IRAS 05189-2524

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IRAS 05189-2524
A tale of galactic collisions.jpg
Hubble Space Telescope image of IRAS 05189-2524
Observation data
Constellation Lepus
Right ascension 05h 21m 01.392s
Declination -25d 21m 45.36s
Redshift 0.042750
Heliocentric radial velocity 12,816 Km/s
Distance 603 Mly (185 Mpc)
Apparent magnitude  (V)15.4
Characteristics
Type Pec; ULIRG, Sy2
Size75,000 ly
Apparent size  (V)0.46 x 0.44 arcmin
Notable features Galaxy 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

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]

Related Research Articles

<span class="mw-page-title-main">Ultraluminous X-ray source</span>

In astronomy and astrophysics, an ultraluminous X-ray source (ULX) is less luminous than an active galactic nucleus but more consistently luminous than any known stellar process (over 1039 erg/s, or 1032 watts), assuming that it radiates isotropically (the same in all directions). Typically there is about one ULX per galaxy in galaxies which host them, but some galaxies contain many. The Milky Way has not been shown to contain an ULX, although SS 433 is a candidate. The main interest in ULXs stems from their luminosity exceeding the Eddington luminosity of neutron stars and even stellar black holes. It is not known what powers ULXs; models include beamed emission of stellar mass objects, accreting intermediate-mass black holes, and super-Eddington emission.

Luminous infrared galaxies or LIRGs are galaxies with luminosities, the measurement of brightness, above 1011 L☉. They are also referred to as submillimeter galaxies (SMGs) through their normal method of detection. LIRGs are more abundant than starburst galaxies, Seyfert galaxies and quasi-stellar objects at comparable luminosity. Infrared galaxies emit more energy in the infrared than at all other wavelengths combined. A LIRG's luminosity is 100 billion times that of the Sun.

<span class="mw-page-title-main">APM 08279+5255</span> Quasar

APM 08279+5255 is a very distant, broad absorption line quasar located in the constellation Lynx. It is magnified and split into multiple images by the gravitational lensing effect of a foreground galaxy through which its light passes. It appears to be a giant elliptical galaxy with a supermassive black hole and associated accretion disk. It possesses large regions of hot dust and molecular gas, as well as regions with starburst activity.

<span class="mw-page-title-main">Markarian 231</span> Seyfert galaxy in the constellation Ursa Major

Markarian 231 is a Type-1 Seyfert galaxy that was discovered in 1969 as part of a search of galaxies with strong ultraviolet radiation. It contains the nearest known quasar. Markarian 231 is located about 581 million light years away from Earth, in the constellation of Ursa Major.

<span class="mw-page-title-main">NGC 7130</span> Galaxy in the constellation Piscis Austrinus

NGC 7130 is a spiral galaxy located in the constellation Piscis Austrinus. It is located at a distance of about 220 million light years from Earth, which, given its apparent dimensions, means that NGC 7130 is about 100,000 light years across. It was discovered by John Herschel on September 25, 1834, and discovered independently by Lewis Swift on September 17, 1897. The location of the galaxy given in the New General Catalogue was off by 30 arcminutes in declination from the location of the galaxy.

<span class="mw-page-title-main">Teacup galaxy</span> Low redshift quasar in the constellation Boötes

The Teacup galaxy, also known as the Teacup AGN or SDSS J1430+1339 is a low redshift type 2 quasar, showing an extended loop of ionized gas resembling a handle of a teacup, which was discovered by volunteers of the Galaxy Zoo project and labeled as a Voorwerpje.

<span class="mw-page-title-main">III Zw 2</span> Seyfert galaxy in the constellation Pisces

III Zw 2 is a Seyfert 1 galaxy located in the Pisces constellation. It has a redshift of 0.089 and is notable as the first of its kind to exhibit a superluminal jet.

<span class="mw-page-title-main">Markarian 273</span> Galaxy in the constellation of Ursa Major

Markarian 273 is a galaxy merger located in the constellation Ursa Major. It is located at a distance of about 500 million light years from Earth, which, given its apparent dimensions, means that Markarian 273 is about 130,000 light years across. It is an ultraluminous infrared galaxy and a Seyfert galaxy.

<span class="mw-page-title-main">IRAS F11119+3257</span> Galaxy in the constellation Ursa Major

IRAS F11119+3257 or simply as F11119+3257, is a galaxy located in constellation Ursa Major. With a redshift of 0.187580, it has a light travel time distance of 2.5 billion light-years and is considered an ultraluminous infrared galaxy (ULIRG).

<span class="mw-page-title-main">IRAS 09104+4109</span> Galaxy in the constellation Lynx

IRAS 09104+4109 is a galaxy located in the constellation Lynx. With a redshift of 0.440797, the light travel time for this galaxy, corresponds to 4.8 billion light-years from Earth. It is the brightest cluster galaxy in MACS J0913.7+4056 galaxy cluster and classified as a hyperluminous infrared galaxy.

<span class="mw-page-title-main">IRAS 13218+0552</span> Galaxy merger located in the constellation Virgo

IRAS 13218+0552 known as SFRS 263, is a galaxy merger located in the Virgo constellation. Its redshift is 0.202806, putting the object at 2.6 billion light-years away from Earth. It is a Seyfert galaxy and a luminous infrared galaxy.

