NGC 5643

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NGC 5643
NGC 5643.png
NGC 5643 imaged by the Hubble Space Telescope
Observation data (J2000 epoch)
Constellation Lupus
Right ascension 14h 32m 40.7s [1]
Declination −44° 10′ 28″ [1]
Redshift 1199 ± 2 km/s [1]
Distance 41  Mly (12.5  Mpc) [2]
Apparent magnitude  (V)10.7
Characteristics
Type SAB(rs)c [1]
Apparent size  (V)4.6′ × 4.0′ [1]
Other designations
ESO 272- G 016, MCG -07-30-003, PGC 51969 [1]

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 (12.5 megaparsecs). [2] NGC 5643 has an active galactic nucleus and is a type II Seyfert galaxy.

Contents

Observation history

The galaxy was first discovered by James Dunlop on May 10, 1826, with his 9-inch reflector telescope, who described it as exceedingly faint. The galaxy was also spotted by John Herschel and added to the General Catalogue of Nebulae and Clusters as number 3572. The galaxy is located only 15 degrees from the galactic plane. [3]

Structure

NGC 5643 is a grand design spiral galaxy, with two well-defined, symmetric arms. In the circumnuclear region are other dust spirals, but the two main dust arms are wider. [4] The galaxy is seen nearly face on, at an inclination of ~ 27°.

Active galactic nucleus

Center of galaxy NGC 5643 taken by ALMA and VLT. Center of galaxy NGC 5643.tif
Center of galaxy NGC 5643 taken by ALMA and VLT.

The galaxy has a low-luminosity active galactic nucleus of Seyfert 2 type and is also a luminous infrared galaxy. The galaxy has a double sided diffuse radiojet. The galaxy exhibits an extended emission line region elongated in a direction close to the radio position angle of 87°±3°. Chris Simpson et al. analysed images takes from the WFPC2 camera of the Hubble Space Telescope in [O III] λ5007 and Hα and found emission extending eastward for at least 1.8 kpc and in the [O III]/Hα map a well-defined V-shaped structure that they identified as the projection of a tridimensional ionisation cone, which shares the same axis with the radio emission. A dust lane perpendicular to this axis obstructs the nucleus from direct view. [6] A disk of material was found when the data cubes of VLT were analysed. It is aligned with the nucleus and circles it and possibly provides gas to the active galactic nucleus. [7] The mass of the supermassive black hole has been estimated based on the galaxy stellar velocity dispersion to be 106.4 M⊙. [8] It has been proposed that the gas outflow has led to star formation on two locations on the bar of the galaxy which lie at the location where the gas from the nucleus encounters the dense material of the bar. [9]

Via observations of the galaxy from the XMM Newton telescope in 2009, the galaxy is found to have a Compton–thick active galactic nucleus. Also the galaxy emits soft X-rays, mainly from photoionized matter. [10] The presence of the compton-thick column which obstructs the nucleus was confirmed from observations by NuSTAR. [11]

Ultraluminous X-ray source

In 2004, Guainazzi et al. detected in the images from XMM-Newton an ultraluminous X-ray source, named NGC 5643 ULX1, located within 0.8 arcminutes from the nucleus. The source outshone the nucleus in X-rays and if it is located within NGC 5643 its luminosity is over 1040 erg/s. Its luminosity is variable. [12] The X-rays could be produced either by an advection dominated disc or a Comptonising corona and the X-ray source is considered to be a black hole of stellar origin of approximately 30 solar masses. [13]

Supernovae

NGC 5643 has been the home of two supernovae:

Nearby galaxies

NGC 5643 has a satellite dwarf galaxy, ESO 273-014. [22] NGC 5643 is the foremost member of a small galaxy group that also includes NGC 5530. [23]

Related Research Articles

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Messier 61 is an intermediate barred spiral galaxy in the Virgo Cluster of galaxies. It was first discovered by Barnaba Oriani on May 5, 1779, six days before Charles Messier discovered the same galaxy. Messier had observed it on the same night as Oriani but had mistaken it for a comet. Its distance has been estimated to be 45.61 million light years from the Milky Way Galaxy. It is a member of the M61 Group of galaxies, which is a member of the Virgo II Groups, a series of galaxies and galaxy clusters strung out from the southern edge of the Virgo Supercluster.

