  We study, for the first time, the shadow of the supermassive black hole Sgr
A$^{*}$ at the center of the Milky Way in dark matter halos. For the Cold Dark
Matter and Scalar Field Dark Matter models considered in this work, the
apparent shape of the shadow depends upon the black hole spin $a$ and the dark
matter parameter $k$. We find that both dark matter models influence the shadow
in a similar way. The shadow is a perfect circle in the non-rotating case
($a=0$) and a deformed one in the rotating case ($a\neq0$). The size of the
shadow increases with increasing $k$ in both non-rotating and rotating cases,
while the shadow gets more and more distorted with increasing $a$ in the
rotating case. We further investigate the black hole emission rate in both dark
matter halos. We find that the emission rate decreases with increasing $k$ and
the peak of the emission shifts to lower frequency. Finally, by calculating the
angular radius of the shadow, we estimate that the dark matter halo could
influence the shadow of Sgr A$^{*}$ at a level of order of magnitude of
$10^{-3}$ $\mu$as and $10^{-5}$ $\mu$as, for CDM and SFDM, respectively. Future
astronomical instruments with high angular resolution would be able to observe
this effect and shed light on the nature of Sgr A$^{*}$. More interestingly, it
may be possible to distinguish between CDM and SFDM models given the
resolutions required differing by two orders of magnitude from each other.
