In this paper , we study the cosmological implications of the 100 square degree Weak Lensing survey ( the CFHTLS-Wide , RCS , VIRMOS-DESCART and GaBoDS surveys ) .
We combine these weak lensing data with the cosmic microwave background ( CMB ) measurements from the WMAP5 , BOOMERanG , CBI , VSA , ACBAR , the SDSS LRG matter power spectrum and the Type Ia Supernoave ( SNIa ) data with the “ Union ” compilation ( 307 sample ) , using the Markov Chain Monte Carlo method to determine the cosmological parameters , such as the equation-of-state ( EoS ) of dark energy w , the density fluctuation amplitude \sigma _ { 8 } , the total neutrino mass \sum m _ { \nu } and the parameters associated with the power spectrum of the primordial fluctuations .
Our results show that the \Lambda CDM model remains a good fit to all of these data .
In a flat universe , we obtain a tight limit on the constant EoS of dark energy , w = -0.97 \pm 0.041 ( 1 \sigma ) .
For the dynamical dark energy model with time evolving EoS parameterized as w _ { { \mathrm { de } } } ( a ) = w _ { 0 } + w _ { a } ( 1 - a ) , we find that the best-fit values are w _ { 0 } = -1.064 and w _ { a } = 0.375 , implying the mildly preference of Quintom model whose EoS gets across the cosmological constant boundary during evolution .
Regarding the total neutrino mass limit , we obtain the upper limit , \sum m _ { \nu } < 0.471 eV ( 95 \% C.L . )
within the framework of the flat \Lambda CDM model .
Due to the obvious degeneracies between the neutrino mass and the EoS of dark energy model , this upper limit will be relaxed by a factor of 2 in the framework of dynamical dark energy models .
Assuming that the primordial fluctuations are adiabatic with a power law spectrum , within the \Lambda CDM model , we find that the upper limit on the ratio of the tensor to scalar is r < 0.35 ( 95 \% C.L . )
and the inflationary models with the slope n _ { s } \geq 1 are excluded at more than 2 ~ { } \sigma confidence level .
In this paper we pay particular attention to the contribution from the weak lensing data and find that the current weak lensing data do improve the constraints on matter density \Omega _ { m } , \sigma _ { 8 } , \sum { m _ { \nu } } , and the EoS of dark energy .