The 111 and 129 GeV gamma-ray lines from annihilations in the Milky Way
  dark matter halo, dark disk and subhalos
  Recently a series of indications have been put forward suggesting the
presence of two gamma-ray lines at 110-130 GeV (centered at 111 and 129 GeV).
Signals of these lines have been observed toward the Galactic center, at some
galaxy clusters and among some of the unassociated point sources of the 2 years
Fermi catalogue. Such a combination of signals could be generated by dark
matter annihilations in the main dark matter halo, its substructures and nearby
galaxy clusters. We discuss in this work the consistency between the number of
events observed at the line energies in the sky and the predictions using
results from the Via Lactea II numerical simulation and extrapolations below
its mass resolution, taking into account that the annihilation cross-section to
the lines can be estimated from the Galactic center signal. We find that some
extrapolations to small substructures can naturally account for the point
sources signal, although the hypothesis of background only cannot be rejected.
We also study the morphology of the gamma-ray sky at the 2 lines energies,
testing different Galactic diffuse background models to account for
interstellar medium uncertainties, and different assumptions on the DM diffuse
component profile. We find from template fits that within reasonable diffuse
background uncertainties the presence of a spherical halo component is
preferred with cuspier dark matter halo profiles being preferable even from the
full sky fit. We finally check the impact of a dark disk component, suggested
by cosmological simulations that include baryons and find that thin dark disks
can not be disfavored, thus possibly accounting for the preferentially closer
to the Galactic disk distribution of the point sources lines signal.
