Editing Virgo Supercluster (section)

==Galaxy distribution==
The [[number density]] of galaxies in the LS falls off with the square of the distance from its center near the [[Virgo Cluster]], suggesting that this cluster is not randomly located. Overall, the vast majority of the luminous galaxies (less than [[absolute magnitude]] −13) are concentrated in a small number of [[Galaxy cloud|clouds]] (groups of [[galaxy cluster]]s). Ninety-eight percent can be found in the following 11 clouds, given in decreasing order of number of luminous galaxies: [[M94 Group#Canes Venatici Cloud|Canes Venatici]], Virgo Cluster, [[Virgo II Groups|Virgo II]] (southern extension), [[Leo II Groups|Leo II]], [[Virgo III Groups|Virgo III]], Crater ([[NGC 3672]]), [[M96 Group|Leo I]], Leo Minor ([[NGC 2841]]), Draco ([[NGC 5907]]), Antlia ([[NGC 2997]]), and [[NGC 5643]].{{citation needed|date=March 2025}}

Of the luminous galaxies located in the disk, one third are in the Virgo Cluster. The remainder are found in the Canes Venatici Cloud and Virgo II Cloud, plus the somewhat insignificant [[NGC 5643 Group]].{{citation needed|date=March 2025}}

The luminous galaxies in the halo are concentrated in a small number of clouds (94% in 7 clouds). This distribution indicates that "most of the volume of the supergalactic plane is a great void."<ref name="tully82" /> A helpful analogy that matches the observed distribution is that of soap bubbles. Flattish clusters and [[superclusters]] are found at the intersection of bubbles, which are large, roughly spherical (on the order of 20–60 [[Parsec|Mpc]] in diameter) voids in space.<ref name="ma96">
{{cite book
 | author = Carroll, Bradley
 | author2 = Ostlie, Dale
 | title = An Introduction to Modern Astrophysics
 | publisher = [[Addison-Wesley]]
 | date = 1996
 | location = New York
 | page = 1136
 | isbn = 0-201-54730-9
}}</ref>
Long filamentary structures seem to predominate. An example of this is the [[Hydra–Centaurus Supercluster]], the nearest supercluster to the Virgo Supercluster, which starts at a distance of roughly 30 Mpc and extends to 60 Mpc.<ref name="fairall89">
{{cite journal
 | last1 = Fairall | first1 = A. P.
 | last2 = Vettolani | first2 = G.
 | last3 = Chincarini | first3 = G.
 | title = A wide angle redshift survey of the Hydra-Centaurus region
 | journal = Astronomy and Astrophysics Supplement Series
 | date = May 1989
 | volume = 78
 | issue = 2
 | page = 270
 | bibcode = 1989A&AS...78..269F
 | issn=0365-0138
}}</ref>