|Observation data (J2000 epoch)|
|Right ascension||19h 59m 28.3566s|
|Declination||+40° 44′ 02.096″|
|Redshift||0.056075 ± 0.000067|
|Apparent magnitude (V)||16.22|
|Apparent size (V)||0.549' × 0.457'|
|4C 40.40, 2E 4309, CYG A, W 57, BWE 1957+4035, NRAO 620, 1C 19.01, QSO B1957+405, 3C 405, 1RXS J195928.7+404405, 3C 405.0, 2U 1957+40, 3CR 405, LEDA 63932, 4U 1957+40, VV2000c J195928.3+404402, DA 500, MCG+07-41-003, DB 117, Mills 19+4, VV 72, PGC 63932.|
Cygnus A (3C 405) is a radio galaxy, and one of the strongest radio sources in the sky. It was discovered by Grote Reber in 1939. In 1951, Cygnus A, along with Cassiopeia A, and Puppis A were the first "radio stars" identified with an optical source. Of these, Cygnus A became the first radio galaxy; the other two being nebulae inside the Milky Way. In 1953 Roger Jennison and M K Das Gupta showed it to be a double source. Like all radio galaxies, it contains an active galactic nucleus. The super massive black hole at the core has a mass of ±0.7)×109 M☉. (2.5
Images of the galaxy in the radio portion of the electromagnetic spectrum show two jets protruding in opposite directions from the galaxy's center. These jets extend many times the width of the portion of the host galaxy which emits radiation at visible wavelengths. At the ends of the jets are two lobes with "hot spots" of more intense radiation at their edges. These hot spots are formed when material from the jets collides with the surrounding intergalactic medium.
In 2016, a radio transient was discovered 460 parsecs away from the center of Cygnus A. Between 1989 and 2016, the object, cospatial with a previously-known infrared source, exhibited at least an eightfold increase in radio flux density, with comparable luminosity to the brightest known supernova. Due to the lack of measurements in the intervening years, the rate of brightening is unknown, but the object has remained at a relatively constant flux density since its discovery. The data are consistent with a second supermassive black hole orbiting the primary object, with the secondary having undergone a rapid accretion rate increase. The inferred orbital timescale is of the same order as the activity of the primary source, suggesting the secondary may be perturbing the primary and causing the outflows.
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- Astrophysical Journal, "Identification of the Radio Sources in Cassiopeia (A), Cygnus A, and Puppis A", Baade, W.; Minkowski, R., vol. 119, p.206, January 1954, doi:10.1086/145812 , Bibcode: 1954ApJ...119..206B
- Jennison, R.C.; Das Gupta, M.K. (1953). "Fine Structure of the extra-terrestrial radio source Cygnus 1". Nature, Vol. 172. p. 996.
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- Perley, D. A.; Perley, R. A.; Dhawan, V.; Carilli, C. L. (2017). "Discovery of a Luminous Radio Transient 460 pc from the Central Supermassive Black Hole in Cygnus A". The Astrophysical Journal. 841 (2): 117. arXiv: . Bibcode:2017ApJ...841..117P. doi:10.3847/1538-4357/aa725b. ISSN 1538-4357.
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A second massive black hole has been discovered in galaxy Cygnus A (Astronomy magazine, September 2017).