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.
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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.