  The "GeV-excess" of the diffuse gamma-rays in the halo is studied with a
template fit based on energy spectra for each possible process of gamma-ray
emission. Such a fit allows to determine the background and signal
simultaneously, so the Galactic Disk can be included in the analysis. We find
evidence that the "excess", characterised by a gamma-ray spectrum peaking at 2
GeV, is much stronger in Molecular Clouds in the disk than the "GeV-excess"
observed up to now in the halo. The possible reason why the emissivity of
Molecular Clouds peaks at 2 GeV are the energy losses and magnetic cutoffs
inside MCs, thus depleting the low energy part of the CR spectra and shifting
the maximum of the gamma-ray spectra to higher energies. This peaking of the
emissivity in Molecular Clouds at 2 GeV was clearly observed from the spectrum
of the Central Molecular Zone, which dominates the emission in the inner few
degrees of the Galactic Centre.
  Although the spectrum of the Central Molecular Zone peaks at 2 GeV, it cannot
be responsible for the "GeV-excess" observed in the halo, since the latitude
extension of the Zone is below $\rm |b|<0.5^\circ$. However, lines-of-sight
into the halo cross Molecular Clouds in the disk, so the emissivity of clouds
in the disk will be observed in the halo as an apparent "GeV-excess". The fact,
that this "GeV-excess" has the same morphology in the disk {\it and} in the
halo as the column density of Molecular Clouds, as traced by the CO map from
the Planck satellite resembling an NFW-like latitude profile, and the fact the
MCs have an emissivity peaking at 2 GeV shows that the "GeV-excess" originates
from Molecular Clouds in the disk, not from a process surrounding the Galactic
Centre.
