Markarian 273

Last updated
Markarian 273
Hubble Interacting Galaxy Mrk 273 (2008-04-24).jpg
Mrk 273 by the Hubble Space Telescope
Observation data (J2000 epoch)
Constellation Ursa Major
Right ascension 13h 44m 42.1s [1]
Declination +55° 53′ 13″ [1]
Redshift 0.037340 ± 0.000008 [1]
Helio radial velocity 11,194 ± 2 km/s [1]
Distance 502 Mly (154 Mpc) [1]
Apparent magnitude  (V)14.8
Characteristics
Type Pec [1]
Apparent size  (V)0.72′ × 0.40′ [1]
Notable featuresUltraluminour infrared galaxy, Seyfert galaxy
Other designations
UGC 8696, VV 851, I Zw 071, MCG +09-23-004, PGC 48711 [1]

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. [1] It is an ultraluminous infrared galaxy and a Seyfert galaxy.

Contents

Characteristics

Markarian 273 is a galaxy merger, the result of two or more galaxies colliding. When observed in mid infrared, two nuclei are visible, with a projected separation of about 0.75 kiloparsec. [2] The southwest nucleus is known to be active, due its X-ray emission, [3] while the northeast nucleus too displays a heavily abosrbed X-ray spectrum, indicating that is also active. [2] The optical emission of the southwest nucleus corresponds to a type II Seyfert galaxy while the north one of a LINER. [4] A third component in the nuclear region is visible at the southeast in the radiowaves and could be a star cluster. [3]

The galaxy experiences a starburst, with a star formation rate of 139 M☉ per year. [5] This activity makes the galaxy shine bright in the infrared and it is categorised as ultra-luminous infrared galaxy, with total infrared luminosity of the galaxy is estimated to be 1012.1  L☉ . [6] The startburst takes place in a rotating disk with a radius 120 pc and a total mass of 2.6×109 M☉ which surrounds the north nucleus. [7] It has been suggested that this is the location of compact luminous supernovae remnants and radio supernovae. [8] The startburst is fed by large amounts of cold molecular gas. The gas has complex kinematics due to the presence of outflows. A kiloparsec scale outflow is visible towards the north in CO imaging, with the flow rate of 600 M☉ per year. [5] The outflows reach about 5 kpc from the nucleus. [9] There is also evidence of a bipolar superbubble. [10]

The merger has a tidal tail extending southwards for 40 kiloparsecs, that is seen edge on. [3] Also south of the galaxy lies a giant X-ray nebula, measuring 40 by 40 kiloparsecs in size, that isn't closely related with the tidal tail. The gas temperature of the nebula is estimated to be 7 million K, possibly heated by galactic outflows. [2] Filaments and clumps of ionised gas visible in OIII are extending about 23 kpc to the east. [11] A warm gas ionised halo extends about 45 kpc from the nucleus, and is probably tidal debris from the merger. [12] When observed in radiowaves the galaxy has two large plumes, one to the south, extending to about 100 kpc, and one dimmer to the north, extending to about 190 kpc. [13]

See also

Related Research Articles

<span class="mw-page-title-main">NGC 6240</span> Galaxy merger remnant in the constellation Ophiuchus

NGC 6240, also known as the Starfish Galaxy, is a nearby ultraluminous infrared galaxy (ULIRG) in the constellation Ophiuchus. The galaxy is the remnant of a merger between three smaller galaxies. The collision between the three progenitor galaxies has resulted in a single, larger galaxy with three distinct nuclei and a highly disturbed structure, including faint extensions and loops.

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">Ionization cone</span> Astronomical phenomenon

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.

<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 4388</span> Galaxy in the constellation Virgo

NGC 4388 is an active spiral galaxy in the equatorial constellation of Virgo. It was discovered April 17, 1784 by Wilhelm Herschel. This galaxy is located at a distance of 57 million light years and is receding with a radial velocity of 2,524 km/s. It is one of the brightest galaxies of the Virgo Cluster due to its luminous nucleus. NGC 4388 is located 1.3° to the west of the cluster center, which translates to a projected distance of ≈400 kpc.

