Large Scale Structure of the Universe

Now it is generally recognized that on large scales the universe is isotropic and homogeneous while on smaller scales it is extremely clumpy. Indeed, detected small variations of CMB anisotropy by COBE - ΔT/T ≈ 10−5- restrict the possible inhomogeneities on larger scales, while existence of so prominent galaxy concentrations as, for example, groups and clusters of galaxies, superclusters similar to the Perseus — Pisces or the Great Wall (de Lapparent, Geller & Huchra 1988), and voids similar to the Bootes void (Kirshner et al. 1983) illustrates the degree of inhomogeneities observed on scales ≤ 100h −1Mpc. These inhomogeneities are usually called the Large Scale Structure of the universe (LSS).

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