Mohamad-Ziad Charif - Antares
Mohamad-Ziad Charif - Antares Mohamad-Ziad Charif - Antares
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 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
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