Mohamad-Ziad Charif - Antares

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6.7 Comparison with 2007-2008 analysisWhile we have provided a comparison between the BBFit multi-lines 2007-2010sensitivities and the 2007-2008 analysis, we have yet to provide a complete comparisonwith the BBFit combined analysis along with the results obtained withAAFit.Figure 6.42 shows us the comparison of the different results for the soft spectrumb + b − , at 50 GeV if we use the sensitivities set by BBFit combined analysis wegain about a factor 35 improvement (mostly from the single lines analysis). Asfor 1000 GeV we have a gain about a factor 10 if we use the results from AAFit.Figure 6.42: Comparison of the sensitivities set by the 2007-2008 analysis (BBFit)and 2007-2010 analysis (BBFit combined and AAFit) for the soft b¯b spectrum.In figure 6.43 we see the comparison of the results for the hard spectrum τ + τ − ,at 50 GeV the sensitivities obtained from BBFit combined analysis gives us animprovement of about a factor 10. As for 1000 GeV if we use AAFit we wouldgain by factor 9. In figure 6.44 we see the comparison of the results for the hardspectrum W + W − , at 80.3 GeV we gain a factor 7 by using BBFit combined analysis,and factor 6 at 1000 GeV if we use AAFit.And finally figures 6.45 & 6.46 shows us the final sensitivities to the spin-dependentand independent cross-sections. While the improvement we get is visible in thecase of spin-dependent, in 2007-2008 analysis (figure 5.32) the limits on spindependentcould not probe models beyond 250 GeV with the limit set by the τ + τ −channel. Additionally the lowest cross-section achieved below 250 GeV was at a148
Figure 6.43: Comparison of the sensitivities set by the 2007-2008 analysis (BBFit)and 2007-2010 analysis (BBFit combined and AAFit) for the soft τ + τ − spectrum.Figure 6.44: Comparison of the sensitivities set by the 2007-2008 analysis (BB-Fit) and 2007-2010 analysis (BBFit combined and AAFit) for the soft W + W −spectrum.149
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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
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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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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
Page 132 and 133: Figure 6.21: Comparison of the opti
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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
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
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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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