  The excess above 1 GeV in the energy spectrum of the diffuse Galactic gamma
radiation, measured with the EGRET experiment, can be interpreted as the
annihilation of Dark Matter (DM) particles. The DM is distributed in a halo
around the Milky Way. Considering the directionality of the gamma ray flux it
is possible to determine the halo profile. The DM within the halo has a smooth
and a clumpy component.These components can have different profiles as
suggested by N-body simulations and the data is indeed compatible with a NFW
profile for the diffuse component and a cored profile for the clumpy
component.These DM clumps can be partly destroyed by tidal forces from
interactions with stars and the gravitational potential of the Galactic
disc.This effect mainly decreases the annihilation signal from the Galactic
centre (GC). In this paper constraints on the different profiles and the
survival probability of the clumps are discussed.
