Ionization cone: Difference between revisions
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{{Short description|Astronomical phenomenon}} |
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{{underlinked|date=November 2012}} |
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[[File:Circinus.galaxy.750pix.jpg|alt=The Circinus Galaxy, a type II Seyfert galaxy in which an ionization cone has been observed|thumb|200x200px|The [[Circinus Galaxy]], a type II Seyfert galaxy a type II Seyfert galaxy in which an ionization cone has been observed.]]'''Ionization cones''' are cones of [[Ionization|ionized material]] extending from [[Active galactic nucleus|active galactic nuclei]], predominantly observed in type II [[Seyfert galaxy|Seyfert galaxies]]. They are detected through their emission of [[electromagnetic radiation]] in the visible and infrared parts of the [[Electromagnetic spectrum|spectrum]]. The main method of observation is through [[Astronomical spectroscopy|spectroscopy]], using [[spectral line]] analysis to measure the shape of the ionized region and the condition of the material such as temperature, density, composition, and degree of ionization. |
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{{Orphan|date=March 2011}} |
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== Characteristics == |
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'''Ionisation cones''' are cones of material extending out from [[spiral galaxy|spiral galaxies]]. They are visible because of their emissions which are believed to be from re-emission of photons produced by nuclear activity within the galaxy itself.<ref>[http://www.springerlink.com/content/j4276u12119nr290/ Paper by Wilson on the properties of such cones]</ref><ref>[http://www.springerlink.com/content/j4276u12119nr290/ Paper proposing a model for Ionisation cone operation]</ref> |
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=== Shape=== |
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There is not yet a scientific consensus on the mechanics of such cones. |
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Ionization cones have a distinct [[Cone|conical]] shape, with the galactic center at the apex. Galaxies with ionization cones are thought to have a dense [[Torus|torus-like]] structure surrounding the central [[Supermassive black hole|black hole]], co-planar with the [[accretion disk]].<ref>{{Cite web |title=University of Maryland - Introductory Astronomy: Seyfert Galaxies |url=https://www.astro.umd.edu/resources/introastro/seyfert.html |access-date=2023-01-03 |website=www.astro.umd.edu}}</ref> The material in this torus, consisting of [[Interstellar medium|interstellar gas]] and dust, obstructs the photons coming from the inner area around the black hole and prevents ionization of the galactic matter outside the torus.<ref name=":1">{{Cite journal |last=Wilson |first=Andrew S. |date=1996-01-01 |title=Ionization cones |url=https://dx.doi.org/10.1016/0083-6656%2895%2900102-6 |journal=Vistas in Astronomy |series=Proceedings of the Oxford Torus Workshop |language=en |volume=40 |issue=1 |pages=63–70 |doi=10.1016/0083-6656(95)00102-6 |bibcode=1996VA.....40...63W |issn=0083-6656}}</ref> Along the [[symmetry axis]], however, the density of interstellar matter is much lower, allowing for ionization. [[Radiation pressure]] then forces this matter away from the center, resulting in a cone of ionized material.<ref name=":7">{{Cite web |title=Seyfert Galaxies: A Review - Stephen J. Curran |url=https://ned.ipac.caltech.edu/level5/Curran/Curran4.html |access-date=2022-10-30 |website=ned.ipac.caltech.edu}}</ref> |
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=== Orientation with respect to the galactic plane === |
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There is no [[scientific consensus]] yet for the [[Orientation (geometry)|orientation]] of ionization cones with respect to the [[galactic plane]] ([[galactic disc]]),<ref name=":8" /> however, ionization cones usually align with [[Astronomical radio source|radio sources]] near the [[Active galactic nucleus|galactic nucleus]].<ref name=":0">{{Cite web |last=Wilson |first=A. S. |date=October 26, 1993 |title=IONIZATION CONES AND RADIO EJECTA IN ACTIVE GALAXIES |url=https://articles.adsabs.harvard.edu/pdf/1994AJ....107.1227W |access-date=28 October 2022 |website=}}</ref> |
