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 (<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. Ausführliche Beschreibung

Gespeichert in:

Autor*in:	Ashraf Ayubinia [verfasserIn] Yongquan Xue [verfasserIn] Jong-Hak Woo [verfasserIn] Huynh Anh Nguyen Le [verfasserIn] Zhicheng He [verfasserIn] Halime Miraghaei [verfasserIn] Xiaozhi Lin [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2022

Schlagwörter:	active galactic nuclei supermassive black holes kinematics and dynamics kinematics and dynamics

Übergeordnetes Werk:	In: Universe - MDPI AG, 2015, 8(2022), 11, p 559
Übergeordnetes Werk:	volume:8 ; year:2022 ; number:11, p 559

Links:	Link aufrufen Link aufrufen Link aufrufen Journal toc

DOI / URN:	10.3390/universe8110559

Katalog-ID:	DOAJ085791784

Internformat


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520			\|a 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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700	0		\|a Xiaozhi Lin \|e verfasserin \|4 aut
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allfields	10.3390/universe8110559 doi (DE-627)DOAJ085791784 (DE-599)DOAJb50d376f7f12433290e1290efc223069 DE-627 ger DE-627 rakwb eng QC793-793.5 Ashraf Ayubinia verfasserin aut Exploring the Fundamental Mechanism in Driving Highest-Velocity Ionized Outflows in Radio AGNs 2022 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier 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. active galactic nuclei supermassive black holes kinematics and dynamics kinematics and dynamics Elementary particle physics Yongquan Xue verfasserin aut Jong-Hak Woo verfasserin aut Huynh Anh Nguyen Le verfasserin aut Zhicheng He verfasserin aut Halime Miraghaei verfasserin aut Xiaozhi Lin verfasserin aut In Universe MDPI AG, 2015 8(2022), 11, p 559 (DE-627)820684236 (DE-600)2813994-X 22181997 nnns volume:8 year:2022 number:11, p 559 https://doi.org/10.3390/universe8110559 kostenfrei https://doaj.org/article/b50d376f7f12433290e1290efc223069 kostenfrei https://www.mdpi.com/2218-1997/8/11/559 kostenfrei https://doaj.org/toc/2218-1997 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2005 GBV_ILN_2009 GBV_ILN_2014 GBV_ILN_2055 GBV_ILN_2111 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 8 2022 11, p 559
spelling	10.3390/universe8110559 doi (DE-627)DOAJ085791784 (DE-599)DOAJb50d376f7f12433290e1290efc223069 DE-627 ger DE-627 rakwb eng QC793-793.5 Ashraf Ayubinia verfasserin aut Exploring the Fundamental Mechanism in Driving Highest-Velocity Ionized Outflows in Radio AGNs 2022 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier 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. active galactic nuclei supermassive black holes kinematics and dynamics kinematics and dynamics Elementary particle physics Yongquan Xue verfasserin aut Jong-Hak Woo verfasserin aut Huynh Anh Nguyen Le verfasserin aut Zhicheng He verfasserin aut Halime Miraghaei verfasserin aut Xiaozhi Lin verfasserin aut In Universe MDPI AG, 2015 8(2022), 11, p 559 (DE-627)820684236 (DE-600)2813994-X 22181997 nnns volume:8 year:2022 number:11, p 559 https://doi.org/10.3390/universe8110559 kostenfrei https://doaj.org/article/b50d376f7f12433290e1290efc223069 kostenfrei https://www.mdpi.com/2218-1997/8/11/559 kostenfrei https://doaj.org/toc/2218-1997 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2005 GBV_ILN_2009 GBV_ILN_2014 GBV_ILN_2055 GBV_ILN_2111 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 8 2022 11, p 559
allfields_unstemmed	10.3390/universe8110559 doi (DE-627)DOAJ085791784 (DE-599)DOAJb50d376f7f12433290e1290efc223069 DE-627 ger DE-627 rakwb eng QC793-793.5 Ashraf Ayubinia verfasserin aut Exploring the Fundamental Mechanism in Driving Highest-Velocity Ionized Outflows in Radio AGNs 2022 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier 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. active galactic nuclei supermassive black holes kinematics and dynamics kinematics and dynamics Elementary particle physics Yongquan Xue verfasserin aut Jong-Hak Woo verfasserin aut Huynh Anh Nguyen Le verfasserin aut Zhicheng He verfasserin aut Halime Miraghaei verfasserin aut Xiaozhi Lin verfasserin aut In Universe MDPI AG, 2015 8(2022), 11, p 559 (DE-627)820684236 (DE-600)2813994-X 22181997 nnns volume:8 year:2022 number:11, p 559 https://doi.org/10.3390/universe8110559 kostenfrei https://doaj.org/article/b50d376f7f12433290e1290efc223069 kostenfrei https://www.mdpi.com/2218-1997/8/11/559 kostenfrei https://doaj.org/toc/2218-1997 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2005 GBV_ILN_2009 GBV_ILN_2014 GBV_ILN_2055 GBV_ILN_2111 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 8 2022 11, p 559
allfieldsGer	10.3390/universe8110559 doi (DE-627)DOAJ085791784 (DE-599)DOAJb50d376f7f12433290e1290efc223069 DE-627 ger DE-627 rakwb eng QC793-793.5 Ashraf Ayubinia verfasserin aut Exploring the Fundamental Mechanism in Driving Highest-Velocity Ionized Outflows in Radio AGNs 2022 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier 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. active galactic nuclei supermassive black holes kinematics and dynamics kinematics and dynamics Elementary particle physics Yongquan Xue verfasserin aut Jong-Hak Woo verfasserin aut Huynh Anh Nguyen Le verfasserin aut Zhicheng He verfasserin aut Halime Miraghaei verfasserin aut Xiaozhi Lin verfasserin aut In Universe MDPI AG, 2015 8(2022), 11, p 559 (DE-627)820684236 (DE-600)2813994-X 22181997 nnns volume:8 year:2022 number:11, p 559 https://doi.org/10.3390/universe8110559 kostenfrei https://doaj.org/article/b50d376f7f12433290e1290efc223069 kostenfrei https://www.mdpi.com/2218-1997/8/11/559 kostenfrei https://doaj.org/toc/2218-1997 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2005 GBV_ILN_2009 GBV_ILN_2014 GBV_ILN_2055 GBV_ILN_2111 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 8 2022 11, p 559
