Mohamad-Ziad Charif - Antares

Figure 6.40: Sensitivity to neutrino flux coming from dark matter annihilationinside the Sun as a function of WIMP mass and the annihilation channel for theAAFit analysis.6.6 Comparison of AAFit & BBFit sensitivitiesComparing the sensitivities is straightforward as we can see in figure 6.41. Thefirst remark we can make is that there is more difference among the sensitivitiesobtained with AAFit, for example the ratio of 50 GeV and 1000 GeV WIMPSsensitivities for b + b − τ + τ − and W + W − are 2.147 × 10 4 , 4.521 × 10 3 & 7.252 ×10 2 respectively. While for BBFit they are 1.032 × 10 3 , 5.943 × 10 2 & 1.378 ×10 2 . So it seem AAFit favors heavier and harder dark matter models while BBFit(combined) favors lighter and softer dark matter models. Additionally this can beseen by the fact that while AAFit has a better angular resolution than BBFit (figure6.39) BBFit combined analysis outperforms AAFit for WIMP masses up to 350GeV for the soft spectrum, but for both the two hard spectra (τ + τ − & W + W − )AAFit start to outperforms BBFit around 130 GeV WIMP mass.Finally, as we can not combine the sensitivities as they are produced using thesame data sample, a different strategy can be employed by selecting the BBFitsensitivities for the soft spectrum below 350 GeV and AAFit for larger masses,and for the hard spectra we select BBFit for WIMP masses below 100 GeV andAAFit above that mass.146