NGC 3259

NGC 3259 is a barred spiral galaxy located approximately 90[2] million light-years from Earth, in the Ursa Major constellation. It has the morphological classification SAB(rs)bc,[3] which indicates that it is a spiral galaxy with a weak bar across the nucleus (SAB), an incomplete inner ring structure circling the bar (rs), and moderate to loosely wound spiral arms (bc).[4] This galaxy is a known source of X-ray emission and it has an active galactic nucleus of the Seyfert 2 type.[2]

NGC 3259
NGC 3259 by Hubble
NGC 3259 is a bright barred spiral galaxy located approximately 110 million light-years from Earth.
Observation data (J2000 epoch)
ConstellationUrsa Major
Right ascension 10h 32m 34.816s[1]
Declination+65° 02′ 27.79″[1]
Helio radial velocity+1,677[2] km/s
Distance89.7 Mly (27.5 Mpc)[2]
Characteristics
TypeSAB(rs)bc[3]
Mass1.26 × 1010[2] M
Other designations
UGC 5717

References

  1. ^ a b Skrutskie, M. F.; et al. (February 2006), "The Two Micron All Sky Survey (2MASS)", The Astronomical Journal, 131 (2): 1163–1183, Bibcode:2006AJ....131.1163S, doi:10.1086/498708.
  2. ^ a b c d e Seth, Anil; et al. (May 2008), "The Coincidence of Nuclear Star Clusters and Active Galactic Nuclei", The Astrophysical Journal, 678 (1): 116–130, arXiv:0801.0439, Bibcode:2008ApJ...678..116S, doi:10.1086/528955. Cite error: Invalid <ref> tag; name "Springob2005" defined multiple times with different content (see the help page).
  3. ^ a b Hughes, M. A.; et al. (August 2003), "An Atlas of Hubble Space Telescope Spectra and Images of Nearby Spiral Galaxies", The Astronomical Journal, 126 (2): 742–761, Bibcode:2003AJ....126..742H, doi:10.1086/376744.
  4. ^ Buta, Ronald J.; et al. (2007), Atlas of Galaxies, Cambridge University Press, pp. 13–17, ISBN 978-0521820486.

Coordinates: Sky map 10h 32m 34.816s, +65° 02′ 27.79″

Seyfert galaxy

Seyfert galaxies are one of the two largest groups of active galaxies, along with quasars. They have quasar-like nuclei (very luminous, distant and bright sources of electromagnetic radiation) with very high surface brightnesses whose spectra reveal strong, high-ionisation emission lines, but unlike quasars, their host galaxies are clearly detectable.Seyfert galaxies account for about 10% of all galaxies and are some of the most intensely studied objects in astronomy, as they are thought to be powered by the same phenomena that occur in quasars, although they are closer and less luminous than quasars. These galaxies have supermassive black holes at their centers which are surrounded by accretion discs of in-falling material. The accretion discs are believed to be the source of the observed ultraviolet radiation. Ultraviolet emission and absorption lines provide the best diagnostics for the composition of the surrounding material.Seen in visible light, most Seyfert galaxies look like normal spiral galaxies, but when studied under other wavelengths, it becomes clear that the luminosity of their cores is of comparable intensity to the luminosity of whole galaxies the size of the Milky Way.Seyfert galaxies are named after Carl Seyfert, who first described this class in 1943.

NGC

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