Mohamad-Ziad Charif - Antares

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Figure 6.28: Comparison of the multi-lines, single-line and combined sensitivitiesto neutrino flux coming from dark matter annihilation inside the Sun as a functionof WIMP mass and the annihilation channel. Top plot is for the soft b + b − , middleis for τ + τ − , while to bottom is for W + W − .136
6.5 Dark matter search with AAFit reconstructionstrategyIn this section we will discuss the analysis using the AAFit reconstruction strategy.6.5.1 Data Monte Carlo comparisonSimilarly to the two previous analyzes, before going on with our analysis weshould first test our data Monte Carlo agreement. In this case no set of preliminarycuts are proposed, so we will go right ahead with the comparison.Figure 6.29 shows us the Λ distribution of data, our MC (atm µ & atm ν ) and twodark matter models which have been normalized to the number of events of atm ν .The agreement between data and atm ν is good for values of Λ > -5 (larger valuesof Λ indicates a good fit), in addition we can see that the agreement between atm µfor λ > -6.5 is very good as well. However, for values smaller than -6.5 we see wehave a bad data Monte Carlo agreement in the region where the lambda reflects abad fit on the muon track. Additionally, we can notice that in contrary to the χ 2variable in BBFit where we saw the dark matter models behave similarly to atm νhere with Λ variable this is not the case. The model 50 GeV b + b − seems to havea the larger portion of its events in the small values of Λ when compared to atm νwhile 1000 GeV τ + τ − on the other hand seem to have more its events in the largevalues of Λ when compared to atm ν .137
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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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Page 94 and 95: Figure 5.15: Estimation of the back
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Page 98 and 99: Figure 5.18: A comparison of the di
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Page 102 and 103: The resulting optimized sensitiviti
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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
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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
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Page 136 and 137: Figure 6.25: Estimation of our back
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Page 144 and 145: Figure 6.34: Comparison of the esti
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Page 150 and 151: 6.7 Comparison with 2007-2008 analy
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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 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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