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Abstract We investigate strong gravitational lensing by quantum-improved charged black holes characterized by an additional parameter denoted as ω, in addition to the mass M and charge Q. Our findings reveal that when both the parameters Q /2 M and /4M² ω / 4 M 2 increase simultaneously, various astrophysical consequences, such as the deflection angle D (u) α D (u) and angular image separation increase. Concurrently, the angular position θ ∞, relative magnification r₌₀₆ r mag, and the time delay T₂, ₁ Δ T 2, 1 between the first and second relativistic images also decrease with the growing values of the parameters Q /2 M and /4M² ω / 4 M 2. It is also observed that the Einstein ring ₁E θ 1 E for the quantum-improved charged black hole is more significant than those for Schwarzschild, quantum-improved Schwarzschild, and Reisner–Nordström black holes. As with supermassive black holes such as M87^* M 87 ∗ and SgrA^* S g r A ∗, it is observed that to be a viable astrophysical black hole, the EHT results constrain the parameter space (/4M² ω / 4 M 2, Q /2 M). Remarkably, the EHT results for SgrA^* S g r A ∗ impose more stringent limits on the parameter space of quantum-improved charged black holes compared to those established by the EHT results for M87^* M 87 ∗. We investigate the radial profiles of orbital and radial harmonic oscillation frequencies as a function of the dimensionless coupling constants and black hole mass. The main characteristics of test particle quasi-periodic oscillations close to stable circular orbits in the black hole equatorial plane are also examined. We study the positioning of resonant radii in the background of quantum-improved charged black holes for high-frequency quasi-periodic oscillations models: warped disc (WD) models, relativistic precession (RP) and its types, and epicyclic resonance (ER) and its variants.
Molla et al. (Fri,) studied this question.