NGC 3891

NGC 3891
NGC 3891 imaged by SDSS
Observation data (J2000 epoch)
ConstellationUrsa Major
Right ascension11h 48m 03.3648s
Declination+30° 21′ 33.621″
Redshift0.020980±0.00000661
Heliocentric radial velocity6,290±2 km/s
Distance330.46 ± 14.72 Mly (101.320 ± 4.514 Mpc)
Group or clusterComa Cluster
Apparent magnitude (V)13.3g
Characteristics
TypeSbc
Size~221,100 ly (67.79 kpc) (estimated)
Apparent size (V)1.54′ × 1.15′
Other designations
2MASX J11480336+3021335, UGC 6772, MCG +05-28-031, PGC 36832, CGCG 157-035

NGC 3891 is a large spiral galaxy in the constellation of Ursa Major. Its velocity with respect to the cosmic microwave background is 6,581±20 km/s, which corresponds to a Hubble distance of 316.6 ± 22.2 Mly (97.06 ± 6.80 Mpc). However, 10 non-redshift measurements give a slightly farther mean distance of 330.46 ± 14.72 Mly (101.320 ± 4.514 Mpc). It was discovered by German-British astronomer William Herschel on 3 February 1788.

NGC 3891 is a LINER galaxy, i.e. a galaxy whose nucleus has an emission spectrum characterized by broad lines of weakly ionized atoms. It is also a radio galaxy, i.e. it has giant regions of radio emission extending well beyond its visible structure.

NGC 3891 is a member of the Coma cluster.

Supernovae

Two supernovae have been observed in NGC 3891:

See also

References

  1. 1 2 3 4 5 6 7 8 9 10 11 "Results for object NGC 3891". NASA/IPAC Extragalactic Database. NASA and Caltech. Retrieved 7 February 2026.
  2. ↑ "Distance Results for NGC 3891". NASA/IPAC EXTRAGALACTIC DATABASE. NASA. Retrieved 7 February 2026.
  3. ↑ Herschel, William (1789). "Catalogue of a Second Thousand of New Nebulae and Clusters of Stars; with a Few Introductory Remarks on the Construction of the Heavens". Philosophical Transactions of the Royal Society of London. 79: 212–255. Bibcode:1789RSPT...79..212H. doi:10.1098/rstl.1789.0021.
  4. ↑ Seligman, Courtney. "New General Catalogue Objects: NGC 3891". Celestial Atlas. Retrieved 7 February 2026.
  5. ↑ Toba, Y.; Oyabu, S.; Matsuhara, H.; Malkan, M. A.; Gandhi, P.; Nakagawa, T.; Isobe, N.; Shirahata, M.; Oi, N.; Ohyama, Y.; Takita, S.; Yamauchi, C.; Yano, K. (2014). "Luminosity and Redshift Dependence of the Covering Factor of Active Galactic Nuclei viewed with WISE and Sloan Digital Sky Survey". The Astrophysical Journal. 788 (1): 45. arXiv:1404.4937. Bibcode:2014ApJ...788...45T. doi:10.1088/0004-637X/788/1/45.
  6. 1 2 3 "NGC 3891". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 7 February 2026.
  7. ↑ Lin, Yen-Ting; Huang, Hung-Jin; Chen, Yen-Chi (2018). "An Analysis Framework for Understanding the Origin of Nuclear Activity in Low-power Radio Galaxies". The Astronomical Journal. 155 (5): 188. arXiv:1803.02482. Bibcode:2018AJ....155..188L. doi:10.3847/1538-3881/aab5b4.
  8. ↑ Fossati, M.; Gavazzi, G.; Savorgnan, G.; Fumagalli, M.; Boselli, A.; Gutiérrez, L.; Hernández Toledo, H.; Giovanelli, R.; Haynes, M. P. (2013). "Hα3: An Hα imaging survey of HI selected galaxies from ALFALFA. IV. Structure of galaxies in the Local and Coma superclusters". Astronomy and Astrophysics. 553: A91. arXiv:1303.0840. Bibcode:2013A&A...553A..91F. doi:10.1051/0004-6361/201220915.
  9. ↑ Puckett, T.; Kroes, A.; Quimby, R.; Castro, F.; Joubert, N.; Li, W. (2006). "Supernovae 2006or, 2006os, 2006ot". International Astronomical Union Circular (8779): 2. Bibcode:2006IAUC.8779....2P.
  10. ↑ "SN 2006or". Transient Name Server. IAU. Retrieved 7 February 2026.
  11. ↑ "SN 2018bdv". Transient Name Server. IAU. Retrieved 7 February 2026.