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{{Short description|Galaxy in the constellation Lepus}}
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{{Infobox galaxy|name=IRAS 05189-2524|image=File:A tale of galactic collisions.jpg|caption=[[Hubble Space Telescope]] image of IRAS 05189-2524
{{Article for deletion/dated|page=2MASX J22550681+0058396|timestamp=20240508171938|year=2024|month=May|day=8|substed=yes}}
|constellation name=[[Lepus (constellation)|Lepus]]
<!-- Once discussion is closed, please place on talk page: {{Old AfD multi|page=2MASX J22550681+0058396|date=8 May 2024|result='''keep'''}} -->
|epoch=J2000
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|ra={{RA|05|21|01.3927s}}<ref name=NED/>
{{Infobox galaxy|name=2MASX J05210136-2521450|image=File:A tale of galactic collisions.jpg|caption=[[Hubble]] image of 2MASX J05210136-2521450|constellation name=[[Lepus (constellation)|Lepus]]|ra=05h 21m 01.392s|dec=-25d 21m 45.36s|h_radial_v=12,816 [[kilometer per second|Km/s]]|dist_ly=603 [[Mly]] (185 [[Megaparsec|Mpc]])|appmag_v=15.4|type=Pec; ULIRG, Sy2|size=75,000 ly|size_v=0.46 x 0.44 arcmin|notes=[[Galaxy merger]], [[luminous infrared galaxy]]|z=0.042750|names=[[Principal Galaxies Catalogue|PGC]] 17155, [[2MASS]] J05210139-2521452, [[IRAS]] 05189-2524, AKARI J0521013-252146, MRSS 486-006230, [[NRAO VLA Sky Survey|NVSS]] J052101-252145, 1WGA J0521.0-2521, SWIFT J0521.0-2522, [[Lyon-Meudon Extragalactic Database|LEDA]] 17155}}
|dec={{DEC|-25|21|45.229}}<ref name=NED/>
|h_radial_v=12,816 [[kilometer per second|km/s]]
|dist_ly=603 [[Mly]] (185 [[Megaparsec|Mpc]])
|appmag_v=15.4
|type=Pec; ULIRG, Sy2
|size=75,000 ly
|size_v=0.46 x 0.44 arcmin
|notes=[[Galaxy merger]], [[luminous infrared galaxy]]
|z=0.042750
|names=[[Principal Galaxies Catalogue|PGC]] 17155, [[2MASS]] J05210139-2521452, AKARI J0521013-252146, MRSS 486-006230, [[NRAO VLA Sky Survey|NVSS]] J052101-252145, 1WGA J0521.0-2521, SWIFT J0521.0-2522, [[Lyon-Meudon Extragalactic Database|LEDA]] 17155, 2MASX J05210136-2521450
}}


'''2MASX J05210136-2521450''' is a type E<ref>{{Cite web |title=HyperLeda -object description |url=http://atlas.obs-hp.fr/hyperleda/ledacat.cgi?o=PGC%2017155 |access-date=2024-05-08 |website=atlas.obs-hp.fr}}</ref> [[elliptical galaxy]] located in the constellation [[Lepus (constellation)|Lepus]]. It is located 603 million [[Light-year|light-years]] away from the [[Solar System]] and has an approximate [[diameter]] of 75,000 light-years.<ref>{{Cite web |title=Your NED Search Results |url=https://ned.ipac.caltech.edu/cgi-bin/objsearch?search_type=Obj_id&objid=95978&objname=1&img_stamp=YES&hconst=73.0&omegam=0.27&omegav=0.73&corr_z=1 |access-date=2024-05-08 |website=ned.ipac.caltech.edu}}</ref>
'''IRAS 05189-2524''' is a [[galaxy merger]] located in the constellation [[Lepus (constellation)|Lepus]]. It is located 603 million [[Light-year|light-years]] away from the [[Solar System]] and has an approximate [[diameter]] of 75,000 light-years.<ref name=NED>{{Cite web |title=Your NED Search Results |url=https://ned.ipac.caltech.edu/cgi-bin/objsearch?search_type=Obj_id&objid=95978&objname=1&img_stamp=YES&hconst=73.0&omegam=0.27&omegav=0.73&corr_z=1 |access-date=2024-05-08 |website=ned.ipac.caltech.edu}}</ref>