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The two large ionization cones in the type II Seyfert galaxy [[NGC 5252]] align with a radio source 10 [[Parsec|kiloparsecs]] ({{Abbr|approx.|approximately}} 32.6 [[Light-year|kly]]) from the galactic nucleus instead of the nucleus itself.<ref name=":0" /> In [[NGC 5728]], its 1.8 [[Parsec|kiloparsec]] ({{Abbr|approx.|approximately}} 5.9 [[Light-year|kly]]) long ionization cone aligns within 3 degrees of a radio source near its nucleus.<ref>{{Cite journal |last=Wilson |first=A. S. |title=The Ionization Cones in the Seyfert Galaxy NGC 5728 |date=September 27, 1993 |journal=The Astrophysical Journal |volume=419 |pages=L61 |doi=10.1086/187137 |bibcode=1993ApJ...419L..61W |doi-access=free }}</ref> Conversely, in [[Messier 77]], the ionization cone's alignment is thought to be influenced by factors such as central radio sources and the torus angle, yet it aligns closely with the radio emissions in the vicinity of the nucleus.{{citation needed|date=January 2023}} The explanation for deviations from the galactic plane tend to focus on the complex interactions of the torus material with both the inflowing gas and dust in the accretion disk and the gas and radiation being pushed outward by the action of the central black hole. In the process of forming the shape of the ionization cone and containing its ionized material away from the interstellar medium, these interactions may lead to possible deviations from a co-planar alignment with the accretion disk and the galactic plane.{{citation needed|date=January 2023}} |
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=== X-ray emission === |
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Using soft X-ray spectroscopy performed with the [[Chandra X-ray Observatory]], [[Plasma (physics)|plasma]] in [[Markarian galaxies|Markarian 3]] photoionized from collision with the [[interstellar medium]] was observed to emit almost no [[X-ray|X-rays]]. Markarian 3 is known to have a bi-conical ionization cone, indicating high ionization activity, yet the spectroscopy results indicate that ionization cones usually do not emit significant quantities of X-rays.<ref name=":6" /> |
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== Mechanics of formation == |
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{{galaxy-stub}} |
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{{Importance section |date=January 2023}} |
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[[ko:이온화 원뿔]] |
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=== Ionization of matter === |
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The [[accretion disk]] of the [[Supermassive black hole|galactic black hole]]'s [[radiation]] is [[Collimated beam|aligned]] with the obscuring torus.<ref name=":9">{{Cite journal |last=Durré |first=Mark |date=October 9, 2018 |title=The AGN Ionization Cones of NGC 5728. I. Excitation and Nuclear Structure |journal=The Astrophysical Journal |volume=867 |issue=2 |page=149 |doi=10.3847/1538-4357/aae68e |arxiv=1810.03258 |bibcode=2018ApJ...867..149D |s2cid=117916655 |doi-access=free }}</ref> Usually, [[ultraviolet]] or [[extreme ultraviolet]] radiation [[Photoionization|ionizes]] the nearby interstellar medium, enlarging the ionization cone.<ref name=":10">{{Cite journal |last=Dopita |first=M. A. |date=1997-02-01 |title=A Hypersonic Entrainment Model for the Ionization Cones of NGC1068 |url=https://doi.org/10.1023/A:1000596604962 |journal=Astrophysics and Space Science |language=en |volume=248 |issue=1 |pages=93–104 |doi=10.1023/A:1000596604962 |bibcode=1997Ap&SS.248...93D |s2cid=116923412 |issn=1572-946X}}</ref><ref name=":8">{{Cite web |title=Resolving the obscuring torus in NGC 1068 with the power of infrared interferometry: revealing the inner funnel of dust |url=https://academic.oup.com/mnras/article/394/3/1325/1065996 |access-date=2022-10-30 |website=academic.oup.com}}</ref> For example, [[Messier 77]] has an ionization cone produced from the [[Hypersonic speed|hypersonic]] collision of [[ejecta]] from its galactic nucleus with material in the [[interstellar medium]] of the galaxy. This collision produces [[extreme ultraviolet]] photons. These photons ionize the colliding material through photoionization.<ref name=":10" /> |