<span class="mw-page-title-main">NGC 1614</span> Galaxy in the constellation Eridanus

NGC 1614 is the New General Catalogue identifier for a spiral galaxy in the equatorial constellation of Eridanus. It was discovered on December 29, 1885 by American astronomer Lewis Swift, who described it in a shorthand notation as: pretty faint, small, round, a little brighter middle. The nebula was then catalogued by Danish-Irish astronomer J. L. E. Drayer in 1888. When direct photography became available, it was noted that this galaxy displayed some conspicuous peculiarities. American astronomer Halton Arp included it in his 1966 Atlas of Peculiar Galaxies. In 1971, Swiss astronomer Fritz Zwicky described it as a "blue post-eruptive galaxy, compact patchy core, spiral plumes, long blue jet SSW".

<span class="mw-page-title-main">NGC 5643</span> Galaxy in the constellation Lupus

NGC 5643 is an intermediate spiral galaxy in the constellation Lupus. Based on the tip of the red-giant branch distance indicator, it is located at a distance of about 40 million light-years. NGC 5643 has an active galactic nucleus and is a type II Seyfert galaxy.

<span class="mw-page-title-main">NGC 2623</span> Interacting galaxy in the constellation Cancer

NGC 2623/Arp 243 is an interacting galaxy located in the constellation Cancer. NGC 2623 is the result of two spiral galaxies that have merged. Scientists believe that this situation is similar to what will occur to the Milky Way, which contains the Solar System, and the neighboring galaxy, the Andromeda Galaxy in four billion years. Studying this galaxy and its properties have provided scientists with a better idea of the coming collision of the Milky Way and the Andromeda. Due to NGC 2623 being in the late stage of merging, the compression of the gas within the galaxy has led to a large amount of star formation, and to its unique structure of a bright core with two extending tidal tails.

<span class="mw-page-title-main">NGC 3256</span> Peculiar galaxy in the constellation Vela

NGC 3256 is a peculiar galaxy formed from the collision of two separate galaxies in the constellation of Vela. NGC 3256 is located about 100 million light-years away and belongs to the Hydra–Centaurus Supercluster complex. NGC 3256 provides a nearby template for studying the properties of young star clusters in tidal tails. The system hides a double nucleus and a tangle of dust lanes in the central region. The telltale signs of the collision are two extended luminous tails swirling out from the galaxy. The tails are studded with a particularly high density of star clusters. NGC 3256 is the most luminous galaxy in the infrared spectrum located within z 0.01 from Earth.

<span class="mw-page-title-main">NGC 7469</span> Galaxy located in the constellation Pegasus

NGC 7469 is an intermediate spiral galaxy in the constellation of Pegasus. NGC 7469 is located about 200 million light-years away from Earth, which means, given its apparent dimensions, that NGC 7469 is approximately 90,000 light-years across. It was discovered by William Herschel on November 12, 1784.

<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">NGC 7674</span> Galaxy located in the constellation Pegasus

NGC 7674 is a spiral galaxy located in the constellation Pegasus. It is located at a distance of circa 350 million light years from Earth, which, given its apparent dimensions, means that NGC 7674 is about 125,000 light years across. It was discovered by John Herschel on August 16, 1830.

<span class="mw-page-title-main">NGC 985</span> Ring galaxy in the constellation Cetus

NGC 985 is a ring galaxy in the constellation of Cetus. It is located about 550 million light years away from Earth, which means, given its apparent dimensions, that NGC 985 is approximately 160,000 light years across. It was discovered by Francis Leavenworth in 1886. It is a type 1 Seyfert galaxy.

<span class="mw-page-title-main">NGC 1386</span> Galaxy in the constellation Eridanus

NGC 1386 is a spiral galaxy located in the constellation Eridanus. It is located at a distance of circa 53 million light years from Earth, which, given its apparent dimensions, means that NGC 1386 is about 50,000 light years across. It is a Seyfert galaxy, the only one in Fornax Cluster.

