assumption that a cumulative probability of $90\%$ is considered strong evidence against the model, we demonstrate that with 390 well-observed galactic strong lensing systems, one can expect the matter density parameter to be estimated with the precision of $\Delta \Omega_m
\sim 0.015$.

Now one issue which should be discussed is the comparison of our cosmological results with those of earlier studies done using alternative probes. First of all, based on the Planck temperature data combined with Planck lensing, Planck Collaboration XIII (2015) gave the best-fit parameters: $\Omega_m=0.308\pm0.012$ and $H_0=67.8\pm0.9$ (at 68.3% confidence level). More recently, the best-fit values of the cosmological parameters in the flat $\Lambda$CDM model were obtained as: ${\Omega_m}=0.255\pm0.030$ and $H_0=70.4\pm2.5 \; \rm{kms}^{-1} \; \rm{Mpc}^{-1}$, based on the latest observations of 41 Hubble parameter $H(z)$ at different redshifts, which were determined from the radial BAO size method and the differential ages of passively evolving galaxies [@Aghanim]. Let us note that the matter density parameter inferred from CMB and OHD data are highly dependent on the value of the Hubble constant. Considering the well known strong degeneracy between $\Omega_m$ and $H_0$. Therefore independent measurement of $\Omega_m$ from strong lensing statistics, with the precision comparable to *Planck* observations of the 