonFigures 6.23 & 6.24 show us the comparison among the different sensitivitieswe get from both analyzes. As predicted we can see the best improvement toour sensitivities we get is for low WIMP masses with b + b − as the annihilationchannel with single-line sensitivity being almost an order of magnitude better. Atthe other end of dark matter models, the limits obtained by multi-lines from 1000GeV hard channels (W and τ) are this time an order of magnitude better thantheir single-line equivalent. While we understand why at low WIMP masses weget almost an order of magnitude better sensitivity, we need to explain those withharder spectra at high mass. If we remember figure 6.13 at high WIMP masses weget as much multi-lines event as single-line, so they must get sensitivities of equalorder. However, the reason with this discrepancy has to do with the expectedbackground. For multi-lines 1000 GeV τ + τ − the optimal cuts for (χ 2 , ∆(Ψ))are (1.6 , 2.7 ◦ ) which yields an expected background of 2.6 events, while in thecase of single-line with (0.9 , 7 ◦ ) as optimized (χ 2 , ∆(θ)) they yield an expectedbackground of 40 events. ¯µ 90% in the case of 2.6 events is about 4.224 while in thecase of 40 events it is 12.586. For this reason if we assume that at their respectivecuts we still have the same number of signal events between the multi-lines andsingle-line 2 we would expect that the sensitives with multi-lines to be at least 3times better than those with single-lines.2 Which is not true as we have more multi-lines events after cuts in this specific case131
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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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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
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Page 124 and 125: 6.4.2 BBFit Single-line analysisThe
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Page 128 and 129: Figure 6.17: Comparison of Nhit dis
Page 130 and 131: Figure 6.19: The estimation of the
Page 134 and 135: Figure 6.23: Comparison of sensitiv
Page 136 and 137: Figure 6.25: Estimation of our back
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Page 140 and 141: Figure 6.29: Comparison of the Λ d
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Page 154 and 155: Chapter 7ConclusionsThe limits pres
Page 156 and 157: Bibliography[1] Volders, L. M. J. S
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Page 164: [102] D. Heck and J. Knapp, “Fors
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Mohamad-Ziad Charif - Antares

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