Mohamad-Ziad Charif - Antares

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Figure 2.8: Energy dependence of the inverse coupling coefficient of the threeforces (strong, weak, and electromagnetic) in Supersymmetry[29].to a gauge anomaly and would cause the theory to be inconsistent. However, ifone more Higgsino is added, then there is no gauge anomaly, making the simplesttheory is the one with two Higgsinos and therefore two scalar Higgs doublets.Additionally, this predicts that the lightest neutral Higgs to be lighter than 130GeV. The Higgs particle candidate found at LHC[31] (mass ∼ 125 GeV) is inagreement with the prediction made in MSSM. However, working with MSSMis quite difficult as the theory has more than 100 free parameters (by contrastStandard Model have less than 20), making any prediction hindered by the largeamount of simulation needed to search all of the parameter space. In responseto this problem a set of assumption have been made in order to constrain theparameters. CMSSM or Constrained MSSM is one of these models that containcertain assumptions. These assumptions are as follows:• Universality of gaugino masses at the GUT scale.• Universality of scalar masses ot the GUT scale.• Universality of the tri-linear scalar (Yukawa) couplings at the GUT scale.• Symmetry breaking by means of Electro-Weak Symmetry Breaking drivenby the renormalization group drives the mass of the H 0 u to negative values(or at least extremely small when compared to H 0 d )These assumptions lead us to a model where we only have 4(+1) parameters:• Gaugino masses at the GUT : m 1/2• Scalar masses at the GUT: m 017
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 17: Figure 2.6: Temporal evolution of t
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
Page 67 and 68: 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,
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Mohamad-Ziad Charif - Antares

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