Investigating the Correlation of Outflow Kinematics with Radio Activity. VII. Gas Outflows in AGNs
Ashraf Ayubinia, Jong-Hak Woo, Suvendu Rakshit, Donghoon Son
Abstract
Abstract We explore the relationship between the ionized gas outflows and radio activity using a sample of ∼6000 active galactic nuclei (AGNs) at z < 0.4 with the kinematical measurement based on the <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mfenced close="]" open="["> <mml:mrow> <mml:mi mathvariant="normal">O</mml:mi> <mml:mspace width="0.25em"/> <mml:mi mathsize="small" mathvariant="normal">III</mml:mi> </mml:mrow> </mml:mfenced> </mml:math> line profile and the radio detection in the VLA FIRST Survey. To quantify radio activity, we divide our sample into a series of binary subclasses based on the radio properties, i.e., radio luminous/radio weak, AGN-dominated/star-formation contaminated, compact/extended, and radio loud/radio quiet. None of the binary subclasses exhibits a significant difference in the normalized <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mfenced close="]" open="["> <mml:mrow> <mml:mi mathvariant="normal">O</mml:mi> <mml:mspace width="0.25em"/> <mml:mi mathsize="small" mathvariant="normal">III</mml:mi> </mml:mrow> </mml:mfenced> </mml:math> velocity dispersion at a given <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mfenced close="]" open="["> <mml:mrow> <mml:mi mathvariant="normal">O</mml:mi> <mml:mspace width="0.25em"/> <mml:mi mathsize="small" mathvariant="normal">III</mml:mi> </mml:mrow> </mml:mfenced> </mml:math> luminosity once we correct for the influence of the host galaxy’s gravitational potential. We only detect a significant difference in <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mfenced close="]" open="["> <mml:mrow> <mml:mi mathvariant="normal">O</mml:mi> <mml:mspace width="0.25em"/> <mml:mi mathsize="small" mathvariant="normal">III</mml:mi> </mml:mrow> </mml:mfenced> </mml:math> kinematics between the high and low radio-Eddington ratio ( L 1.4 GHz / L Edd ) AGNs. In contrast, we find a remarkable difference in ionized gas kinematics between high and low bolometric-Eddington ratio AGNs. These results suggest that accretion rate is the primary mechanism in driving ionized gas outflows, while radio activity may play a secondary role providing additional influence on gas kinematics.