Mohamad-Ziad Charif - Antares

More documents

Recommendations

Info

Chapter 7ConclusionsThe limits presented in figure 5.32 for the 2007-2008 data analysis are not yetcompetitive with other experiments ( due to life-time ). However, they have shownthe potential to be make ANTARES competitive if we introduce improvements tothe analysis. This was done with the analysis introduced in Chapter 6. We sawthat by increasing the livetime of the data ( a natural evolution of the analysis )we immediately gain an important factor that allows us to be competitive ( BB-Fit Multi-lines analysis ). Moreover, the introduction of the single-line data setshowed us that we can further improve our sensitivities specially for light WIMPs.On the other hand the use of the AAFit reconstruction strategy also showed us thatthe sensitivities can also be improved for heavier WIMPs while sacrificing thosefor lighter ones. What we can conclude from this is that with the amelioration introducedin 2007-2010 analysis such as the increased livetime, extra optimizationvariables, and a new reconstruction strategy, can put ANTARES in a place whereit is competitive with other experiments. All of this is accomplished by using asimple analysis strategy focusing on cutting on variables and counting remainingevents. The cuts optimization also ignored ( for computational time-scale reasons) two promising variables such as Nhit ( figures 6.17 & 6.30 ) and cos(θ) ( figure6.31 ). These two variables can be used to further discriminate the dark mattersignal from the background. The problem posed by repeating the same analysisusing these two extra variables, with each yielding two cuts ( a minimum valueand a maximum value ), is that not we will be left optimizing for at least six variableswhich is an extremely time consuming process. A better way to fully usethe effects of these two variable ( and the original ones) is to do it with the helpof new methods. One is use a likelihood-ratio method. Another is to use ArtificialNeutral Networks ( tests on the 2007-2008 analysis showed an improvement ofsensitivities by 15% to 30% ).It is important to note that the work presented in this thesis shows that indirectdetection is complementary to direct detection techniques and the LHC in search152
for dark matter. Additionally ANTARES is still collecting data ( and it will upto 2015 ), henceforth finding a dark matter signal remains a possibility, speciallywith the fact that other types of analysis can be done. Analysis such as findingsignal of dark matter WIMPs annihilating in the Galactic Center, Galactic Halo,and in Dwarf galaxies.153
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 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 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
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
Page 130 and 131: Figure 6.19: The estimation of the
Page 132 and 133: Figure 6.21: Comparison of the opti
Page 134 and 135: Figure 6.23: Comparison of sensitiv
Page 136 and 137: Figure 6.25: Estimation of our back
Page 138 and 139: Figure 6.28: Comparison of the mult
Page 140 and 141: Figure 6.29: Comparison of the Λ d
Page 142 and 143: Figure 6.31: Comparison of the cos(
Page 144 and 145: Figure 6.34: Comparison of the esti
Page 146 and 147: The optimal Λ cut for all dark mat
Page 148 and 149: Figure 6.40: Sensitivity to neutrin
Page 150 and 151: 6.7 Comparison with 2007-2008 analy
Page 152 and 153: mass of 200 GeV and a cross-section
Page 156 and 157: Bibliography[1] Volders, L. M. J. S
Page 158 and 159: [22] S. Burles et al., “Big bang
Page 160 and 161: [46] G. Debrassi, S. Heinemeyer, W.
Page 162 and 163: [74] C. Hettlage, K. Mannheim, and
Page 164: [102] D. Heck and J. Knapp, “Fors
show all

Mohamad-Ziad Charif - Antares

You also want an ePaper? Increase the reach of your titles

Delete template?

Save as template?