Strong gravitational lensing by rotating Simpson-Visser black holes

We investigate strong field gravitational lensing by rotating Simpson-Visser black hole, which has an additional parameter (0≤ l/2M ≤1), apart from mass (M) and rotation parameter (a). A rotating Simpson-Visser metric correspond to (i) a Schwarzschild metric for $l/2M=a/2M=0$ and M ≠ 0, (ii) a Kerr metric for $l/2M=0$, $|a/2M|< 0.5$ and M ≠ 0 (iii) a rotating regular black hole metric for $|a/2M|< 0.5$, M ≠ 0 and $l/2M$ in the range $00.5$ and l/2M≠ 0. We find a decrease in the deflection angle αD and also in the ratio of the flux of the first image and all other images rmag. On the other hand, angular position θ₁ increases more slowly and photon sphere radius xₘ decreases more quickly, but angular separation s increases more rapidly, and their behaviour is similar to that of the Kerr black hole. The formalism is applied to discuss the astrophysical consequences in the supermassive black holes and find that the rotating Simpson-Visser black holes can be distinguished from the Kerr black hole via gravitational lensing. The deviation of the lensing observables Δθ₁ and $Δs$ of rotating Simpson Visser black holes from Kerr black hole for $0