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== A luminous galaxy ==
== A luminous galaxy ==
2MASX J05210136-2521450 is classified as an [[Luminous infrared galaxy|ultraluminous infrared galaxy]],<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 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 |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 |website=academic.oup.com}}</ref> It 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> and 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>
2MASX J05210136-2521450 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 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 |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 |website=academic.oup.com}}</ref> There are signs left by [[Galaxy merger|merging process]], such as 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 formed through [[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 one of the brightest local ULIRG in X-ray with a ''E'' = 2–10 keV continuum [[luminosity]] of ∼1043 erg s−1<ref>{{Cite journal |last=Teng |first=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 |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" />
⚫
An observation by [[XMM-Newton|XMM Newton]] and [[NuSTAR]], shows there is 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" /> Not to mention, there is evidence for a relative disk reflection in the broadband [[X-ray]] [[Spectral line|spectrum]], showing 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>


Moreover, it 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 |last=Veilleux |first=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 |issn=0004-637X}}</ref> presenting a hidden [[Broad-line region|broadline region]].<ref>{{Cite journal |last=Veilleux |first=Sylvain |last2=Sanders |first2=D. B. |last3=Kim |first3=D.‐C. |date=1999-09 |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 |issn=0004-637X}}</ref> A study noticed there is ∼70% percent of the bolometric luminosity attributed to its [[active galactic nucleus]],<ref>{{Cite journal |last=Veilleux |first=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).
It is proposed that 2MASX J05210136-2521450 represents the dust-enshrouded stages of a [[quasar]].<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://ui.adsabs.harvard.edu/abs/1988ApJ...325...74S |journal=The Astrophysical Journal |volume=325 |pages=74 |doi=10.1086/165983 |bibcode=1988ApJ...325...74S |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" />
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 |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://ui.adsabs.harvard.edu/abs/1988ApJ...325...74S |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 [[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 |last=González-Alfonso |first=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=2017-02 |title=Molecular Outflows in Local ULIRGs: Energetics from Multitransition OH Analysis |url=https://dx.doi.org/10.3847/1538-4357/836/1/11 |journal=The Astrophysical Journal |language=en |volume=836 |issue=1 |pages=11 |doi=10.3847/1538-4357/836/1/11 |issn=0004-637X}}</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>
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 |author1=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>

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 which has projected velocities up to 2000 km s−1. 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 |last=Rupke |first=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 |issn=1538-4357}}</ref>


== References ==
== References ==

Revision as of 08:32, 11 May 2024

2MASX J05210136-2521450
Hubble image of 2MASX J05210136-2521450
Observation data
ConstellationLepus
Right ascension05h 21m 01.392s
Declination-25d 21m 45.36s
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, IRAS 05189-2524, AKARI J0521013-252146, MRSS 486-006230, NVSS J052101-252145, 1WGA J0521.0-2521, SWIFT J0521.0-2522, LEDA 17155

2MASX J05210136-2521450 is a type E[1] elliptical galaxy 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.[2]

A luminous galaxy

2MASX J05210136-2521450 is classified as an ultraluminous infrared galaxy (ULIRG),[3] which is caused by the end product of two interacting gas-rich spiral galaxies that merged together.[4] There are signs left by merging process, such as single bright nucleus and an outer structure consisting one-sided extension of the inner arms, with its tidal tail heading towards the opposite direction formed through material ripped from the galaxies by gravitational forces.[5]

It is one of the brightest local ULIRG in X-ray with a E = 2–10 keV continuum luminosity of ∼1043 erg s−1[6] 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.[7] The galaxy has a power output above 10 times that of our sun,[8] emitting a tremendous amount of light at infrared wavelengths.[5]

Moreover, it is classified an optical Seyfert 2 galaxy,[7][9] presenting a hidden broadline region.[10] A study noticed there is ∼70% percent of the bolometric luminosity attributed to its active galactic nucleus,[11] thus making it a quasar. It is represented by its dust enshrouded stage[12] which is shed overtime by the nuclei.[12] There is a sign of high-velocity large-scale outflows detached in neutral, ionized and molecular gas phrases.[13]

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.[7] 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.[14]

There are Na i D emission in the system traces dusty filaments on the near side of an extended active galactic nucleus which has projected velocities up to 2000 km s−1. 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