<span class="mw-page-title-main">NGC 4725</span> Galaxy in the constellation Coma Berenices

NGC 4725 is an intermediate barred spiral galaxy with a prominent ring structure, located in the northern constellation of Coma Berenices near the north galactic pole. It was discovered by German-born British astronomer William Herschel on April 6, 1785. The galaxy lies at a distance of approximately 40 megalight-years from the Milky Way. NGC 4725 is the brightest member of the Coma I Group of the Coma-Sculptor Cloud, although it is relatively isolated from the other members of this group. This galaxy is strongly disturbed and is interacting with neighboring spiral galaxy NGC 4747, with its spiral arms showing indications of warping. The pair have an angular separation of 24′, which corresponds to a projected linear separation of 370 kly. A tidal plume extends from NGC 4747 toward NGC 4725.

<span class="mw-page-title-main">NGC 7793</span> Galaxy in the constellation Sculptor

NGC 7793 is a flocculent spiral galaxy in the southern constellation of Sculptor. It was discovered in 1826 by Scottish astronomer James Dunlop. The galaxy is located at a distance of 12.2 million light years and is receding with a heliocentric radial velocity of 227 km/s. NGC 7793 is one of the five brightest galaxies within the Sculptor Group.

<span class="mw-page-title-main">NGC 3227</span> Galaxy in the constellation Leo

NGC 3227 is an intermediate spiral galaxy that is interacting with the dwarf elliptical galaxy NGC 3226. The two galaxies are one of several examples of a spiral with a dwarf elliptical companion that are listed in the Atlas of Peculiar Galaxies. Both galaxies may be found in the constellation Leo. It is a member of the NGC 3227 Group of galaxies, which is a member of the Leo II Groups, a series of galaxies and galaxy clusters strung out from the right edge of the Virgo Supercluster.

<span class="mw-page-title-main">NGC 4945</span> Galaxy in the constellation Centaurus

NGC 4945 (also known as Caldwell 83) is a barred spiral galaxy in the constellation Centaurus, visible near the star Xi Centauri. The galaxy was discovered by James Dunlop in 1826 and is thought to be similar to the Milky Way Galaxy, although X-ray observations show that NGC 4945 has an unusual energetic Seyfert 2 nucleus that might house a supermassive black hole. Around the nucleus of the galaxy, there is a dense disk of dust and gas, along with many dense star clusters. This object has an estimated mass of 1.4+1.4
−0.7×1011 M☉.

<span class="mw-page-title-main">NGC 5033</span> Galaxy in the constellation Canes Venatici

NGC 5033 is an inclined spiral galaxy located in the constellation Canes Venatici. Distance estimates vary from between 38 and 60 million light years from the Milky Way. The galaxy has a very bright nucleus and a relatively faint disk. Significant warping is visible in the southern half of the disk. The galaxy's relatively large angular size and relatively high surface brightness make it an object that can be viewed and imaged by amateur astronomers. The galaxy's location relatively near Earth and its active galactic nucleus make it a commonly studied object for professional astronomers.

<span class="mw-page-title-main">NGC 1566</span> Galaxy in the constellation Dorado

NGC 1566, sometimes known as the Spanish Dancer, is an intermediate spiral galaxy in the constellation Dorado, positioned about 3.5° to the south of the star Gamma Doradus. It was discovered on May 28, 1826 by Scottish astronomer James Dunlop. At 10th magnitude, it requires a telescope to view. The distance to this galaxy remains elusive, with measurements ranging from 6 Mpc up to 21 Mpc.

