Galaxy groups and clusters

MACS J0152.5-2852 is a massive galaxy cluster. Almost every object seen in the image is a galaxy, each containing billions of stars.[1]

Galaxy groups and clusters are the largest known gravitationally bound objects to have arisen thus far in the process of cosmic structure formation.[2] They form the densest part of the large-scale structure of the Universe. In models for the gravitational formation of structure with cold dark matter, the smallest structures collapse first and eventually build the largest structures, clusters of galaxies. Clusters are then formed relatively recently between 10 billion years ago and now. Groups and clusters may contain ten to thousands of individual galaxies. The clusters themselves are often associated with larger, non-gravitationally bound, groups called superclusters.

Groups of galaxies

Main article: Galaxy group
Map of the positions of thousands of galaxies in the VIPERS survey[3]

Groups of galaxies are the smallest aggregates of galaxies. They typically contain no more than 50 galaxies in a diameter of 1 to 2 megaparsecs (Mpc)(see 1022 m for distance comparisons). Their mass is approximately 1013 solar masses. The spread of velocities for the individual galaxies is about 150 km/s. However, this definition should be used as a guide only, as larger and more massive galaxy systems are sometimes classified as galaxy groups.[4] Groups are the most common structures of galaxies in the universe, comprising at least 50% of the galaxies in the local universe. Groups have a mass range between those of the very large elliptical galaxies and clusters of galaxies.[5]

Our own Galaxy, the Milky Way, is contained in the Local Group of more than 40 galaxies.[6]

Clusters of galaxies

Main article: Galaxy cluster
Rich scattering of galaxies was captured by the MPG/ESO telescope.

Clusters are larger than groups, although there is no sharp dividing line between the two. When observed visually, clusters appear to be collections of galaxies held together by mutual gravitational attraction. However, their velocities are too large for them to remain gravitationally bound by their mutual attractions, implying the presence of either an additional invisible mass component, or an additional attractive force besides gravity. X-ray studies have revealed the presence of large amounts of intergalactic gas known as the intracluster medium. This gas is very hot, between 107K and 108K, and hence emits X-rays in the form of bremsstrahlung and atomic line emission.

Galaxy cluster ACO 3341 seen by VLT's VIMOS

The total mass of the gas is greater than that of the galaxies by roughly a factor of two. However this is still not enough mass to keep the galaxies in the cluster. Since this gas is in approximate hydrostatic equilibrium with the overall cluster gravitational field, the total mass distribution can be determined. It turns out the total mass deduced from this measurement is approximately six times larger than the mass of the galaxies or the hot gas. The missing component is known as dark matter and its nature is unknown. In a typical cluster perhaps only 5% of the total mass is in the form of galaxies, maybe 10% in the form of hot X-ray emitting gas and the remainder is dark matter. Brownstein and Moffat[7] use a theory of modified gravity to explain X-ray cluster masses without dark matter. Observations of the Bullet Cluster are the strongest evidence for the existence of dark matter;[8][9][10] however, Brownstein and Moffat[11] have shown that their modified gravity theory can also account for the properties of the cluster.

Observational methods

Galaxy Cluster LCDCS-0829 acting like a giant magnifying glass. This strange effect is called gravitational lensing.

Clusters of galaxies have been found in surveys by a number of observational techniques and have been studied in detail using many methods:

Temperature and density

The Most Distant Mature Galaxy Cluster[12] taken with ESO's Very Large Telescope in Chile and with NAOJ's Subaru Telescope in Hawaii

Clusters of galaxies are the most recent and most massive objects to have arisen in the hierarchical structure formation of the Universe and the study of clusters tells one about the way galaxies form and evolve. Clusters have two important properties: their masses are large enough to retain any energetic gas ejected from member galaxies and the thermal energy of the gas within the cluster is observable within the X-Ray bandpass. The observed state of gas within a cluster is determined by a combination of shock heating during accretion, radiative cooling, and thermal feedback triggered by that cooling. The density, temperature, and substructure of the intracluster X-Ray gas therefore represents the entire thermal history of cluster formation. To better understand this thermal history one needs to study the entropy of the gas because entropy is the quantity most directly changed by increasing or decreasing the thermal energy of intracluster gas.[13]

List of groups and clusters

Name / Designation Notes
Local Group The group where the Milky Way, including the Earth is located
Virgo Cluster This cluster of galaxies is the nearest one to us

See also

References

  1. "A scattering of spiral and elliptical galaxies". ESA/Hubble Picture of the Week. Retrieved 25 September 2013.
  2. Voit, G.M.; "Tracing cosmic evolution with clusters of galaxies"; Reviews of Modern Physics, vol. 77, Issue 1, pp. 207-258
  3. "Huge Map of the Distant Universe Reaches Halfway Point". ESO. Retrieved 2 April 2013.
  4. UTK Physics Dept. "Groups of Galaxies". University of Tennessee, Knoville. Retrieved September 27, 2012.
  5. Muñoz, R. P.; et al. (11 December 2012). "Dynamical analysis of strong-lensing galaxy groups at intermediate redshift". Astronomy & Astrophysics (April 2013) 552: 18. arXiv:1212.2624. Bibcode:2013A&A...552A..80M. doi:10.1051/0004-6361/201118513. A80.
  6. Mike Irwin. "The Local Group". Retrieved 2009-11-07.
  7. Brownstein, J. R.; Moffat, J. W. (2006). "Galaxy Cluster Masses Without Non-Baryonic Dark Matter". Monthly Notices of the Royal Astronomical Society 367 (2): 527–540. arXiv:astro-ph/0507222. Bibcode:2006MNRAS.367..527B. doi:10.1111/j.1365-2966.2006.09996.x.
  8. Markevitch; Gonzalez; Clowe; Vikhlinin; David; Forman; Jones; Murray; 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.
  9. Coe, Dan; Benítez, Narciso; Broadhurst, Tom; Moustakas, Leonidas A.; Benítez; Broadhurst; Moustakas (2010). "A High-resolution Mass Map of Galaxy Cluster Substructure: LensPerfect Analysis of A1689". The Astrophysical Journal 723 (2): 1678. arXiv:1005.0398. Bibcode:2010ApJ...723.1678C. doi:10.1088/0004-637X/723/2/1678.
  10. McDermott, Samuel D.; Yu, Hai-Bo; Zurek, Kathryn M.; Yu; Zurek (2011). "Turning off the lights: How dark is dark matter?". Physical Review D 83 (6): 063509. arXiv:1011.2907. Bibcode:2011PhRvD..83f3509M. doi:10.1103/PhysRevD.83.063509.
  11. Brownstein, J. R.; Moffat, J. W. (2007). "The Bullet Cluster 1E0657-558 evidence shows Modified Gravity in the absence of Dark Matter". Monthly Notices of the Royal Astronomical Society 382: 29–47. arXiv:astro-ph/0702146v3. Bibcode:2007MNRAS.382...29B. doi:10.1111/j.1365-2966.2007.12275.x.
  12. "The Most Distant Mature Galaxy Cluster". ESO Science Release. ESO. Retrieved 9 March 2011.
  13. Galaxies. Wikimedia Foundation. p. 55.

Further reading

This article is issued from Wikipedia - version of the Sunday, February 28, 2016. The text is available under the Creative Commons Attribution/Share Alike but additional terms may apply for the media files.