Bullet Cluster

Not to be confused with Bullet Group or Bullet Galaxy.
Bullet Cluster

X-ray photo by Chandra X-ray Observatory. Exposure time was 140 hours. The scale is shown in megaparsecs. Redshift (z) = 0.3, meaning its light has wavelengths stretched by a factor of 1.3.
Observation data (Epoch J2000)
Constellation(s) Carina
Right ascension 06h 58m 37.9s
Declination −55° 57′ 0″
Number of galaxies ~40
Redshift 0.296[1]
Distance
(co-moving)		 1.141 Gpc (3.7 billion light-years).[2]
ICM temperature 17.4 ± 2.5 keV
X-ray luminosity 1.4 ± 0.3 × 1046 h50−2 ergs2/s (bolometric).[1]
X-ray flux 5.6 ± 0.6 × 10−12 ergs2/cm2/s (0.1–2.4 keV).[1]
Other designations
1E 0657-56, 1E 0657-558
See also: Galaxy groups, Galaxy clusters, List of galaxy clusters

The Bullet Cluster (1E 0657-558) consists of two colliding clusters of galaxies. Strictly speaking, the name Bullet Cluster refers to the smaller subcluster, moving away from the larger one. It is at a co-moving radial distance of 1.141 Gpc (3.7 billion light-years).[2]

Gravitational lensing studies of the Bullet Cluster are claimed to provide the best evidence to date for the existence of dark matter.[3][4]

Observations of other galaxy cluster collisions, such as MACS J0025.4-1222, are similarly claimed to support the existence of dark matter.

Overview

The major components of the cluster pair—stars, gas and the putative dark matter—behave differently during collision, allowing them to be studied separately. The stars of the galaxies, observable in visible light, were not greatly affected by the collision, and most passed right through, gravitationally slowed but not otherwise altered. The hot gas of the two colliding components, seen in X-rays, represents most of the baryonic, i.e. ordinary, matter in the cluster pair. The gases interact electromagnetically, causing the gases of both clusters to slow much more than the stars. The third component, the dark matter, was detected indirectly by the gravitational lensing of background objects. In theories without dark matter, such as Modified Newtonian Dynamics (MOND), the lensing would be expected to follow the baryonic matter; i.e. the X-ray gas. However, the lensing is strongest in two separated regions near (possibly coincident with) the visible galaxies. This provides support for the idea that most of the mass in the cluster pair is in the form of two regions of dark matter, which bypassed the gas regions during the collision. This accords with predictions of dark matter as only weakly interacting, other than via the gravitational force.

The Bullet Cluster is one of the hottest known clusters of galaxies. It provides an observable constraint for cosmological models, which may diverge at temperatures beyond their predicted critical cluster temperature.[1] Observed from Earth, the subcluster passed through the cluster center 150 million years ago, creating a "bow-shaped shock wave located near the right side of the cluster" formed as "70 million degree Celsius gas in the sub-cluster plowed through 100 million degree Celsius gas in the main cluster at a speed of about 6 million miles per hour".[5][6][7] This energy output is equivalent to that of 10 typical quasars.[1]

Significance to dark matter

The Bullet Cluster provides the best current evidence for the nature of dark matter[4][8] and provides "evidence against some of the more popular versions of Modified Newtonian Dynamics (MOND)" as applied to large galactic clusters.[9] At a statistical significance of 8σ, it was found that the spatial offset of the center of the total mass from the center of the baryonic mass peaks cannot be explained with an alteration of the gravitational force law alone.[10]

Mass density contours superimposed over photograph taken with Hubble Space Telescope.

"Particularly compelling results were inferred from the Chandra observations of the 'bullet cluster' (1E0657-56; Fig. 2) by Markevitch et al. (2004) and Clowe et al. (2004). Those authors report that the cluster is undergoing a high-velocity (around 4500 km/s) merger, evident from the spatial distribution of the hot, X-ray emitting gas, but this gas lags behind the subcluster galaxies. Furthermore, the dark matter clump, revealed by the weak-lensing map, is coincident with the collisionless galaxies, but lies ahead of the collisional gas. This—and other similar observations—allow good limits on the cross-section of the self-interaction of dark matter."[11]

"The velocity of the bullet subcluster is not exceptionally high for a cluster substructure, and can be accommodated within the currently favoured Lambda-CDM model cosmology."[12]

However, a more recent 2010 study has concluded that the velocities of the collision as currently measured are "incompatible with the prediction of a LCDM model".[13]

In an independent confirmation of results from the Bullet Cluster, more recent observations of the cluster MACS J0025.4-1222 indicate that a titanic collision has separated the dark from ordinary matter, resulting in a significant displacement between the clusters' center of visible matter and their gravitational potential.[14]

However, while the Bullet Cluster phenomenon may provide direct evidence for dark matter on large cluster scales, it offers no specific insight into the original galaxy rotation problem. In fact, the observed ratio of dark matter to visible matter in a typical rich galaxy cluster is much lower than predicted.[15] This may indicate that the prevailing cosmological model is insufficient to describe the mass discrepancy on galaxy scales, or that its predictions about the shape of the universe are incorrect.

