Mohamad-Ziad Charif - Antares

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[46] G. Debrassi, S. Heinemeyer, W. Hollik, P. Slavich, and G. Weiglein, “Towardshigh-precision predictions for the mssm higgs sector,” Eur. Phys. J.,vol. C28, p. 133, 2003.[47] M. Frank, T. Hahn, S. Heinemeyer, W. Hollik, H. Rzehak, and G. Weiglein,“The higgs boson masses and mixings of the complex mssm in thefeynman-diagrammatic approach,” JHEP, vol. 02, p. 047, 2007.[48] L. Roszkowski, R. Ruiz de Austri, R. Trotta, and J. Silk, “On prospects fordark matter indirect detection in the constrained mssm,” 2007.[49] L. Roszkowski, R. R. de Austri, and R. Trotta, “On the detectability of thecmssm light higgs boson at the tevatron,” JHEP, vol. 04, p. 084, 2007.[50] R. Trotta, R. R. de Austri, and L. Roszkowski, “Prospects for direct darkmatter detection in the constrained mssm,” New Astron. Rev., vol. 51,pp. 316–320, 2007.[51] R. R. de Austri, R. Trotta, and L. Roszkowski, “A markov chain montecarlo analysis of the cmssm,” JHEP, vol. 05, p. 002, 2006.[52] F. Feroz, M. P. Hobson, and M. Bridges, “MultiNest: an efficient and robustBayesian inference tool for cosmology and particle physics,” 2008.[53] R. T. et al, “The impact of priors and observables on parameter inferencesin the constrained mssm,” 2008.[54] S. Piccardi, “The PAMELA experiment,” 1999.[55] J. Beatty, A. Bhattacharyya, C. Bower, S. Coutu, M. DuVernois, et al.,“New measurement of the cosmic-ray positron fraction from 5 to 15-GeV,”Phys.Rev.Lett., vol. 93, p. 241102, 2004.[56] M. Aguilar et al., “Cosmic-ray positron fraction measurement from 1 to30-GeV with AMS-01,” Phys.Lett., vol. B646, pp. 145–154, 2007.[57] A. A. Abdo et al., “Measurement of the Cosmic Ray e+ plus e- spectrumfrom 20 GeV to 1 TeV with the Fermi Large Area Telescope,”Phys.Rev.Lett., vol. 102, p. 181101, 2009.[58] J. Chang, J. Adams, H. Ahn, G. Bashindzhagyan, M. Christl, et al., “An excessof cosmic ray electrons at energies of 300-800 GeV,” Nature, vol. 456,pp. 362–365, 2008.158
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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
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 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 162 and 163: [74] C. Hettlage, K. Mannheim, and
Page 164: [102] D. Heck and J. Knapp, “Fors
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