Interactions between the Jet and Disk Wind in Nearby Radio-intermediate Quasar III Zw 2

Ailing Wang; Tao An; Shaoguang Guo; Prashanth Mohan; Wara Chamani; Willem A. Baan; Talvikki Hovatta; Heino Falcke; Tim J. Galvin; Natasha Hurley-Walker; Sumit Jaiswal; Anne Lahteenmaki; Baoqiang Lao; Weijia Lv; Merja Tornikoski; Yingkang Zhang

doi:10.3847/1538-4357/acaf02

Interactions between the Jet and Disk Wind in Nearby Radio-intermediate Quasar III Zw 2

Ailing Wang
, Tao An^*
, Shaoguang Guo
, Prashanth Mohan
, Wara Chamani
, Willem A. Baan
, Talvikki Hovatta
, Heino Falcke
, Tim J. Galvin
, Natasha Hurley-Walker
, Sumit Jaiswal
, Anne Lahteenmaki
, Baoqiang Lao
, Weijia Lv
, Merja Tornikoski
, Yingkang Zhang

^*Corresponding author for this work

Research output: Contribution to journal › Article › Scientific › peer-review

8 Citations (Scopus)

116 Downloads (Pure)

Abstract

Disk winds and jets are ubiquitous in active galactic nuclei (AGN), and how these two components interact remains an open question. We study the radio properties of the radio-intermediate quasar III Zw 2. We detect two jet knots, J1 and J2, on parsec scales that move at a mildly apparent superluminal speed of 1.35c. Two gamma-ray flares were detected in III Zw 2 in 2009-2010, corresponding to the primary radio flare in late 2009 and the secondary radio flare in early 2010. The primary 2009 flare was found to be associated with the ejection of J2. The secondary 2010 flare occurred at a distance of similar to 0.3 pc from the central engine, probably resulting from the collision of the jet with the accretion disk wind. The variability characteristics of III Zw 2 (periodic radio flares, unstable periodicity, multiple quasiperiodic signals and the possible harmonic relations between them) can be explained by the global instabilities of the accretion disk. These instabilities originating from the outer part of the warped disk propagate inward and can lead to modulation of the accretion rate and consequent jet ejection. At the same time, the wobbling of the outer disk may also lead to oscillations of the boundary between the disk wind and the jet tunnel, resulting in changes in the jet-wind collision site. Object III Zw 2 is one of the few cases observed with jet-wind interactions, and the study in this paper is of general interest for gaining insight into the dynamic processes in the nuclear regions of AGN.

Original language	English
Article number	187
Number of pages	18
Journal	Astrophysical Journal
Volume	944
Issue number	2
DOIs	https://doi.org/10.3847/1538-4357/acaf02
Publication status	Published - 1 Feb 2023
MoE publication type	A1 Journal article-refereed

Funding

This work was supported by resources provided by the China SKA Regional Centre prototype (An et al. 2019, 2022) funded by the Ministry of Science and Technology of China (MOST; 2018YFA0404603). This research has been supported by the National SKA Program of China (2022SKA0120102). S.G. is supported by the CAS Youth Innovation Promotion Association (2021258). The authors acknowledge the use of the Astrogeo Center database maintained by L. Petrov. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This publication makes use of data obtained at the Metsähovi Radio Observatory, operated by Aalto University in Finland. This research has made use of data from the MOJAVE database that is maintained by the MOJAVE team (Lister et al. 2018). This work makes use of the Murchison Radio-astronomy Observatory, operated by CSIRO. We acknowledge the Wajarri Yamatji people as the traditional owners of the observatory site. Support for the operation of the MWA is provided by the Australian Government (NCRIS) under a contract to Curtin University, administered by Astronomy Australia Limited. We acknowledge Paul Hancock, Gemma Anderson, John Morgan, and Stefan Duchesne for their contributions to the GLEAM-X pipeline that bring great convenience to us. This research has made use of data from the OVRO 40 m monitoring program, which was supported in part by NASA grants NNX08AW31G, NNX11A043G, and NNX14AQ89G; NSF grants AST-0808050 and AST-1109911; and private funding from Caltech and the MPIfR. This research has made use of the NASA/IPAC Extragalactic Database (NED 2019), which is funded by the National Aeronautics and Space Administration and operated by the California Institute of Technology. This work was supported by resources provided by the China SKA Regional Centre prototype (An et al. , ) funded by the Ministry of Science and Technology of China (MOST; 2018YFA0404603). This research has been supported by the National SKA Program of China (2022SKA0120102). S.G. is supported by the CAS Youth Innovation Promotion Association (2021258). The authors acknowledge the use of the Astrogeo Center database maintained by L. Petrov. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This publication makes use of data obtained at the Metsähovi Radio Observatory, operated by Aalto University in Finland. This research has made use of data from the MOJAVE database that is maintained by the MOJAVE team (Lister et al. ). This work makes use of the Murchison Radio-astronomy Observatory, operated by CSIRO. We acknowledge the Wajarri Yamatji people as the traditional owners of the observatory site. Support for the operation of the MWA is provided by the Australian Government (NCRIS) under a contract to Curtin University, administered by Astronomy Australia Limited. We acknowledge Paul Hancock, Gemma Anderson, John Morgan, and Stefan Duchesne for their contributions to the GLEAM-X pipeline that bring great convenience to us. This research has made use of data from the OVRO 40 m monitoring program, which was supported in part by NASA grants NNX08AW31G, NNX11A043G, and NNX14AQ89G; NSF grants AST-0808050 and AST-1109911; and private funding from Caltech and the MPIfR. This research has made use of the NASA/IPAC Extragalactic Database (NED ), which is funded by the National Aeronautics and Space Administration and operated by the California Institute of Technology.

