  The recent results from the PAMELA, ATIC, FERMI and HESS experiments have
focused attention on the possible existence of high energy cosmic ray e^+ e^-
that may originate from dark matter (DM) annihilations or decays in the Milky
Way.
  Here we examine the morphology of the gamma-ray emission after propagation of
the electrons generated by both annihilating and decaying dark matter models.
We focus on photon energies of 1 GeV, 10 GeV, 50 GeV (relevant for the FERMI
satellite) and consider different propagation parameters. Our main conclusion
is that distinguishing annihilating from decaying dark matter may only be
possible if the propagation parameters correspond to the most optimistic
diffusion models. In addition, we point to examples where morphology can lead
to an erroneous interpretation of the source injection energy.
