Mohamad-Ziad Charif - Antares

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Figure 3.1: The neutral current (NC), charged current (CC) and total cross sectionof neutrinos (left) and anti-neutrinos (right), with matter as a function of theneutrino energy.ν µ + N/P → ν µ + Xν τ + N/P → ν τ + XHowever, since the NC cross-section is about an order of magnitude lower thanthe CC cross-section, the most significant signature of a neutrino comes from thelatter. Since the nuclear interaction length is less than one meter, we would expectthe hadronic shower signature to dissipate before having a chance to be detectedif it was produced far from our apparatus, henceforth the accompanying leptonoffers a higher chance for detection inside a medium such as water.We would expect a charged particle (our corresponding lepton) with relativisticspeeds to dissipate its energy in several ways:3.1.1 Bremsstrahlung radiationBremsstrahlung radiation is an electromagnetic radiation emitted by a chargedparticle when it decelerates under the influence of the electrical field of anothercharged particle (Figure 3.2 ). In this case the first particle would be our leptonand the second the atomic nucleus of the matter of our environment (ex: water).However, its contribution to the total energy dissipated [87] depends on the massof the lepton or implicitly on its flavor, it depends on γ 6 or γ 4 as seen in eq 3.3& 3.4 (γ is the Lorentz factor) and we have γ ∼ m −1 . So we can see that thismradiation is more important for an electron than for a muon or a tau. µm e∼ 200m τm µ∼ 17 so the Bremsstrahlung contribution to a muon who has the same energyas an electron would be between 9 and 13 orders of magnitude lower.34
Figure 3.2: The process of production of a Bremsstrahlung radiation.The total power P emitted depends on whether the charged particle is beingaccelerated (a) in the same direction of its velocity or perpendicular to it. But italso depends on the charge q of the particle as well.P a||v = q2 a 2 γ 66πε 0 c 3 (3.3)P a⊥v = q2 a 2 γ 46πε 0 c 3 (3.4)3.1.2 Medium ionizationA charged particle traveling through matter would interacts with the electrons ofthe medium. This interaction if energetic enough can lead to the ionization of theatoms and henceforth a loss of energy (eq 3.5) of the traveling particle.− dEdx = 4π nz 2 ( e2) 2 [ ( 2me c 2 β 2 ) ]m e c 2 β 2 log4πε 0 I (1 − β 2 − β 2)35(3.5)
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 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 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 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
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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
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Chapter 6Dark Matter search in the
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Figure 6.1: . True Position of the
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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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