New light on Dark Cosmos
  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 $\Omm$, the higher the dark energy contend, $\Ol$, the lower the ISW cross-correlation amplitude. At 68% confidence level, the data finds new independent evidence of dark energy: $\Ol =0.42-1.22$ . It also confirms, to higher significance, the presence of a large dark matter component: $\Omm =0.18-0.34$, 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 $\Ol = 0.71 \pm 0.13$, $\Omm = 0.29 \pm 0.04$. If we also assume a flat universe, we find $\Ol = 0.70 \pm 0.05$ and $w = -1.02 \pm 0.17$ for a constant dark energy equation of state. 
E.Gaztanaga (IEEC/CSIC), M.Manera (IEEC/CSIC), T.Multamaki (Nordita)