Mohamad-Ziad Charif - Antares

The optimal Λ cut for all dark matter models is Λ > −5.6 (with the exceptionof 50 GeV b + b − with Λ > −5.9). For Nhit max the range of this is from 50 (lighterWIMPS) to 90 (heavier WIMPs). The β cuts can be seen in figure 6.37. Not alot of variation can be seen in the value of β cuts, most dark matter models havea cut of β < 0.8 ◦ &β < 0.6 ◦ . However, the cut behaves as predicted, larger cutsbelong to lighter WIMPs and softer spectra while tighter cuts belong to heavierWIMPs and harder spectra. On a side note, 50 GeV b + b − does not converge on acut for β (value larger than 70 ◦ ). As for the ∆(Ψ) optimal cuts we present themFigure 6.37: Optimal β [ ◦ ] cuts as a function of WIMP mass and annihilationchannel.in figure 6.38, again we see larger ∆(Ψ) cuts for lighter WIMPs (3.5 ◦ ∼ 4.5 ◦ ) andtighter cuts for heavier WIMPs (1.6 ◦ ∼ 2.4 ◦ ). When these values are comparedto those who obtained with BBFit Multi-lines analysis in figure 6.11 we see thatfor the cuts obtained here are between 1 ◦ and 2 ◦ tighter. This is due to the factthat the AAFit angular resolution is better than BBFit’s angular resolution. Thisdifference can be clearly seen in figure 6.39. This result should be obvious forus, as AAFit’s reconstruction strategy is supposed to be more accurate than BBFit(better treatment of the detector and its geometry).Finally figure 6.40 shows the expected sensitivities to dark matter annihilatingin the Sun using AAFit reconstruction strategy. The values presented here areat the same order of magnitude of those obtained with BBFit combined analysis.However, a more detailed comparison will be presented in the following section.144