the signal of WIMP self-annihilation towards the GC as a function of WIMP masses $\rm 25\,GeV < M_{WIMP} < 10\,TeV$. The acceptances for the primary self-annihilation channels (from bottom to top) $\rm WIMP\,WIMP \rightarrow b\bar{b}(green),W^{+}W^{-} (blue),\tau^{+}\tau^{-} (red),\mu^{+}\mu^{-} (black),\nu_{\mu}\bar{\nu}_{\mu} (orange)$ are shown. $\rm QFit$ (dashed lines) and $\rm \Lambda Fit$ (solid lines) are compared.[]{data-label="aeffmwimpfig"}](./Channels_Legend.eps "fig:")]{} (15,55)[![Example of the acceptance $\rm \bar{A}_{eff}(M_{\rm WIMP}) \times T_{eff}$ ($\rm m^{2}\cdot yr$) to the signal of WIMP self-annihilation towards the GC as a function of WIMP masses $\rm 25\,GeV < M_{WIMP} < 10\,TeV$. The acceptances for the primary self-annihilation channels (from bottom to top) $\rm WIMP\,WIMP \rightarrow b\bar{b}(green),W^{+}W^{-} (blue),\tau^{+}\tau^{-} (red),\mu^{+}\mu^{-} (black),\nu_{\mu}\bar{\nu}_{\mu} (orange)$ are shown. $\rm QFit$ (dashed lines) and $\rm \Lambda Fit$ (solid lines) are compared.[]{data-label="aeffmwimpfig"}](./Fits_Legend.eps "fig:")]{}

where $\rm E_{\nu_{\mu}}^{th}\simeq15$ GeV is the energy threshold for neutrino detection in ANTARES, $\rm dN_{\nu_{\mu}}/dE_{\nu_{\mu}}\Big|_{\oplus}=dN_{\bar{\nu}_{\mu}}/dE_{\bar{\nu}_{\mu}}\Big|_{\oplus}$ is the energy spectrum of the neutrinos at the surface of the Earth as shown in Figure \[benchchfig\], and $\rm A_{eff}^{\nu_{\mu}/\bar{\nu}_{\mu}}$ is the effective area of ANTARES as a function of the neutrino or anti-neutrino energy for tracks coming from the direction of the GC (Figure \[aefffig\] for illustration). Due to their different cross-sections, the effective areas for neutrinos and anti-neutrinos are slightly different 