Other, less established bounds, are not included. In particular, ref. [39] finds that angular regions distinct from the one observed by FERMI and so far observed only by EGRET, provide stronger constraints. We do not use here the controversial EGRET observations. Once FERMI will present **data** corresponding to other regions, it will be easy to establish bounds with the use of our approximation described in the previous section. This is done by simply rescaling our predictions for the '10 • ÷ 20 • ' region using the new J factors for the additional (yet unknown) regions. Furthermore, we do not consider the 'WMAP haze' [40] which is a hint that a possible excess in synchrotron radiation could be due to DM. The haze has been shown to be consistent with a wide variety of DM masses and final states and therefore will not constrain the space of models compared to other measurements. It would however, be interesting to study in more detail the precise predictions for the haze for those models that can fit the rest of the data.  5 shows the χ 2 as function of the DM mass for various DM annihilation (left) or DM decay (right) modes. We find that, independently of the non-observation of an excess in thē p PAMELA data, only some leptonic modes can reproduce all data. Here HESS observations play a key role demanding that the e ± excess terminates in a sharper way than what typical of non-leptonic channels, irrespectively of the DM density profile. DM heavier than 10 TeV that annihilates or decays into light quarks still provides a reasonable fit to PAMELA and FERMI data, if fitted conservatively. However it is disfavored by the HESS e + + e − data, and presumably the photon **data** as well ( in the annihilating case).