Editing Virgo Supercluster (section)

==Structure==
In 1982, [[R. Brent Tully]] presented the conclusions of his research concerning the basic structure of the LS. It consists of two components: an appreciably flattened disk containing two thirds of the supercluster's luminous galaxies, and a roughly spherical halo containing the remaining third.<ref name="hu06">
{{cite journal
 | author = Hu, F. X.
 | display-authors = etal
 | title = Orientation of Galaxies in the Local Supercluster: A Review
 | journal = Astrophysics and Space Science
 | date = April 2006
 | volume = 302
 | issue = 1–4
 | pages = 43–59
 | bibcode = 2006Ap&SS.302...43H
 | doi = 10.1007/s10509-005-9006-7
 | arxiv = astro-ph/0508669
| s2cid = 18837475
 }}</ref> The disk itself is a thin (~1 [[Parsec|Mpc]]) ellipsoid with a long axis / short axis ratio of at least 6 to 1, and possibly as high as 9 to 1.<ref name="tully82">
{{cite journal
 | author = Tully, R. B.
 | title = The Local Supercluster
 | journal = Astrophysical Journal
 | date = 15 Jun 1982
 | volume = 257
 | issue = 1
 | pages = 389–422
 | bibcode = 1982ApJ...257..389T
 | doi = 10.1086/159999
| doi-access = free
 }}</ref> Data released in June 2003 from the 5-year [[2dF Galaxy Redshift Survey|Two-degree-Field Galaxy Redshift Survey (2dF)]] has allowed astronomers to compare the LS to other superclusters. The LS represents a typical poor (that is, lacking a high density core) supercluster of rather small size. It has one rich galaxy cluster in the center, surrounded by filaments of galaxies and poor groups.<ref name="ein07">
{{cite journal
 | author = Einasto, M.
 | display-authors = etal
 | title = The richest superclusters. I. Morphology
 | journal = Astronomy and Astrophysics
 | date = December 2007
 | volume = 476
 | issue = 2
 | pages = 697–711
 | bibcode = 2007A&A...476..697E
 | doi = 10.1051/0004-6361:20078037
|arxiv = 0706.1122 | s2cid = 15004251
 }}</ref> 

The [[Local Group]] is located on the outskirts of the LS in a small filament extending from the [[Fornax Cluster]] to the [[Virgo Cluster]].<ref name="klypin03" /> The Virgo Supercluster's volume is roughly 7,000 times that of the Local Group, or 100 billion times that of the Milky Way.

The main body of the Virgo Supercluster, the flattened disk of galaxies is simply part of a larger [[galaxy filament]] known as the [[Virgo Strand]] or [[Centaurus–Virgo–PP Filament]].<ref name=":0">{{Cite journal |last1=Courtois |first1=Hélène M. |last2=Pomarède |first2=Daniel |last3=Tully |first3=R. Brent |last4=Hoffman |first4=Yehuda |last5=Courtois |first5=Denis |date=September 2013 |title=Cosmography of the Local Universe |url=https://ui.adsabs.harvard.edu/abs/2013AJ....146...69C/abstract |journal=The Astronomical Journal |language=en |volume=146 |issue=3 |pages=69 |doi=10.1088/0004-6256/146/3/69 |arxiv=1306.0091 |bibcode=2013AJ....146...69C |issn=0004-6256}}</ref><ref name=":1">{{Cite journal |last1=Pomarède |first1=Daniel |last2=Hoffman |first2=Yehuda |last3=Courtois |first3=Hélène M. |last4=Tully |first4=R. Brent |date=August 2017 |title=The Cosmic V-Web |journal=The Astrophysical Journal |language=en |volume=845 |issue=1 |pages=55 |doi=10.3847/1538-4357/aa7f78 |doi-access=free |arxiv=1706.03413 |bibcode=2017ApJ...845...55P |issn=0004-637X}}</ref> This filament eminates from the [[Centaurus Cluster]] through the [[Virgo Cluster]] and continues through the [[Ursa Major Cluster]] all the way to the [[Perseus–Pisces Supercluster]].<ref name=":1" />  The [[Virgo Strand]] constits of two branches, an upper branch constisting of the main body of the supercluster though the [[Virgo Southern Extension]], the [[Virgo Cluster|Virgo]] and the [[Ursa Major Cluster]], and a lower branch consting of the [[Crater Cloud|Crater]] and [[Leo Cloud|Leo Clouds]].<ref name=":0" /> The rest of remaing third of the galaxies in Virgo Supercluster, including the Milky Way, lie outside the main body of the Supercluster which is the [[Virgo Strand]].<ref name="tully82" /><ref name=":0" />