== A luminous galaxy ==
== A luminous galaxy ==
2MASX J05210136-2521450 is classified as an [[Luminous infrared galaxy|ultraluminous infrared galaxy]],<ref>{{Cite journal |last=Sanders |first=D. B. |last2=Surace |first2=J. A. |last3=Ishida |first3=C. M. |date=1999 |editor-last=Barnes |editor-first=J. E. |editor2-last=Sanders |editor2-first=D. B. |title=Ultraluminous Infrared Galaxies |url=https://link.springer.com/chapter/10.1007/978-94-011-4665-4_73 |journal=Galaxy Interactions at Low and High Redshift |language=en |location=Dordrecht |publisher=Springer Netherlands |pages=289–294 |doi=10.1007/978-94-011-4665-4_73 |isbn=978-94-011-4665-4}}</ref> which is caused by the end product of two [[Interacting galaxy|interacting]] gas-rich [[Spiral galaxy|spiral galaxies]] that [[Galaxy merger|merged]] together.<ref name=":0">{{Cite web |last=Nandi |first=S |last2=Das |first2=M |last3=Dwarakanath |first3=K S |title=Tracing the evolution of ultraluminous infrared galaxies into radio galaxies with low frequency radio observations |url=https://academic.oup.com/mnras/article/503/4/5746/6225362?login=false |access-date=2024-05-08 |website=academic.oup.com}}</ref> It has a power output above 10 times that of our [[sun]],<ref>{{Cite thesis |title=Ultraluminous Infrared Galaxies: Power Sources and Ages Along the Merger Sequence |url=https://resolver.caltech.edu/CaltechETD:etd-08292008-130426 |publisher=California Institute of Technology |date=2000 |degree=phd |language=en |first=Thomas Williams |last=Murphy}}</ref> in which emits a tremendous amount of [[light]] at infrared [[Wavelength|wavelengths]].<ref name=":1">{{Cite web |last=information@eso.org |title=A tale of galactic collisions |url=https://www.spacetelescope.org/images/potw1318a/ |access-date=2024-05-08 |website=www.spacetelescope.org |language=en}}</ref> Not to mention, it is characterized by large dust masses and vigorous [[Star formation|star formation activity]]<ref name=":0" /> which was caused by the collision between the [[Galaxy|galaxies]]<ref name=":1" /> and also the [[Accretion disk|accretion]] activity around its [[supermassive black hole]], which [[radiation]] is produced that heats up [[dust]].<ref>{{Cite web |title=Are Ultra-Luminous Galaxies Colliding? {{!}} Center for Astrophysics {{!}} Harvard & Smithsonian |url=https://www.cfa.harvard.edu/news/are-ultra-luminous-galaxies-colliding |access-date=2024-05-08 |website=www.cfa.harvard.edu}}</ref>
IRAS 05189-2524 is classified as an [[Luminous infrared galaxy|ultraluminous infrared galaxy]] (ULIRG),<ref>{{Cite book |last1=Sanders |first1=D. B. |last2=Surace |first2=J. A. |last3=Ishida |first3=C. M. |chapter=Ultraluminous Infrared Galaxies |date=1999 |editor-last=Barnes |editor-first=J. E. |editor2-last=Sanders |editor2-first=D. B. |title=Galaxy Interactions at Low and High Redshift |chapter-url=https://resolver.caltech.edu/CaltechAUTHORS:20170301-143909957 |language=en |location=Dordrecht |publisher=Springer Netherlands |pages=289–294 |doi=10.1007/978-94-011-4665-4_73 |isbn=978-94-011-4665-4}}</ref> which is formed by two [[Interacting galaxy|interacting]] gas-rich [[Spiral galaxy|spiral galaxies]] that merged together.<ref name=":0">{{Cite journal |last1=Nandi |first1=S |last2=Das |first2=M |last3=Dwarakanath |first3=K S |title=Tracing the evolution of ultraluminous infrared galaxies into radio galaxies with low frequency radio observations |url=https://academic.oup.com/mnras/article/503/4/5746/6225362?login=false |access-date=2024-05-08 |journal=Monthly Notices of the Royal Astronomical Society|date=2021 |volume=503 |issue=4 |pages=5746–5762 |doi=10.1093/mnras/stab275 |doi-access=free |arxiv=2102.10600 }}</ref> Signs left by [[Galaxy merger|merging process]], included a single bright nucleus and an outer structure consisting one-sided extension of the [[Structure|inner arms]], with its [[tidal tail]] formed by [[Interstellar medium|material]] ripped from the galaxies by [[Gravity|gravitational forces]].<ref name=":1">{{Cite web |last=information@eso.org |title=A tale of galactic collisions |url=https://www.spacetelescope.org/images/potw1318a/ |access-date=2024-05-08 |website=www.spacetelescope.org |language=en}}</ref>


