- Page 2 and 3: "The most exciting phrase to hear i
- Page 4 and 5: 3.2.1.4 Performance and characteris
- Page 6 and 7: Chapter 1IntroductionThe early hist
- Page 8 and 9: Chapter 2Dark MatterIn this chapter
- Page 10 and 11: Figure 2.2: Comparison of the measu
- Page 12 and 13: Figure 2.4: CMB anisotropy observed
- Page 14 and 15: Figure 2.5: Combination of the WMAP
- Page 19 and 20: Figure 2.8: Energy dependence of th
- Page 21 and 22: 2.3 Methods of detection2.3.1 Direc
- Page 23: Pressure on Proximal Emitters• As
- Page 27 and 28: Figure 2.15: Upper limit on the dar
- Page 29 and 30: Figure 2.16: Conversion factor from
- Page 31 and 32: Figure 2.18: Flux of ν µ / ¯ν
- Page 33 and 34: • δ ∈ [0,2π[• ∆m 2 12 = (
- Page 35 and 36: Chapter 3The ANTARES Neutrino Teles
- Page 37 and 38: Figure 3.2: The process of producti
- Page 39 and 40: Figure 3.3: Diagram of a particle u
- Page 41 and 42: Figure 3.5: Mean kinematic angle be
- Page 43 and 44: Figure 3.7: Particle shower that is
- Page 45 and 46: Figure 3.10: Detector layoutFigure
- Page 47 and 48: Figure 3.13: ANTARES storeyStoreyTh
- Page 49 and 50: Figure 3.14: Instrumentation line I
- Page 51 and 52: Figure 3.15: The LFLBL system, meas
- Page 53 and 54: Figure 3.18: Distribution of zenith
- Page 55 and 56: Figure 3.21: Diagram of how the HFL
- Page 57 and 58: Figure 3.23: OM time offset calibra
- Page 59 and 60: Figure 3.25: Comparison of the dist
- Page 61 and 62: Figure 3.27: Median angles between
- Page 63 and 64: Figure 3.28: ANTARES visibility of
- Page 65 and 66: Figure 3.30: Effective area at trig
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Chapter 4Monte-Carlo & DataIn this
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Figure 4.2: Typical rates on OMs on
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QB=1The QB=1 flag is given when :QB
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Figure 4.5: Percentage of muons sim
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• Flavor of the neutrino to be si
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give the distribution of arrival ti
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Figure 5.1: Dark Matter neutrino di
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The spectrum obtained via WIMPSIM w
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• Take the start date of the firs
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Figure 5.6: Dark Matter neutrino di
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Figure 5.8: Tchi2 distribution for
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Figure 5.10: Distribution of Cos[Ze
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Figure 5.12: Comparison between the
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Figure 5.14: Comparison between the
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5.7 Search strategyIf we look again
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n ν =E=M χˆE minn signal = n ν
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Figure 5.20: An example of minimiza
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Figure 5.22: Normalized cumulative
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It is important to note that there
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Figure 5.27: Limits on neutrino flu
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Figure 5.29: Charged Current cross-
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those by ICECUBE[69] dominate at ma
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with 2.10 8 neutrinos per run.• S
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Figure 6.2: . Comparison of two dif
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Figure 6.4: The true distribution o
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6.4.1.1 Data Monte Carlo comparison
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6.4.1.2 Background estimationThe ba
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Figure 6.10: Comparison of the opti
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Figure 6.12: Comparison of sensitiv
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tween the direction of the Sun and
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Figure 6.16: Comparison of χ 2 dis
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Figure 6.18: Comparison of χ 2 dis
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The good data-MC agreement in figur
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6.4.3 Single & Multi line combined
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Figure 6.24: Ratio of multi-lines n
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Figure 6.27: Distribution of ¯Φ 9
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6.5 Dark matter search with AAFit r
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Figure 6.30: Comparison of the Nhit
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6.5.2 Background estimationAs previ
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Figure 6.35: Comparison of the esti
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Figure 6.38: Optimal ∆(Ψ) [ ◦
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Figure 6.41: Comparison of the BBFi
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Figure 6.43: Comparison of the sens
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Figure 6.46: Sensitivities to spin-
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for dark matter. Additionally ANTAR
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[10] D. Clowe, M. Bradac, A. H. Gon
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[34] D. Akerib, P. Barnes, P. Brink
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[59] L. Goodenough and D. Hooper,
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[88] D. J. Bailey, “Dark Matter,