Mohamad-Ziad Charif - Antares

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Figure 3.31: The effective area for ν/ ¯ν with and without quality cuts in the lowenergy regime. 64
Chapter 4Monte-Carlo & DataIn this chapter the data acquisition is discussed followed by how each event isreconstructed. And then how the background is simulated.4.1 Data acquisitionThe acquisition of data[94] is divided into frames, each frame is 104 ms long.After the data are collected from the detector they are then sent to an offshorecomputing center (located in Toulon, France) where each frame is sent to a dedicatedprocessor to minimize the congestion. However, not all frames are sent butonly when the L0 hardware trigger has been triggered. L0 trigger in reality representsa threshold of 0.3 photo-electron (p.e) of a hit on the PMT, below this valuethe electrical noise of the PMT dominates the signal. If L0 is triggered then onthe offshore station a series of trigger algorithms (will be explained in 4.1.2) areapplied to the frame and if any eventis found then the frame is saved on a run file.The process continues until the size of this file reaches a size of 2 GB. Dependingon how many trigger algorithms are applied, a single run file can contain from 1hour and up to 3 hours of data.4.1.1 Optical backgroundWhile the depth of ANTARES ensures that no light coming from the Sun reachesthe detector the sea bed is not in total obscurity[95]. As previously mentionedthe decay of 40 K[96] can produce photons (eq 4.1 and 4.2) which can be detectedby ANTARES OMs. In the case of eq 4.1 the produced electron can be energeticenough to produce a Cherenkov effect in water. The average decay rate of 40 Kis stable over time and produce a constant rate of hit on the OMs of the order of65
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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
Page 17: Figure 2.6: Temporal evolution of t
Page 20 and 21: Figure 2.9: Parameter space of m 1/
Page 22 and 23: 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 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 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
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For BBFit all variables mentioned i
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Figure 6.6: The distribution of χ
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annihilation channel W + W − the
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lowering the total contribution of
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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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