  We study the full-sky distribution of the radio emission from the stimulated
decay of axions which are assumed to compose the dark matter in the Galaxy.
Besides the constant extragalactic and CMB components, the decays are
stimulated by a Galactic radio emission with a spatial distribution that we
empirically determine from observations. We compare the diffuse emission to the
counterimages of the brightest supernovae remnants, and take into account the
effects of free-free absorption. We show that, if the dark matter halo is
described by a cuspy NFW profile, the expected signal from the Galactic center
is the strongest. Interestingly, the emission from the Galactic anti-center
provides competitive constraints that do not depend on assumptions on the
uncertain dark matter density in the inner region. Furthermore, the anti-center
of the Galaxy is the brightest spot if the Galactic dark matter density follows
a cored profile. The expected signal from stimulated decays of axions of mass
$m _{a} \sim 10 ^{-6}$ eV is within reach of the Square Kilometer Array for an
axion-photon coupling $g _{a\gamma} \gtrsim (2-3) \times 10 ^{-11}$ GeV$^{-1}$.
