Rotating charged nonsingular black holes in loop quantum gravity and their observational imprints from EHT

We study the observational signatures of charged non-singular black holes (BHs) in loop quantum gravity (LQG), focusing on their shadows and constraints from Event Horizon Telescope (EHT) data. We employ a modified Newman-Janis algorithm (MNJA) to obtain a rotating BH metric from a static LQG-corrected solution characterized by spin a, charge Q, and the LQG parameter $b_0$. The EHT observed shadows of Sgr A* and M87*, with angular diameters $d_{sh}=48.7\pm 7\mu$as and ${\theta }_d=42\pm 3\mu$as, and masses $M\sim 4\times {10}^6{M}_{\odot }$ and $6.5\times {10}^9{M}_{\odot }$, respectively. We analyze shadow observables—areal radius $R_s$, distortion ${\delta }_s$, and oblateness $D_s$—to constrain $(Q,b_0,a)$ using EHT data. For M87* ($a\sim 0.9M$), it turns out that $4.31M\le R_a\le 6.08M$, $1\le D_s\le 1.33$; for Sgr A*, $4.3M\le R_a\le 5.5M$. At ${\theta }_o={50}^{\circ }$, Sgr A* yields $1.021\le b_0\le 1.1$ and $a\in (0.05003M,0.7124M)$; whereas for M87* at ${\theta }_o={17}^{\circ }$, we find that $0.9985\le b_0\le 1.1$ and $a\in (0.04961M,0.7464M)$. The bounds on RQBH parameters obtained from the EHT results of SgrA * are more stringent than those obtained from the EHT image of M87*. We also compute the energy emission rate, revealing enhanced high-frequency emission from quantum effects. These results offer testable LQG signatures and connect quantum gravity with BH imaging, providing a framework for comparing polymerized BHs with observations. Thus, suggest that RQBHs are viable candidates for astrophysical black holes.