Observed jet power and radiative efficiency of black hole candidates in the Kerr+PFDM model

Abstract In this research, we explore the electromagnetic energy emitted by astrophysical black holes within the Kerr+PFDM (Kerr + perfect fluid dark matter) spacetime, a model comprising rotating black holes surrounded by dark matter. Our investigation focuses on black holes within X-ray binary systems, namely GRS 1915+105, GRO J1655-40, XTE J1550-564, A0620-00, H1743-322, and GRS 1124-683. Our findings indicate that the Kerr+PFDM spacetime can account for the radiative efficiency of these sources as determined through the continuum-fitting method (CFM). Additionally, employing the Blandford–Znajek mechanism, we demonstrate the ability to replicate the observed jet power. By combining the outcomes of both analyses for the selected objects, we establish more rigorous constraints on the spacetime parameters. Notably, our results reveal that, similar to the Kerr spacetime, the Kerr+PFDM spacetime cannot simultaneously account for the observed jet power and radiative efficiency of GRS 1915+105.