It is proposed that 2MASX J05210136-2521450 represents the dust-enshrouded stages of a [[quasar]].<ref name=":2">{{Cite journal |last=Sanders |first=D. B. |last2=Soifer |first2=B. T. |last3=Elias |first3=J. H. |last4=Madore |first4=B. F. |last5=Matthews |first5=K. |last6=Neugebauer |first6=G. |last7=Scoville |first7=N. Z. |date=1988-02-01 |title=Ultraluminous Infrared Galaxies and the Origin of Quasars |url=https://ui.adsabs.harvard.edu/abs/1988ApJ...325...74S |journal=The Astrophysical Journal |volume=325 |pages=74 |doi=10.1086/165983 |issn=0004-637X}}</ref> Once the nuclei shed the [[Cosmic dust|obscuring dust]], it allows the [[active galactic nucleus]] to dominate the decaying starburst, to become an optically selected quasar.<ref name=":2" />
IRAS 05189-2524 is one of the brightest local ULIRG in X-ray with a ''E'' = 2–10 keV continuum [[luminosity]] of ~1043 erg/s<ref>{{Cite journal |last1=Teng |first1=Stacy H. |last2=Veilleux |first2=Sylvain |last3=Anabuki |first3=Naohisa |last4=Dermer |first4=Charles D. |last5=Gallo |first5=Luigi C. |last6=Nakagawa |first6=Takao |last7=Reynolds |first7=Christopher S. |last8=Sanders |first8=D. B. |last9=Terashima |first9=Yuichi |last10=Wilson |first10=Andrew S. |date=2009-01-09 |title=<i>SUZAKU</i>OBSERVATIONS OF LOCAL ULTRALUMINOUS INFRARED GALAXIES |url=https://iopscience.iop.org/article/10.1088/0004-637X/691/1/261 |journal=The Astrophysical Journal |volume=691 |issue=1 |pages=261–276 |doi=10.1088/0004-637x/691/1/261 |bibcode=2009ApJ...691..261T |issn=0004-637X}}</ref> This tend to vary overtime in which the ''E'' = 0.5–2 keV was relatively constant during the 2001-2002 observation done by XMM Newton and Chandra. But in 2006 study done by Suzaku shows it was a factor of ~30 lower.<ref name=":3" /> The galaxy has a power output above 10 times that of our [[sun]],<ref>{{Cite thesis |title=Ultraluminous Infrared Galaxies: Power Sources and Ages Along the Merger Sequence |url=https://resolver.caltech.edu/CaltechETD:etd-08292008-130426 |publisher=California Institute of Technology |date=2000 |degree=phd |language=en |first=Thomas Williams |last=Murphy}}</ref> emitting a tremendous amount of [[light]] at infrared [[Wavelength|wavelengths]].<ref name=":1" />


