Equivalent width radial profile and the 3σ error bars of the Hα + [N II] excess or deficiency (ΔW_{Hα + [N II]}) in different RDAGN subsamples. The panels from top to bottom show the results when dividing RDAGN by jet luminosity, radio morphology, and stellar mass, respectively. The profiles of the different subsamples are shown in different colors and markers. Positive ΔW_{Hα + [N II]} represents that RDAGN have stronger emission lines and vice versa. Low-luminosity ($\overline{L_{\mathrm{AGN}}}={10}^{22}$ W Hz⁻¹), compact (< 6″), and lower mass RDAGN ($\overline{M_{\ast }}={10}^{10.5}{\mathrm{M}}_{\odot }$) contribute most to the nuclear excess. Weak emission line deficiencies are found in the outskirts of the large-size RDAGN population.