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10.3847/1538-4357/acaf02Licence: CC BY

Wang_2023_ApJ_944_187Final published version, 25.2 MBLicence: CC BY

Cite this

Wang, A., An, T., Guo, S., Mohan, P., Chamani, W., Baan, W. A., Hovatta, T., Falcke, H., Galvin, T. J., Hurley-Walker, N., Jaiswal, S., Lahteenmaki, A., Lao, B., Lv, W., Tornikoski, M., & Zhang, Y. (2023). Interactions between the Jet and Disk Wind in Nearby Radio-intermediate Quasar III Zw 2. Astrophysical Journal, 944(2), Article 187. https://doi.org/10.3847/1538-4357/acaf02

@article{7a4a74ac1e124089b99f06f562af895a,

title = "Interactions between the Jet and Disk Wind in Nearby Radio-intermediate Quasar III Zw 2",

abstract = "Disk winds and jets are ubiquitous in active galactic nuclei (AGN), and how these two components interact remains an open question. We study the radio properties of the radio-intermediate quasar III Zw 2. We detect two jet knots, J1 and J2, on parsec scales that move at a mildly apparent superluminal speed of 1.35c. Two gamma-ray flares were detected in III Zw 2 in 2009-2010, corresponding to the primary radio flare in late 2009 and the secondary radio flare in early 2010. The primary 2009 flare was found to be associated with the ejection of J2. The secondary 2010 flare occurred at a distance of similar to 0.3 pc from the central engine, probably resulting from the collision of the jet with the accretion disk wind. The variability characteristics of III Zw 2 (periodic radio flares, unstable periodicity, multiple quasiperiodic signals and the possible harmonic relations between them) can be explained by the global instabilities of the accretion disk. These instabilities originating from the outer part of the warped disk propagate inward and can lead to modulation of the accretion rate and consequent jet ejection. At the same time, the wobbling of the outer disk may also lead to oscillations of the boundary between the disk wind and the jet tunnel, resulting in changes in the jet-wind collision site. Object III Zw 2 is one of the few cases observed with jet-wind interactions, and the study in this paper is of general interest for gaining insight into the dynamic processes in the nuclear regions of AGN.",

author = "Ailing Wang and Tao An and Shaoguang Guo and Prashanth Mohan and Wara Chamani and Baan, \{Willem A.\} and Talvikki Hovatta and Heino Falcke and Galvin, \{Tim J.\} and Natasha Hurley-Walker and Sumit Jaiswal and Anne Lahteenmaki and Baoqiang Lao and Weijia Lv and Merja Tornikoski and Yingkang Zhang",