<span class="mw-page-title-main">NGC 4639</span> Galaxy in the constellation Virgo

NGC 4639 is a barred spiral galaxy located in the equatorial constellation of Virgo. It was discovered by German-born astronomer William Herschel on 12 April 1784. John L. E. Dreyer described it as "pretty bright, small, extended, mottled but not resolved, 12th magnitude star 1 arcmin to southeast". This is a relatively nearby galaxy, lying approximately 72 million light-years away from the Milky Way. It is a companion to NGC 4654, and the two appear to have interacted roughly 500 million years ago. NGC 4639 is a member of the Virgo Cluster.

<span class="mw-page-title-main">NGC 4051</span> Galaxy in the constellation Ursa Major

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<span class="mw-page-title-main">NGC 3169</span> Galaxy in the constellation Sextans

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<span class="mw-page-title-main">NGC 2782</span> Galaxy in the constellation Lynx

NGC 2782 is a peculiar spiral galaxy that formed after a galaxy merger in the constellation Lynx. The galaxy lies 75 million light years away from Earth, which means, given its apparent dimensions, that NGC 2782 is approximately 100,000 light years across. NGC 2782 has an active galactic nucleus and it is a starburst and a type 1 Seyfert galaxy. NGC 2782 is mentioned in the Atlas of Peculiar Galaxies in the category galaxies with adjacent loops.

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

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<span class="mw-page-title-main">NGC 3147</span> Galaxy in the constellation Draco

NGC 3147 is a spiral galaxy located in the constellation Draco. It is located at a distance of about 130 million light years from Earth, which, given its apparent dimensions, means that NGC 3147 is about 140,000 light years across. It was discovered by William Herschel on April 3, 1785.

<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 3367</span> Spiral galaxy in the constellation Leo

NGC 3367 is a barred spiral galaxy located in the constellation Leo. It is located at a distance of about 120 million light years from Earth, which, given its apparent dimensions, means that NGC 3367 is about 85,000 light years across. It was discovered by William Herschel on March 19, 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 4636</span> Galaxy in the constellation Virgo

NGC 4636 is an elliptical galaxy located in the constellation Virgo. It is a member of the NGC 4753 Group of galaxies, which is a member of the Virgo II Groups, a series of galaxies and galaxy clusters strung out from the southern edge of the Virgo Supercluster. It is located at a distance of about 55 million light years from Earth, which, given its apparent dimensions, means that NGC 4636 is about 105,000 light years across.

<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">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.

