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ABSTRACT Accretion disc winds can leave active galactic nuclei (AGNs) and interact with the interstellar medium (ISM) of their host galaxies. We perform two-dimensional numerical simulations to investigate the interaction of AGN winds and ISM. We study the properties of outflows in the 1–1000 pc region under different gravitational potentials and ISM gas densities, and compare these ionized outflows with the observed warm absorbers (WAs). We find that AGN winds drag the ISM and transfer their momentum/energy to the ISM. The properties of winds depend on the gas density of the initial ISM. The higher the initial ISM density, the lower the wind speed, and the narrower the opening angle of the winds. For the case of ρ0 = 10−25 g cm−3, the winds have the strongest intensity at the outer boundary. They can blow the ISM gas, giving feedback on star formation and galaxy evolution. We also find that the interaction of AGN winds and ISM can generate WAs in certain conditions and AGN winds play some roles in generating WAs.
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