allfieldsSound	10.3390/universe8110559 doi (DE-627)DOAJ085791784 (DE-599)DOAJb50d376f7f12433290e1290efc223069 DE-627 ger DE-627 rakwb eng QC793-793.5 Ashraf Ayubinia verfasserin aut Exploring the Fundamental Mechanism in Driving Highest-Velocity Ionized Outflows in Radio AGNs 2022 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier 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. active galactic nuclei supermassive black holes kinematics and dynamics kinematics and dynamics Elementary particle physics Yongquan Xue verfasserin aut Jong-Hak Woo verfasserin aut Huynh Anh Nguyen Le verfasserin aut Zhicheng He verfasserin aut Halime Miraghaei verfasserin aut Xiaozhi Lin verfasserin aut In Universe MDPI AG, 2015 8(2022), 11, p 559 (DE-627)820684236 (DE-600)2813994-X 22181997 nnns volume:8 year:2022 number:11, p 559 https://doi.org/10.3390/universe8110559 kostenfrei https://doaj.org/article/b50d376f7f12433290e1290efc223069 kostenfrei https://www.mdpi.com/2218-1997/8/11/559 kostenfrei https://doaj.org/toc/2218-1997 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2005 GBV_ILN_2009 GBV_ILN_2014 GBV_ILN_2055 GBV_ILN_2111 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 8 2022 11, p 559
language	English
source	In Universe 8(2022), 11, p 559 volume:8 year:2022 number:11, p 559
sourceStr	In Universe 8(2022), 11, p 559 volume:8 year:2022 number:11, p 559
format_phy_str_mv	Article
institution	findex.gbv.de
topic_facet	active galactic nuclei supermassive black holes kinematics and dynamics kinematics and dynamics Elementary particle physics
isfreeaccess_bool	true
container_title	Universe
authorswithroles_txt_mv	Ashraf Ayubinia @@aut@@ Yongquan Xue @@aut@@ Jong-Hak Woo @@aut@@ Huynh Anh Nguyen Le @@aut@@ Zhicheng He @@aut@@ Halime Miraghaei @@aut@@ Xiaozhi Lin @@aut@@
publishDateDaySort_date	2022-01-01T00:00:00Z
hierarchy_top_id	820684236
id	DOAJ085791784
language_de	englisch
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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. 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callnumber-first	Q - Science
author	Ashraf Ayubinia
spellingShingle	Ashraf Ayubinia misc QC793-793.5 misc active galactic nuclei misc supermassive black holes misc kinematics and dynamics kinematics and dynamics misc Elementary particle physics Exploring the Fundamental Mechanism in Driving Highest-Velocity Ionized Outflows in Radio AGNs
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topic_title	QC793-793.5 Exploring the Fundamental Mechanism in Driving Highest-Velocity Ionized Outflows in Radio AGNs active galactic nuclei supermassive black holes kinematics and dynamics kinematics and dynamics
topic	misc QC793-793.5 misc active galactic nuclei misc supermassive black holes misc kinematics and dynamics kinematics and dynamics misc Elementary particle physics
topic_unstemmed	misc QC793-793.5 misc active galactic nuclei misc supermassive black holes misc kinematics and dynamics kinematics and dynamics misc Elementary particle physics
topic_browse	misc QC793-793.5 misc active galactic nuclei misc supermassive black holes misc kinematics and dynamics kinematics and dynamics misc Elementary particle physics
format_facet	Elektronische Aufsätze Aufsätze Elektronische Ressource
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title	Exploring the Fundamental Mechanism in Driving Highest-Velocity Ionized Outflows in Radio AGNs
ctrlnum	(DE-627)DOAJ085791784 (DE-599)DOAJb50d376f7f12433290e1290efc223069
title_full	Exploring the Fundamental Mechanism in Driving Highest-Velocity Ionized Outflows in Radio AGNs
author_sort	Ashraf Ayubinia
journal	Universe
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author_browse	Ashraf Ayubinia Yongquan Xue Jong-Hak Woo Huynh Anh Nguyen Le Zhicheng He Halime Miraghaei Xiaozhi Lin
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author-letter	Ashraf Ayubinia
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title_sort	exploring the fundamental mechanism in driving highest-velocity ionized outflows in radio agns
callnumber	QC793-793.5
title_auth	Exploring the Fundamental Mechanism in Driving Highest-Velocity Ionized Outflows in Radio AGNs
abstract	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.
abstractGer	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.
abstract_unstemmed	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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container_issue	11, p 559
title_short	Exploring the Fundamental Mechanism in Driving Highest-Velocity Ionized Outflows in Radio AGNs
url	https://doi.org/10.3390/universe8110559 https://doaj.org/article/b50d376f7f12433290e1290efc223069 https://www.mdpi.com/2218-1997/8/11/559 https://doaj.org/toc/2218-1997
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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. 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Exploring the Fundamental Mechanism in Driving Highest-Velocity Ionized Outflows in Radio AGNs

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