Subhankar Patra, Bibhas Ranjan Majhi

We investigate the transonic accretion flow in the spacetime of a supermassive black hole (BH) coupled to an anisotropic dark matter fluid, as proposed by Cardoso {\it et al}. We essentially compare the accretion properties of the Cardoso BH with those of an isolated Schwarzschild BH. The Cardoso BH is described by the halo mass ($M_{\rm H}$) and its characteristic length scale ($a_0$). Various classes of accretion solution topologies (e.g., O, A, and I-types), including the shock solutions, are obtained by solving the dynamical equations of the flow in a fully general relativistic framework. We find that the accretion solutions are substantially influenced by the halo parameters ($M_{\rm H}, a_0$) when the dark matter distribution is concentrated near the BH horizon. In this context, we also observe that various shock properties, such as the shock radius, flow density compression, and temperature compression across the shock fronts, are potentially affected by the dark halo. Interestingly, the existing shock parameter space, defined by the flow angular momentum and energy, is largely reduced for higher halo compactness compared to that of the Schwarzschild BH. Furthermore, different observational signatures of the accretion disc, like the spectral energy distribution (SED), slope of the SED, and bolometric luminosity, are found to exhibit strong deviations from the known results in the usual Schwarzschild BH model. These unique features offer a possible valuable tool for characterizing the presence or absence of a dark matter halo around a galactic BH.