Mohamad-Ziad Charif - Antares

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Figure 5.2: Annihilation spectrum for ν µ + ¯ν µ from WIMPS with masses of 1, 2,5 TeV normalized to one.Figure 5.3: Differential fluxes for the Dark Matter models shown as examples inthis paper. We use two soft models representing Mχ= (200, 1000) GeV models,and two hard τ + τ− representing Mχ= (100, 500) GeV models.78
The spectrum obtained via WIMPSIM will be used later in the 2007-2008and 2007-2010 data analysis to estimate a signal as a function of the soft/hardspectrum and the WIMP mass.5.2 Data selectionThe data that were used in the analysis is composed of the 2007-2008 silver runsgiven by the official data quality list(with quality basic >2) that includes the 3peand 10pe higher threshold of the 5,9,10, and 12 lines configuration of the detector.This results in 2692 runs, for a total livetime of 293.4 days.5.3 Reconstruction strategyThe selected reconstruction strategy for this analysis was BBFit. The output ofBBFit algorithm is stored in a ROOT file containing more then 30 variables, butin the course of this analysis only a few will be used:• tchi2 : It is the χ 2 of the Cherenkov-like fit of the event. The hits on the OMsof the track are fitted in corresponding to a Cherenkov light cone, tchi2 isa reflection of how good that fit was (after this section all references to χ 2variable refers to tchi2).• bchi2: It is the χ 2 of the bright point-like fit of the event. The hits on theOMs of the track are fitted in corresponding to a spherical light wave that areproduced by a hadronic and electromagnetic showers, bchi2 is a reflectionof how good that fit was.• nhit: Number of hits used in the fit.• nlines: Number of detector lines used in the fit.• tcosth: Cos[zenith] of the fitted track.• tphi: φ (azimuth) of the fitted track (variable is empty when the number oflines used in the fit is equal to one).The output of BBFit also holds extra variables that are not an output of the algorithmitself, but will be used nevertheless in the analysis:• prct: Cos[zenith] of the neutrino generated by Genhen.• prphi: φ of the neutrino generated by Genhen.• pre: Energy of the neutrino.79
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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
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 74 and 75: 4.2.1 Neutrino simulationFigure 4.6
Page 76 and 77: • Multiplicity range of the muon
Page 78 and 79: Chapter 5Dark Matter search in the
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
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
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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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