NGC 3079

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NGC 3079
NGC 3079.jpg
A Hubble Space Telescope (HST) image of NGC 3079.
Observation data (J2000 epoch)
Constellation Ursa Major
Right ascension 10h 01m 57.8s[1]
Declination +55° 40′ 47″[1]
Redshift 1116 ± 1 km/s[1]
Distance 50 Mly[2]
Apparent magnitude (V) 11.5[1]
Characteristics
Type SB(s)c[1]
Apparent size (V) 7′.9 × 1′.4[1]
Other designations
UGC 5387,[1] PGC 29050[1]
See also: Galaxy, List of galaxies

NGC 3079 is a barred spiral galaxy about 50 million light-years away, and located in the constellation Ursa Major. A prominent feature of this galaxy is the "bubble" forming in the very center (see picture below). The Supermassive black hole at the core has a mass of 2.4+2.4
−1.2
×106 M
.[3]

Center Bubble[edit]

The bubble forming in the center of NGC 3079 is believed to be about 3000 light-years wide and to rise more than 3500 light-years above the disc of the galaxy. It is speculated that the bubble is being formed by particles streaming at high speeds, which were in turn caused by a large burst of star formation. This current bubble is thought to have been created about one million years ago, and computer modeling suggests that there is an ongoing cycle of forming bubbles, with a new bubble forming approximately every 10 million years. Galaxies that contain an active Supermassive black hole are knowen as Seyfert galaxyies.

Hubble space telescope, (visible light) Seyfert galaxy NGC 3079.this image shows the lumpy bubble of hot gas located at the center of the NGC 3079 galaxy's disk

See also[edit]

External links[edit]

References[edit]

  1. ^ a b c d e f g h "NASA/IPAC Extragalactic Database". Results for NGC 3079. Retrieved 2006-11-25.
  2. ^ "Burst of Star Formation Drives Bubble in Galaxy's Core - Fast Facts". Retrieved 2007-10-06.
  3. ^ Graham, Alister W. (November 2008), "Populating the Galaxy Velocity Dispersion - Supermassive Black Hole Mass Diagram: A Catalogue of (Mbh, σ) Values", Publications of the Astronomical Society of Australia, 25 (4): 167–175, arXiv:0807.2549, Bibcode:2008PASA...25..167G, doi:10.1071/AS08013.