  The EGRET excess of diffuse Galactic gamma rays shows all the key features of
dark matter annihilation (DMA) for a WIMP mass in the range 50-100 GeV,
especially the distribution of the excess is compatible with a standard halo
profile with some additional ringlike substructures at 4 and 13 kpc from the
Galactic centre. These substructures coincide with the gravitational potential
well expected from the ring of dust at 4 kpc and the tidal stream of dark
matter from the Canis Major satellite galaxy at 13 kpc, as deduced from N-body
simulations fitting to the Monoceros ring of stars. Strong independent support
for this substructure is given by the gas flaring in our Galaxy.
  The gamma rays from DMA are originating predominantly from the hadronization
of mono-energetic quarks, which should produce also a small, but known fraction
of protons and antiprotons. Bergstrom et al. an antiproton flux far above the
observed antiproton flux and they conclude that the DMA interpretation of the
EGRET excess can therefore be excluded. However, they used an isotropic
propagation model, i.e. the same diffusive propagation in the disk and the
halo. It is shown that an anisotropic propagation model is consistent with the
EGRET gamma ray excess, the antiproton flux and the ratios of secondary/primary
and unstable/stable cosmic ray particles. Such an anisotropic propagation is
supported by the large bulge/disk ratio of the positron annihilation line, as
observed by the INTEGRAL satellite. In this case no need for new sources
specific to the bulge are needed, so the claimed evidence for strong DMA in the
bulge from these observations is strongly propagation model dependent.
