tokens: the host galaxy potential. The average difference between AGNs and SF galaxies is 0.16 dex. Note that even among the objects with single Gaussian [O iii ], we clearly detect the systematic difference of the ratio between AGNs and SF galaxies (the average difference is 0.11 dex). 3.2. [O <sc>iii</sc>] Velocity Dispersion versus Luminosity We investigate how the [O iii ] kinematics are related to [O iii ] luminosity for AGNs and SF galaxies in Figure 5 . There is an increasing trend of σ O iii with increasing luminosity in AGNs, though the trend is very broad. The increasing trend is also present among composite objects while the the luminosity range of [O iii ] is an order of magnitude narrower. These trends show that gas outflows are stronger in AGNs with higher luminosity, indicating that AGN energetics are responsible for the outflow kinematics. In contrast, we find no clear increasing trend among SF galaxies. On average σ O iii is lower in SF galaxies, while the range of σ O iii is as broad as that of AGNs. Since the average stellar mass of AGNs and SF galaxies is very different, as we pointed out in S.2.2, we plot the same comparison after limiting stellar mass between 10 10 and 10 10.5 (bottom panels in Figure 5 ). Again, we find that AGNs and SF galaxies show different trends, suggesting that these different trends are not due to the difference in mass scales between AGN and SF galaxy samples. Figure 5. Comparison of [O iii ] velocity dispersion with [O iii ] luminosity, respectively, for AGNs (left), composite objects (middle), and SF galaxies (right), using the entire sample (top) and the stellar mass-limited sample (bottom). The colors represent the number density in each bin with Δ x = 0.03 dex and Δ y = 0.01 dex. 3.3. [O <sc>iii</sc>] Velocity–Velocity Dispersion Diagram In Figure 6 , we combine the velocity and velocity dispersion of [O iii ] to investigate the difference of gas kinematics between AGNs and SF galaxies. We find a dramatic contrast between AGNs and SF galaxies in terms of the range of gas velocities. While SF galaxies are concentrated at the lower center with a limited range of velocity shift and velocity dispersion ( σ O iii ∼150 km s −1 ), AGNs show a much larger distribution, including AGNs with extreme kinematics (i.e., and σ O iii > 400 km s −1 ). Figure 6. [O iii ] Velocity–velocity dispersion diagrams, respectively, for AGNs (left), composite objects (middle), and SF galaxies (right), using the total sample (top) and the stellar mass-limited subsample (bottom). The average σ O iii is 175.1 ± 76, 125.3 ± 49.9, and 73.2 ± 28.6 km s −1 , respectively, for AGNs, composite objects, and SF galaxies, indicating that AGNs have more than a factor of two broader [O iii ] than SF galaxies. Also, the dispersion of the σ O iii distribution is significantly different with a factor of ∼3 broader distribution in AGNs. Note that the σ O iii distribution is skewed toward high values, indicating the presence of extreme
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