NGC 3982

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NGC 3982
NGC 3982 galaxy hubble.jpg
Observation data (J2000 epoch)
Constellation Ursa Major
Right ascension 11h 56m 28.1s[1]
Declination +55° 07′ 31″[1]
Redshift 1109 ± 6 km/s[1]
Distance 68.1 ± 2.5 Mly (20.89 ± 0.77 Mpc)[2]
Type SAB(r)b[1]
Apparent dimensions (V) 1′.7 × 1′.5[1]
Apparent magnitude (V) 12.0[1]
Other designations
UGC 6918,[1]PGC 37520[1]
See also: Galaxy, List of galaxies

NGC 3982 is an intermediate spiral galaxy approximately 68 million light-years away in the constellation Ursa Major. It is also known as UGC 6918. It was discovered by William Herschel on April 14, 1789 and misclassified as planetary nebula.[3] NGC 3982 is a part of the M109 Group.

At an apparent magnitude of 12.0, NGC 3982 needs a telescope to be viewed. Using small telescopes, the galaxy appears as a very faint, diffuse patch of light with its central region appearing as a slightly brighter diffuse ball.


NGC 3982 is a Seyfert 2 galaxy that spans about 30,000 light-years, about one-third of the size of our Milky Way galaxy. The galaxy is receding from us at about 1109 km/s. The galaxy is a typical spiral galaxy, similar to our Milky Way. It harbors a supermassive black hole at its core and has massive regions of star formation in the bright blue knots in the spiral arms.[4] Supernovae are likely to be found within these regions.

NGC 3982 has a high rate of star birth within its arms, which are lined by pink star-forming regions of glowing hydrogen and newborn blue star clusters. Its bright nucleus is home to older populations of stars, which grow more densely packed toward the center. The galaxy also has active star formation in the circumnuclear region estimated at 0.52 M⊙/year. The HST image of NGC 3982 shows a mini-spiral between the circumnuclear star-forming region and the galaxy's nucleus, which could be the channel through which gas is transported to the supermassive black hole from the star-forming region.

NGC 3982 is a member of the M109 Group, a group of galaxies located in the constellation Ursa Major that may contain over 50 galaxies. The group was named after the brightest galaxy in the group, the spiral galaxy M109.[5][6][7]

Astronomers are interested in studying this galaxy as it can help in measuring extragalactic distances. It is helpful because it possesses two tools used to estimate astronomical distances: a stellar explosion, or supernova; and Cepheid variable stars.

Supernova 1998aq[edit]

In 1998, the light from a supernova in NGC 3982 (later called SN 1998aq) reached earth and was discovered by British amateur astronomer Mark Armstrong. It was discovered when it had an apparent magnitude of 14.9 and it had grown considerably brighter by two days after its initial sighting (it reached a maximum magnitude of 14.0). The explosion resulted from a binary system where a white dwarf star was capturing mass from its companion star. When the white dwarf had gathered enough mass and was no longer able to support itself, the star detonated in a violent and extremely bright explosion. Since a supernova explosion roughly occurs in a typical spiral galaxy every 100 years, astronomers use high-resolution images of NGC 3982 and other galaxies to detect stars which are nearing a similar explosive descent into supernovae.

NGC 3982


  1. ^ a b c d e f g h "NASA/IPAC Extragalactic Database". Results for NGC 3982. Retrieved 2006-11-16. 
  2. ^ Riess, Adam G.; Li, Weidong; Stetson, Peter B.; Filippenko, Alexei V.; et al. (2005). "Cepheid Calibrations from the Hubble Space Telescope of the Luminosity of Two Recent Type Ia Supernovae and a Redetermination of the Hubble Constant". Astrophysical Journal 627 (2): 579–607. arXiv:astro-ph/0503159. Bibcode:2005ApJ...627..579R. doi:10.1086/430497. 
  3. ^ NGC 3982. Students for the Exploration and Development of Space. Retrieved March 3, 2009
  4. ^ Zhang, Shui-Nai; Gu, Qiu-Sheng; Wang, Yi-Peng (21 April 2008). "Circumnuclear Star Forming Activity in NGC 3982" (PDF). Chinese Journal of Astronomy and AstrophysicsEmail alert RSS feed. IOP Publishing. Retrieved 25 June 2014. 
  6. ^ P. Fouque; E. Gourgoulhon; P. Chamaraux; G. Paturel (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. 
  7. ^ G. Giuricin; C. Marinoni; L. Ceriani; A. Pisani (2000). "Nearby Optical Galaxies: Selection of the Sample and Identification of Groups". Astrophysical Journal 543 (1): 178–194. arXiv:astro-ph/0001140. Bibcode:2000ApJ...543..178G. doi:10.1086/317070. 

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