Shadow and weak deflection angle of extended uncertainty principle black hole surrounded with dark matter

TL;DR

This paper explores how dark matter and extended uncertainty principle parameters influence the properties of black holes, including shadow radius, ISCO, and deflection angles, revealing minimal impact on event horizon but notable effects on orbits and light deflection.

Contribution

It provides analytic expressions for shadow radius and weak deflection angle of EUP black holes with dark matter, highlighting the influence of EUP parameters and dark matter density on observable features.

Findings

Event horizon remains unaffected by dark matter.

EUP parameters influence ISCO, photon sphere, and shadow radius.

Weak deflection angle is enhanced by EUP corrections.

Abstract

In this paper, we discuss the possible effects of dark matter on a Schwarzschild black hole with the correction of extended uncertainty principle (EUP), such as the parameter $\alpha$ and the large fundamental length scale $L_*$. In particular, we surround the EUP black hole of mass $m$ with a static spherical shell of dark matter described by the parameters mass $M$, inner radius $r_s$, and thickness $\Delta r_s$. In this study, we find that there is no deviation in the event horizon, which readily implies that the black hole temperature due to the Hawking radiation is independent of any dark matter concentration. In addition, we show some effects of the EUP parameter on the innermost stable circular orbit (ISCO) radius of time-like particles, photon sphere, shadow radius, and weak deflection angle. It is found that time-like orbits are affected by deviation of low values of mass $M$. A greater dark matter density is needed to have remarkable effects on the null orbits. Using the analytic expression for the shadow radius and the approximation $\Delta r_s>>r_s$, it is revealed that $L_*$ should not be lower than $2m$. To broaden the scope of this study, we also calculate the analytic expression for the weak deflection angle using the Ishihara et al. method \cite{Ishihara_2016}. As a result, we show that $\Delta r_s$ is improved by a factor of $(1+4\alpha m^2/L_*^2)$ due to the EUP correction parameters. The calculated shadow radius and weak deflection angle are then compared using the estimated values of the galactic mass from Sgr A*, M87, and UGC 7232, as well as the mass of the supermassive black hole at their center.