note = "Funding Information: This work was supported by resources provided by the China SKA Regional Centre prototype (An et al. 2019, 2022) funded by the Ministry of Science and Technology of China (MOST; 2018YFA0404603). This research has been supported by the National SKA Program of China (2022SKA0120102). S.G. is supported by the CAS Youth Innovation Promotion Association (2021258). The authors acknowledge the use of the Astrogeo Center database maintained by L. Petrov. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This publication makes use of data obtained at the Mets{\"a}hovi Radio Observatory, operated by Aalto University in Finland. This research has made use of data from the MOJAVE database that is maintained by the MOJAVE team (Lister et al. 2018). This work makes use of the Murchison Radio-astronomy Observatory, operated by CSIRO. We acknowledge the Wajarri Yamatji people as the traditional owners of the observatory site. Support for the operation of the MWA is provided by the Australian Government (NCRIS) under a contract to Curtin University, administered by Astronomy Australia Limited. We acknowledge Paul Hancock, Gemma Anderson, John Morgan, and Stefan Duchesne for their contributions to the GLEAM-X pipeline that bring great convenience to us. This research has made use of data from the OVRO 40 m monitoring program, which was supported in part by NASA grants NNX08AW31G, NNX11A043G, and NNX14AQ89G; NSF grants AST-0808050 and AST-1109911; and private funding from Caltech and the MPIfR. This research has made use of the NASA/IPAC Extragalactic Database (NED 2019), which is funded by the National Aeronautics and Space Administration and operated by the California Institute of Technology. Funding Information: This work was supported by resources provided by the China SKA Regional Centre prototype (An et al. , ) funded by the Ministry of Science and Technology of China (MOST; 2018YFA0404603). This research has been supported by the National SKA Program of China (2022SKA0120102). S.G. is supported by the CAS Youth Innovation Promotion Association (2021258). The authors acknowledge the use of the Astrogeo Center database maintained by L. Petrov. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This publication makes use of data obtained at the Mets{\"a}hovi Radio Observatory, operated by Aalto University in Finland. This research has made use of data from the MOJAVE database that is maintained by the MOJAVE team (Lister et al. ). This work makes use of the Murchison Radio-astronomy Observatory, operated by CSIRO. We acknowledge the Wajarri Yamatji people as the traditional owners of the observatory site. Support for the operation of the MWA is provided by the Australian Government (NCRIS) under a contract to Curtin University, administered by Astronomy Australia Limited. We acknowledge Paul Hancock, Gemma Anderson, John Morgan, and Stefan Duchesne for their contributions to the GLEAM-X pipeline that bring great convenience to us. This research has made use of data from the OVRO 40 m monitoring program, which was supported in part by NASA grants NNX08AW31G, NNX11A043G, and NNX14AQ89G; NSF grants AST-0808050 and AST-1109911; and private funding from Caltech and the MPIfR. This research has made use of the NASA/IPAC Extragalactic Database (NED ), which is funded by the National Aeronautics and Space Administration and operated by the California Institute of Technology. Publisher Copyright: {\textcopyright} 2023. The Author(s). Published by the American Astronomical Society.",

year = "2023",

month = feb,

day = "1",

doi = "10.3847/1538-4357/acaf02",

language = "English",

volume = "944",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "Institute of Physics Publishing",

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TY - JOUR

T1 - Interactions between the Jet and Disk Wind in Nearby Radio-intermediate Quasar III Zw 2

AU - Wang, Ailing

AU - An, Tao

AU - Guo, Shaoguang

AU - Mohan, Prashanth

AU - Chamani, Wara

AU - Baan, Willem A.

AU - Hovatta, Talvikki

AU - Falcke, Heino

AU - Galvin, Tim J.

