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In this paper we study the gravitational lensing effect for the Schwarzschildsolution with holonomy corrections. We use two types of approximation methodsto calculate the deflection angle, namely the weak and strong field limits. Forthe first method, we calculate the deflection angle up to the fifth order ofapproximation and show the influence of the parameter $\lambda$ (in terms ofloop quantum gravity) on it. In addition, we construct expressions for themagnification, the position of the lensed images and the time delay asfunctions of the coefficients from the deflection angle expansion. We find that$\lambda$ increases the deflection angle. In the strong field limit, we use alogarithmic approximation to compute the deflection angle. We then write fourobservables, in terms of the coefficients $b_1$, $b_2$ and $u_m$, namely: theasymptotic position approached by a set of images $\theta_{\infty}$, thedistance between the first image and the others $s$, the ratio between the fluxof the first image and the flux of all other images $r_m$, and the time delaybetween two photons $\Delta T_{2,1}$. We then use the experimental data of theblack hole Sagittarius $A^{\star}$ and calculate the observables and thecoefficients of the logarithmic expansion. We find that the parameter $\lambda$increases the deflection angle, the separation between the lensed images andthe delay time between them. In contrast, it decreases the brightness of thefirst image compared to the others.

Gravitational lens effect of a holonomy corrected Schwarzschild black hole