Mohamad-Ziad Charif - Antares

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Figure 2.2: Comparison of the measured rotation curve of NGC-3198[5] as afunction of the radial distance from its galactic center with the expected curvefrom visible matter, from a dark halo, and the sum of the two distributions.baryonic matter still separated, it was shown that independently of any assumptionon the laws of gravity that the gravitational potential of the cluster tracedthe overall shape of the merging clusters and not that of the baryonic component.This proved that the mass peak is not located with the baryonic mass but witha dark halo combining the two clusters. Additionally about 87.5% of the massbeing invisible and the remaining 12.5% being baryonic. These two studies alsoheavily favors a particle component to dark matter as opposed to modified laws ofgravity[12] as a solution to the missing mass.2.1.4 Velocity Dispersions of galaxies & Mass to light ratioThe velocity dispersion σ, is the dispersion range(statistical) of velocities aboutthe mean velocity for objects bound gravitationally such as stars in a galaxy orgalaxies in a galaxies cluster. The mass to light ratio is the ratio between the massof a specific volume and its luminosity denoted ϒ. ϒ is an extremely well knownobservable for objects such as stars and other astrophysical objects. One wouldexpect when making measurements of entire galaxies to find a ratio that is theaverage of the ratio of the luminous objects located inside.Measurements of velocity dispersion σ and ϒ in spiral and elliptical galaxies[13]again showing a missing large mass component[13, 14]. These studies showedthat the velocity dispersion can not be explained by means of the visible massdistribution found in galaxy clusters[14]. Thus indicating that more than 5 times8
Figure 2.3: Diagram on the apparent and real path of light around a massive object.that of the visible mass being located in a dark halo surrounding the clusters.Additionally the measurement of the mass to light ratio showed that the value ismuch larger than the average of the individual components indicating again thatthere is at least 3 times more invisible matter than visible.2.1.5 Cosmic microwave backgroundThe Cosmic Microwave Background (CMB) is thermal radiation (∼ 2.725K) thatpermeates with a high degree of uniformity the observable universe. The CMBwas first theorized in 1948 as the thermal residual of the big bang and its detectionwas delayed until 1964. Since that several experiments were built to measurethe CMB radiation such as COBE experiment[15], WMAP[16] (figure 2.4), andPLANCK[17].While CMB is not in itself evidence for dark matter, it validates the ΛCDM model(section 2.1.6 ) which predicts the existence of dark matter. The model is furthervalidated by other measurement such as the Baryon acoustic oscillations[18],distance measurements by type Ia supernovae[19], and the Lymann-alpha forestmeasurements[20] (Figure 2.5).2.1.6 ΛCDM modelThe ΛCDM model is referred to as the Standard Model of cosmology, the modelis built on solutions to Einstein equation of General Relativity (eq 2.1)Where:R µν − R 2 g µν − Λg µν = 8πT µν (2.1)9
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 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 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
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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
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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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