Mohamad-Ziad Charif - Antares

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4.2.1 Neutrino simulationFigure 4.6: The can.The simulation of atmospheric neutrinos starts with GENEHN ([88] & [99]) whichhas the role of generating the initial neutrino and then its interaction with matter,followed by GEASIM[100] which handles the hadronic showers created with thesimulated neutrinos.4.2.1.1 GENHENGENHEN (GENerator of High Energy Neutrinos) is a neutrino Monte Carlo simulatorwhich simulates according to an input provided by the user the distributionof muon’s induced neutrinos on and inside a surface that surrounds the detector.This surface is named “can” (Figure 4.6), it represents the surface of a cylindersurrounding the detector. If the detector is thought to be of cylindrical shape, theradius of the can is the radius of the detector plus ∼ 3 times the absorption lengthof the Cherenkov light (the absorption length will be defined later in section 4.2.3).The user can select through input data cards the parameters of the simulation,we’ll list some of the most important of them:• Number of neutrino event to be simulated72
• Flavor of the neutrino to be simulated• Energy range of the simulation• Whether to do charged current interactions or neutral current interactions• Choice of the parton model of interacting matter• Model of neutrino interactions• Neutrino flux (-1.4 for atmospheric neutrinos (insert reference to that number))• Whether to generate isotropic neutrinos or from a point with a fixed declinationin the RA-DEC coordinate systemAfter the user has selected the input parameter and the simulation is over, theoutput of the simulation is then parsed into an ASCII file.4.2.1.2 GEASIMGEASIM is a particle and shower Monte Carlo simulator based on GEANT, inthe case of ANTARES the input is the files simulated previously with GENHEN.However it goes further than GENHEN, by simulating the propagation of showersand the eventual radiation produced by these particles.4.2.2 Muon simulationThe simulation of atmospheric muons is done directly via MUPAGE[101]:MUPAGEMUPAGE (MUon GEnerator from PArametric formulas), as the name suggest itis an atmospheric muon Monte Carlo generator. They are not simulated usingcollisions between cosmic rays and the atmosphere, but rather using parametricformulas for the expected muon flux at the detector level. MUPAGE takes asinput many variables, the most important of them:• Position of the detector below sea level• Size of the can• The θ range of simulation• Energy range of the muons73
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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
Page 26 and 27: Figure 2.14: Detected gamma ray flu
Page 28 and 29: 600km/s. If we assume the worst cas
Page 30 and 31: Figure 2.17: Conversion factor from
Page 32 and 33: The eigenstate mixing can be writte
Page 34 and 35: Figure 2.19: Flux of ν µ / ¯ν
Page 36 and 37: Figure 3.1: The neutral current (NC
Page 38 and 39: Muon Energy (GeV )1p| dEdx | (GeV.c
Page 40 and 41: Figure 3.4: Energy loss of per dist
Page 42 and 43: Figure 3.6: Effective muon range as
Page 44 and 45: Figure 3.8: Differential flux of at
Page 46 and 47: 3.2.1.1 Detector layoutOptical Modu
Page 48 and 49: • The LED (light emitting diode)
Page 50 and 51: Anchor & BuoyEach line is anchored
Page 52 and 53: Figure 3.17: Distribution of azimut
Page 54 and 55: Figure 3.20: Height and radial disp
Page 56 and 57: Figure 3.22: Distribution of sea cu
Page 58 and 59: Figure 3.24: Time offset among OMs
Page 60 and 61: Figure 3.26: Distribution of time d
Page 62 and 63: Line number Connection Date Mainten
Page 64 and 65: Figure 3.29: Comparison between sky
Page 66 and 67: Figure 3.31: The effective area for
Page 68 and 69: Figure 4.1: Median counting rate of
Page 70 and 71: Figure 4.4: Average neutrino events
Page 72 and 73: 2. All hits on the same floor are m
Page 76 and 77: • Multiplicity range of the muon
Page 78 and 79: Chapter 5Dark Matter search in the
Page 80 and 81: Figure 5.2: Annihilation spectrum f
Page 82 and 83: Livetime(days) 5 Lines 9 Lines 10 L
Page 84 and 85: Figure 5.4: Monte Carlo Truth distr
Page 86 and 87: Figure 5.7: Tchi2 distribution for
Page 88 and 89: Figure 5.9: Tchi2 distribution for
Page 90 and 91: Figure 5.11: Sun’s position taken
Page 92 and 93: Figure 5.13: Comparison between the
Page 94 and 95: Figure 5.15: Estimation of the back
Page 96 and 97: Figure 5.16: Mean angle between the
Page 98 and 99: Figure 5.18: A comparison of the di
Page 100 and 101: a look at figure 5.22 we find a cle
Page 102 and 103: The resulting optimized sensitiviti
Page 104 and 105: Figure 5.26: A comparison plot of t
Page 106 and 107: dΦ µdE ν= dΦ νdE νP earth ρN
Page 108 and 109: 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
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6.4.2 BBFit Single-line analysisThe
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Figure 6.15: Comparison between the
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Figure 6.17: Comparison of Nhit dis
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Figure 6.19: The estimation of the
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Figure 6.21: Comparison of the opti
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Figure 6.23: Comparison of sensitiv
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Figure 6.25: Estimation of our back
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Figure 6.28: Comparison of the mult
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Figure 6.29: Comparison of the Λ d
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Figure 6.31: Comparison of the cos(
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Figure 6.34: Comparison of the esti
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The optimal Λ cut for all dark mat
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Figure 6.40: Sensitivity to neutrin
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6.7 Comparison with 2007-2008 analy
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mass of 200 GeV and a cross-section
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Chapter 7ConclusionsThe limits pres
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Bibliography[1] Volders, L. M. J. S
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[22] S. Burles et al., “Big bang
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[46] G. Debrassi, S. Heinemeyer, W.
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[74] C. Hettlage, K. Mannheim, and
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[102] D. Heck and J. Knapp, “Fors
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Mohamad-Ziad Charif - Antares

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