Alternative interpretations

Mordehai Milgrom, the original proposer of MOND (Modified Newtonian Dynamics), has posted an on-line rebuttal[16] of claims that the Bullet Cluster proves the existence of dark matter. Milgrom claims that MOND correctly accounts for the dynamics of galaxies outside of galaxy clusters, and even in clusters such as the Bullet Cluster it removes the need for most dark matter, leaving only a factor of two which Milgrom expects to be simply unseen ordinary matter (non-luminous baryonic matter) rather than cold dark matter. Without MOND, or some similar theory, the matter discrepancy in galaxy clusters is a factor of 10, i.e. MOND reduces this discrepancy five-fold to a factor of 2. Another study in 2006[17] cautions against "simple interpretations of the analysis of weak lensing in the bullet cluster", leaving it open that even in the non-symmetrical case of the Bullet Cluster, MOND, or rather its relativistic version TeVeS (Tensor–vector–scalar gravity), could account for the observed gravitational lensing.

See also

References

  1. 1 2 3 4 5 Tucker, W.; Blanco, P.; Rappoport, S.; David, L.; Fabricant, D.; Falco, E. E.; Forman, W.; Dressler, A.; Ramella, M. (March 1998). "1E 0657-56: A Contender for the Hottest Known Cluster of Galaxies". Astrophysical Journal Letters (APJ) 496: L5. arXiv:astro-ph/9801120. Bibcode:1998ApJ...496L...5T. doi:10.1086/311234. Retrieved March 4, 2012.
  2. 1 2 "NED results for object Bullet Cluster". NASA Extragalactic Database. Retrieved March 4, 2012.
  3. ↑ http://xxx.tau.ac.il/abs/astro-ph/0312273
  4. 1 2 M. Markevitch; A. H. Gonzalez; D. Clowe; A. Vikhlinin; L. David; W. Forman; C. Jones; S. Murray & W. Tucker (2003). "Direct constraints on the dark matter self-interaction cross-section from the merging galaxy cluster 1E0657-56". Astrophys. J. 606 (2): 819–824. arXiv:astro-ph/0309303. Bibcode:2004ApJ...606..819M. doi:10.1086/383178.
  5. ↑ Harvard photo and description
  6. ↑ spaceimages.com
  7. ↑ The dynamical status of the cluster of galaxies 1E0657-56
  8. ↑ M. Markevitch; S. Randall; D. Clowe; A. Gonzalez; et al. (16–23 July 2006). "Dark Matter and the Bullet Cluster" (PDF). 36th COSPAR Scientific Assembly. Beijing, China. Abstract only
  9. ↑ Lunch-time talk at Harvard University by Scott Randall on 31 May 2006. Abstract only
  10. ↑ Clowe, Douglas; et al. (2006). "A Direct Empirical Proof of the Existence of Dark Matter". The Astrophysical Journal Letters 648 (2): L109–L113. arXiv:astro-ph/0608407. Bibcode:2006ApJ...648L.109C. doi:10.1086/508162.
  11. ↑ Recent and Future Observations in the X-ray and Gamma-ray Bands
  12. ↑ Eric Hayashi; White (2006). "How Rare is the Bullet Cluster?". Mon.Not.Roy.Astron.Soc.Lett. 370: L38–L41. arXiv:astro-ph/0604443. Bibcode:2006MNRAS.370L..38H. doi:10.1111/j.1745-3933.2006.00184.x.
  13. ↑ Jounghun Lee; Komatsu (2010). "Bullet Cluster: A Challenge to LCDM Cosmology". ApJ 718. arXiv:1003.0939. Bibcode:2010ApJ...718...60L. doi:10.1088/0004-637X/718/1/60.
  14. ↑ A Clash of Clusters Provides New Clue to Dark Matter Newswise, Retrieved on September 1, 2008.
  15. ↑ http://imagine.gsfc.nasa.gov/docs/features/topics/clusters_group/composition.html
  16. ↑ http://www.astro.umd.edu/~ssm/mond/moti_bullet.html
  17. ↑ G.W. Angus; B. Famaey & H. Zhao (September 2006). "Can MOND take a bullet? Analytical comparisons of three versions of MOND beyond spherical symmetry". Mon.Not.Roy.Astron.Soc. 371 (1): 138–146. arXiv:astro-ph/0606216v1. Bibcode:2006MNRAS.371..138A. doi:10.1111/j.1365-2966.2006.10668.x.

Further reading

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Coordinates: 06h 58m 37.9s, −55° 57′ 00″

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