The center of the galaxy contains a supermassive black hole with a mass equivalent to 55 million solar masses, which ejects a relativistic jet that is responsible for emissions in the X-ray and radio wavelengths. By taking radio observations of the jet separated by a decade, astronomers have determined that the inner parts of the jet are moving at about half of the speed of light. X-rays are produced farther out as the jet collides with surrounding gases resulting in the creation of highly energetic particles. The X-ray jets of Centaurus A are thousands of light-years long, while the radio jets are over a million light-years long.
Like other starburst galaxies, a collision is suspected to be responsible for the intense burst of star formation. Models have suggested that Centaurus A was a large elliptical galaxy that collided and merged with a smaller spiral galaxy.
NGC 5128 was discovered on 29 April 1826 by James Dunlop during a survey at the Parramatta Observatory.
In 1847 John Herschel described the galaxy as "two semi-ovals of elliptically formed nebula appearing to be cut asunder and separated by a broad obscure band parallel to the larger axis of the nebula, in the midst of which a faint streak of light parallel to the sides of the cut appears."
In 1949 John Gatenby Bolton, Bruce Slee and Gordon Stanley localized NGC 5128 as one of the first extragalactical radio sources. Five years later, Walter Baade and Rudolph Minkowski suggested that the peculiar structure is the result of a merge event of a giant elliptical galaxy and a small spiral galaxy. The first detection of X-ray emissions, using a sounding rocket, was performed in 1970. In 1975–76 gamma-ray emissions from Centaurus A were observed through the atmospheric Cerenkov technique.
The Einstein Observatory detected an X-ray jet emanating from the nucleus in 1979. Ten years later, young blue stars were found along the central dust band with the Hubble Space Telescope.
Centaurus A may be described as having a peculiar morphology. As seen from Earth, the galaxy looks like a lenticular or elliptical galaxy with a superimposed dust lane. The peculiarity of this galaxy was first identified in 1847 by John Herschel, and the galaxy was included in Halton Arp's Atlas of Peculiar Galaxies (published in 1966) as one of the best examples of a "disturbed" galaxy with dust absorption. The galaxy's strange morphology is generally recognized as the result of a merger between two smaller galaxies.
Zoom movie of the galaxy Centaurus A, showing different aspects of the galaxy in several wavelengths.
Schematic diagram of the components of the Centaurus A galaxy
The bulge of this galaxy is composed mainly of evolved red stars. The dusty disk, however, has been the site of more recent star formation; over 100 star formation regions have been identified in the disk.
Two supernovae have been detected in Centaurus A.
The first supernova, named SN 1986G, was discovered within the dark dust lane of the galaxy by R. Evans in 1986.
It was later identified as a Type Ia supernova,
which forms when a white dwarf's mass grows large enough to ignite carbon fusion in its center, touching off a runaway thermonuclear reaction, as may happen when a white dwarf in a binary star system strips gas away from the other star. SN 1986G was used to demonstrate that the spectra of type Ia supernovae are not all identical, and that type Ia supernovae may differ in the way that they change in brightness over time.
The second supernova, a type IIb dubbed SN2016adj, was discovered by Backyard Observatory Supernova Search in February 2016.
Centaurus A is at the center of one of two subgroups within the Centaurus A/M83 Group, a nearby group of galaxies.Messier 83 (the Southern Pinwheel Galaxy) is at the center of the other subgroup. These two groups are sometimes identified as one group and sometimes identified as two groups. However, the galaxies around Centaurus A and the galaxies around M83 are physically close to each other, and both subgroups appear not to be moving relative to each other. The Centaurus A/M83 Group is located in the Virgo Supercluster.
Overview over the radio structure of Centaurus A. The whole radio emitting region extends about 1.8 million light years (about 8° degrees in the sky). Through observations with the VLBI technique structures of the jet and the core smaller than a light year could be resolved (corresponding to a resolution of 0.68 x 0.41 milli-arcseconds.)
This view of the jets of Centaurus A was created through observations in radio waves with a wavelength of 20 cm with the VLA. The position of the radio jet and the knots within the jets matches very well with the structures seen in the x-ray jet. This region of the jet is named „Inner Lobe“.
Elliptical galaxy Centaurus A and its globular clusters
Centaurus A is located approximately 4° north of Omega Centauri (a globular cluster visible with the naked eye). Because the galaxy has a high surface brightness and relatively large angular size, it is an ideal target for amateur astronomy observations. The bright central bulge and dark dust lane are visible even in finderscopes and large binoculars, and additional structure may be seen in larger telescopes. Centaurus A is visible to the naked eye under exceptionally good conditions.
^Grindlay, J. E.; Helmken, H. F.; Brown, R. H.; Davis, J.; Allen, L. R. (1 April 1975). "Evidence for the detection of gamma rays from Centaurus A at gamma-ray energies above 300 GeV". Astrophysical Journal Letters. 197: L9–L12. Bibcode:1975ApJ...197L...9G. doi:10.1086/181764 – via NASA ADS.
^E. J. Schreier; E. Feigelson; J. Delvaille; R. Giacconi; D. A. Schwartz (1979). "EINSTEIN Observations of The X-Ray Structure of Centaurus A: Evidence For The Radio-Lobe Energy Source". Astrophysical Journal, Part 2. 234: 39–43. Bibcode:1979ApJ...234L..39S. doi:10.1086/183105.
^ abM. M. Phillips; A. C. Phillips; S. R. Heathcote; V. M. Blanco; et al. (1987). "The type 1a supernova 1986G in NGC 5128 – Optical photometry and spectra". Publications of the Astronomical Society of the Pacific. 99: 592–605. Bibcode:1987PASP...99..592P. doi:10.1086/132020.
^R. B. Tully (1988). Nearby Galaxies Catalog. Cambridge: Cambridge University Press. ISBN 0-521-35299-1.
^P. Fouque; E. Gourgoulhon; P. Chamaraux; G. Paturel (1992). "Groups of galaxies within 80 Mpc. II – The catalogue of groups and group members". Astronomy and Astrophysics Supplement. 93: 211–233. Bibcode:1992A&AS...93..211F.
^A. Garcia (1993). "General study of group membership. II – Determination of nearby groups". Astronomy and Astrophysics Supplement. 100: 47–90. Bibcode:1993A&AS..100...47G.
^Roopesh Ojha; M. Kadler; M. Böck; R. Booth; M. S. Dutka (2009-12-30). "TANAMI: Milliarcsecond Resolution Observations of Extragalactic Gamma-ray Sources". 2009 Fermi Symposium. arXiv:1001.0059. Bibcode:2010arXiv1001.0059O.
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