combined.[]{data-label="sigmalimitfig"}](./Channels_Legend.eps "fig:")]{}

![The $90$% C.L. upper limit 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 channel $\rm WIMP\,WIMP \rightarrow \tau^{+}\tau^{-}$ for ANTARES 2007-2012 (red) with $\rm QFit$ and $\rm \Lambda Fit$ results combined. This is compared to the limits from IceCube 59 2009-2010 [@icecube59] for the Virgo cluster (black), Fermi-LAT 2008-2014 [@fermilat] for the combined analysis of 15 satellite galaxies (green) and MAGIC 2011-2013 [@magic] for Segue 1 (purple), and the IceCube-DeepCore 79 2010-2011 sensitivity [@icecube79] for the GC (blue) is also shown. Interpreting observed electron/positron excesses as dark matter self-annihilations, the orange (PAMELA) and green (PAMELA, Fermi-LAT and H.E.S.S.) ellipses have been obtained [@pamelainterp]. The dashed line indicates the natural scale for which a WIMP is a thermal relic of the early Universe [@naturalscale].[]{data-label="sigmalimitothersfig"}](./sigmav_Limit_MwimpVersus_LogScale_Others_New_New.eps){width="0.8\linewidth"}

[./sigmav\_Limit\_MwimpVersus\_LogScale\_Syst\_New.eps]{} (15,15)[![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 channel $\rm WIMP\,WIMP \rightarrow \tau^{+}\tau^{-}$. The dark matter density profiles used in the $\rm <\sigma_{A}v>$ computation are NFW [@nfw] (solid line), 