Bullet Cluster

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Bullet Cluster
Bullet cluster.jpg
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 ascension06h 58m 37.9s
Declination−55° 57′ 0″
Number of galaxies~40
Redshift0.296[1]
Distance
(co-moving)
1.141 Gpc (3.7 billion light-years).[2]
ICM temperature17.4 ± 2.5 keV
X-ray luminosity1.4 ± 0.3 × 1039 h50−2 joule/s (bolometric).[1]
X-ray flux5.6 ± 0.6 × 10−19 watt/cm2 (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[edit]

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 kelvin gas in the sub-cluster plowed through [1 E6 K|100 million ] kelvin gas in the main cluster at a speed of about 6 million miles per hour (nearly 10 million km/h)".[5][6][7] This energy output is equivalent to that of 10 typical quasars.[1]

Significance to dark matter[edit]

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]

X-ray image (pink) superimposed over a visible light image (galaxies), with matter distribution calculated from gravitational lensing (blue).

According to Greg Madejski:

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]

According to Eric Hayashi:

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]

A 2010 study has concluded that the velocities of the collision as currently measured are "incompatible with the prediction of a LCDM model".[13] However subsequent work has found the collision to be consistent with LCDM simulations,[14] with the previous discrepancy stemming from small simulations and the methodology of identifying pairs. Earlier work claiming the Bullet Cluster was inconsistent with standard cosmology was based on an erroneous estimate of the in-fall velocity based on the speed of the shock in the X-ray emitting gas.[14]

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 Lambda-CDM model, 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[edit]

Mordehai Milgrom, the original proposer of 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[edit]

References[edit]

  1. ^ a b c d e Tucker, W.; Blanco, P.; Rappoport, S. (March 1998). David, L.; Fabricant, D.; Falco, E. E.; Forman, W.; Dressler, A.; Ramella, M. "1E 0657-56: A Contender for the Hottest Known Cluster of Galaxies". Astrophysical Journal Letters. 496 (1): L5. arXiv:astro-ph/9801120. Bibcode:1998ApJ...496L...5T. doi:10.1086/311234. Retrieved March 4, 2012.
  2. ^ a b "NED results for object Bullet Cluster". NASA Extragalactic Database. Retrieved March 4, 2012.
  3. ^ Clowe, Douglas; Gonzalez, Anthony; Markevich, Maxim (2004). "Weak lensing mass reconstruction of the interacting cluster 1E0657-558: Direct evidence for the existence of dark matter". Astrophys. J. 604 (2): 596–603. arXiv:astro-ph/0312273. Bibcode:2004ApJ...604..596C. doi:10.1086/381970.
  4. ^ a b M. Markevitch; A. H. Gonzalez; D. Clowe; A. Vikhlinin; L. David; W. Forman; C. Jones; S. Murray & W. Tucker (2004). "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. ^ Tucker, W; Blanco, P; Rappoport, S; David, L; Fabricant, D; Falco, E. E; Forman, W; Dressler, A; Ramella, M (2006). "Recent and Future Observations in the X-ray and Gamma-ray Bands: Chandra, Suzaku, GLAST, and NuSTAR". AIP Conference Proceedings. 801: 21–30. arXiv:astro-ph/0512012. Bibcode:2005AIPC..801...21M. doi:10.1063/1.2141828.
  12. ^ Eric Hayashi; White (2006). "How Rare is the Bullet Cluster?". Mon. Not. R. Astron. Soc. Lett. 370 (1): 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". Astrophysical Journal. 718 (1): 60–65. arXiv:1003.0939. Bibcode:2010ApJ...718...60L. doi:10.1088/0004-637X/718/1/60.
  14. ^ a b Thompson, Robert; Davé, Romeel; Nagamine, Kentaro (2015-09-01). "The rise and fall of a challenger: the Bullet Cluster in Lambda cold dark matter simulations". Monthly Notices of the Royal Astronomical Society. 452 (3): 3030–3037. arXiv:1410.7438. Bibcode:2015MNRAS.452.3030T. doi:10.1093/mnras/stv1433. ISSN 0035-8711.
  15. ^ "Archived copy". Archived from the original on 2009-08-25. Retrieved 2010-01-05.
  16. ^ Milgrom, Moti, "Milgrom's perspective on the Bullet Cluster", The MOND Pages, archived from the original on July 21, 2016, retrieved December 27, 2016
  17. ^ G.W. Angus; B. Famaey & H. Zhao (2006). "Can MOND take a bullet? Analytical comparisons of three versions of MOND beyond spherical symmetry". Mon. Not. R. 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[edit]

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