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{{Importance section |date=January 2023}} |
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=== Infrared emission and obscuring tori === |
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Ionization cones tend to emit [[Infrared|infrared light]]. Infrared emissions can be used to explain the properties of ionization cones. For example, [[Torus|tori]] that obscure the nuclei of [[Seyfert galaxy|Seyfert galaxies]] may have an effect on the [[photoionization]] by [[ultraviolet]] [[Photon|photons]] of the material found in an ionization cone. This can be determined with infrared emissions as the infrared emissions of ionization cones are not affected by the ionization of the matter in the cone. For example, the ionization cone in [[Messier 77]] has the same symmetry in [[Light|visible light]] and in infrared light, showing there is no impact of the torus on the ionization cone.<ref name=":8" /> |
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== Examples == |
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In line with the prevalence of Seyfert galaxies, ionization cones are thought to be present only in a small fraction of galaxies.<ref name=":7" /> |
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The [[Circinus Galaxy]], which is the closest Seyfert type II galaxy to the [[Milky Way]],<ref name=":4">{{Cite journal |last1=Maiolino |first1=R. |last2=Krabbe |first2=A. |last3=Thatte |first3=N. |last4=Genzel |first4=R. |date=February 1998 |title=Seyfert Activity and Nuclear Star Formation in the Circinus Galaxy |journal=The Astrophysical Journal |volume=493 |issue=2 |pages=650–665 |doi=10.1086/305150 |arxiv=astro-ph/9709091 |bibcode=1998ApJ...493..650M |s2cid=16365899 |issn=0004-637X}}</ref> has been observed to have a large, prominent ionization cone.<ref <ref name="Marconi-1994">{{cite journal |last1=Marconi |first1=A. |last2=Moorwood |first2=A.F.M. |last3=Origla |first3=L. |last4=Oliva |first4=E. |title=A Prominent Ionization Cone and Starburst Ring in the Nearby Circinus Galaxy |journal=The Messenger |date=December 1994 |volume=78 |pages=20–24 |url=https://www.eso.org/sci/publications/messenger/archive/no.78-dec94/messenger-no78-20-24.pdf |access-date=8 November 2022 |language=en |bibcode=1994Msngr..78...20M}}</ref> [[Messier 77]]'s ionization cone was produced from the [[Hypersonic speed|hypersonic]] collision of [[ejecta]] from its galactic nucleus with material in the [[interstellar medium]] of the galaxy. This collision produced [[extreme ultraviolet]] photons which then ionized the colliding material which is highly visible in an [[emission spectrum]]. The Seyfert galaxies [[Markarian 348]] (type II) and [[Markarian galaxies|Markarian 3]] (disputed type II, possible type I) have very intense [[Bicone|inverse bi-conical]] ionization cones.<ref name=":6">{{Cite journal |last=Sako |first=Masao |date=October 26, 2000 |title=The Chandra High-Energy Transmission Grating Observation of an X-Ray Ionization Cone in Markarian 3 |journal=The Astrophysical Journal |url=https://iopscience.iop.org/article/10.1086/317282/fulltext/ |access-date=2022-10-30 |volume=543 |issue=2 |doi=10.1086/317282|arxiv=astro-ph/0009323 |bibcode=2000ApJ...543L.115S |s2cid=14379913 }}</ref><ref>{{Cite journal |last=Simpson |first=Chris |date=November 3, 1995 |title=An Ionization Cone and Dusty Disk in Markarian 348: The Obscuring Torus Revealed? |journal=The Astrophysical Journal |volume=457 |doi=10.1086/309886 |s2cid=120411865 |doi-access=free }}</ref> |
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=== In X-ray binaries === |
