Left: merger fractions in MIR AGNs and non-AGNs for the SDSS and GAMA sample. We also divide the GAMA sample into three redshift bins. Right: merger fractions in OPT AGNs and non-AGNs for the SDSS and GAMA sample. We also divide the GAMA sample into two redshift bins. Errors are calculated through binomial statistics. Bottom panels: ratio of merger fraction in AGNs relative to that in non-AGNs (i.e., merger excess) for the main sample and a stricter merger identification threshold. The dashed lines indicate the excess value of one, which means no difference in the merger fraction in AGNs relative to non-AGNs. Again, we find a qualitatively consistent picture between the SDSS and GAMA samples in which the merger fraction is higher in AGNs compared to non-AGNs.