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Abell 2256 is a rich nearby galaxy cluster in the Abell catalogue that exhibits a population of ~ 100 – 200 kpc long steep spectrum synchrotron filaments surrounding the cluster center[3] with significant evidence of merger activity deduced by the presence of two separate X-ray peaks in the X-ray surface brightness distribution.[4] One feature is a Large Relic. The other striking feature in the cluster is a Long Tail whose morphology suggests it is either a one-sided jet or a twin tail structure. The bending of the tails takes place very near the galaxy core where one might expect little impact from the galaxy's motion through the intergalactic medium, unless the parent galaxy has undergone extreme stripping.[5]

Abell 2256
Observation data (Epoch J2000)
Constellation(s)Ursa Minor
Right ascension17h 03m 43.5s[1]
Declination+78° 43′ 03″[1]
Richness class1[2]
Redshift0.058100 (17 418 km/s)[1]
See also: Galaxy group, Galaxy cluster, List of galaxy groups and clusters

See also



References


  1. "NED results for object ABELL 2256". NASA/IPAC Extragalactic Database (NED). Retrieved March 10, 2015.
  2. Abell, George O.; Corwin, Harold G., Jr.; Olowin, Ronald P. (May 1989). "A catalog of rich clusters of galaxies". Astrophysical Journal Supplement Series. 70 (May 1989): 1–138. Bibcode:1989ApJS...70....1A. doi:10.1086/191333. ISSN 0067-0049.
  3. Clarke, Tracy E; Enßlin, Torsten; Finoguenov, Alexis; Intema, Huib; Pfrommer, Christoph; Reinout van Weeren; Röttgering, Huub; Oonk, Raymond (2011). "The Curious Case of Abell 2256". arXiv:1102.5539v1 [astro-ph.CO].
  4. DEEP 1.4 GHz VERY LARGE ARRAY OBSERVATIONS OF THE RADIO HALO AND RELIC IN ABELL 2256
  5. Clarke, Tracy E; Enßlin, Torsten; Finoguenov, Alexis; Intema, Huib; Pfrommer, Christoph; Reinout van Weeren; Röttgering, Huub; Oonk, Raymond (2014). "Wideband VLA Observations of Abell 2256 I: Continuum, Rotation Measure and Spectral Imaging". The Astrophysical Journal. 794: 24. arXiv:1408.5931. Bibcode:2014ApJ...794...24O. doi:10.1088/0004-637X/794/1/24. S2CID 117010036.


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