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Although ionization cones have to date been observed mostly in Seyfert galaxies, they are not exclusive to active galactic nuclei. The [[X-ray binary]] LMC-X1 contains an ionization cone similar to those found in galactic nuclei.<ref>{{Cite journal |last=Cooke |first=R. |date=November 1, 2008 |title=Ionization Cone in the X-Ray Binary LMC X-1 |journal=The Astrophysical Journal |volume=687 |issue=1 |pages=L29–L32 |doi=10.1086/593169 |arxiv=0809.2140 |bibcode=2008ApJ...687L..29C |s2cid=14270518 |url=https://iopscience.iop.org/article/10.1086/593169/fulltext/23048.text.html |access-date=October 29, 2022}}</ref> As X-ray binary systems have comparable X-ray [[power density]] to active galactic nuclei, they have the ability to generate similar ionization cones, although the scale of the regions differ by many orders of magnitude.<ref>{{Cite journal |last=Edelson |first=Rick |date=November 4, 1998 |title=A Cutoff in the X-Ray Fluctuation Power Density Spectrum of the Seyfert 1 Galaxy NGC 3516 |journal=The Astrophysical Journal |volume=514 |issue=2 |pages=682–690 |doi=10.1086/306980 |hdl=2060/19990064013 |s2cid=16666296 |doi-access=free |hdl-access=free }}</ref> |
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== Significance == |
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The study of ionization cones has been used to support the existence of a Seyfert flare event that is thought to have occurred in the [[Milky Way]] several million years ago. [[Interstellar cloud|Interstellar clouds]] at the Milky Way's [[Galactic Pole|galactic poles]] have been observed to be highly ionized, which could indicate a period of high activity in the [[Galactic Center]] that sent pockets of ionized gas outside of the Milky Way's [[Galactic Bulge|central bulge]].<ref>{{Cite journal |last=Bland-Hawthorn |first=Joss |date=October 15, 2019 |title=The Large-scale Ionization Cones in the Galaxy |journal=The Astrophysical Journal |volume=886 |issue=1 |page=45 |doi=10.3847/1538-4357/ab44c8 |arxiv=1910.02225 |bibcode=2019ApJ...886...45B |s2cid=203837628 |doi-access=free }}</ref> |
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== See also == |
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* [[Active galactic nucleus]] |
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* [[Seyfert galaxy]] |
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Latest revision as of 08:10, 4 January 2024
Ionization cones are cones of ionized material extending from active galactic nuclei, predominantly observed in type II Seyfert galaxies. They are detected through their emission of electromagnetic radiation in the visible and infrared parts of the spectrum. The main method of observation is through spectroscopy, using spectral line analysis to measure the shape of the ionized region and the condition of the material such as temperature, density, composition, and degree of ionization.
Characteristics
[edit]Shape
[edit]Ionization cones have a distinct conical shape, with the galactic center at the apex. Galaxies with ionization cones are thought to have a dense torus-like structure surrounding the central black hole, co-planar with the accretion disk.[1] The material in this torus, consisting of interstellar gas and dust, obstructs the photons coming from the inner area around the black hole and prevents ionization of the galactic matter outside the torus.[2] Along the symmetry axis, however, the density of interstellar matter is much lower, allowing for ionization. Radiation pressure then forces this matter away from the center, resulting in a cone of ionized material.[3]
Orientation with respect to the galactic plane
[edit]There is no scientific consensus yet for the orientation of ionization cones with respect to the galactic plane (galactic disc),[4] however, ionization cones usually align with radio sources near the galactic nucleus.[5]
The two large ionization cones in the type II Seyfert galaxy NGC 5252 align with a radio source 10 kiloparsecs (approx. 32.6 kly) from the galactic nucleus instead of the nucleus itself.[5] In NGC 5728, its 1.8 kiloparsec (approx. 5.9 kly) long ionization cone aligns within 3 degrees of a radio source near its nucleus.[6] Conversely, in Messier 77, the ionization cone's alignment is thought to be influenced by factors such as central radio sources and the torus angle, yet it aligns closely with the radio emissions in the vicinity of the nucleus.[citation needed] The explanation for deviations from the galactic plane tend to focus on the complex interactions of the torus material with both the inflowing gas and dust in the accretion disk and the gas and radiation being pushed outward by the action of the central black hole. In the process of forming the shape of the ionization cone and containing its ionized material away from the interstellar medium, these interactions may lead to possible deviations from a co-planar alignment with the accretion disk and the galactic plane.[citation needed]
