NGC 2336

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NGC 2336
NGC 2336 by Adam Block/Mount Lemmon SkyCenter
Observation data (J2000 epoch)
Right ascension 07h 27m 04.1s[1]
Declination+80° 10′ 41″[1]
Redshift0.007352 +/- 0.000003 [1]
Helio radial velocity2204 ± 1 km/s[1]
Distance90.7 ± 28 Mly (27.8 ± 8.6 Mpc)[1]
Apparent magnitude (V)10.3
TypeSAB(r)bc [1]
Apparent size (V)7′.1 × 3′.9[1]
Other designations
UGC 3809, MCG +13-06-006, PGC 21033[1]
See also: Galaxy, List of galaxies

NGC 2336 is a spiral galaxy located in the constellation Camelopardalis. It is located at a distance of circa 100 million light years from Earth, which, given its apparent dimensions, means that NGC 2336 is about 200,000 light years across. It was discovered by Wilhelm Tempel in 1876.[2]


The central area of NGC 2336 by Hubble Space Telescope.

NGC 2336 is a barred spiral galaxy, featuring a small optical bar.[3] At least 8 spiral arms, with numerous HII regions,[4] emanate from the ring-like structure around the bar. This ring has a radius of approximately 34 arcseconds, which corresponds to 5.3 kpc at the distance of NGC 2336.[5]

In the large arms of the galaxy have been observed 28 HII regions that may host young massive star clusters, and for two of them the nebular emission comprises most of the flux. Three of these HII areas have ages calculated to be 100 to 300 million years and have sizes between 300 and 600 parsecs. It is suggested they are star complexes that may coexist with younger ones. The most massive of the HII regions, number 13, has a mass estimated to be (550±169)×104 M and is 2,600 ly (810 pc) across.[6] Observations in the ultraviolet showed 78 star forming regions, with two them between the spiral arms and six at the galaxy ring. Their size is comparable to NGC 604, one of the largest nebulae in the Local Group. Star formation is more intense in the inner parts of the arms and at the ring.[7]

Scattered dust lanes which don't fit into a spiral structure have been observed in the nuclear region of the galaxy.[8] No emission has been detected in the radiowaves[3] and HI and Ha imaging of the nucleus of NGC 2336.[9] The nucleus is small, with an apparent diameter of 5 arcseconds, while the bulge is large, with a radius of 17 arcseconds.[5] In the centre of NGC 2336 lies a supermassive black hole whose mass is estimated to be 30 million (107.5) M based on Ks bulge luminosity.[10]


One supernova has been observed in NGC 2336, SN 1987L. It was discovered on 16 August 1987 at mag. 14.2. Spectrography performed by William Herschel Telescope on 20-21 October 1987 concluded that it was a type Ia supernova with its maximum approximately 100 days before.[11]

Nearby galaxies[edit]

NGC 2336 is the foremost galaxy of a small galaxy group known as the NGC 2336 group.[12] It forms a non-interacting pair with IC 467, which lies 20 arcminutes away.[13]


  1. ^ a b c d e f g h "NASA/IPAC Extragalactic Database". Results for NGC 2336. Retrieved 2016-01-18.
  2. ^ Seligman, Courtney. "NGC 2336". Celestial Atlas. Retrieved 19 November 2018.
  3. ^ a b Beck, R.; Shoutenkov, V.; Ehle, M.; Harnett, J. I.; Haynes, R. F.; Shukurov, A.; Sokoloff, D. D.; Thierbach, M. (29 July 2002). "Magnetic fields in barred galaxies". Astronomy & Astrophysics. 391 (1): 83–102. doi:10.1051/0004-6361:20020642.
  4. ^ Sandage, A., Bedke, J. (1994), The Carnegie Atlas of Galaxies. Volume I, Carnegie Institution of Washington, p. 15
  5. ^ a b Gusev, A. S.; M.–G. Park (17 November 2003). "Structure and stellar population of ringed barred galaxy NGC 2336". Astronomy & Astrophysics. 410 (1): 117–129. Bibcode:2003A&A...410..117G. doi:10.1051/0004-6361:20031215.
  6. ^ Gusev, A. S.; Sakhibov, F.; Piskunov, A. E.; Kharchenko, N. V.; Bruevich, V. V.; Ezhkova, O. V.; Guslyakova, S. A.; Lang, V.; Shimanovskaya, E. V.; Efremov, Y. N. (11 April 2016). "A spectral and photometric study of 102 star-forming regions in seven spiral galaxies". Monthly Notices of the Royal Astronomical Society. 457 (3): 3334–3355. arXiv:1601.07470. Bibcode:2016MNRAS.457.3334G. doi:10.1093/mnras/stw212.
  7. ^ Rahna, P T; Das, M; Murthy, Jayant; Gudennavar, S B; Bubbly, S G (17 August 2018). "A study of the star forming regions in the spiral galaxy NGC 2336 using the Ultraviolet Imaging Telescope (UVIT)". Monthly Notices of the Royal Astronomical Society. 481 (1): 1212. arXiv:1803.00506. Bibcode:2018MNRAS.481.1212R. doi:10.1093/mnras/sty2250.
  8. ^ 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.
  9. ^ Garrido, O.; Marcelin, M.; Amram, P. (21 March 2004). "GHASP: an Hα kinematic survey of spiral and irregular galaxies – III. 15 new velocity fields and study of 46 rotation curves". Monthly Notices of the Royal Astronomical Society. 349 (1): 225–239. Bibcode:2004MNRAS.349..225G. doi:10.1111/j.1365-2966.2004.07483.x.
  10. ^ Dong, X. Y.; De Robertis, M. M. (March 2006). "Low-Luminosity Active Galaxies and Their Central Black Holes". The Astronomical Journal. 131 (3): 1236–1252. arXiv:astro-ph/0510694. Bibcode:2006AJ....131.1236D. doi:10.1086/499334.
  11. ^ Pearce, Gillian; Patchett, Bruce; Allington-Smith, Jeremy; Parry, Ian (1988). "Observations of the supernova SN1987L with the new Faint Object Spectrograph on the 4.2 m William Herschel Telescope". Astrophysics and Space Science. 150 (2): 267–271. doi:10.1007/BF00641721.
  12. ^ 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.
  13. ^ de Vaucouleurs, G.; de Vaucouleurs, A.; Corwin, J. R. (1976). "Second reference catalogue of bright galaxies". Second Reference Catalogue of Bright Galaxies. 1976. Bibcode:1976RC2...C......0D.CS1 maint: Multiple names: authors list (link)

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