CMB secondary anisotropies constrain the clustered fraction in unified Chaplygin gas models to f greater than or similar to 0.99, leaving little room for deviations from LambdaCDM.
Integrated Sachs Wolfe Effect and Rees Sciama Effect
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abstract
It has been around fifty years since R. K. Sachs and A. M. Wolfe predicted the existence of anisotropy in the Cosmic Microwave Background (CMB) and ten years since the integrated Sachs Wolfe effect (ISW) was first detected observationally. The ISW effect provides us with a unique probe of the accelerating expansion of the Universe. The cross-correlation between the large-scale structure and CMB has been the most promising way to extract the ISW effect from the data. In this article, we review the physics of the ISW effect and summarize recent observational results and interpretations.
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Clustered unified dark sector cosmology: Background evolution and linear perturbations in light of observations
CMB secondary anisotropies constrain the clustered fraction in unified Chaplygin gas models to f greater than or similar to 0.99, leaving little room for deviations from LambdaCDM.