References

  1. 1 2 3 4 5 6 "NASA/IPAC Extragalactic Database". Results for NGC 5643. Retrieved 2016-01-18.
  2. 1 2 Hoyt, Taylor J.; Beaton, Rachael L.; Freedman, Wendy L.; Jang, In Sung; Lee, Myung Gyoon; Madore, Barry F.; Monson, Andrew J.; Neeley, Jillian R.; Rich, Jeffrey A.; Seibert, Mark (2021). "The Carnegie Chicago Hubble Program X: Tip of the Red Giant Branch Distances to NGC 5643 and NGC 1404". The Astrophysical Journal. 915 (1): 34. arXiv: 2101.12232 . Bibcode:2021ApJ...915...34H. doi: 10.3847/1538-4357/abfe5a . S2CID   231728270.
  3. ↑ O'Meara, Stephen James (2013). Southern gems. Cambridge: Cambridge University Press. p. 272. ISBN   978-1107015012.
  4. ↑ Martini, Paul; Regan, Michael W.; Mulchaey, John S.; Pogge, Richard W. (June 2003). "Circumnuclear Dust in Nearby Active and Inactive Galaxies. I. Data". The Astrophysical Journal Supplement Series. 146 (2): 353–406. arXiv: astro-ph/0212396 . Bibcode:2003ApJS..146..353M. doi:10.1086/367817. S2CID   15161097.
  5. ↑ "Hidden from view". www.eso.org. Retrieved 28 May 2018.
  6. ↑ Simpson, Chris; Wilson, A. S.; Bower, Gary; Heckman, T. M.; Krolik, J. H.; Miley, G. K. (January 1997). "A One-sided Ionization Cone in the Seyfert 2 Galaxy NGC 5643". The Astrophysical Journal. 474 (1): 121–128. Bibcode:1997ApJ...474..121S. doi: 10.1086/303466 .
  7. ↑ Menezes, R. B.; da Silva, P.; Ricci, T. V.; Steiner, J. E.; May, D.; Borges, B. W. (16 April 2015). "A treatment procedure for VLT/SINFONI data cubes: application to NGC 5643". Monthly Notices of the Royal Astronomical Society. 450 (1): 369–396. arXiv: 1504.02933 . Bibcode:2015MNRAS.450..369M. doi: 10.1093/mnras/stv629 .
  8. ↑ Goulding, A. D.; Alexander, D. M.; Lehmer, B. D.; Mullaney, J. R. (21 July 2010). "Towards a complete census of active galactic nuclei in nearby galaxies: the incidence of growing black holes". Monthly Notices of the Royal Astronomical Society. 406 (1): 597–611. arXiv: 1003.3015 . Bibcode:2010MNRAS.406..597G. doi: 10.1111/j.1365-2966.2010.16700.x . S2CID   53579415.
  9. ↑ Cresci, G.; Marconi, A.; Zibetti, S.; Risaliti, G.; Carniani, S.; Mannucci, F.; Gallazzi, A.; Maiolino, R.; Balmaverde, B.; Brusa, M.; Capetti, A.; Cicone, C.; Feruglio, C.; Bland-Hawthorn, J.; Nagao, T.; Oliva, E.; Salvato, M.; Sani, E.; Tozzi, P.; Urrutia, T.; Venturi, G. (8 October 2015). "The MAGNUM survey: positive feedback in the nuclear region of NGC 5643 suggested by MUSE". Astronomy & Astrophysics. 582: A63. arXiv: 1508.04464 . Bibcode:2015A&A...582A..63C. doi:10.1051/0004-6361/201526581. S2CID   55222207.
  10. ↑ Matt, G.; Bianchi, S.; Marinucci, A.; Guainazzi, M.; Iwawasa, K.; Jimenez Bailon, E. (2 August 2013). "X-ray observations of the Compton-thick Seyfert 2 galaxy, NGC 5643". Astronomy & Astrophysics. 556: A91. arXiv: 1307.1591 . Bibcode:2013A&A...556A..91M. doi:10.1051/0004-6361/201321293. S2CID   53347282.
  11. ↑ Annuar, A.; Gandhi, P.; Alexander, D. M.; Lansbury, G. B.; Arévalo, P.; Ballantyne, D. R.; Baloković, M.; Bauer, F. E.; Boggs, S. E.; Brandt, W. N.; Brightman, M.; Christensen, F. E.; Craig, W. W.; Moro, A. Del; Hailey, C. J.; Harrison, F. A.; Hickox, R. C.; Matt, G.; Puccetti, S.; Ricci, C.; Rigby, J. R.; Stern, D.; Walton, D. J.; Zappacosta, L.; Zhang, W. (4 December 2015). "NuSTAR Observations of the Compton-thick Active Galactic Nucleus and Ultraluminous X-ray Source Candidate in NGC 5643". The Astrophysical Journal. 815 (1): 36. arXiv: 1509.03322 . Bibcode:2015ApJ...815...36A. doi:10.1088/0004-637X/815/1/36. S2CID   11400958.
