tokens: The best-fit relation for Type 2 AGNs from Woo et al. ( 2016 ) is also shown (dashed line). The right panel shows the distributions of the ratio of σ [O iii ] to σ * for Type 1 AGNs: double Gaussian [O iii ] (red) and single Gaussian [O iii ] (blue). We perform regression analysis after accounting for the measurement uncertainties in both σ [O iii ] and σ * . The best fit for Type 1 AGNs is shown by the solid line in Figure 4 , while for comparison, we also plotted the best fit for Type 2 AGNs from Woo et al. ( 2016 ; dashed line). Interestingly, when the wing component is present in [O iii ] (left panel), the best fit deviates from unity (dash-dotted line), having a steeper slope of 2.79 ± 0.14 for Type 1 AGNs and 1.66 ± 0.01 for Type 2 AGNs (see Woo et al. 2016 for Type 2 AGNs). However, when the wing component is absent (middle panel), the best-fit line has a slope of 1.32 ± 0.11 for Type 1 and 1.18 ± 0.01 for Type 2 AGNs much closer to the unity relation. We also present the distribution of the velocity dispersion ratio of [O iii ] to σ * (right panel in Figure 4 ). While [O iii ] fitted with a double Gaussian is much broader than stellar lines (red histogram), for many objects, [O iii ] fitted with a single Gaussian (blue histogram) is also broader than stellar lines, suggesting that an outflow signature is significantly present. Considering that [O iii ] dispersion is a combined effect of gravitational potential ( σ gr ) and nongravitational effect, e.g., outflow components ( σ non-gr ), the measured velocity dispersion can be expressed asNote that although σ total may represent a more complex nature of gas kinematics, we simply assume that the line of sight velocity distribution of gas manifests the convolution of gravitational and nongravitational components. We expect σ [O iii ] to be a factor of 1.4 larger than σ gr if σ non-gr = σ gr . Assuming σ gr = σ * , we find that an error-weighted mean ratio of σ total to σ gr is 1.0 and 2.3, respectively, for Type 1 AGNs with single Gaussian [O iii ] and double Gaussian [O iii ]. The nonlinearity of the σ [O iii ] – σ * relation suggests that the effect of the nongravitational component is significant and outflows are common phenomena in both Type 1 and Type 2 AGNs. 3.2. Outflow Fractions To study the outflow fractions, we estimated the fraction of AGNs with double Gaussian [O iii ] in the sample. In the case of Type 1 AGNs, 89% have double Gaussian [O iii ], while only 11% have single Gaussian [O iii ]. The double Gaussian [O iii ] fraction in Type 1 AGNs is a factor of 2 larger than that of Type 2 AGNs (43%). Since the mean luminosity of Type 1 AGNs is much higher than that of Type 2 AGNs, the difference of the double Gaussian [O iii ] fraction is due to the luminosity effect. In Figure 5 , we present the fraction of double Gaussian [O iii ] as a function of [O iii ] luminosity (left panel). The double Gaussian fraction steeply increases with increasing [O iii ] luminosity, from ∼20% to
ner_tags: O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O B-Model I-Model O O O O O B-Model I-Model O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Model I-Model O O O O O O O O O O O O O O O O O B-Model I-Model O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Formula I-Formula I-Formula I-Formula I-Formula O O B-Formula I-Formula I-Formula I-Formula I-Formula O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Model I-Model O O O O O O O O O O O O O O O B-Model I-Model O O O O O O O B-Model I-Model O O O O B-Model I-Model O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Model I-Model O O O O O O O O O O O O O O O O O O O B-Model I-Model O O O O O O O O O O O O O O B-Model I-Model O O O O O O O O O O O O