Recent studies by a number of independent collaborations , have correlated the CMB temperatures measured by the WMAP satellite with different galaxy surveys that trace the matter distribution with light from the whole range of the electromagnetic spectrum : radio , far-infrared , optical and X-ray surveys .
The new data systematically finds positive correlations , indicating a rapid slow down in the growth of structure in the universe .
Individual cross-correlation measurements are of low significance , but we show that combining data at different redshifts introduces important new constraints .
Contrary to what happens at low redshifts , for a fixed \Omega _ { m } , the higher the dark energy contend , \Omega _ { \Lambda } , the lower the ISW cross-correlation amplitude .
At 68 % confidence level , the data finds new independent evidence of dark energy : \Omega _ { \Lambda } = 0.42 - 1.22 .
It also confirms , to higher significance , the presence of a large dark matter component : \Omega _ { m } = 0.18 - 0.34 , exceeding the density of baryonic matter , but far from the critical value .
Combining these new constraints with the prior of a flat universe , or the prior of an accelerating universe provides strong new evidence for a dark cosmos .
Combination with supernova data yields \Omega _ { \Lambda } = 0.71 \pm 0.13 , \Omega _ { m } = 0.29 \pm 0.04 .
If we also assume a flat universe , we find \Omega _ { \Lambda } = 0.70 \pm 0.05 and w = -1.02 \pm 0.17 for a constant dark energy equation of state .