Editing Supergalactic coordinate system (section)

==History==
In the 1950s the astronomer [[Gérard de Vaucouleurs]] recognized the existence of a flattened “local supercluster” from the [[Shapley-Ames Catalog]] in the environment of the Milky Way. He noticed that when one plots nearby galaxies in 3D, they lie more or less on a plane. A flattened distribution of [[nebula]]e had earlier been noted by [[William Herschel]]. [[Vera Rubin]] had also identified the supergalactic plane in the 1950s, but her data remained unpublished.<ref>{{cite news |last=Scoles |first=Sarah|date=4 October 2016|title=How Vera Rubin confirmed dark matter |magazine=[[Astronomy (magazine)|Astronomy]] |url=http://www.astronomy.com/news/2016/10/vera-rubin}}</ref> The plane delineated by various galaxies defined in 1976 the equator of the supergalactic coordinate system de Vaucouleurs developed. In years thereafter with more observation data available de Vaucouleurs' and Rubin's findings about the existence of the plane proved right.

Based on the supergalactic coordinate system of de&nbsp;Vaucouleurs, surveys<ref>{{Cite arXiv |last=Lahav |display-authors=etal |first=O. |date=1998 |title=The Supergalactic Plane revisited with the Optical Redshift Survey |eprint=astro-ph/9809343}}</ref> in recent years determined the positions of nearby [[galaxy cluster]]s relative to the supergalactic plane. Amongst others the [[Virgo cluster]], the Norma cluster (including the [[Great Attractor]]), the Coma cluster, the [[Pisces-Perseus supercluster]], the Hydra cluster, the Centaurus cluster, the Pisces-Cetus supercluster and the Shapley Concentration were found to be near the supergalactic plane.