X-ray emission
[edit]Using soft X-ray spectroscopy performed with the Chandra X-ray Observatory, plasma in Markarian 3 photoionized from collision with the interstellar medium was observed to emit almost no X-rays. Markarian 3 is known to have a bi-conical ionization cone, indicating high ionization activity, yet the spectroscopy results indicate that ionization cones usually do not emit significant quantities of X-rays.[7]
Mechanics of formation
[edit] | This section may contain information not important or relevant to the article's subject. (January 2023) |
Ionization of matter
[edit]The accretion disk of the galactic black hole's radiation is aligned with the obscuring torus.[8] Usually, ultraviolet or extreme ultraviolet radiation ionizes the nearby interstellar medium, enlarging the ionization cone.[9][4] For example, Messier 77 has an ionization cone produced from the hypersonic collision of ejecta from its galactic nucleus with material in the interstellar medium of the galaxy. This collision produces extreme ultraviolet photons. These photons ionize the colliding material through photoionization.[9]
| This section may contain information not important or relevant to the article's subject. (January 2023) |
Infrared emission and obscuring tori
[edit]Ionization cones tend to emit infrared light. Infrared emissions can be used to explain the properties of ionization cones. For example, tori that obscure the nuclei of Seyfert galaxies may have an effect on the photoionization by ultraviolet photons of the material found in an ionization cone. This can be determined with infrared emissions as the infrared emissions of ionization cones are not affected by the ionization of the matter in the cone. For example, the ionization cone in Messier 77 has the same symmetry in visible light and in infrared light, showing there is no impact of the torus on the ionization cone.[4]
Examples
[edit]In line with the prevalence of Seyfert galaxies, ionization cones are thought to be present only in a small fraction of galaxies.[3]
The Circinus Galaxy, which is the closest Seyfert type II galaxy to the Milky Way,[10] has been observed to have a large, prominent ionization cone.[11] Messier 77's ionization cone was produced from the hypersonic collision of ejecta from its galactic nucleus with material in the interstellar medium of the galaxy. This collision produced extreme ultraviolet photons which then ionized the colliding material which is highly visible in an emission spectrum. The Seyfert galaxies Markarian 348 (type II) and Markarian 3 (disputed type II, possible type I) have very intense inverse bi-conical ionization cones.[7][12]
In X-ray binaries
[edit]Although ionization cones have to date been observed mostly in Seyfert galaxies, they are not exclusive to active galactic nuclei. The X-ray binary LMC-X1 contains an ionization cone similar to those found in galactic nuclei.[13] As X-ray binary systems have comparable X-ray power density to active galactic nuclei, they have the ability to generate similar ionization cones, although the scale of the regions differ by many orders of magnitude.[14]
Significance
[edit]The study of ionization cones has been used to support the existence of a Seyfert flare event that is thought to have occurred in the Milky Way several million years ago. Interstellar clouds at the Milky Way's galactic poles have been observed to be highly ionized, which could indicate a period of high activity in the Galactic Center that sent pockets of ionized gas outside of the Milky Way's central bulge.[15]
See also
[edit]References
[edit]- ^ "University of Maryland - Introductory Astronomy: Seyfert Galaxies". www.astro.umd.edu. Retrieved 2023-01-03.
- ^ Wilson, Andrew S. (1996-01-01). "Ionization cones". Vistas in Astronomy. Proceedings of the Oxford Torus Workshop. 40 (1): 63–70. Bibcode:1996VA.....40...63W. doi:10.1016/0083-6656(95)00102-6. ISSN 0083-6656.
