Abstract
The discovery of the surprisingly rich texture of galaxies, only faintly anticipated from photographies, is of deep cosmological significance. In fact, the homogeneity of the early universe is a fundamental hypothesis of the standard world model. One has to assume that the structures now seen in the galaxy universe were formed by gravitational clustering from initial small seeds. The predicted growth of the large-scale structure may be checked by current observational means thanks to the great progress in measuring distances by redshifts. At small redshifts (z<0.5), huge redshift surveys have been completed. At redshifts up to 5, there are many deep multi-band galaxy surveys, some completed and others being planned.
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Notes
- 1.
Abellās six richness classes were based on the number N of galaxies that are at most 2 mag fainter than the 3rd brightest galaxy: for class 0 30ā¤Nā¤49; for class 5 Nā„300.
- 2.
- 3.
The multifractal picture, characterized by a continuous set of fractal dimensions, is a generalization of fractal properties (Paladin and Vulpiani 1987; Benzi et al. 1984). Multifractals may be viewed in different ways because of the complexity of the problem (even for fractals there is no unique definition). They are in contrast with homogeneity exactly like fractals are. Such an approach was first suggested for galaxy distributions by Pietronero (1987) (see Gabrielli et al. 2005; Martinez and Saar 2002; Jones et al. 2004).
- 4.
The angular correlation exponent Ī± is related to D as Ī±=2āD=Ī³ā1. The last equality follows from the relation between the spatial and angular Ī-functions (the 3D Ī(r)ār āĪ³ with Ī³=3āD and the angular Īang(Īø)āĪø āĪ± with Ī±=2āD.)
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Baryshev, Y., Teerikorpi, P. (2012). The Inhomogeneous Galaxy Universe: Observational Results. In: Fundamental Questions of Practical Cosmology. Astrophysics and Space Science Library, vol 383. Springer, Dordrecht. https://doi.org/10.1007/978-94-007-2379-5_11
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