Fig. 8.
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Marginalized constraints on log|fR0| and the galaxy bias of CMASS when using CMB observations and the full 3 × 2 pt observables (blue) or only the galaxy and CMB lensing auto power spectra (red). It can be seen that adding the galaxy–CMB lensing cross-correlation reduces the degeneracy between the two parameters. Those contours correspond to the 68th and 95th percentiles of the posterior samples.
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