- ^ a b "Seyfert Galaxies: A Review - Stephen J. Curran". ned.ipac.caltech.edu. Retrieved 2022-10-30.
- ^ a b c "Resolving the obscuring torus in NGC 1068 with the power of infrared interferometry: revealing the inner funnel of dust". academic.oup.com. Retrieved 2022-10-30.
- ^ a b Wilson, A. S. (October 26, 1993). "IONIZATION CONES AND RADIO EJECTA IN ACTIVE GALAXIES". Retrieved 28 October 2022.
- ^ Wilson, A. S. (September 27, 1993). "The Ionization Cones in the Seyfert Galaxy NGC 5728". The Astrophysical Journal. 419: L61. Bibcode:1993ApJ...419L..61W. doi:10.1086/187137.
- ^ a b Sako, Masao (October 26, 2000). "The Chandra High-Energy Transmission Grating Observation of an X-Ray Ionization Cone in Markarian 3". The Astrophysical Journal. 543 (2). arXiv:astro-ph/0009323. Bibcode:2000ApJ...543L.115S. doi:10.1086/317282. S2CID 14379913. Retrieved 2022-10-30.
- ^ Durré, Mark (October 9, 2018). "The AGN Ionization Cones of NGC 5728. I. Excitation and Nuclear Structure". The Astrophysical Journal. 867 (2): 149. arXiv:1810.03258. Bibcode:2018ApJ...867..149D. doi:10.3847/1538-4357/aae68e. S2CID 117916655.
- ^ a b Dopita, M. A. (1997-02-01). "A Hypersonic Entrainment Model for the Ionization Cones of NGC1068". Astrophysics and Space Science. 248 (1): 93–104. Bibcode:1997Ap&SS.248...93D. doi:10.1023/A:1000596604962. ISSN 1572-946X. S2CID 116923412.
- ^ Maiolino, R.; Krabbe, A.; Thatte, N.; Genzel, R. (February 1998). "Seyfert Activity and Nuclear Star Formation in the Circinus Galaxy". The Astrophysical Journal. 493 (2): 650–665. arXiv:astro-ph/9709091. Bibcode:1998ApJ...493..650M. doi:10.1086/305150. ISSN 0004-637X. S2CID 16365899.
- ^ Marconi, A.; Moorwood, A.F.M.; Origla, L.; Oliva, E. (December 1994). "A Prominent Ionization Cone and Starburst Ring in the Nearby Circinus Galaxy" (PDF). The Messenger. 78: 20–24. Bibcode:1994Msngr..78...20M. Retrieved 8 November 2022.
- ^ Simpson, Chris (November 3, 1995). "An Ionization Cone and Dusty Disk in Markarian 348: The Obscuring Torus Revealed?". The Astrophysical Journal. 457. doi:10.1086/309886. S2CID 120411865.
- ^ Cooke, R. (November 1, 2008). "Ionization Cone in the X-Ray Binary LMC X-1". The Astrophysical Journal. 687 (1): L29 – L32. arXiv:0809.2140. Bibcode:2008ApJ...687L..29C. doi:10.1086/593169. S2CID 14270518. Retrieved October 29, 2022.
- ^ Edelson, Rick (November 4, 1998). "A Cutoff in the X-Ray Fluctuation Power Density Spectrum of the Seyfert 1 Galaxy NGC 3516". The Astrophysical Journal. 514 (2): 682–690. doi:10.1086/306980. hdl:2060/19990064013. S2CID 16666296.
- ^ Bland-Hawthorn, Joss (October 15, 2019). "The Large-scale Ionization Cones in the Galaxy". The Astrophysical Journal. 886 (1): 45. arXiv:1910.02225. Bibcode:2019ApJ...886...45B. doi:10.3847/1538-4357/ab44c8. S2CID 203837628.