1.5$ TeV to compute the best $b\bar{b}$ limit. Furthermore, this evolves according to the self-annihilation channel spectrum and the WIMP mass, as described in the following Section \[results\].

[./Data\_VS\_Bkg\_Derived\_SymmErrors\_SmoothBkg.eps]{} (15,52) [$\displaystyle QFit$]{} (30,35) [$\displaystyle\Lambda Fit$]{}

[./Limit\_Phinu\_Versus\_Mwimp\_Color\_Other\_New.eps]{} (70,50)[![$90$% C.L. upper limits on the neutrino flux, $\rm \Phi_{\nu_{\mu}+\bar{\nu}_\mu}$, as a function of the WIMP mass in the range $\rm 25\,GeV < M_{WIMP} < 10\,TeV$ for the self-annihilation channels (from top to bottom) $\rm WIMP\,WIMP \rightarrow b\bar{b} (green),W^{+}W^{-} (blue),\tau^{+}\tau^{-} (red),\mu^{+}\mu^{-} (black),\nu_{\mu}\bar{\nu}_{\mu} (orange)$. The $\rm QFit$ and $\rm \Lambda Fit$ results are combined.[]{data-label="phinulimitfig"}](./Channels_Legend.eps "fig:")]{}

[./JFactor\_Psi.eps]{} (60,20)[![Distributions of the integrated J-Factor ($\rm GeV^{2} \cdot cm^{-5}$) as a function of the angular separation to the GC, $\rm \Psi$. The dark matter density profiles: a contracted NFW [@contrnfw] (dotted line), Einasto [@einasto] (dot-dashed line), NFW [@nfw] (solid line) and isothermal [@isoth] (dashed line), are compared.[]{data-label="jfactorpsi"}](./Halos_Legend.eps "fig:")]{}

[./sigmav\_Limit\_MwimpVersus\_LogScale\_New.eps]{} (70,50)[![The $90$% C.L. upper limits on the WIMP velocity averaged self-annihilation cross-section, $\rm <\sigma_{A}v>$, as a function of the WIMP mass in the range $\rm 25\,GeV < M_{WIMP} < 10\,TeV$ for the self-annihilation channels $\rm WIMP\,WIMP \rightarrow b\bar{b} (green)$, $\rm W^{+}W^{-} (blue)$, $\rm \tau^{+}\tau^{-} (red)$, $\rm \mu^{+}\mu^{-} (black)$, $\rm \nu_{\mu}\bar{\nu}_{\mu} (orange)$. The $\rm QFit$ and $\rm \Lambda Fit$ results are 