  12. ↑ Guainazzi, M.; Rodriguez-Pascual, P.; Fabian, A. C.; Iwasawa, K.; Matt, G. (November 2004). "Unveiling the nature of the highly obscured active galactic nucleus in NGC 5643 with". Monthly Notices of the Royal Astronomical Society. 355 (1): 297–306. arXiv: astro-ph/0408300 . Bibcode:2004MNRAS.355..297G. doi: 10.1111/j.1365-2966.2004.08317.x . S2CID   119067322.
  13. ↑ Pintore, Fabio; Zampieri, Luca; Sutton, Andrew D.; Roberts, Timothy P.; Middleton, Matthew J.; Gladstone, Jeanette C. (11 June 2016). "The ultraluminous X-ray source NGC 5643 ULX1: a large stellar mass black hole accreting at super-Eddington rates?". Monthly Notices of the Royal Astronomical Society. 459 (1): 455–466. arXiv: 1603.05542 . Bibcode:2016MNRAS.459..455P. doi: 10.1093/mnras/stw669 .
  14. ↑ Parker, S.; Amorim, A.; Parrent, J. T.; Sand, D.; Valenti, S.; Graham, M. L.; Howell, D. A. (2013). "Supernova 2013aa in NGC 5643 = PSN J14323388-4413278". Central Bureau Electronic Telegrams. 3416: 1. Bibcode:2013CBET.3416....1P.
  15. ↑ "SN 2013aa". Transient Name Server. IAU . Retrieved 6 December 2024.
  16. ↑ Sternberg, A.; Gal-Yam, A.; Simon, J. D.; Patat, F.; Hillebrandt, W.; Phillips, M. M.; Foley, R. J.; Thompson, I.; Morrell, N.; Chomiuk, L.; Soderberg, A. M.; Yong, D.; Kraus, A. L.; Herczeg, G. J.; Hsiao, E. Y.; Raskutti, S.; Cohen, J. G.; Mazzali, P. A.; Nomoto, K. (25 July 2014). "Multi-epoch high-spectral-resolution observations of neutral sodium in 14 Type Ia supernovae". Monthly Notices of the Royal Astronomical Society. 443 (2): 1849–1860. arXiv: 1311.3645 . Bibcode:2014MNRAS.443.1849S. doi: 10.1093/mnras/stu1202 .
  17. ↑ Bishop, David. "Bright Supernovae - 2013". Rochester Astronomy. Retrieved 8 December 2024.
  18. ↑ Tartaglia, L.; Sand, D.; Wyatt, S.; Valenti, S.; Bostroem, K. A.; Reichart, D. E.; Haislip, J. B.; Kouprianov, V. (2017). "The discovery of DLT17u/AT 2017cbv". The Astronomer's Telegram. 10158: 1. Bibcode:2017ATel10158....1T.
  19. ↑ "SN 2017cbv". Transient Name Server. IAU . Retrieved 6 December 2024.
  20. ↑ Coulter, D. A.; Kilpatrick, C. D.; Foley, R. J.; Anais, J.; Phillips, M. M.; Drout, M. R.; Madore, B. F.; Piro, A. L.; Shappee, B. J.; Hsiao, E. Y. (2017). "Swope Photometric Observations of SN 2017cbv = DLT17u". The Astronomer's Telegram. 10167: 1. Bibcode:2017ATel10167....1C.
  21. ↑ Bishop, David. "Bright Supernovae - 2017". Rochester Astronomy. Retrieved 9 December 2024.
  22. ↑ Karachentsev, Igor D.; Kaisina, Elena I.; Makarov, Dmitry I. (3 December 2013). "Suites of Dwarfs Around Nearby Giant Galaxies". The Astronomical Journal. 147 (1): 13. arXiv: 1310.6838 . Bibcode:2014AJ....147...13K. doi:10.1088/0004-6256/147/1/13. S2CID   119245124.
  23. ↑ Makarov, Dmitry; Karachentsev, Igor (21 April 2011). "Galaxy groups and clouds in the local (z~ 0.01) Universe". Monthly Notices of the Royal Astronomical Society. 412 (4): 2498–2520. arXiv: 1011.6277 . Bibcode:2011MNRAS.412.2498M. doi: 10.1111/j.1365-2966.2010.18071.x . S2CID   119194025.
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