<span class="mw-page-title-main">PKS 1345+125</span> Galaxy merger in the constellation Boötes

PKS 1345+125 known as PKS 1345+12 and 4C +12.50, is an ultraluminous infrared galaxy (ULIG) with an active galactic nucleus, located in the constellation Boötes. With a redshift of 0.121740, the galaxy is located 1.7 billion light-years from Earth.

<span class="mw-page-title-main">NGC 4325</span> Galaxy

NGC 4325 is an elliptical galaxy located about 330 million light-years away in the constellation Virgo. It was discovered by astronomer Heinrich d'Arrest on April 15, 1865, who described it as "vF, vS, iR, nf of 2". Despite being listed in the Virgo Cluster catalog as VCC 616, it is not a member of the Virgo Cluster but instead a background galaxy.

<span class="mw-page-title-main">Markarian 463</span> Galaxy in the constellation of Boötes

Markarian 463 known as UGC 8850, is a galaxy merger located in the constellation Boötes. It is located 706 million light years from Earth. It is classified a double nucleus Seyfert galaxy.

<span class="mw-page-title-main">ESO 286-19</span> Galaxy in the constellation Microscopium

ESO 286-19 known as IRAS 20551-4250, is a galaxy merger located in the constellation of Microscopium. It is located 609 million light years away from Earth. It is an ultraluminous infrared galaxy.

<span class="mw-page-title-main">IRAS 10565+2448</span> Galaxy in the constellation Leo

IRAS 10565+2448 known as IRAS F10565+2448, is a galaxy merger located in the constellation of Leo. It is located at a distance of 625 million light years from Earth. It is classified as an ultraluminous infrared galaxy with an infrared luminosity of 1.2 x 1012 LΘ. It has a star formation rate of 131.8 MΘ yr−1.

<span class="mw-page-title-main">Markarian 1014</span> Quasar in the constellation Cetus

Markarian 1014 known as PG 0157+001 is a quasar located in the constellation Cetus. It is located at a distance of 2.47 billion light years from Earth and is classified as a Seyfert galaxy as well as an ultraluminous infrared galaxy (ULIRG).

<span class="mw-page-title-main">IRAS 07598+6508</span> Quasar in the constellation Camelopardalis

IRAS 07598+6508 known as IRAS F07599+6508, is a quasar located in the constellation of Camelopardalis. It is located 2.37 billion light years from Earth and is classified as both an ultraluminous infrared galaxy and a Seyfert galaxy.

<span class="mw-page-title-main">IRAS 01003-2238</span> Galaxy in the constellation Cetus

IRAS 01003-2238 also known as IRAS F01004-2237 or simply F01004-2237, is a galaxy located in the constellation of Cetus. It is located 1.65 billion light years away from Earth and is a Seyfert galaxy and an ultraluminous infrared galaxy. IRAS 01003-2238 is also classified as a Wolf-Rayet galaxy, making the object one of the most distant known.

References

  1. ↑ "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. "Tracing the evolution of ultraluminous infrared galaxies into radio galaxies with low frequency radio observations". academic.oup.com. Retrieved 2024-05-08.
  4. 1 2 information@eso.org. "A tale of galactic collisions". www.spacetelescope.org. Retrieved 2024-05-08.
  5. ↑ 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. Bibcode:2009ApJ...691..261T. doi:10.1088/0004-637x/691/1/261. ISSN   0004-637X.
  6. 1 2 3 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.
  7. ↑ Murphy, Thomas Williams (2000). Ultraluminous Infrared Galaxies: Power Sources and Ages Along the Merger Sequence (phd thesis). California Institute of Technology.
  8. ↑ 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. arXiv: astro-ph/9904149 . Bibcode:1999ApJ...522..113V. doi:10.1086/307634. ISSN   0004-637X.
  9. ↑ Veilleux, Sylvain; Sanders, D. B.; Kim, D.-C. (September 1999). "New Results from a Near-Infrared Search for Hidden Broad-Line Regions in Ultraluminous Infrared Galaxies". The Astrophysical Journal. 522 (1): 139–156. arXiv: astro-ph/9904148 . Bibcode:1999ApJ...522..139V. doi:10.1086/307635. ISSN   0004-637X.
  10. ↑ 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. arXiv: 0905.1577 . Bibcode:2009ApJS..182..628V. doi:10.1088/0067-0049/182/2/628. ISSN   0067-0049.
  11. 1 2 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.
  12. ↑ 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. (February 2017). "Molecular Outflows in Local ULIRGs: Energetics from Multitransition OH Analysis". The Astrophysical Journal. 836 (1): 11. arXiv: 1612.08181 . Bibcode:2017ApJ...836...11G. doi: 10.3847/1538-4357/836/1/11 . ISSN   0004-637X.
  13. ↑ 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.
  14. 1 2 Severgnini, P.; Risaliti, G.; Marconi, A.; Maiolino, R.; Salvati, M. (2001-03-01). "An X-ray and near-IR spectroscopic analysis of the ULIRG IRAS 05189-2524". Astronomy & Astrophysics. 368 (1): 44–51. arXiv: astro-ph/0012506 . Bibcode:2001A&A...368...44S. doi:10.1051/0004-6361:20000522. ISSN   0004-6361.
  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. arXiv: 1411.3744 . Bibcode:2015ApJ...801..126R. doi:10.1088/0004-637x/801/2/126. ISSN   1538-4357.
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