Bullet Cluster facts for kids
Quick facts for kids Bullet Cluster |
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| 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.
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| Observation data (Epoch J2000) | |
| Constellation(s) | Carina |
| Right ascension | 06h 58m 37.9s |
| Declination | -55° 57′ 0″ |
| Number of galaxies | ~40 |
| Redshift | 0.296 |
| Distance (co-moving) |
1.141 Gpc (3.7 billion light-years). |
| ICM temperature | 17.4 ± 2.5 keV |
| X-ray luminosity | 1.4 ± 0.3 × 1039 h50−2 joule/s (bolometric) |
| X-ray flux | 5.6 ± 0.6 × 10−19 watt/cm2 (0.1–2.4 keV) |
| Other designations | |
| 1E 0657-56, 1E 0657-558 | |
The Bullet Cluster (1E 0657-56) 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 comoving radial distance of 1.141 Gpc (3.72 billion light-years).
Gravitational lensing studies of the Bullet Cluster are claimed to provide the best evidence to date for the existence of dark matter.
Observations of other galaxy cluster collisions, such as MACS J0025.4-1222, similarly 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, or "ordinary", matter in the cluster pair. The gases of the Intracluster medium 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 gravitation 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 gravitationally interacting, other than weakly interacting.
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. 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 100 million kelvin gas in the main cluster at a speed of about nearly 10 million km/h (6 million miles per hour)". The bow shock radiation output is equivalent to the energy of 10 typical quasars.
Significance to dark matter
The Bullet Cluster provides the best current evidence for the nature of dark matter and provides "evidence against some of the more popular versions of Modified Newtonian dynamics (MOND)" as applied to large galactic clusters. 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.
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 4,500 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.
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."
A 2010 study claimed that the velocities of the collision as currently measured are "incompatible with the prediction of a LCDM model". However, subsequent work has found the collision to be consistent with LCDM simulations, 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. Based on the analysis of the shock driven by the merger, it was recently argued that a lower merger velocity ~3,950 km/s is consistent with the Sunyaev–Zeldovich effect and X-ray data, provided that the equilibration of the electron and ion downstream temperatures is not instantaneous.
See also
In Spanish: Cúmulo Bala para niños
- Abell 520 – a similar galaxy cluster whose dark and luminous matter may have been separated during a major collision
- NGC 1052-DF2
- List of galaxy groups and clusters
