Superclusters and Large-Scale Structure

Superclusters

The discovery of the fundamental plane of the properties of elliptical galaxies (interpreted as a consequence of the virial theorem), related to their structure and also globular cluster population, has made it possible to study the spatial distribution of galaxies with higher accuracy than possible with spectroscopy alone.

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  4. Djorgovski, S., Santiago, B.X., Astrophys. J. 391 (1992) L85.
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  11. Recillas-Cruz, E., Carrasco, L., Serrano, P.G.A., Cruz-Gonzalez, I., Astron. Astrophys. 249 (1991) 312.

There are, as a result of the extended surveys, now catalogues of superclusters, as well as a large body of data on known superclusters.

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Large-Scale Structure Beyond Superclusters

Thus the many surveys in number counts on the sky and in spectral lines as well as the studies of the distribution of clusters have shown that the universe has structure on rather large scales: observations like redshift surveys, source counts at various wavelengths, simple interpretative modelling,

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Theory:

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  2. Coles, P., Jones, B., Mon. Not. R. Astron. Soc. 248 (1991) 1.
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  4. Doroshkevich, A.G., Sov. Astron. A.J. 33 (1989) 229 (orig. Astron. Zh. 66 (1989) 449).
  5. Guiderdoni, B., Rocca-Volmerange, B., Astron. Astrophys. 227 (1990) 362.
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The structure is maybe best described as a multitude of bubbles or voids, with clusters of galaxies making tip the walls and superclusters the filaments when three bubbles touch in such an analogy.

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This structure is clearly related to the physics of galaxy formation, possibly also to the early activity of quasars.

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Locally the structure is best described as large scale streaming in a certain direction, also sometimes referred to as motion towards a great attractor.

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Many scientists favor models in which the X-ray and Gamma-ray background is dominated by AGN, and their clustering properties then reflect presumably the early evolution of galaxies; the heavy elements observed through emission lines in quasars are clearly the product of intense star formation in the inner part of the host galaxies.

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Simple cold dark matter models appear to be ruled out.

A final judgement is still out, and one of the fundamental difficulties clearly remains that there is no clue what the nature of dark matter really is.


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