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We present 3D models of biconical outflows combined with a thin dust planefor investigating the physical properties of the ionized gas outflows and theireffect on the observed gas kinematics in type 2 active galactic nuclei (AGNs).Using a set of input parameters, we construct a number of models in 3D andcalculate the spatially integrated velocity and velocity dispersion for eachmodel. We find that three primary parameters, i.e., intrinsic velocity, biconeinclination, and the amount of dust extinction, mainly determine the simulatedvelocity and velocity dispersion. Velocity dispersion increases as theintrinsic velocity or the bicone inclination increases, while velocity (i.e.,velocity shifts with respect to systemic velocity) increases as the amount ofdust extinction increases. Simulated emission-line profiles well reproduce theobserved [O III] line profiles, e.g., a narrow core and a broad wingcomponents. By comparing model grids and Monte Carlo simulations with theobserved [O III] velocity-velocity dispersion (VVD) distribution of ~39,000type 2 AGNs, we constrain the intrinsic velocity of gas outflows ranging from~500 km/s to ~1000 km/s for the majority of AGNs, and up to ~1500-2000 km/s forextreme cases. The Monte Carlo simulations show that the number ratio of AGNswith negative [O III] velocity to AGNs with positive [O III] velocitycorrelates with the outflow opening angle, suggesting that outflows with higherintrinsic velocity tend to have wider opening angles. These results demonstratethe potential of our 3D models for studying the physical properties of gasoutflows, applicable to various observations, including spatially integratedand resolved gas kinematics.

The Prevalence of Gas Outflows in Type 2 AGNs. II. 3D Biconical Outflow Models