5 and the spectral effects from the cosmological redshift- ing and the intrinsic variation of the emission spec- trum, as described by f$_{SUSY}$ (see Fig. 1). The lower panel of Fig. 3 shows the accumulated mean value of the specific intensity as a function of redshift. This clearly shows that the most relevant contributions come from maps up to z ∼ 2. Overall, applying the maximum boost increases the mean value of I$_{γ,}$$_{0}$ of the ReHS case by three orders of magnitude. For most energies, the f$_{SUSY}$ spectrum is monotoni- cally decreasing. In these regions, the dependence on I$_{γ,}$$_{0}$ with redshift will have the generic form shown in Fig. 3. However, at the highest energies the shape is expected to change dramatically due to the impor- tance of Internal Bremsstrahlung and/or of monochro- matic lines (see Fig. 1) close to the rest mass energy of the dark matter particle. Such an effect is clearly visible in the black dotted line in Fig. 3, which is the ReHS case for an energy of 100 GeV and features a bump in the redshift distribution, a reflection of the importance of IB at the highest energies. The angular power spectrum of the EGB is an im- portant tool to study the statistical properties of its anisotropy on the sky. In fact, certain classes of γ - ray sources are expected to exhibit different power spectra, making this a potential means to identify the origin of the unresolved EGB. In Fig. 4, we show the angular power spectrum l ( l + 1) C$_{l}$/ 2 π as a function of the multipole l , at an observed energy of E$_{γ,}$$_{0}$ = 10 GeV, for all the cases discussed in Fig. 3. At large scales, l < ∼ 10, the power spectrum is related to the clustering of dark matter eConf C091122 Figure 2: Upper panel: A partial map showing the EGB produced by dark matter annihilation in nearby structures. Only sources within 68 Mpc from the observer are considered for the map. The color scale gives a visual impression of the values of the specific gamma-ray intensity for each pixel in the map; the red color corresponds to the highest values of specific intensity. The observed energy of the simulated gamma-ray radiation is 10 GeV. Lower panel: The full gamma-ray sky map from dark matter annihilation containing sources up to z ∼ 10. In both maps only the contribution of the smallest halos resolved by the simulation ( ∼ 10 9 h − $^{1}$M ⊙ ) has been taken into account. 2009 Fermi Symposium, Washington, D.C., Nov. 2-5