Einasto [@einasto] (dot-dashed line), isothermal [@isoth] (dashed line) and a contracted NFW [@contrnfw] (dotted line).[]{data-label="sigmalimitsystfig"}](./Halos_Legend_Red.eps "fig:")]{}

Results and discussion {#results}
======================

Given the pre-selection and optimisation processes described in Section \[antares\] and \[optimisation\], a total of 369 and 401 events for the unblinded 2007-2012 data are found within an angular separation $\rm \Psi$ of $\rm 20^{\circ}$ from $\rm QFit$ and $\rm \Lambda Fit$, respectively. This angle is large enough to contain all values of the optimal angular separation $\rm \Psi$ for all WIMP masses and for each channel. Figure \[databkgfig\] shows the integrated distribution of the reconstructed event numbers as a function of their relative angular separation to the GC, $\rm \Psi$. Data are in good agreement with the expected background for both reconstruction algorithms. As no statistically significant excess is observed in the direction of the GC, upper limits on a neutrino flux can be set.

The $90$% C.L. upper limits on the $\rm \nu_{\mu}+\bar{\nu}_{\mu}$ flux at Earth, $\rm \Phi_{\nu_{\mu}+\bar{\nu}_\mu}$, are computed from the data according to Equation \[mrfeq\], where the average $90$% C.L. upper limit $\rm \bar{\mu}^{90\%}$ is replaced by the upper limit at $90$% C.L. on the number of observed events, $\rm \mu^{90\%}$. Systematic uncertainties are taken 