  We analyse the excess in the $\gamma$-ray emission from the center of our
galaxy observed by Fermi-LAT in terms of dark matter annihilation within the
scalar Higgs portal model. In particular, we include the astrophysical
uncertainties from the dark matter distribution and allow for unspecified
additional dark matter components. We demonstrate through a detailed numerical
fit that the strength and shape of the $\gamma$-ray spectrum can indeed be
described by the model in various regions of dark matter masses and couplings.
Constraints from invisible Higgs decays, direct dark matter searches, indirect
searches in dwarf galaxies and for $\gamma$-ray lines, and constraints from the
dark matter relic density reduce the parameter space to dark matter masses near
the Higgs resonance. We find two viable regions: one where the Higgs-dark
matter coupling is of ${\cal O}(10^{-2})$, and an additional dark matter
component beyond the scalar WIMP of our model is preferred, and one region
where the Higgs-dark matter coupling may be significantly smaller, but where
the scalar WIMP constitutes a significant fraction or even all of dark matter.
Both viable regions are hard to probe in future direct detection and collider
experiments.
