Editing Virgo Cluster (section)

== Characteristics ==
The cluster is a fairly [[heterogeneous]] mixture of [[Spiral galaxy|spiral]] and [[Elliptical galaxy|elliptical]] galaxies.<ref>{{Cite journal | doi = 10.1086/421490| last1 = Côté | first1 = Patrick| last2 = Blakeslee |first2 = John P.| last3 = Ferrarese | first3 = Laura| last4 = Jordán | first4 = Andrés| last5 = Mei | first5 = Simona| last6 = Merritt | first6 = David| author6-link = David Merritt| last7 = Milosavljević | first7 = Miloš| last8 = Peng | first8 = Eric W.
| last9= Tonry |first9= John L. |title= The ACS Virgo Cluster Survey | journal= [[The Astrophysical Journal]] | volume= 153 | issue= 1 |pages= 223–242 |date=July 2004 |bibcode= 2004ApJS..153..223C | arxiv = astro-ph/0404138 | display-authors = 9| last10 = West| first10 = Michael J.| s2cid = 18021414 }}</ref> {{As of|2004}}, it is believed that the spiral galaxies of the cluster are distributed in an oblong [[prolate spheroid|prolate]] [[Galaxy filament|filament]], approximately four times as long as it is wide, stretching along the line of sight from the [[Milky Way]].<ref name="Fukugitaetal1993">{{cite journal | author = M. Fukugita | author2 = S. Okamura | author3 = N. Yasuda | title = Spatial distribution of spiral galaxies in the Virgo Cluster from the Tully-Fisher relation | journal = [[Astrophysical Journal]] | date = 1993 | volume = 412 | pages = L13–L16 | bibcode = 1993ApJ...412L..13F | doi = 10.1086/186928}}</ref> The elliptical galaxies are more centrally concentrated than the spiral galaxies.<ref>{{Cite web | url=https://ned.ipac.caltech.edu/level5/ESSAYS/Binggeli/binggeli.html| title=Virgo Cluster|website=ned.ipac.caltech.edu|access-date=2018-06-24}}</ref>

The cluster is an aggregate of at least three separate [[subclump]]s: Virgo A, centered on [[Elliptical galaxy M87|M87]], a second centered on the galaxy [[Lenticular Galaxy M86|M86]], and Virgo B, centered on [[Elliptical Galaxy M49|M49]], with some authors including a Virgo C subcluster, centered on the galaxy [[Elliptical Galaxy M60|M60]] as well as a Low Velocity Cloud (LVC) subclump, centered on the large spiral galaxy [[NGC 4216]].<ref name=Boselli2014>{{cite journal |last1=Boselli |first1=A. |last2=Voyer |first2=E. |last3=Boissier |first3= S. |last4=Cucciati |first4= O. | last5= Consolandi | first5=G. |last6=Cortese |first6=L. |last7=Fumagalli |first7=M. |last8=Gavazzi |first8=G. |last9=Heinis |first9=S. |last10=Roehlly |first10=Y. |last11=Toloba |first11=E. |date=2014 |title=The GALEX Ultraviolet Virgo Cluster Survey (GUViCS). IV. The role of the cluster environment on galaxy evolution |journal=Astronomy & Astrophysics |volume=570 |id=A69 |arxiv=1407.4986 | doi= 10.1051/0004-6361/201424419 |bibcode=2014A&A...570A..69B |pages=A69|s2cid=119244700 }}</ref> The giant [[elliptical galaxy]] M87 contains a [[supermassive black hole]], whose [[event horizon]] was observed by the [[Event Horizon Telescope]] Collaboration in 2019.<ref>{{Cite journal | last1=Event Horizon Telescope Collaboration| last2=Akiyama| first2=Kazunori| last3=Alberdi| first3=Antxon| last4=Alef| first4=Walter| last5=Asada| first5=Keiichi|last6=Azulay|first6=Rebecca|last7=Baczko|first7=Anne-Kathrin| last8=Ball| first8=David| last9=Balokovic| first9=Mislav| last10=Barrett| first10=John| last11=Bintley|first11=Dan|date=2019-04-01|title=First M87 Event Horizon Telescope Results. I. The Shadow of the Supermassive Black Hole| journal=The Astrophysical Journal Letters|volume=875| issue=1|pages=L1|doi=10.3847/2041-8213/ab0ec7 |arxiv=1906.11238| bibcode=2019ApJ...875L...1E|doi-access=free}}</ref><ref>{{Cite web | title=Publications {{!}} Event Horizon Telescope| url=https://eventhorizontelescope.org/publications| access-date=2020-09-10| website=eventhorizontelescope.org| language=en}}</ref>

