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Coordinates: Sky map 13h 37m 00.9s, −29° 51′ 57″
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=== Supernovae ===
=== Supernovae ===
Six [[supernova]]e have been observed in M83:
Six [[supernova]]e have been observed in M83: SN 1923A (mag. 14),<ref>[https://www.wis-tns.org/object/1923A Transient Name Server entry for SN 1923A.] Retrieved 8 July 2023.</ref> SN 1945B (mag. 14.2),<ref>[https://www.wis-tns.org/object/1945B Transient Name Server entry for SN 1945B.] Retrieved 8 July 2023.</ref> SN 1950B (mag. 14.5),<ref>[https://www.wis-tns.org/object/1950B Transient Name Server entry for SN 1950B.] Retrieved 8 July 2023.</ref> SN 1957D (mag. 15),<ref>[https://www.wis-tns.org/object/1957D Transient Name Server entry for SN 1957D.] Retrieved 8 July 2023.</ref><ref name=Romaniello2005 /> SN 1968L ([[Type II supernova|type II-P]], mag. 11.9),<ref>{{cite journal
* SN 1923A (type unknown, mag. 14)<ref>[https://www.wis-tns.org/object/1923A Transient Name Server entry for SN 1923A.] Retrieved 8 July 2023.</ref> was discovered by [[Carl Otto Lampland]] on 5 May 1923.<ref>{{cite journal | bibcode=1923PASP...35..166L | title=Note on a Nova | last1=Lampland | first1=C. O. | journal=Publications of the Astronomical Society of the Pacific | date=1923 | volume=35 | issue=205 | page=166 | doi=10.1086/123293}}</ref>
* SN 1945B (type unknown, mag. 14.2)<ref>[https://www.wis-tns.org/object/1945B Transient Name Server entry for SN 1945B.] Retrieved 8 July 2023.</ref> was discovered by [[William Liller]] on 13 July 1945.<ref>{{cite journal | bibcode=1990IAUC.5091....2L | title=Supernova 1945B in NGC 5236 | last1=Liller | first1=W. | journal=International Astronomical Union Circular | date=1990 | issue=5091 | page=2}}</ref>
* SN 1950B (type unknown, mag. 14.5)<ref>[https://www.wis-tns.org/object/1950B Transient Name Server entry for SN 1950B.] Retrieved 8 July 2023.</ref> was discovered by [[Guillermo Haro]] on 15 March 1950.
* SN 1957D (type unknown, mag. 15)<ref>[https://www.wis-tns.org/object/1957D Transient Name Server entry for SN 1957D.] Retrieved 8 July 2023.</ref><ref name=Romaniello2005 /> was discovered by H. S. Gates on 28 December 1957.<ref>{{cite journal | bibcode=1959LAstr..73..453B | title=Les cinq supernovæ découvertes depuis 1957 | last1=Bertaud | first1=Ch. | journal=L'Astronomie | date=1959 | volume=73 | page=453}}</ref>
* SN 1968L ([[Type II supernova|type II-P]], mag. 11.9)<ref>{{cite journal
| bibcode = 1996AJ....111.2017V
| bibcode = 1996AJ....111.2017V
| title = Supernovae and Massive Star Formation Regions
| title = Supernovae and Massive Star Formation Regions
Line 50: Line 55:
| page = 2017
| page = 2017
| doi = 10.1086/117937
| doi = 10.1086/117937
}}</ref><ref>[https://www.wis-tns.org/object/1968L Transient Name Server entry for SN 1968L.] Retrieved 8 July 2023.</ref> and SN 1983N ([[type Ia supernova|type&nbsp;Ia]], mag. 11.9).<ref>[https://www.wis-tns.org/object/1983N Transient Name Server entry for SN 1983N.] Retrieved 8 July 2023.</ref>
}}</ref><ref>[https://www.wis-tns.org/object/1968L Transient Name Server entry for SN 1968L.] Retrieved 8 July 2023.</ref> was discovered on 17 July 1968.
⚫
* SN 1983N ([[type Ia supernova|type&nbsp;Ia]], mag. 11.9)<ref>[https://www.wis-tns.org/object/1983N Transient Name Server entry for SN 1983N.] Retrieved 8 July 2023.</ref> was discovered by [[Robert Evans (astronomer)|Robert Evans]] from Australia on July 3, 1983.<ref name=Thompson_et_al_1983 /> On July 6, it was observed with the [[Very Large Array]] and became the first type I supernova to have a [[Astronomical radio source|radio emission]] detected. The supernova reached peak optical brightness on July 17, achieving an [[apparent visual magnitude]] of 11.54.<ref name=Sramek_et_al_1984 /> Although identified as type I, the spectrum was considered peculiar. A year after the explosion, about {{val|0.3|ul=Solar mass}} of iron was discovered in the ejecta. This was the first time that such a large amount of iron was unambiguously detected from a supernova explosion.<ref name=Graham_et_al_1986 /> SN 1983N became the modern prototype of a hydrogen deficient [[type Ib supernova]], with the progenitor being inferred as a [[Wolf–Rayet star]].<ref name=Gaskell_et_al_1986 />

