Abell 520

From Wikipedia, the free encyclopedia
Jump to navigation Jump to search
Abell 520
Abell 520. Imaged January 2012.
Credit: NASA
Observation data (Epoch J2000)
Right ascension04h 54m 03.80s[1]
Declination+02° 53′ 33.00″[1]
Number of galaxies289+[2]
Richness class3[3]
Bautz–Morgan classificationIII[3]
Velocity dispersion1,066 km/s[2]
811 Mpc (2,645 Mly) h−1
ICM temperature9.8 keV[5]
Binding mass17×1014 h−1
[2] M
X-ray luminosity14.44×1044 erg/s (0.1–2.4 keV)[5]
X-ray flux8.4×1012 erg s−1 cm−2 (0.1–2.4 keV)[5]
Other designations
The Train Wreck Cluster
See also: Galaxy group, Galaxy cluster, List of galaxy groups and clusters
A520 pictured in X-ray, optical, and an inferred mass distribution based on the observed weak gravitational lensing. Imaged April 2007.

The Abell 520 galaxy cluster possesses an unusual substructure resulting from a major merger. It has been popularly nicknamed The Train Wreck Cluster,[6][7][8] due to its chaotic structure, and is classified as a Bautz-Morgan type III cluster.[3] It is at a co-moving radial distance of 811 Mpc (2,645 Mly) and subtends 25 arcminutes on the sky.[1] Analysis[2] of the motions of 293 galaxies in the cluster field suggested that Abell 520 was a cluster forming at the crossing of three filaments of the large scale structure.

The surprising substructure of Abell 520 was reported in 2007 from a weak gravitational lensing study based on Canada-France-Hawaii-Telescope (CFHT) imaging data. It was surprising at first, because the study found the "dark core" with a significant amount of mass in the region, where there is no concentration of bright cluster galaxies. No conventional understanding of dark matter could explain this peculiar concentration of dark matter.[7][6] At the time, some thought that the substructure may arise from non-gravitational interaction of dark matter.

However, in the year 2012 two international teams of astronomers published conflicting results on Abell 520. While one study[9] based on the Wide Field Planetary Camera 2 (WFPC2) on Hubble Space Telescope (HST) confirmed the previous claim of the dark core in Abell 520, the other study[10] based on the Advanced Camera for Surveys (ACS) did not support the claim. Although the latter group found the "dark core", they also found luminous matter, which made the "dark core" not so dark—in particular, just as bright as any other galaxy with dark matter.[11]

In 2014, a study[12] of the ACS images by the original team claims to again have found evidence of a dark core, but is in a different location from the first two studies. A subsequent analysis[13] by an independent third team of the gravitational shear catalogs of the two competing ACS analyses indicates marginal evidence for the core in both data sets and the authors "do not consider A520 as posing a significant challenge to the collisionless dark matter scenario."

See also[edit]


  1. ^ a b c d "NED results for object ABELL 0520 - BASIC DATA for ABELL 0520". NASA/IPAC EXTRAGALACTIC DATABASE. Retrieved March 3, 2012.
  2. ^ a b c d Girardi, M.; Barrena, R.; Boschin, W.; Ellingson, E. (Nov 2008). "Cluster Abell 520: a perspective based on member galaxies. A cluster forming at the crossing of three filaments?". Astronomy and Astrophysics. 491 (2): 379–395. arXiv:0809.3139. Bibcode:2008A&A...491..379G. doi:10.1051/0004-6361:200810549. S2CID 1880613.
  3. ^ a b c Table 3, page 24 in Abell, George O.; Corwin, Harold G. Jr.; Olowin, Ronald P. (May 1989). "A catalog of rich clusters of galaxies" (PDF). Astrophysical Journal Supplement Series. 70 (May 1989): 1–138. Bibcode:1989ApJS...70....1A. doi:10.1086/191333.
  4. ^ Struble, Mitchell F.; Rood, Herbert J. (November 1999). "A Compilation of Redshifts and Velocity Dispersions for ACO Clusters". The Astrophysical Journal Supplement Series. 125 (1): 35–71. Bibcode:1999ApJS..125...35S. doi:10.1086/313274.
  5. ^ a b c d Ebeling, H.; Edge, A. C.; et al. (December 1998). "The ROSAT Brightest Cluster Sample - I. The compilation of the sample and the cluster log N-log S distribution". Monthly Notices of the Royal Astronomical Society. 301 (4): 881–914. arXiv:astro-ph/9812394. Bibcode:1998MNRAS.301..881E. doi:10.1046/j.1365-8711.1998.01949.x. S2CID 119104724.
  6. ^ a b "'Cosmic train wreck' stumps dark-matter physicists". Physics World.
  7. ^ a b "Cosmic 'train wreck' defies dark matter theories - space -". New Scientist. Retrieved 16 August 2007.
  8. ^ "Abell 520: Dark Matter Mystery Deepens in Cosmic "Train Wreck"". Retrieved 16 August 2007.
  9. ^ Jee, M. J.; Mahdavi, A.; Hoekstra, H.; Babul, A.; Dalcanton, J. J.; Carroll, P.; Capak, P. (2012-03-01). "A Study of the Dark Core in A520 with the Hubble Space Telescope: The Mystery Deepens". The Astrophysical Journal. 747 (2): 96. arXiv:1202.6368. Bibcode:2012ApJ...747...96J. doi:10.1088/0004-637X/747/2/96. S2CID 12492388.
  10. ^ Clowe, Douglas; Markevitch, Maxim; Bradac, Marusa; Gonzalez, Anthony H.; Chung, Sun Mi; Massey, Richard; Zaritsky, Dennis (2012-10-01). "On Dark Peaks and Missing Mass: A Weak-lensing Mass Reconstruction of the Merging Cluster System A520". The Astrophysical Journal. 758 (2): 128. arXiv:1209.2143. Bibcode:2012ApJ...758..128C. doi:10.1088/0004-637X/758/2/128. S2CID 13607147.
  11. ^ ""Dark core" may not be so dark after all: Scientists report new dark matter finding from merging galaxy cluster". Physics World.
  12. ^ Jee, M. J.; Hoekstra, H.; Mahdavi, A.; Babul, A. (2014-03-01). "Hubble Space Telescope/Advanced Camera for Surveys Confirmation of the Dark Substructure in A520". The Astrophysical Journal. 783 (2): 78. arXiv:1401.3356. Bibcode:2014ApJ...783...78J. doi:10.1088/0004-637X/783/2/78. S2CID 119196763.
  13. ^ Peel, A.; Lanusse, F.; Starck, J.-L. (2017-09-01). "Sparse Reconstruction of the Merging A520 Cluster System". The Astrophysical Journal. 847 (1): 13. arXiv:1708.00269. Bibcode:2017ApJ...847...23P. doi:10.3847/1538-4357/aa850d. S2CID 119504376.

External links[edit]

Coordinates: Sky map 04h 54m 03.80s, +02° 53′ 33.00″