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In this paper we present a new black hole solution surrounded by dark matterhalo in the galactic center using the mass model of M87 and that coming fromthe Universal Rotation Curve (URC) dark matter profile representing family ofspiral 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], thenby 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 blackhole surrounded by dark matter halo. We find that, the apparent shape of theshadow beside the black hole spin $a$, it also depends on the central densityof the surrounded dark matter $\rho_0$. As a specific example we consider thegalaxy 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, ouranalyses show that the effect of dark matter on the size of the black holeshadow is almost negligible compared to the shadow size of the Kerr vacuumsolution hence the angular diameter $ 42$ $\mu$as remains almost unaltered whenthe dark matter is considered. For a small totally dark matter dominated spiralsuch as UGC 7232, we find similar effect of dark matter on the shadow imagescompared to the M87. However, in specific conditions having a core radiuscomparable to the black hole mass and dark matter with very high density, weshow 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 infuture observations as an indirect way to detect dark matter using the shadowimages.

Black Hole Surrounded by a Dark Matter Halo in the M87 Galactic Center and its Identification with Shadow Images