NGC 3185

Coordinates: Sky map 10h 17m 38.584s, +21° 41′ 17.82″

NGC 3185
Stalking our celebrity neighbours
NGC 3185, imaged by the Hubble Space Telescope
Observation data (J2000 epoch)
Right ascension 10h 17m 38.584s[1]
Declination+21° 41′ 17.82″[1]
Helio radial velocity1217[2]
Distance74.62 ± 16.07 Mly (22.879 ± 4.928 Mpc)[2]
Group or clusterHCG 44[3]
Apparent magnitude (V)12.17[4]
Apparent magnitude (B)12.99[4]
Apparent size (V)2.373′ &times 1.234′[4]
Other designations
NGC 3185, UGC 5554, MCG+04-24-024, HCG 44c, PGC 30059

NGC 3185 is a spiral galaxy located 20.4 Mpc away in the Leo constellation. NGC 3185 is a member of a four-galaxy group called HCG 44.


  1. ^ a b Skrutskie, M. (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 "NED Results for NGC 3185". NASA/IPAC Extragalactic Database. Retrieved 2 September 2016.
  3. ^ "Stalking our celebrity neighbours". 2013. Retrieved 9 February 2017.
  4. ^ a b c "NGC 3185". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 9 February 2017.
NGC 3190

NGC 3190 is a spiral galaxy with tightly wound arms and lying in the constellation Leo. It was discovered by William Herschel in 1784. NGC 3190 is member of Hickson 44 galaxy group, estimated at around 80 million light years away, and consisting of four galaxies in a tight group - NGC 3193 is fairly featureless, NGC 3187 is a dim but striking spiral galaxy and NGC 3185 has a barred spiral structure with an outer ring.

In 2002 two supernovae were observed in the galaxy. A Brazilian amateur astronomer Paulo Cacella detected one supernova in the southeastern part in March 2002 (SN 2002bo), and then an Italian team, while studying the first one, detected a second supernova (SN 2002cv) on the other side two months later.In 2012 Apple Inc used a blue tinted image of NGC 3190 as their desktop image for their release of OS X Mountain Lion.

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.


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