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

We explore the relationship between the ionized gas outflows and radio activity using a sample of $\sim$ 6000 AGNs at z < 0.4 with the kinematical measurement based on the [O III] 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 [O III] velocity dispersion at a given [O III] luminosity once we correct for the influence of the host galaxy gravitational potential. We only detect a significant difference of [O III] kinematics between 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 kinematicsComment: 15 pages, 11 figures. Accepted for publication in Ap

Investigation of Stellar Kinematics and Ionized gas Outflows in Local [U]LIRGs

We explore properties of stellar kinematics and ionized gas in a sample of 1106 local [U]LIRGs from the AKARI telescope. We combine data from $Wide-field\ Infrared\ Survey\ Explorer$(WISE) and Sloan Digital Sky Survey (SDSS) Data Release 13 (DR13) to fit the spectral energy distribution (SED) of each source to constrain the contribution of AGN to the total IR luminosity and estimate physical parameters such as stellar mass and star-formation rate (SFR). We split our sample into AGNs and weak/non-AGNs. We find that our sample is considerably above the main sequence. The highest SFRs and stellar masses are associated with ULIRGs. We also fit the H$\beta$and H$\alpha$regions to characterize the outflows. We find that the incidence of ionized gas outflows in AGN [U]LIRGs ($\sim$72\%) is much higher than that in weak/non-AGN ones ($\sim$39\%). The AGN ULIRGs have extreme outflow velocities (up to$\sim$2300 km s$^{-1}$) and high mass outflow rates (up to$\sim 60 \solarm~yr^{-1}$). Our results suggest that starbursts are insufficient to produce such powerful outflows. We explore the correlations of SFR and specific SFR (sSFR) with ionized gas outflows. We find that AGN hosts with the highest SFRs exhibit a negative correlation between outflow velocity and sSFR. Therefore, in AGNs containing large amounts of gas, the negative feedback scenario might be suggested.Comment: 20 pages, 14 figures, accepted for publication in Ap

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

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 $\left[{\rm{O}}\,{\rm\small{III}}\right]$ 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 $\left[{\rm{O}}\,{\rm\small{III}}\right]$ velocity dispersion at a given $\left[{\rm{O}}\,{\rm\small{III}}\right]$ luminosity once we correct for the influence of the host galaxy’s gravitational potential. We only detect a significant difference in $\left[{\rm{O}}\,{\rm\small{III}}\right]$ 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

Investigation of Stellar Kinematics and Ionized Gas Outflows in Local (U)LIRGs

We explore the properties of stellar kinematics and ionized gas in a sample of 1106 local (U)LIRGs from the AKARI telescope. We combine data from Wide-field Infrared Survey Explorer and Sloan Digital Sky Survey Data Release 13 to fit the spectral energy distribution (SED) of each source to constrain the contribution of active galactic nuclei (AGNs) to the total IR luminosity and estimate physical parameters such as stellar mass and star formation rate (SFR). We split our sample into AGNs and weak/non-AGNs. We find that our sample is considerably above the main sequence. The highest SFRs and stellar masses are associated with ULIRGs. We also fit the H β and H α regions to characterize the outflows. We find that the incidence of ionized gas outflows in AGN (U)LIRGs (∼72%) is much higher than that in weak/non-AGN ones (∼39%). The AGN ULIRGs have extreme outflow velocities (up to ∼2300 km s ^−1 ) and high mass-outflow rates (up to ∼60 M _⊙ yr ^−1 ). Our results suggest that starbursts are insufficient to produce such powerful outflows. We explore the correlations of SFR and specific SFR (sSFR) with ionized gas outflows. We find that AGN hosts with the highest SFRs exhibit a negative correlation between outflow velocity and sSFR. Therefore, in AGNs containing large amounts of gas, the negative feedback scenario might be suggested

Exploring the Fundamental Mechanism in Driving Highest-Velocity Ionized Outflows in Radio AGNs

We investigate the ionized gas kinematics relationship with X-ray, radio and accreting properties using a sample of 348 nearby (z&lt;0.4) SDSS-FIRST-X-ray detected AGNs. X-ray properties of our sample are obtained from XMM-Newton, Swift and Chandra observations. We unveil the ionized gas outflows in our sample manifested by the non-gravitational broad component in [O III]lambda 5007 angstrom 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 III] 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(lambda(Edd)) similar or equal to -1.3 when we explore the dependency of outflow velocity on Eddington ratio. It can be interpreted considering the role of high radiation pressure (log(lambda(Edd)) greater than or similar to -1.3) in causing drastic reduction in the covering factor of the circumnuclear materials.Y

Exploring the Fundamental Mechanism in Driving Highest-Velocity Ionized Outflows in Radio AGNs

We investigate the ionized gas kinematics relationship with X-ray, radio and accreting properties using a sample of 348 nearby (z&lt;0.4) SDSS-FIRST-X-ray detected AGNs. X-ray properties of our sample are obtained from XMM-Newton, Swift and Chandra observations. We unveil the ionized gas outflows in our sample manifested by the non-gravitational broad component in [O iii]&lambda;5007&Aring; 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 iii] 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(&lambda;Edd)&#8771;&minus;1.3 when we explore the dependency of outflow velocity on Eddington ratio. It can be interpreted considering the role of high radiation pressure (log(&lambda;Edd)&#8819;&minus;1.3) in causing drastic reduction in the covering factor of the circumnuclear materials