Moreover, IRAS 05189-2524 is classified an optical [[Seyfert galaxy|Seyfert]] 2 galaxy,<ref name=":3">{{Cite journal |last1=Smith |first1=Robyn N. |last2=Tombesi |first2=Francesco |last3=Veilleux |first3=Sylvain |last4=Lohfink |first4=Anne M. |last5=Luminari |first5=Alfredo |date=2019-12-10 |title=Discovery of an X-Ray Quasar Wind Driving the Cold Gas Outflow in the Ultraluminous Infrared Galaxy IRAS F05189-2524 |journal=The Astrophysical Journal |volume=887 |issue=1 |pages=69 |doi=10.3847/1538-4357/ab4ef8 |doi-access=free |arxiv=1910.14583 |bibcode=2019ApJ...887...69S |issn=0004-637X}}</ref><ref>{{Cite journal |last1=Veilleux |first1=Sylvain |last2=Kim |first2=D.-C. |last3=Sanders |first3=D. B. |date=1999-09-01 |title=Optical Spectroscopy of the IRAS 1 Jy Sample of Ultraluminous Infrared Galaxies |url=https://iopscience.iop.org/article/10.1086/307634/meta |journal=The Astrophysical Journal |language=en |volume=522 |issue=1 |pages=113 |doi=10.1086/307634 |arxiv=astro-ph/9904149 |bibcode=1999ApJ...522..113V |issn=0004-637X}}</ref> presenting a hidden [[Broad-line region|broadline region]].<ref>{{Cite journal |last1=Veilleux |first1=Sylvain |last2=Sanders |first2=D. B. |last3=Kim |first3=D.-C. |date=September 1999 |title=New Results from a Near-Infrared Search for Hidden Broad-Line Regions in Ultraluminous Infrared Galaxies |url=https://iopscience.iop.org/article/10.1086/307635 |journal=The Astrophysical Journal |volume=522 |issue=1 |pages=139–156 |doi=10.1086/307635 |arxiv=astro-ph/9904148 |bibcode=1999ApJ...522..139V |issn=0004-637X}}</ref> A study noticed there is ~70% percent of the bolometric luminosity attributed to its [[active galactic nucleus]],<ref>{{Cite journal |last1=Veilleux |first1=S. |last2=Rupke |first2=D. S. N. |last3=Kim |first3=D.-C. |last4=Genzel |first4=R. |last5=Sturm |first5=E. |last6=Lutz |first6=D. |last7=Contursi |first7=A. |last8=Schweitzer |first8=M. |last9=Tacconi |first9=L. J. |last10=Netzer |first10=H. |last11=Sternberg |first11=A. |last12=Mihos |first12=J. C. |last13=Baker |first13=A. J. |last14=Mazzarella |first14=J. M. |last15=Lord |first15=S. |date=2009-05-21 |title=SPITZER QUASAR AND ULIRG EVOLUTION STUDY (QUEST). IV. COMPARISON OF 1 Jy ULTRALUMINOUS INFRARED GALAXIES WITH PALOMAR-GREEN QUASARS |url=https://iopscience.iop.org/article/10.1088/0067-0049/182/2/628 |journal=The Astrophysical Journal Supplement Series |volume=182 |issue=2 |pages=628–666 |doi=10.1088/0067-0049/182/2/628 |arxiv=0905.1577 |bibcode=2009ApJS..182..628V |issn=0067-0049}}</ref> thus making it a [[quasar]]. It is represented by its dust enshrouded stage<ref name=":2">{{Cite journal |last1=Sanders |first1=D. B. |last2=Soifer |first2=B. T. |last3=Elias |first3=J. H. |last4=Madore |first4=B. F. |last5=Matthews |first5=K. |last6=Neugebauer |first6=G. |last7=Scoville |first7=N. Z. |date=1988-02-01 |title=Ultraluminous Infrared Galaxies and the Origin of Quasars |url=https://authors.library.caltech.edu/74642/1/1988ApJ___325___74S.pdf |journal=The Astrophysical Journal |volume=325 |pages=74 |bibcode=1988ApJ...325...74S |doi=10.1086/165983 |issn=0004-637X}}</ref> which is shed overtime by the [[Active galactic nucleus|nuclei]].<ref name=":2" /> There is a sign of high-velocity large-scale outflows detached in neutral, ionized and molecular gas phrases.<ref>{{Cite journal |last1=González-Alfonso |first1=E. |last2=Fischer |first2=J. |last3=Spoon |first3=H. W. W. |last4=Stewart |first4=K. P. |last5=Ashby |first5=M. L. N. |last6=Veilleux |first6=S. |last7=Smith |first7=H. A. |last8=Sturm |first8=E. |last9=Farrah |first9=D. |last10=Falstad |first10=N. |last11=Meléndez |first11=M. |last12=Graciá-Carpio |first12=J. |last13=Janssen |first13=A. W. |last14=Lebouteiller |first14=V. |date=February 2017 |title=Molecular Outflows in Local ULIRGs: Energetics from Multitransition OH Analysis |journal=The Astrophysical Journal |language=en |volume=836 |issue=1 |pages=11 |doi=10.3847/1538-4357/836/1/11 |doi-access=free |arxiv=1612.08181 |bibcode=2017ApJ...836...11G |issn=0004-637X}}</ref>
Moreover, the [[Galaxy merger|merging process]] left its signs; 2MASX J05210136-2521450 presents a single bright nucleus and an outer structure consisting one-sided extension of the [[Structure|inner arms]], with its [[tidal tail]] heading towards the opposite direction which was formed through [[Interstellar medium|material]] ripped from the galaxies by [[Gravity|gravitational forces]].<ref name=":1" /> Possibly, the merger could strip the galaxies of both [[Galaxy formation and evolution|star-forming gas]] which could hint the signs of no new [[Star|stars]] forming anytime.<ref>{{Cite web |last=published |first=Robert Lea |date=2022-09-06 |title=Violent mergers might be robbing galaxies of their star-birthing material |url=https://www.space.com/galaxy-collisions-end-star-formation |access-date=2024-05-08 |website=Space.com |language=en}}</ref>

