median of the difference between $\rm \theta_{rec}$ and $\rm \theta_{nu}$, $\rm \tilde{\alpha} = med[\mid\theta_{rec}-\theta_{nu}\mid]$. $\rm \Lambda Fit$ yields a median angular resolution $\rm 6^{\circ} > \tilde{\alpha} > 0.5^{\circ}$ for the primary neutrino energy range $\rm 100\,GeV < E_{\nu} < 10\,TeV$, whilst $\rm QFit$ reaches a $\rm 5.5^{\circ} > \tilde{\alpha} > 3.8^{\circ}$ for $\rm 15\,GeV < E_{\nu} < 1\,TeV$.

Both reconstruction algorithms are used in the search and the one with the best performance in a given energy range is selected to obtain the best possible limits in that range.

![Median angular resolution, $\rm \tilde{\alpha}$ ($^{\circ}$), on the muon neutrino direction, for the complete 12 line configuration of the detector. The performances for $\rm QFit$ (dashed line) and $\rm \Lambda Fit$ (solid line) are illustrated, as is the kinematic counterpart (dotted line), the median angle between the primary neutrino and the outgoing muon at the vertex of interaction. For $\rm QFit$, $\rm \tilde{\alpha}$ is defined as the median resolution on the zenith angles $\rm \theta_{rec,nu}$ (see text for details).[]{data-label="angresfig"}](./AngRes_12Line_2012_woBBFitM_wKinematic_New_New.eps){width="0.8\linewidth"}

Signal and background simulation {#simulation}
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The energy spectrum of muon neutrinos arriving at the Earth’s surface from WIMP self-annihilation occurring in the GC’s vicinity is computed using Ref. [@cirelli]. The muon 