<span class="mw-page-title-main">NGC 5728</span> Spiral galaxy in the constellation Libra

NGC 5728 is an active barred spiral galaxy located 146 million light years away in the southern constellation of Libra. It was discovered on May 7, 1787 by William Herschel. The designation comes from the New General Catalogue of J. L. E. Dreyer, published in 1888. It has an apparent visual magnitude of 13.40 and spans an angle of 3.4 arcminutes. The galaxy shows a red shift of 0.00935 and has a heliocentric radial velocity of 2,803 km/s. It has an estimated mass of 72 billion times the mass of the Sun and stretches around 30 kpc across.

<span class="mw-page-title-main">NGC 7592</span> Interacting galaxy system in the constellation Aquarius

NGC 7592 is an interacting galaxy system located 300 million light years away in the constellation Aquarius. It was discovered by William Herschel on September 20, 1784. The total infrared luminosity is 1011.33 L☉, and thus it is categorised as a luminous infrared galaxy. One of the galaxies hosts a type 2 Seyfert nucleus.

<span class="mw-page-title-main">NGC 5252</span> Galaxy in the constellation of Virgo

NGC 5252 is a lenticular galaxy located in the constellation Virgo. It is located at a distance of about 220 to 320 million light years from Earth, which, given its apparent dimensions, means that NGC 5252 is about 100,000 light years across. It was discovered by William Herschel on February 2, 1786.

<span class="mw-page-title-main">Markarian 590</span> Galaxy in the constellation of Cetus

Markarian 590, also known as NGC 863, NGC 866, and NGC 885, is a spiral galaxy located in the constellation Cetus. It is located at a distance of about 300 million light years from Earth, which, given its apparent dimensions, means that NGC 863 is about 110,000 light years across. It is a change looking Seyfert galaxy.

<span class="mw-page-title-main">UGC 5101</span> Galaxy in the constellation of Ursa Major

UGC 5101 is a galaxy merger located in the constellation Ursa Major. It is located at a distance of about 530 million light years from Earth. It is an ultraluminous infrared galaxy. The total infrared luminosity of the galaxy is estimated to be 1011.95 L☉ and the galaxy has a total star formation rate of 105 M☉ per year.

