Fig. B.2.
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Joint posterior distributions of the kSZ and tSZ amplitudes at ℓ = 3000 with the amplitude of the tSZxCIB correlations at the same multipole, ξ. In all the results presented, the cosmology is free to vary, and different methods are used to model the contribution of the SZ effects to the observed small-scale temperature power spectrum of the CMB.
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