  Motivated by the complex gamma-ray spectrum of the Galactic Center source now
measured over five decades in energy, we revisit the issue of the role of dark
matter annihilations in this interesting region. We reassess whether the
emission measured by the HESS collaboration could be a signature of dark matter
annihilation, and we use the {\em Fermi} LAT spectrum to model the emission
from SgrA*, using power-law spectral fits. We find that good fits are achieved
by a power law with an index $\sim 2.5-2.6$, in combination with a spectrum
similar to the one observed from pulsar population and with a spectrum from a
$\gsi10$ TeV DM annihilating to a mixture of $b{\bar b}$ and harder $\tau^+
\tau^-$ channels and with boost factors of the order of a hundred.
Alternatively, we also consider the combination of a log-parabola fit with the
DM contribution. Finally, as both the spectrum of gamma rays from the Galactic
Center and the spectrum of cosmic ray electrons exhibit a cutoff at TeV
energies, we study the dark matter fits to both data-sets. Constraining the
spectral shape of the purported dark matter signal provides a robust way of
comparing data. We find a marginal overlap only between the 99.999% C.L.
regions in parameter space.