References

  1. 1 2 3 4 5 6 7 8 9 "NASA/IPAC Extragalactic Database". Results for MRK 273. Retrieved 2023-05-06.
  2. 1 2 3 Liu, Weizhe; Veilleux, Sylvain; Iwasawa, Kazushi; Rupke, David S. N.; Teng, Stacy; U, Vivian; Tombesi, Francesco; Sanders, David; Max, Claire E.; Meléndez, Marcio (8 February 2019). "Elliptical Galaxy in the Making: The Dual Active Galactic Nuclei and Metal-enriched Halo of Mrk 273". The Astrophysical Journal. 872 (1): 39. arXiv: 1901.04118 . doi:10.3847/1538-4357/aafdfc.
  3. 1 2 3 Iwasawa, K.; Mazzarella, J. M.; Surace, J. A.; Sanders, D. B.; Armus, L.; Evans, A. S.; Howell, J. H.; Komossa, S.; Petric, A.; Teng, S. H.; U, V.; Veilleux, S. (April 2011). "The location of an active nucleus and a shadow of a tidal tail in the ULIRG Mrk 273". Astronomy & Astrophysics. 528: A137. doi:10.1051/0004-6361/201015872.
  4. ↑ Colina, Luis; Arribas, Santiago; Borne, Kirk D. (10 December 1999). "Integral Field Spectroscopy of Markarian 273: Mapping High-Velocity Gas Flows and an Off-Nucleus Seyfert 2 Nebula". The Astrophysical Journal. 527 (1): L13–L16. doi:10.1086/312389. hdl: 10261/199205 .
  5. 1 2 Cicone, C.; Maiolino, R.; Sturm, E.; Graciá-Carpio, J.; Feruglio, C.; Neri, R.; Aalto, S.; Davies, R.; Fiore, F.; Fischer, J.; García-Burillo, S.; González-Alfonso, E.; Hailey-Dunsheath, S.; Piconcelli, E.; Veilleux, S. (February 2014). "Massive molecular outflows and evidence for AGN feedback from CO observations". Astronomy & Astrophysics. 562: A21. doi:10.1051/0004-6361/201322464.
  6. ↑ Kim, D.-C.; Veilleux, S.; Sanders, D. B. (December 2002). "Optical and Near-Infrared Imaging of the IRAS 1 Jy Sample of Ultraluminous Infrared Galaxies. I. The Atlas". The Astrophysical Journal Supplement Series. 143 (2): 277–314. doi: 10.1086/343843 .
  7. ↑ Downes, D.; Solomon, P. M. (10 November 1998). "Rotating Nuclear Rings and Extreme Starbursts in Ultraluminous Galaxies". The Astrophysical Journal. 507 (2): 615–654. doi: 10.1086/306339 .
  8. ↑ Bondi, M.; Pérez-Torres, M-A.; Dallacasa, D.; Muxlow, T. W. B. (September 2005). "A supernova factory in Mrk 273?". Monthly Notices of the Royal Astronomical Society. 361 (2): 748–752. doi: 10.1111/j.1365-2966.2005.09206.x .
  9. ↑ Leung, Gene C. K.; Coil, Alison L.; Rupke, David S. N.; Perrotta, Serena (1 June 2021). "KCWI Observations of the Extended Nebulae in Mrk 273". The Astrophysical Journal. 914 (1): 17. arXiv: 2011.09587 . doi:10.3847/1538-4357/abf4da.
  10. ↑ Rupke, David S. N.; Veilleux, Sylvain (16 April 2013). "THE MULTIPHASE STRUCTURE AND POWER SOURCES OF GALACTIC WINDS IN MAJOR MERGERS". The Astrophysical Journal. 768 (1): 75. arXiv: 1303.6866 . doi:10.1088/0004-637X/768/1/75.
  11. ↑ Rodríguez Zaurín, J.; Tadhunter, C. N.; Rupke, D. S. N.; Veilleux, S.; Spoon, H. W. W.; Chiaberge, M.; Ramos Almeida, C.; Batcheldor, D.; Sparks, W. B. (November 2014). "Extended warm gas in the ULIRG Mrk273: Galactic outflows and tidal debris". Astronomy & Astrophysics. 571: A57. arXiv: 1407.6301 . doi:10.1051/0004-6361/201423540.
  12. ↑ Spence, R. A. W.; Zaurín, J. Rodríguez; Tadhunter, C. N.; Rose, M.; Cabrera-Lavers, A.; Spoon, H.; Muñoz-Tuñón, C. (11 June 2016). "No evidence for large-scale outflows in the extended ionized halo of ULIRG Mrk273". Monthly Notices of the Royal Astronomical Society: Letters. 459 (1): L16–L20. arXiv: 1603.00488 . doi:10.1093/mnrasl/slw033.
  13. ↑ Kukreti, P.; Morganti, R.; Bondi, M.; Oosterloo, T.; Tadhunter, C.; Morabito, L. K.; Adams, E. A. K.; Adebahr, B.; de Blok, W. J. G.; de Gasperin, F.; Drabent, A.; Hess, K. M.; Ivashina, M. V.; Kutkin, A.; Mika, á. M.; Oostrum, L. C.; Shimwell, T. W.; van der Hulst, J. M.; van Leeuwen, J.; van Weeren, R. J.; Vohl, D.; Ziemke, J. (August 2022). "Seeing the forest and the trees: A radio investigation of the ULIRG Mrk 273". Astronomy & Astrophysics. 664: A25. doi:10.1051/0004-6361/202243174.
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.