⚫
'''SN 1983N''' was discovered by [[Robert Evans (astronomer)|Robert Evans]] from Australia on July 3, 1983.<ref name=Thompson_et_al_1983 /> On July 6, it was observed with the [[Very Large Array]] and became the first type I supernova to have a [[Astronomical radio source|radio emission]] detected. The supernova reached peak optical brightness on July 17, achieving an [[apparent visual magnitude]] of 11.54.<ref name=Sramek_et_al_1984 /> Although identified as type I, the spectrum was considered peculiar. A year after the explosion, about {{val|0.3|ul=Solar mass}} of iron was discovered in the ejecta. This was the first time that such a large amount of iron was unambiguously detected from a supernova explosion.<ref name=Graham_et_al_1986 /> SN 1983N became the modern prototype of a hydrogen deficient [[type Ib supernova]], with the progenitor being inferred as a [[Wolf–Rayet star]].<ref name=Gaskell_et_al_1986 />


== Environment ==
== Environment ==

Revision as of 21:32, 26 November 2024

This article is about the galaxy. For the band, see M83 (band).

Messier 83
Messier 83 captured by the Wide Field Imager at ESO's La Silla Observatory in September 2008
Observation data (J2000 epoch)
ConstellationHydra
Right ascension13h 37m 00.919s[1]
Declination−29° 51′ 56.74″[1]
Redshift0.001721±0.000013[2]
Heliocentric radial velocity508 km/s[3]
Distance14.7 Mly (4.50 Mpc)[3]
Apparent magnitude (V)7.6[4]
Characteristics
TypeSAB(s)c[2]
Size36.24 kiloparsecs (118,000 light-years)
(diameter; 26.0 mag/arcsec2 B-band isophote)[2]
Apparent size (V)12′.9 × 11′.5[5]
Other designations
Southern Pinwheel Galaxy, ESO 444- G 081, IRAS 13341-2936, NGC 5236, UGCA 366, MCG -05-32-050, PGC 48082[6]

Messier 83 or M83, also known as the Southern Pinwheel Galaxy and NGC 5236, is a barred spiral galaxy[7] approximately 15 million light-years away in the constellation borders of Hydra and Centaurus. Nicolas-Louis de Lacaille discovered M83 on 17 February 1752 at the Cape of Good Hope.[8] Charles Messier added it to his catalogue of nebulous objects (now known as the Messier Catalogue) in March 1781.[8]

It is one of the closest and brightest barred spiral galaxies in the sky, and is visible with binoculars.[9] It has an isophotal diameter at about 36.24 kiloparsecs (118,000 light-years). Its nickname of the Southern[a] Pinwheel derives from its resemblance to the Pinwheel Galaxy (M101).

Characteristics

M83 is a massive, grand design spiral galaxy.[10] Its morphological classification in the De Vaucouleurs system is SAB(s)c,[2] where the 'SAB' denotes a weak-barred spiral, '(s)' indicates a pure spiral structure with no ring, and 'c' means the spiral arms are loosely wound.[11] The peculiar dwarf galaxy NGC 5253 lies near M83,[12] and the two likely interacted within the last billion years resulting in starburst activity in their central regions.[10]

The star formation rate in M83 is higher along the leading edge of the spiral arms, as predicted by density wave theory.[13] NASA's Galaxy Evolution Explorer project on 16 April 2008 reported finding large numbers of new stars in the outer reaches of the galaxy—20 kpc from the center. It had been thought that these areas lacked the materials necessary for star formation.[14][15]

Supernovae

Six supernovae have been observed in M83:

  • SN 1923A (type unknown, mag. 14)[16] was discovered by Carl Otto Lampland on 5 May 1923.[17]
  • SN 1945B (type unknown, mag. 14.2)[18] was discovered by William Liller on 13 July 1945.[19]
  • SN 1950B (type unknown, mag. 14.5)[20] was discovered by Guillermo Haro on 15 March 1950.
  • SN 1957D (type unknown, mag. 15)[21][22] was discovered by H. S. Gates on 28 December 1957.[23]
  • SN 1968L (type II-P, mag. 11.9)[24][25] was discovered on 17 July 1968.
  • SN 1983N (type Ia, mag. 11.9)[26] was discovered by Robert Evans from Australia on July 3, 1983.[27] On July 6, it was observed with the Very Large Array and became the first type I supernova to have a radio emission detected. The supernova reached peak optical brightness on July 17, achieving an apparent visual magnitude of 11.54.[28] Although identified as type I, the spectrum was considered peculiar. A year after the explosion, about 0.3 M☉ of iron was discovered in the ejecta. This was the first time that such a large amount of iron was unambiguously detected from a supernova explosion.[29] SN 1983N became the modern prototype of a hydrogen deficient type Ib supernova, with the progenitor being inferred as a Wolf–Rayet star.[30]

