  We investigate the linear amplitude of mass fluctuations in the universe,
$\sigma_8$, and the present mass density parameter of the Universe,
$\Omega_\mathrm{m}$, from the statistical strong gravitational lensing. We use
the two populations of lens halos model with fixed cooling mass scale
$M_\mathrm{c}=3\times 10^{13}h^{-1}M_{\sun}$ to match the observed lensing
probabilities, and leave $\sigma_8$ or $\Omega_\mathrm{m}$ as a free parameter
to be constrained by data. Another varying parameter is the equation of state
of dark energy $\omega$, and its typical values of -1, -2/3, -1/2 and -1/3 are
investigated. We find that $\sigma_8$ is degenerate with $\Omega_\mathrm{m}$ in
a way similar to that suggested by present day cluster abundance as well as
cosmic shear lensing measurements: $\sigma_8\Omega_\mathrm{m}^{0.6}\approx
0.33$ (Bahcall & Bode\cite{bahcall03a} and references therein). However, both
$\sigma_8\leq 0.7$ and $\Omega_\mathrm{m}\leq 0.2$ can be safely ruled out, the
best value is when $\sigma_8=1.0$, $\Omega_\mathrm{m}=0.3$ and $\omega=-1$.
This result is different from that obtained by Bahcall & Bode
(\cite{bahcall03a}), who gives $\sigma_8 =0.98\pm 0.1$ and $\Omega_m =0.17\pm
0.05$. For $\sigma_8=1.0$, higher value of $\Omega_\mathrm{m}=0.35$ requires
$\omega=-2/3$ and $\Omega_\mathrm{m}=0.40$ requires $\omega=-1/2$.