An observation by [[XMM-Newton|XMM Newton]] and [[NuSTAR]], shows evidence for a blueshifted Fe K absorption feature at E = 7.8 [[KeV]] which indicates there is an ultrafast outflow (UFO) with ''v''out = 0.11 ± 0.01''c.''<ref name=":3" /> A relative disk reflection in the broadband [[X-ray]] [[Spectral line|spectrum]], shows a highly asymmetric board Fe K''α'' emission line that extends down to 3 KeV with a Compton scattering component above 10 KeV.<ref>{{Cite journal |last1=Xu |first1=Yanjun |last2=Baloković |first2=Mislav |last3=Walton |first3=Dominic J. |last4=Harrison |first4=Fiona A. |last5=García |first5=Javier A. |last6=Koss |first6=Michael J. |date=2017-02-28 |title=Evidence for Relativistic Disk Reflection in the Seyfert 1h Galaxy/ULIRG IRAS 05189–2524 Observed by NuSTAR and XMM-Newton |journal=The Astrophysical Journal |volume=837 |issue=1 |pages=21 |doi=10.3847/1538-4357/aa5df4 |doi-access=free |arxiv=1702.00073 |bibcode=2017ApJ...837...21X |issn=0004-637X}}</ref>

Further studies shows there is a new, quasi-luminous hard X-ray and near-IR spectra in IRAS 05189-2524. The Seyfert nucleus is Compton-thin and the near-IR board lines are seen in transmission, similar to X-rays and the medium has an Aṿ/ɴH [[ratio]] that is lower than Galactic.<ref name=":4">{{Cite journal |last1=Severgnini |first1=P. |last2=Risaliti |first2=G. |last3=Marconi |first3=A. |last4=Maiolino |first4=R. |last5=Salvati |first5=M. |date=2001-03-01 |title=An X-ray and near-IR spectroscopic analysis of the ULIRG IRAS 05189-2524 |url=https://www.aanda.org/articles/aa/abs/2001/10/aa10444/aa10444.html |journal=Astronomy & Astrophysics |language=en |volume=368 |issue=1 |pages=44–51 |doi=10.1051/0004-6361:20000522 |arxiv=astro-ph/0012506 |bibcode=2001A&A...368...44S |issn=0004-6361}}</ref> Also, the increase in obscuration at latter approach shows less △Aṿ/△Nн compared to Galactic, thus supporting a correlation between the proximity to the center and properties of obscuring matter. Most of the observed [[Polarization (waves)|polarization]] is due to [[dichroism]] given the fact, the measured ''A<sub>V</sub>'' is compatible with the broad component of Н''α'' seen in transmission.<ref name=":4" />

There are Na i D [[Emission spectrum|emission]] in the system traces dusty [[Filaments of galaxies|filaments]] on the near side of an extended active galactic nucleus in IRAS 05189-2524 which has projected velocities up to 2000 km/s. These filaments simultaneously obscure the stellar continuum, serving as complementary probe of the wind, in which they are the strongest in regions of low foreground obscuration.<ref>{{Cite journal |last1=Rupke |first1=David S. N. |last2=Veilleux |first2=Sylvain |date=2015-03-12 |title=SPATIALLY EXTENDED NA i D RESONANT EMISSION AND ABSORPTION IN THE GALACTIC WIND OF THE NEARBY INFRARED-LUMINOUS QUASAR F05189-2524 |url=https://iopscience.iop.org/article/10.1088/0004-637X/801/2/126 |journal=The Astrophysical Journal |volume=801 |issue=2 |pages=126 |doi=10.1088/0004-637x/801/2/126 |arxiv=1411.3744 |bibcode=2015ApJ...801..126R |issn=1538-4357}}</ref>


== References ==
== References ==
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[[Category:Lepus (constellation)]]
[[Category:Lepus (constellation)]]
[[Category:Luminous infrared galaxies]]
[[Category:Luminous infrared galaxies]]
[[Category:Elliptical galaxies]]
[[Category:Seyfert galaxies]]
[[Category:Seyfert galaxies]]
[[Category:Interacting galaxies]]
[[Category:Galaxy mergers]]
[[Category:Principal Galaxies Catalogue objects]]
[[Category:Principal Galaxies Catalogue objects|017155]]
[[Category:IRAS catalogue objects]]
[[Category:IRAS catalogue objects]]
[[Category:LEDA objects]]
[[Category:LEDA objects|017155]]

Latest revision as of 03:36, 6 January 2025

IRAS 05189-2524
Hubble Space Telescope image of IRAS 05189-2524
Observation data (J2000 epoch)
ConstellationLepus
Right ascension05h 21m 01.3927ss[1]
Declination−25° 21′ 45.229″[1]
Redshift0.042750
Heliocentric radial velocity12,816 km/s
Distance603 Mly (185 Mpc)
Apparent magnitude (V)15.4
Characteristics
TypePec; ULIRG, Sy2
Size75,000 ly
Apparent size (V)0.46 x 0.44 arcmin
Notable featuresGalaxy merger, luminous infrared galaxy
Other designations
PGC 17155, 2MASS J05210139-2521452, AKARI J0521013-252146, MRSS 486-006230, NVSS J052101-252145, 1WGA J0521.0-2521, SWIFT J0521.0-2522, LEDA 17155, 2MASX J05210136-2521450

