  We promote the idea of multi-component Dark Matter (DM) to explain results
from both direct and indirect detection experiments. In these models as
contribution of each DM candidate to relic abundance is summed up to meet
WMAP/Planck measurements of $\Omega_{\rm DM}$, these candidates have larger
annihilation cross-sections compared to the single-component DM models. This
results in larger $\gamma$-ray flux in indirect detection experiments of DM. We
illustrate this fact by introducing an extra scalar to the popular single real
scalar DM model. We also present detailed calculations for the vacuum stability
bounds, perturbative unitarity and triviality constraints on this model. As
direct detection experimental results still show some conflict, we kept our
options open, discussing different scenarios with different DM mass zones. In
the framework of our model we make an interesting observation: The existing
direct detection experiments like CDMS II, CoGeNT, CRESST II, XENON 100 or LUX
together with the observation of excess low energy $\gamma$-ray from Galactic
Centre and Fermi Bubble by FGST already have the capability to distinguish
between different DM halo profiles.
