  We discuss the gamma-ray signal from dark matter annihilation in our Galaxy
and in external objects, namely the Large Magellanic Cloud, the Andromeda
Galaxy (M31) and M87. We derive predictions for the fluxes in a low energy
realization of the Minimal Supersymmetric Standard Model and compare them with
current data from EGRET, CANGAROO-II and HEGRA and with the capabilities of
new-generation satellite-borne experiments, like GLAST, and ground-based
Cerenkov telescopes, like VERITAS. We find fluxes below the level required to
explain the possible indications of a gamma-ray excess shown by CANGAROO-II
(toward the Galactic Center) and HEGRA (from M87). As far as future experiments
are concerned, we show that only the signal from the galactic center could be
accessible to both satellite-borne experiments and to ACTs, even though this
requires very steep dark matter density profiles.