AU - Hurley-Walker, Natasha

AU - Jaiswal, Sumit

AU - Lahteenmaki, Anne

AU - Lao, Baoqiang

AU - Lv, Weijia

AU - Tornikoski, Merja

AU - Zhang, Yingkang

N1 - Funding Information: This work was supported by resources provided by the China SKA Regional Centre prototype (An et al. 2019, 2022) funded by the Ministry of Science and Technology of China (MOST; 2018YFA0404603). This research has been supported by the National SKA Program of China (2022SKA0120102). S.G. is supported by the CAS Youth Innovation Promotion Association (2021258). The authors acknowledge the use of the Astrogeo Center database maintained by L. Petrov. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This publication makes use of data obtained at the Metsähovi Radio Observatory, operated by Aalto University in Finland. This research has made use of data from the MOJAVE database that is maintained by the MOJAVE team (Lister et al. 2018). This work makes use of the Murchison Radio-astronomy Observatory, operated by CSIRO. We acknowledge the Wajarri Yamatji people as the traditional owners of the observatory site. Support for the operation of the MWA is provided by the Australian Government (NCRIS) under a contract to Curtin University, administered by Astronomy Australia Limited. We acknowledge Paul Hancock, Gemma Anderson, John Morgan, and Stefan Duchesne for their contributions to the GLEAM-X pipeline that bring great convenience to us. This research has made use of data from the OVRO 40 m monitoring program, which was supported in part by NASA grants NNX08AW31G, NNX11A043G, and NNX14AQ89G; NSF grants AST-0808050 and AST-1109911; and private funding from Caltech and the MPIfR. This research has made use of the NASA/IPAC Extragalactic Database (NED 2019), which is funded by the National Aeronautics and Space Administration and operated by the California Institute of Technology. Funding Information: This work was supported by resources provided by the China SKA Regional Centre prototype (An et al. , ) funded by the Ministry of Science and Technology of China (MOST; 2018YFA0404603). This research has been supported by the National SKA Program of China (2022SKA0120102). S.G. is supported by the CAS Youth Innovation Promotion Association (2021258). The authors acknowledge the use of the Astrogeo Center database maintained by L. Petrov. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This publication makes use of data obtained at the Metsähovi Radio Observatory, operated by Aalto University in Finland. This research has made use of data from the MOJAVE database that is maintained by the MOJAVE team (Lister et al. ). This work makes use of the Murchison Radio-astronomy Observatory, operated by CSIRO. We acknowledge the Wajarri Yamatji people as the traditional owners of the observatory site. Support for the operation of the MWA is provided by the Australian Government (NCRIS) under a contract to Curtin University, administered by Astronomy Australia Limited. We acknowledge Paul Hancock, Gemma Anderson, John Morgan, and Stefan Duchesne for their contributions to the GLEAM-X pipeline that bring great convenience to us. This research has made use of data from the OVRO 40 m monitoring program, which was supported in part by NASA grants NNX08AW31G, NNX11A043G, and NNX14AQ89G; NSF grants AST-0808050 and AST-1109911; and private funding from Caltech and the MPIfR. This research has made use of the NASA/IPAC Extragalactic Database (NED ), which is funded by the National Aeronautics and Space Administration and operated by the California Institute of Technology. Publisher Copyright: © 2023. The Author(s). Published by the American Astronomical Society.

PY - 2023/2/1

Y1 - 2023/2/1

N2 - Disk winds and jets are ubiquitous in active galactic nuclei (AGN), and how these two components interact remains an open question. We study the radio properties of the radio-intermediate quasar III Zw 2. We detect two jet knots, J1 and J2, on parsec scales that move at a mildly apparent superluminal speed of 1.35c. Two gamma-ray flares were detected in III Zw 2 in 2009-2010, corresponding to the primary radio flare in late 2009 and the secondary radio flare in early 2010. The primary 2009 flare was found to be associated with the ejection of J2. The secondary 2010 flare occurred at a distance of similar to 0.3 pc from the central engine, probably resulting from the collision of the jet with the accretion disk wind. The variability characteristics of III Zw 2 (periodic radio flares, unstable periodicity, multiple quasiperiodic signals and the possible harmonic relations between them) can be explained by the global instabilities of the accretion disk. These instabilities originating from the outer part of the warped disk propagate inward and can lead to modulation of the accretion rate and consequent jet ejection. At the same time, the wobbling of the outer disk may also lead to oscillations of the boundary between the disk wind and the jet tunnel, resulting in changes in the jet-wind collision site. Object III Zw 2 is one of the few cases observed with jet-wind interactions, and the study in this paper is of general interest for gaining insight into the dynamic processes in the nuclear regions of AGN.

AB - Disk winds and jets are ubiquitous in active galactic nuclei (AGN), and how these two components interact remains an open question. We study the radio properties of the radio-intermediate quasar III Zw 2. We detect two jet knots, J1 and J2, on parsec scales that move at a mildly apparent superluminal speed of 1.35c. Two gamma-ray flares were detected in III Zw 2 in 2009-2010, corresponding to the primary radio flare in late 2009 and the secondary radio flare in early 2010. The primary 2009 flare was found to be associated with the ejection of J2. The secondary 2010 flare occurred at a distance of similar to 0.3 pc from the central engine, probably resulting from the collision of the jet with the accretion disk wind. The variability characteristics of III Zw 2 (periodic radio flares, unstable periodicity, multiple quasiperiodic signals and the possible harmonic relations between them) can be explained by the global instabilities of the accretion disk. These instabilities originating from the outer part of the warped disk propagate inward and can lead to modulation of the accretion rate and consequent jet ejection. At the same time, the wobbling of the outer disk may also lead to oscillations of the boundary between the disk wind and the jet tunnel, resulting in changes in the jet-wind collision site. Object III Zw 2 is one of the few cases observed with jet-wind interactions, and the study in this paper is of general interest for gaining insight into the dynamic processes in the nuclear regions of AGN.

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DO - 10.3847/1538-4357/acaf02

M3 - Article

AN - SCOPUS:85149145921

SN - 0004-637X

VL - 944

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2

M1 - 187

ER -

Interactions between the Jet and Disk Wind in Nearby Radio-intermediate Quasar III Zw 2

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Interactions between the Jet and Disk Wind in Nearby Radio-intermediate Quasar III Zw 2

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