NGC 6300

NGC 6300 is a barred Seyfert spiral galaxy located in the constellation Ara. It is designated as SB(rs)b in the galaxy morphological classification scheme and was discovered by the Scottish astronomer James Dunlop on 30 June 1826. NGC 6300 is located at about 51 million light years away from earth. It is suspected that a massive black hole (300,000 times the mass of Sun) may be at its center, pulling all the nearby objects into it. In turn, it emits large amounts of X-rays.[1][2][3][4][5]

NGC 6300
NGC 6300 hst 09042 R814B450
NGC 6300 as seen through the Hubble Space Telescope
Observation data (J2000 epoch)
Right ascension 17h 16m 59.5s
Declination−62° 49′ 40″
Redshift0.003699±0.000010
Helio radial velocity1109±3 km/s
Galactocentric velocity997±5 km/s
Distance (comoving)15.6 million parsecs
Distance50.9 million light years
Apparent magnitude (V)8.78
Absolute magnitude (V)-21.90
Characteristics
TypeSB(rs)b
Size64,000 light years
Apparent size (V)4.30′ × 2.8′
Other designations
ESO 101-25, VV 734, IRAS17123-6245 and PGC 60001
References: NASA/IPAC extragalactic datatbase, http://spider.seds.org/

See also

References

  1. ^ "Object No. 1 - NGC 6300". NASA/IPAC extragalactic database. NASA/IPAC. Retrieved 4 October 2015.
  2. ^ "Revised NGC Data for NGC 6300". Seds. Retrieved 4 October 2015.
  3. ^ "NGC 6300 (= PGC 60001)". cseligman. Retrieved 4 October 2015.
  4. ^ "NGC 6300". The NGC/IC Project. Archived from the original on 20 May 2012. Retrieved 4 October 2015.
  5. ^ "ESO's New Technology Telescope Revisits NGC 6300". ESO. Retrieved 4 October 2015.
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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