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 [ ] 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 ( [ ] ) , 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 .