Mohamad-Ziad Charif - Antares

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[102] D. Heck and J. Knapp, “Forschungszentrum Karlsruhe Report FZKA 6097(1998),” http://www-ik.fzk.de/corsika.[103] G. J. Feldman and R. D. Cousins, “A Unified approach to the classicalstatistical analysis of small signals,” Phys.Rev., vol. D57, pp. 3873–3889,1998.[104] S. Loucatos, “Systematics of the indirect DM search,” ANTARES-PHYS-2011-015, Internal Note.[105] e. a. C.Bogazzi, “Point Source Search with 2007 and 2008 data,”ANTARES-PHYS-2010-008, Internal Note.[106] G. Halladjian, “Search for high energy neutrinos from point sources withANTARES,” Dec2010, Ph.D thesis.[107] J. C. et al., “Discovery and Upper Limits in Search for Exotic Physics withNeutrino Telescopes,” Phys. Rev. D 67 (2003) 012002.[108] G. Lim, “Searching for Dark Matter with the <strong>Antares</strong> Neutrino Telescope,”Ph.D. thesis, Faculteit der Natuurwetenschappen, Wiskunde en Informatica.[109] T. Tanaka et al., “An Indirect Search for WIMPs in the Sun using3109.6 days of upward-going muons in Super-Kamiokande,” Astrophys.J.,vol. 742, p. 78, 2011.[110] C. Riviere, “Run-by-run Monte Carlo simulation for ANTARES: v2,”ANTARES internal note, ANTARES-PHYS-2012-001.[111] Adrian-Martinez, S. and others, “Measurement of Atmospheric NeutrinoOscillations with the ANTARES Neutrino Telescope,” Phys.Lett.,vol. B714, pp. 224–230, 2012.162
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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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a look at figure 5.22 we find a cle
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The resulting optimized sensitiviti
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Figure 5.26: A comparison plot of t
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dΦ µdE ν= dΦ νdE νP earth ρN
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Figure 5.31: Limits on the muon flu
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Chapter 6Dark Matter search in the
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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 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
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Mohamad-Ziad Charif - Antares

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