Virgo A is the dominant subclump; its mass of approximately 10<sup>14</sup> {{solar mass|link=y}} is approximately ten times larger than the other two subclumps.<ref name=BinggeliNED>[http://nedwww.ipac.caltech.edu/level5/Binggeli/frames.html The Virgo Super Cluster: home of M87] (with frames)</ref> It contains a mixture of [[elliptical galaxy|elliptical]], [[lenticular galaxy|lenticular]], and [[spiral galaxy|spiral galaxies]] which are generally gas-poor,<ref name=Chamaraux1980>{{cite journal |last1=Chamaraux |first1=P. |last2=Balkowski |first2=C. |last3=Gerard |first3=E. |date=1980 |title=The H I deficiency of the Virgo cluster spirals |journal=Astronomy & Astrophysics |volume=83 |issue=1–2 |pages=38–51 |bibcode=1980A&A....83...38C}}</ref>
[[File:14-296-GalaxyClusters-PerseusVirgo-ChandraXRay-20141027.jpg|thumb|left|[[Turbulence]] may prevent galaxy clusters from cooling ([[Chandra X-ray Observatory|Chandra X-ray]]).]]
The three subgroups are in the process of merging to form a larger single cluster,<ref name=BinggeliNED/> and are surrounded by other smaller [[galaxy cloud]]s, mostly composed of spiral galaxies, known as N Cloud, S Cloud, and Virgo E that are in the process of infalling to merge with them,<ref name="Gavazzietal1999">{{cite journal
  | author=Gavazzi, G.
  | author2=Boselli, A.
  | author3=Scodeggio, M.
  | author4=Pierini, D.
  | author5=Belsole, E.
  | title=The 3D structure of the Virgo cluster from H-band Fundamental Plane and Tully-Fisher distance determinations
  | journal=[[Monthly Notices of the Royal Astronomical Society]]
  | date=1999
  | volume=304
  | pages=595–610
  |arxiv = astro-ph/9812275 |bibcode = 1999MNRAS.304..595G |doi = 10.1046/j.1365-8711.1999.02350.x | issue=3
  | doi-access=free
 | s2cid=41700753
 }}</ref> plus other farther isolated galaxies and galaxy groups (like the galaxy cloud [[Coma I]]) that are also attracted by the gravity of Virgo to merge with it in the future.<ref name="Tully1984">{{cite journal
  | author=Tully, R. B.
  | author2=Shaya, E. J.
  | title=Infall of galaxies into the Virgo cluster and some cosmological constraints
  | journal=Astrophysical Journal
  | date=1984
  | volume=281
  | pages=31–55
  |bibcode = 1984ApJ...281...31T |doi = 10.1086/162073 | doi-access=free
  }}</ref> This strongly suggests the Virgo cluster is a dynamically young cluster that is still forming.<ref name=Gavazzietal1999/>

Nearby aggregations known as M Cloud, W Cloud, and W' Cloud seem to be background systems independent of the main cluster.<ref name=Boselli2014/><ref name=Gavazzietal1999/>

The large mass of the cluster is indicated by the high [[peculiar velocity|peculiar velocities]] of many of its galaxies, sometimes as high as 1,600 [[kilometre|km]]/[[second|s]] with respect to the cluster's center.

The Virgo cluster lies within the [[Virgo Supercluster]], and its gravitational effect slows down the nearby galaxies. The large mass of the cluster has the effect of slowing down the recession of the Local Group from the cluster by approximately ten percent.

Molecular gasses in Virgo Cluster has been swept away by a huge cosmic broom that is preventing nearby galaxies from birthing new stars. The actual cause of it has been a long standing mystery in [[astrophysics]]. According to scientists, it occurs because of the extreme environment of the Virgo Cluster.<ref>{{Cite journal|last1=Brown|first1=Toby|last2=Wilson|first2=Christine D.|last3=Zabel|first3=Nikki|last4=Davis|first4=Timothy A.|last5=Boselli|first5=Alessandro|last6=Chung|first6=Aeree|last7=Ellison|first7=Sara L.|last8=Lagos|first8=Claudia D. P.|last9=Stevens|first9=Adam R. H.|last10=Cortese|first10=Luca|last11=Bahé|first11=Yannick M.|date=2021-12-01|title=VERTICO: The Virgo Environment Traced In CO Survey|journal=The Astrophysical Journal Supplement Series|volume=257|issue=2|pages=21|doi=10.3847/1538-4365/ac28f5|arxiv=2111.00937 |bibcode=2021ApJS..257...21B |s2cid=240354399 |issn=0067-0049 |doi-access=free }}</ref>