Environment

M83 is at the center of one of two subgroups within the Centaurus A/M83 Group, a nearby galaxy group.[31] Centaurus A is at the center of the other subgroup. These are sometimes identified as one group,[32][33] and sometimes as two.[34] However, the galaxies around Centaurus A and the galaxies around M83 are physically close to each other, and both subgroups appear not to be moving relative to each other.[35]

See also

References

  1. ^ a b Skrutskie, Michael F.; Cutri, Roc M.; Stiening, Rae; Weinberg, Martin D.; Schneider, Stephen E.; Carpenter, John M.; Beichman, Charles A.; Capps, Richard W.; Chester, Thomas; Elias, Jonathan H.; Huchra, John P.; Liebert, James W.; Lonsdale, Carol J.; Monet, David G.; Price, Stephan; Seitzer, Patrick; Jarrett, Thomas H.; Kirkpatrick, J. Davy; Gizis, John E.; Howard, Elizabeth V.; Evans, Tracey E.; Fowler, John W.; Fullmer, Linda; Hurt, Robert L.; Light, Robert M.; Kopan, Eugene L.; Marsh, Kenneth A.; McCallon, Howard L.; Tam, Robert; Van Dyk, Schuyler D.; Wheelock, Sherry L. (1 February 2006). "The Two Micron All Sky Survey (2MASS)". The Astronomical Journal. 131 (2): 1163–1183. Bibcode:2006AJ....131.1163S. doi:10.1086/498708. ISSN 0004-6256. S2CID 18913331.
  2. ^ a b c d De Vaucouleurs, Gerard; De Vaucouleurs, Antoinette; Corwin, Herold G., Jr.; Buta, Ronald J.; Paturel, Georges; Fouque, Pascal (1991). Third Reference Catalogue of Bright Galaxies. Bibcode:1991rc3..book.....D.{{cite book}}: CS1 maint: multiple names: authors list (link)
  3. ^ a b Tully, R. Brent; et al. (August 2016). "Cosmicflows-3". The Astronomical Journal. 152 (2): 21. arXiv:1605.01765. Bibcode:2016AJ....152...50T. doi:10.3847/0004-6256/152/2/50. S2CID 250737862. 50.
  4. ^ "Messier 83". SEDS Messier Catalog. Retrieved 30 April 2022.
  5. ^ "NASA/IPAC Extragalactic Database". Results for NGC 5236. Retrieved 8 December 2006.
  6. ^ "M 83". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 29 November 2009.
  7. ^ "Multimedia Gallery: M83 – Southern Pinwheel Galaxy". NASA/JPL-Caltech/WISE Team. 25 June 2010.
  8. ^ a b Jones, K. G. (1991). Messier's Nebulae and Star Clusters (2nd ed.). Cambridge: Cambridge University Press. ISBN 978-0-521-37079-0.
  9. ^ "M 83". messierobjects101.com. 11 October 2016. Retrieved 19 April 2018.
  10. ^ a b Calzetti, Daniela; Conselice, Christopher J.; Gallagher, John S. III; Kinney, Anne L. (August 1999). "The Structure and Morphology of the Ionized Gas in Starburst Galaxies: NGC 5253/5236". The Astronomical Journal. 118 (2): 797–816. arXiv:astro-ph/9904428. Bibcode:1999AJ....118..797C. doi:10.1086/300972. S2CID 16296827.
  11. ^ de Vaucouleurs, Gérard (April 1963). "Revised Classification of 1500 Bright Galaxies". Astrophysical Journal Supplement. 8: 31. Bibcode:1963ApJS....8...31D. doi:10.1086/190084.
  12. ^ Thim, Frank; et al. (June 2003), "The Cepheid Distance to NGC 5236 (M83) with the ESO Very Large Telescope", The Astrophysical Journal, 590 (1): 256–270, arXiv:astro-ph/0303101, Bibcode:2003ApJ...590..256T, doi:10.1086/374888, S2CID 121984029
  13. ^ Silva-Villa, E.; Larsen, S. S. (January 2012). "The relation between surface star formation rate density and spiral arms in NGC 5236 (M 83)". Astronomy & Astrophysics. 537: 9. arXiv:1111.1249. Bibcode:2012A&A...537A.145S. doi:10.1051/0004-6361/201117432. S2CID 119295019. A145.
  14. ^ "Stellar Birth in the Galactic Wilderness". 16 April 2008. Archived from the original on 4 March 2016. Retrieved 15 December 2018.
  15. ^ Dong, Hui; et al. (July 2008). "Spitzer Observations of Star Formation in the Extreme Outer Disk of M83 (NGC5236)". The Astronomical Journal. 136 (1): 479–497. arXiv:0804.3632. Bibcode:2008AJ....136..479D. doi:10.1088/0004-6256/136/1/479. S2CID 119189782.
