Comparison between Hα properties and other emission lines. Left panel: Observed Paα vs. Hα fluxes for the subset of galaxies with both measurements. The dashed line shows the intrinsic ratio, corresponding to a temperature of T = 10⁴ K and an electron density of n_e = 10² cm⁻³ for Case B recombination (Osterbrock 1989). The dotted line corresponds to the ratio obtained assuming an E(B-V) = 0.41, which is the best fit to our data. Right panel: Comparison between the dust-corrected SFRs obtained from Hα and PAH_3.3. In both panels, cluster galaxies are shown in red, and field galaxies are shown in blue.