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We study the possibility of identifying dark matter in the galactic centerfrom the physical properties of the electromagnetic radiation emitted from aoptical-thin disk region around a static and spherically symmetric black hole.In particular, we consider two specific models for the optical-thin diskregion: a gas at rest and a gas in a radial free fall. Due to the effect ofdark matter on the spacetime geometry, we find that the dark matter canincrease or decrease the intensity of the electromagnetic flux radiationdepending on the dark matter model. To this end, we analyze two simple darkmatter models having different mass functions $\mathcal{M}(r)$, with a mattermass $M$, thickness $\Delta r_s$ along with a dark matter core radiussurrounding the black hole. In addition to that, we explore the scenario of aperfect fluid dark matter surrounding the black hole. We show that in order tohave significant effect of dark matter on the intensity of the electromagneticflux radiation, a high energy density of dark matter near the black hole isneeded. We also find that the surrounding dark matter distribution plays a keyrole on the shadow radius and the intensity of the electromagnetic fluxradiation, respectively. Finally, we have used the relation between the shadowradius and the quasinormal modes (QNMs) to compute the real part of QNMfrequencies.

Imprints of Dark Matter on Black Hole Shadows using Spherical Accretions