  16. ^ Transient Name Server entry for SN 1923A. Retrieved 8 July 2023.
  17. ^ Lampland, C. O. (1923). "Note on a Nova". Publications of the Astronomical Society of the Pacific. 35 (205): 166. Bibcode:1923PASP...35..166L. doi:10.1086/123293.
  18. ^ Transient Name Server entry for SN 1945B. Retrieved 8 July 2023.
  19. ^ Liller, W. (1990). "Supernova 1945B in NGC 5236". International Astronomical Union Circular (5091): 2. Bibcode:1990IAUC.5091....2L.
  20. ^ Transient Name Server entry for SN 1950B. Retrieved 8 July 2023.
  21. ^ Transient Name Server entry for SN 1957D. Retrieved 8 July 2023.
  22. ^ Romaniello, Martino; Patat, Ferdinando; Panagia, Nino; Sparks, William B.; Gilmozzi, Roberto; Spyromilio, Jason (August 2005), "Very Large Telescope FORS1 Imaging Polarimetry of M83 (NGC 5236). I. Search for Light Echoes from Historical Supernovae", The Astrophysical Journal, 629 (1): 250–258, arXiv:astro-ph/0505100, Bibcode:2005ApJ...629..250R, doi:10.1086/431470, S2CID 118978264
  23. ^ Bertaud, Ch. (1959). "Les cinq supernovæ découvertes depuis 1957". L'Astronomie. 73: 453. Bibcode:1959LAstr..73..453B.
  24. ^ Van Dyk, Schuyler D.; Hamuy, Mario; Filippenko, Alexei V. (1996). "Supernovae and Massive Star Formation Regions". The Astronomical Journal. 111: 2017. Bibcode:1996AJ....111.2017V. doi:10.1086/117937.
  25. ^ Transient Name Server entry for SN 1968L. Retrieved 8 July 2023.
  26. ^ Transient Name Server entry for SN 1983N. Retrieved 8 July 2023.
  27. ^ Thompson, G. D.; et al. (1983). Green, D. W. E. (ed.). "Supernovae". IAU Circular. 3835: 1. Bibcode:1983IAUC.3835....1T.
  28. ^ Sramek, R. A.; et al. (October 1984). "Radio emission from a type I supernova : SN 1983.51 in NGC 5236". Astrophysical Journal. 285: L59–L62. Bibcode:1984ApJ...285L..59S. doi:10.1086/184365.
  29. ^ Graham, J. R.; et al. (January 1986). "Discovery of a large mass of iron in a type I supernova". Monthly Notices of the Royal Astronomical Society. 218: 93–102. Bibcode:1986MNRAS.218...93G. doi:10.1093/mnras/218.1.93.
  30. ^ Gaskell, C. M.; et al. (July 1986). "Type Ib Supernovae 1983n and 1985f: Oxygen-rich Late Time Spectra". Astrophysical Journal Letters. 306: L77. Bibcode:1986ApJ...306L..77G. doi:10.1086/184709.
  31. ^ Karachentsev, I. D.; et al. (2002). "New distances to galaxies in the Centaurus A group". Astronomy and Astrophysics. 385 (1): 21–31. Bibcode:2002A&A...385...21K. doi:10.1051/0004-6361:20020042.
  32. ^ R. B. Tully (1988). Nearby Galaxies Catalog. Cambridge: Cambridge University Press. ISBN 978-0-521-35299-4.
  33. ^ Fouque, P.; Gourgoulhon, E.; Chamaraux, P.; Paturel, G. (1992). "Groups of galaxies within 80 Mpc. II – The catalogue of groups and group members". Astronomy and Astrophysics Supplement. 93: 211–233. Bibcode:1992A&AS...93..211F.
  34. ^ Garcia, A. (1993). "General study of group membership. II – Determination of nearby groups". Astronomy and Astrophysics Supplement. 100: 47–90. Bibcode:1993A&AS..100...47G.
  35. ^ Karachentsev, I. D. (2005). "The Local Group and Other Neighboring Galaxy Groups". Astronomical Journal. 129 (1): 178–188. arXiv:astro-ph/0410065. Bibcode:2005AJ....129..178K. doi:10.1086/426368. S2CID 119385141.
  1. ^ Its declination means every day it passes the zenith of the sky at the matching parallel of the earth, which is that of northern Argentina. It can be viewed more than an ideal 15° above the horizon for a further 75° to the north, placing such a northern limit of good observation at the 45th parallel north
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