“The distribution of galaxies is clumpy on all scales, ranging from binaries, triples, and multiples, through groups containing a few and a hundred galaxies, to rich clusters with thousands of members, masses up to 1015±1M☉, and diameters of the order of 10 Mpc. The latter have been discussed by Neta A. Bahcall in a preceding volume of this series. The clusters are at the end of the scale of the more or less regular structures in the Universe.”

—  Jan Oort

[Superclusters, Annual Review of Astronomy and Astrophysics, 21, 1, 373–428, 1983, 10.1146/annurev.aa.21.090183.002105] (quote from p. 373)

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Jan Oort5
Dutch astronomer 1900–1992

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“There exists also another type of galaxy agglomeration. These have diameters between roughly one and ten times those of large clusters, but have much smaller densitities; they are usually irregular, with patchy density variations and no central concentration. The larger and most conspicuous of these agglomerations may contain several clusters, which explains why they have been given the name "superclusters." In their longer dimensions, crossing times exceed the age of the Universe. They are thus unrelaxed. Unrelaxed apperance, together with large size, might be taken as a definition of superclusters.”

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