Quenching level (ΔSFR compared to the main sequence SFR at the same stellar mass) of MaNGA galaxies as a function of their radio AGN luminosities (or the upper limits). The L_AGN upper limits of nondetections and are plotted as green arrows. The upper limits of non-RDAGN detections are calculated based on the star formation contribution to the total radio luminosity and are shown as blue arrows. Below the black line (3σ lower than the SFMS) are quenched galaxies. The lack of galaxies in the upper right panel indicates that almost all the hosts of luminous radio AGN are quenched. At L_AGN > 10²³ W Hz⁻¹, the fraction of radio AGN hosts that are quenched galaxies, f_quenched, increases with L_AGN from ∼50% to 100%, as shown in the upper panel. The uncertainty shown as the gray region is due to the L_AGN limits. Δlog(SFR) shows no correlation with L_AGN (Pearson correlation coefficient ρ ∼ −0.11).