including sample incompleteness, the determination of length of lens redshift bin, and the choice of lens redshift shells, in order to verify their effect on the cosmological constraints.** Firstly, based on the flat $\Lambda$CDM with the full sample ($N=390$ lenses), we now estimate the systematic errors due to statistical sample incompleteness, which could directly affect the reconstructed function of the observable $\mathcal{D}_{\rm
obs}$. Fig. 7 shows the precision of the $\Omega_m$ parameter assessment as a function of SGL sample size and Table 2 shows more detailed results. One can see that, even with 50 SGL systems one can effectively place stringent fits on the matter density in the Universe ($\Delta \Omega_m \sim 0.05$), which furthermore strengthens the probative power of our method to inspire new observing programs or theoretical work in the moderate future. **Secondly, after identifying the constraints on $\Omega_m$ obtained with the minimum acceptable $\Delta z_l=0.02$ and the errors that it introduced, we should consider different values of $\Delta z_l$ for examining the role $\Delta z_l$ plays in cosmological constraints. It should be noted that the selected length of lens redshift $\Delta z_l$ not only directly determines the selection of simulated lensing systems, but also introduces systematical uncertainties 