Fig. 6.
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Marginalized posterior of log|fR0| using observations of CMB temperature and polarization, and the 3 × 2 pt observables (CMB lensing, galaxy distribution, and their cross-correlation). The CMB observations including the CMB lensing auto power spectrum are always modeled using MGCLASS, while the galaxy power spectra and the galaxy–CMB lensing cross-correlations are modeled with ReACT (red) or MGCLASS (black).
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