Mohamad-Ziad Charif - Antares

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Figure 6.29: Comparison of the Λ distribution of data, MC: atm µ and atm ν , andtwo dark matter models ( 50 GeV b + b − & 1000 GeV τ + τ − ) which were normalizedto the number of events of atm ν . The muon and neutrino Monte Carlo arenormalized to the lifetime of the data taking.Figure 6.30 present us the Nhit distribution with a cut of Λ >-5.6 . Here we finda very good agreement between data and our background Monte Carlo as a directconsequence of the good agreement we saw in 6.29 for high values. However, theinteresting part of this distribution is the behavior of the two dark matter modelswe used an example. The 1000 GeV τ + τ − model seems to behave for most part(up to Nhit 40. In consequencewe can use Nhit as a discriminating variable as we did in the BBFit single-lineanalysis. However, the effect of a Nhit max cut will only be significant on lighterWIMPs with softer spectra.138
Figure 6.30: Comparison of the Nhit distribution of data, MC: atm µ &atm ν , andtwo dark matter models ( 50 GeV b + b − & 1000 GeV τ + τ − ) which were normalizedto the number of events of atm ν . A cut of Λ >-5.6 was applied here.The muon and neutrino Monte Carlo are normalized to the lifetime of the datataking.XSIn figure 6.31 we can see the distribution of cos(θ) with a cut of Λ >-5.6 .Again the agreement is pretty good between data and our background MC, theloose cut of Λ ensures that atm µ dominates our data sample.Finally in figure 6.32 we can see the distribution of β. This variable is an estimationon the uncertainty on the direction of the reconstructed muon. This variableis a good separator of atm ν from atm µ . However, we can see that the distributionof this variable changes as a function of the dark matter model as well. HeavierWIMPs who have harder spectra seem to peak higher and drops quicker whencompared to lighter WIMPs with softer spectra (1000 GeV τ + τ − Vs. 50 GeVb + b − ). We would expect when β is used in the optimization process to play therole of another discriminator between background and signal (in addition to Nhitand ∆(ψ)) and heavier WIMPs would have a tighter cut on β when compared tolighter ones, and the same with harder when compared with softer spectra.139
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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
Page 90 and 91: Figure 5.11: Sun’s position taken
Page 92 and 93: Figure 5.13: Comparison between the
Page 94 and 95: 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 142 and 143: Figure 6.31: Comparison of the cos(
Page 144 and 145: Figure 6.34: Comparison of the esti
Page 146 and 147: The optimal Λ cut for all dark mat
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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