The resolved SFE of the molecular gas, SFE_mol = Σ_SFR/Σ_mol (panels (A) and (B)); the resolved molecular-to-stellar mass fraction, ﹩{{rR}}_{\star }^{\mathrm{mol}}={{\rm{\Sigma }}}_{\mathrm{mol}}/{{\rm{\Sigma }}}_{\star }﹩ (panels (C) and (D)); and the sSFR, sSFR = Σ_SFR/Σ_⋆ (panels (E) and (F)) in radial bins of 0.3R _e (∼1.5 kpc) vs. galactocentric radius for pixels from the 30 galaxies included in Figure 6. The figure is color-coded according to the three main groups. Panels (A), (C), and (E) encompass pixels from 20 galaxies classified as SF (or with NNA; see column (5) in Table 2), split by the ΔSFMS (i.e., main sequence, green valley, and red cloud) of the host galaxy. Panels (B), (D), and (F) include pixels from 30 ACA EDGE galaxies grouped according to the nuclear activity of the host galaxy. The gray shaded areas correspond to the regions where our Hα-based SFR estimator is susceptible to AGN/LINER contamination, so SFR and related quantities are only taken as upper limits. In all panels, the vertical extent of the shaded areas is the 1σ scatter distribution for any group. Also, the vertical black dashed lines are located at r = R _e, which we use to divide galaxy regions in central and disk pixels. While efficiencies in main-sequence galaxies remain almost constant with galactocentric radius, in green valley galaxies, we note a systematic increase of SFE_mol, ﹩{{rR}}_{\star }^{\mathrm{mol}}﹩, and sSFR with increasing radius. We also observe slightly higher SFE_mol in the regions near the centers (0.5R _e ≲ r ≲ 1.2R _e) of AGNs when compared to their outskirts.