| Summary: | We investigate the ionized gas kinematics relationship with X-ray, radio and accreting properties using a sample of 348 nearby (<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>z</mi><mo><</mo><mn>0.4</mn></mrow></semantics></math></inline-formula>) SDSS-FIRST-X-ray detected AGNs. X-ray properties of our sample are obtained from <i>XMM-Newton</i>, <i>Swift</i> and <i>Chandra</i> observations. We unveil the ionized gas outflows in our sample manifested by the non-gravitational broad component in [O <span style="font-variant: small-caps;">iii</span>]λ5007Å emission line profiles. From the comparison of the correlation of non-parametric outflow velocities (i.e., the velocity width, the maximal velocity of outflow and line dispersion) with X-ray luminosity and radio luminosity, we find that outflow velocities have similarly positive correlations with both X-ray and radio luminosity. After correcting for the gravitational component, we find that the [O <span style="font-variant: small-caps;">iii</span>] velocity dispersion normalized by stellar mass also increases with both X-ray luminosity and radio luminosity. We also find that, for a given X-ray (radio) luminosity, radio (X-ray) luminous AGNs have higher outflow velocities than non-radio (non-X-ray) luminous AGNs. Therefore, we find no clear preference between X-ray luminosity and radio luminosity in driving high-velocity ionized outflows and conclude that both AGN activity and small-scale jets contribute comparably. Moreover, there is no evidence that our obscured AGNs are preferentially associated with higher velocity outflows. Finally, we find a turning point around log<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mo>(</mo><msub><mi mathvariant="sans-serif">λ</mi><mrow><mi>E</mi><mi>d</mi><mi>d</mi></mrow></msub><mo>)</mo><mo>≃</mo><mo>−</mo><mn>1.3</mn></mrow></semantics></math></inline-formula> when we explore the dependency of outflow velocity on Eddington ratio. It can be interpreted considering the role of high radiation pressure (log<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mo>(</mo><msub><mi mathvariant="sans-serif">λ</mi><mrow><mi>E</mi><mi>d</mi><mi>d</mi></mrow></msub><mo>)</mo><mo>≳</mo><mo>−</mo><mn>1.3</mn></mrow></semantics></math></inline-formula>) in causing drastic reduction in the covering factor of the circumnuclear materials.
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