Brightest cluster galaxy

This image from NASA's Hubble Space Telescope shows the galaxy cluster Abell S0740 that is over 450 million light-years away in the direction of the constellation Centaurus. The giant elliptical galaxy ESO 325-G004 looms large at the cluster's center. This BCG is as massive as 100 billion of our suns.

A brightest cluster galaxy (BCG) is defined as the brightest galaxy in a cluster of galaxies. BCGs include the most massive galaxies in the universe. They are generally elliptical galaxies which lie close to the geometric and kinematical center of their host galaxy cluster, hence at the bottom of the cluster potential well. They are also generally coincident with the peak of the cluster X-ray emission.[1]

Formation scenarios for BCGs include:

The study of accretion populations in BCGs[2] has cast doubt over this theory and astronomers have seen no evidence of cooling flows in radiative cooling clusters.[3] The two remaining theories exhibit healthier prospects.

It is possible to differentiate the cannibalism model from the merging model by considering the formation period of the BCGs. In the cannibalism model, there are numerous small galaxies present in the evolved cluster, whereas in the merging model, a hierarchical cosmological model is expected due to the collapse of clusters. It has been shown that the orbit decay of cluster galaxies is not effective enough to account for the growth of BCGs.[6] The merging model is now generally accepted as the most likely one,[7] but recent observations are at odds with some of its predictions. For example, it has been found that the stellar mass of BCG's was assembled much earlier than the merging model predicts.[8]

BCGs are divided into various classes of galaxies: giant ellipticals (gE), D galaxies and cD galaxies.[9] cD and D galaxies both exhibit an extended diffuse envelope surrounding an elliptical-like nucleus akin to regular elliptical galaxies. The light profiles of BCGs are often described by a Sersic surface brightness law, a double Sersic profile or a de Vaucouleurs law. The different parametrizations of the light profile of BCG's, as well as the faintness of the diffuse envelope lead to discrepancies in the reported values of the sizes of these objects.

References

  1. ↑ Lin and Mohr (2004), K-band Properties of Galaxy Clusters and Groups: Brightest Cluster Galaxies and Intracluster Light
  2. ↑ McNamara and O’Connell (1989), Star formation in cooling flows in clusters of galaxies
  3. ↑ Motl et al. (2004), Formation of Cool Cores in Galaxy Clusters via Hierarchical Mergers
  4. ↑ J. Ostriker and M. Hausman (1977), Cannibalism among the galaxies - Dynamically produced evolution of cluster luminosity functions
  5. ↑ D. Merritt (1984), Relaxation and tidal stripping in rich clusters of galaxies. II - Evolution of the luminosity distribution
  6. ↑ D. Merritt (1985), Relaxation and tidal stripping in rich clusters of galaxies. III Growth of a massive central galaxy
  7. ↑ J. Dubinski (1998), The Origin of the Brightest Cluster Galaxies
  8. ↑ Collins et al. (2009) Early assembly of the most massive galaxies
  9. ↑ Matthews, T. A., Morgan, W. W. and Schmidt, M. (1964),A Discussion of Galaxies Identified with Radio Sources

See also

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