  1. ^ "HyperLeda -object description". atlas.obs-hp.fr. Retrieved 2024-05-08.
  2. ^ "Your NED Search Results". ned.ipac.caltech.edu. Retrieved 2024-05-08.
  3. ^ 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.
  4. ^ Nandi, S; Das, M; Dwarakanath, K S. "Tracing the evolution of ultraluminous infrared galaxies into radio galaxies with low frequency radio observations". academic.oup.com. Retrieved 2024-05-08.
  5. ^ a b information@eso.org. "A tale of galactic collisions". www.spacetelescope.org. Retrieved 2024-05-08.
  6. ^ Teng, Stacy H.; Veilleux, Sylvain; Anabuki, Naohisa; Dermer, Charles D.; Gallo, Luigi C.; Nakagawa, Takao; Reynolds, Christopher S.; Sanders, D. B.; Terashima, Yuichi; Wilson, Andrew S. (2009-01-09). "SUZAKUOBSERVATIONS OF LOCAL ULTRALUMINOUS INFRARED GALAXIES". The Astrophysical Journal. 691 (1): 261–276. doi:10.1088/0004-637x/691/1/261. ISSN 0004-637X.
  7. ^ a b c Smith, Robyn N.; Tombesi, Francesco; Veilleux, Sylvain; Lohfink, Anne M.; Luminari, Alfredo (2019-12-10). "Discovery of an X-Ray Quasar Wind Driving the Cold Gas Outflow in the Ultraluminous Infrared Galaxy IRAS F05189-2524". The Astrophysical Journal. 887 (1): 69. arXiv:1910.14583. Bibcode:2019ApJ...887...69S. doi:10.3847/1538-4357/ab4ef8. ISSN 0004-637X.
  8. ^ Murphy, Thomas Williams (2000). Ultraluminous Infrared Galaxies: Power Sources and Ages Along the Merger Sequence (phd thesis). California Institute of Technology.
  9. ^ Veilleux, Sylvain; Kim, D.-C.; Sanders, D. B. (1999-09-01). "Optical Spectroscopy of the IRAS 1 Jy Sample of Ultraluminous Infrared Galaxies". The Astrophysical Journal. 522 (1): 113. doi:10.1086/307634. ISSN 0004-637X.
  10. ^ Veilleux, Sylvain; Sanders, D. B.; Kim, D.‐C. (1999-09). "New Results from a Near‐Infrared Search for Hidden Broad‐Line Regions in Ultraluminous Infrared Galaxies". The Astrophysical Journal. 522 (1): 139–156. doi:10.1086/307635. ISSN 0004-637X. {{cite journal}}: Check date values in: |date= (help)
  11. ^ Veilleux, S.; Rupke, D. S. N.; Kim, D.-C.; Genzel, R.; Sturm, E.; Lutz, D.; Contursi, A.; Schweitzer, M.; Tacconi, L. J.; Netzer, H.; Sternberg, A.; Mihos, J. C.; Baker, A. J.; Mazzarella, J. M.; Lord, S. (2009-05-21). "SPITZER QUASAR AND ULIRG EVOLUTION STUDY (QUEST). IV. COMPARISON OF 1 Jy ULTRALUMINOUS INFRARED GALAXIES WITH PALOMAR-GREEN QUASARS". The Astrophysical Journal Supplement Series. 182 (2): 628–666. doi:10.1088/0067-0049/182/2/628. ISSN 0067-0049. {{cite journal}}: line feed character in |title= at position 50 (help)
  12. ^ a b Sanders, D. B.; Soifer, B. T.; Elias, J. H.; Madore, B. F.; Matthews, K.; Neugebauer, G.; Scoville, N. Z. (1988-02-01). "Ultraluminous Infrared Galaxies and the Origin of Quasars". The Astrophysical Journal. 325: 74. Bibcode:1988ApJ...325...74S. doi:10.1086/165983. ISSN 0004-637X.
  13. ^ González-Alfonso, E.; Fischer, J.; Spoon, H. W. W.; Stewart, K. P.; Ashby, M. L. N.; Veilleux, S.; Smith, H. A.; Sturm, E.; Farrah, D.; Falstad, N.; Meléndez, M.; Graciá-Carpio, J.; Janssen, A. W.; Lebouteiller, V. (2017-02). "Molecular Outflows in Local ULIRGs: Energetics from Multitransition OH Analysis". The Astrophysical Journal. 836 (1): 11. doi:10.3847/1538-4357/836/1/11. ISSN 0004-637X. {{cite journal}}: Check date values in: |date= (help)CS1 maint: unflagged free DOI (link)
  14. ^ Xu, Yanjun; Baloković, Mislav; Walton, Dominic J.; Harrison, Fiona A.; García, Javier A.; Koss, Michael J. (2017-02-28). "Evidence for Relativistic Disk Reflection in the Seyfert 1h Galaxy/ULIRG IRAS 05189–2524 Observed by NuSTAR and XMM-Newton". The Astrophysical Journal. 837 (1): 21. arXiv:1702.00073. Bibcode:2017ApJ...837...21X. doi:10.3847/1538-4357/aa5df4. ISSN 0004-637X.
  15. ^ Rupke, David S. N.; Veilleux, Sylvain (2015-03-12). "SPATIALLY EXTENDED NA i D RESONANT EMISSION AND ABSORPTION IN THE GALACTIC WIND OF THE NEARBY INFRARED-LUMINOUS QUASAR F05189-2524". The Astrophysical Journal. 801 (2): 126. doi:10.1088/0004-637x/801/2/126. ISSN 1538-4357.
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