Upper panel: CO(4–3) auto-power spectrum at z = 0.5. The dashed gray line shows the simulation-based auto-power spectrum P^tot(k). It is the average over the five auto-power spectra of CO(4–3) maps, each map spanning δz = 0.05. The dotted gray line shows the average shot noise component. Subtracting the shot noise yields the clustering P^clust(k) shown with the solid gray line. The clustering (Eq. (11)) is fit to P^clust at large scales only, using the red points. From this fit, the effective clustering bias in SIDES, $b_{\mathrm{eff}}^{\mathrm{fit}}$, is estimated. Lower panel: Same procedure for galaxies’ auto-power spectra and $b_{\mathrm{gal}}^{\mathrm{fit}}$, still at z = 0.5.