  In this paper we present a new black hole solution surrounded by dark matter
halo in the galactic center using the mass model of M87 and that coming from
the Universal Rotation Curve (URC) dark matter profile representing family of
spiral galaxies. In both cases the DM halo density is cored with a size $r_0$
and a central density $\rho_0$: $\rho(r)= \rho_0/(1+r/r_0)(1+(r/r_0)^2)$. Since
$r_0\rho_0=120 M_{\odot}$/pc$^2$ [Donato et al., MNRAS, 397, 1169, 2009], then
by varying the central density one can reproduce the DM profile in any spiral.
Using the Newman-Jains method we extend our solution to obtain a rotating black
hole surrounded by dark matter halo. We find that, the apparent shape of the
shadow beside the black hole spin $a$, it also depends on the central density
of the surrounded dark matter $\rho_0$. As a specific example we consider the
galaxy M87, with a central density $\rho_0=6.9\,\times 10^{6}
M_{\odot}$/kpc$^3$ and a core radius $r_0=91.2$ kpc. In the case of M87, our
analyses show that the effect of dark matter on the size of the black hole
shadow is almost negligible compared to the shadow size of the Kerr vacuum
solution hence the angular diameter $ 42$ $\mu$as remains almost unaltered when
the dark matter is considered. For a small totally dark matter dominated spiral
such as UGC 7232, we find similar effect of dark matter on the shadow images
compared to the M87. However, in specific conditions having a core radius
comparable to the black hole mass and dark matter with very high density, we
show that the shadow images decreases compared to the Kerr vacuum black hole.
The effect of dark matter on the apparent shadow shape can shed some light in
future observations as an indirect way to detect dark matter using the shadow
images.
