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tokens: lag between the formation of the jet and the outflows. Because our analysis depends on the long-slit data with a specific P.A., the estimated size of the NLR based on [O iii ] may be underestimated if the slit is off from the outflow direction. Figure 8. Photometric size–luminosity relations for AGNs. Black and magenta dots show the measured sizes from Husemann et al. ( 2013 , 2014 ). Green dots present the results from Karouzos et al. ( 2016a ). The measured values from Bae et al. ( 2017 ) are denoted by blue dots. Our measured [O iii ] sizes are shown by red dots. In this plot, the [O iii ] luminosity is the extinction-uncorrected values. Dashed and solid lines present the slope values from linear regression of Husemann et al. ( 2014 ) and Bae et al. ( 2017 ). The flux distribution of [O iii ] is often used to define the size of the NLR. However, the extent of the photoionization region is different from that of gas outflows, as gas can be ionized by the central source while the kinematics of the ionized gas can simply follow the gravitational potential of the host galaxy without showing any outflows. Therefore, Karouzos et al. ( 2016a ) and Bae et al. ( 2017 ) measured the size of the outflows based on the [O iii ] kinematics compared to stellar kinematics instead of measuring the extent of the photoionization region. A detailed comparison between the photoionization and outflow sizes will be presented in the future (D. Kang et al. 2017, in preparation). While the outflow size measured based on the spatially resolved kinematics provides much better representation of the outflow energetics, it requires high quality data with a good spatial resolution, which are missing in our MMT observations. Future IFU observations with high S/N may overcome the limitations of our analysis based on MMT long-slit spectra. 5. Discussion and Conclusions Various studies in the literature showed the connection between gas kinematics and radio emissions. For example, Mullaney et al. ( 2013 ) reported that in AGNs with moderate radio luminosity, the radio luminosity has strong effects on the [O iii ] profile. The morphology and position angle of the radio emission and the ionized-gas emission have strong connections. In the case of the targets in which the jet and ionized-gas emissions are aligned, the radio jets may be responsible for driving outflows and shock ionization, hence driving the correlations between radio emissions and gas kinematics (e.g., Veilleux 1991 ; Bower et al. 1995 ; Zakamska Greene 2014 ). In a radio-loud AGN, 4C12.50 fast outflows in HI gas are detected with an extremely blueshifted velocity, ∼1000 km s −1 relative to the systematic velocity at the location of the southern jet. These outflows are considered as a result of the interaction between radio jet and the ISM (Morganti et al. 2013 ). By using near-infrared data, Tadhunter et al. ( 2014 ) reported the highly distorted kinematic profiles in the H 2 1-0 S(1) λ 2.128 μ m line, showing