IRAS 05189-2524 is a galaxy merger located in the constellation Lepus. It is located 603 million light-years away from the Solar System and has an approximate diameter of 75,000 light-years.[1]

A luminous galaxy

[edit]

IRAS 05189-2524 is classified as an ultraluminous infrared galaxy (ULIRG),[2] which is formed by two interacting gas-rich spiral galaxies that merged together.[3] Signs left by merging process, included a single bright nucleus and an outer structure consisting one-sided extension of the inner arms, with its tidal tail formed by material ripped from the galaxies by gravitational forces.[4]

IRAS 05189-2524 is one of the brightest local ULIRG in X-ray with a E = 2–10 keV continuum luminosity of ~1043 erg/s[5] This tend to vary overtime in which the E = 0.5–2 keV was relatively constant during the 2001-2002 observation done by XMM Newton and Chandra. But in 2006 study done by Suzaku shows it was a factor of ~30 lower.[6] The galaxy has a power output above 10 times that of our sun,[7] emitting a tremendous amount of light at infrared wavelengths.[4]

Moreover, IRAS 05189-2524 is classified an optical Seyfert 2 galaxy,[6][8] presenting a hidden broadline region.[9] A study noticed there is ~70% percent of the bolometric luminosity attributed to its active galactic nucleus,[10] thus making it a quasar. It is represented by its dust enshrouded stage[11] which is shed overtime by the nuclei.[11] There is a sign of high-velocity large-scale outflows detached in neutral, ionized and molecular gas phrases.[12]

An observation by XMM Newton and NuSTAR, shows evidence for a blueshifted Fe K absorption feature at E = 7.8 KeV which indicates there is an ultrafast outflow (UFO) with vout = 0.11 ± 0.01c.[6] A relative disk reflection in the broadband X-ray spectrum, shows a highly asymmetric board Fe Kα emission line that extends down to 3 KeV with a Compton scattering component above 10 KeV.[13]

Further studies shows there is a new, quasi-luminous hard X-ray and near-IR spectra in IRAS 05189-2524. The Seyfert nucleus is Compton-thin and the near-IR board lines are seen in transmission, similar to X-rays and the medium has an Aṿ/ɴH ratio that is lower than Galactic.[14] Also, the increase in obscuration at latter approach shows less △Aṿ/△Nн compared to Galactic, thus supporting a correlation between the proximity to the center and properties of obscuring matter. Most of the observed polarization is due to dichroism given the fact, the measured AV is compatible with the broad component of Нα seen in transmission.[14]

There are Na i D emission in the system traces dusty filaments on the near side of an extended active galactic nucleus in IRAS 05189-2524 which has projected velocities up to 2000 km/s. These filaments simultaneously obscure the stellar continuum, serving as complementary probe of the wind, in which they are the strongest in regions of low foreground obscuration.[15]

References

[edit]
  1. ^ a b c "Your NED Search Results". ned.ipac.caltech.edu. Retrieved 2024-05-08.
  2. ^ Sanders, D. B.; Surace, J. A.; Ishida, C. M. (1999). "Ultraluminous Infrared Galaxies". In Barnes, J. E.; Sanders, D. B. (eds.). Galaxy Interactions at Low and High Redshift. Dordrecht: Springer Netherlands. pp. 289–294. doi:10.1007/978-94-011-4665-4_73. ISBN 978-94-011-4665-4.
  3. ^ Nandi, S; Das, M; Dwarakanath, K S (2021). "Tracing the evolution of ultraluminous infrared galaxies into radio galaxies with low frequency radio observations". Monthly Notices of the Royal Astronomical Society. 503 (4): 5746–5762. arXiv:2102.10600. doi:10.1093/mnras/stab275. Retrieved 2024-05-08.
  4. ^ a b information@eso.org. "A tale of galactic collisions". www.spacetelescope.org. Retrieved 2024-05-08.
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