# Investigating the Correlation of Outflow Kinematics with Radio Activity. Gas Outflows in AGNs. VII

**Authors:** Ashraf Ayubinia, Jong-Hak Woo, Suvendu Rakshit, Donghoon Son  
**arXiv:** [2306.12692](https://arxiv.org/abs/2306.12692)  
**Date:** 2023-06-22  
**Summary page:** https://www.summarizepaper.com/en/paper/2306.12692v1/

## Key points

- The study investigates the relationship between ionized gas outflows and radio activity in active galactic nuclei (AGNs)
- Approximately 6,000 AGNs at redshifts below 0.4 were analyzed using kinematic measurements and radio detection
- Different binary subclasses based on radio properties were used to quantify radio activity
- No significant difference was found in the normalized [O III] velocity dispersion for different binary subclasses after correcting for gravitational potential
- A significant difference in [O III] kinematics was observed between high and low radio-Eddington ratio AGNs
- A notable difference in ionized gas kinematics was observed between high and low bolometric-Eddington ratio AGNs
- Accretion rate is likely the primary factor driving ionized gas outflows, while radio activity may play a secondary role
- The study contributes valuable insights into how ionized gas outflows are affected by accretion rate and radio activity in AGNs

## Summary

In this study, the authors investigate the relationship between ionized gas outflows and radio activity in active galactic nuclei (AGNs). They analyze a sample of approximately 6,000 AGNs at redshifts below 0.4, using kinematic measurements based on the [O III] line profile and radio detection from the VLA FIRST Survey. To quantify radio activity, they divide their sample into several binary subclasses based on different radio properties such as radio-luminous/radio-weak, AGN-dominated/star-formation-contaminated, compact/extended and radio-loud/radio-quiet. The authors find that none of these binary subclasses show a significant difference in the normalized [O III] velocity dispersion at a given [O III] luminosity after correcting for the influence of the host galaxy's gravitational potential. However, when examining high and low radio-Eddington ratio AGNs (L$_{1.4 GHz}$/L$_{Edd}$), they detect a significant difference in [O III] kinematics. On the other hand, they observe an impressive difference in ionized gas kinematics between high and low bolometric-Eddington ratio AGNs. This suggests that accretion rate is likely to be the primary factor driving ionized gas outflows while radio activity may play a secondary role by providing additional influence on gas kinematics. Overall, this study provides valuable insights into how ionized gas outflows are affected by both accretion rate and radio activity in AGNs. By analyzing a large sample of AGNs and considering various binary subclasses based on their radio properties, the authors contribute to our understanding of these complex astrophysical processes.