The Virgo Cluster is a cluster of galaxies whose center is 53.8 ± 0.3 Mly (16.5 ± 0.1 Mpc) away in the constellation Virgo. Comprising approximately 1300 (and possibly up to 2000) member galaxies, the cluster forms the heart of the larger Virgo Supercluster, of which the Local Group (containing the Milky Way galaxy) is an outlying member. The Local Group actually experiences the mass of the Virgo Supercluster as the Virgocentric flow. It is estimated that the Virgo Cluster's mass is 1.2×1015 M☉ out to 8 degrees of the cluster's center or a radius of about 2.2 Mpc.
Many of the brighter galaxies in this cluster, including the giant elliptical galaxy Messier 87, were discovered in the late 1770s and early 1780s and subsequently included in Charles Messier's catalogue of non-cometary fuzzy objects. Described by Messier as nebulae without stars, their true nature was not recognized until the 1920s.
The cluster subtends a maximum arc of approximately 8 degrees centered in the constellation Virgo. Many of the member galaxies of the cluster are visible with a small telescope. Its brightest member is the elliptical galaxy Messier 49; however its most famous member is the elliptical galaxy Messier 87, which is located in the center of the cluster, unlike M49.
|Observation data (Epoch J2000)|
|Constellation(s)||Virgo & Coma Berenices|
|Right ascension||12h 27m|
|Brightest member||Messier 49|
|Number of galaxies||~1500|
The cluster is a fairly heterogeneous mixture of spirals and ellipticals. As of 2004, it is believed that the spiral galaxies of the cluster are distributed in an oblong prolate filament, approximately four times as long as it is wide, stretching along the line of sight from the Milky Way. The elliptical galaxies are more centrally concentrated than the spiral galaxies.
The cluster is an aggregrate of at least three separate subclumps: Virgo A, centered on M87, a second centered on the galaxy M86, and Virgo B, centered on M49, with some authors including a Virgo C subcluster, centered on the galaxy M60 as well as a LVC (Low Velocity Cloud) subclump, centered on the large spiral galaxy NGC 4216.
Of all of the subclumps, Virgo A, formed by a mixture of elliptical, lenticular, and (usually) gas-poor spiral galaxies, is the dominant one, with a mass of approximately 1014 M☉, which is approximately an order of magnitude larger than the other two subclumps.
The three subgroups are in the process of merging to form a larger single cluster and are surrounded by other smaller galaxy clouds, 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, 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. This strongly suggests the Virgo cluster is a dynamically young cluster that is still forming.
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.
As with many other rich galaxy clusters, Virgo's intracluster medium is filled with a hot, rarefied plasma at temperatures of 30 million kelvins that emits X-Rays. Within the intracluster medium (ICM) are found a large number of intergalactic stars (up to 10% of the stars in the cluster), including some planetary nebulae. It is theorized that these were expelled from their home galaxies by interactions with other galaxies. The ICM also contains some globular clusters, possibly stripped off dwarf galaxies, and even at least one star formation region.
Below is given a table of bright or notable objects in the Virgo Cluster and the subunit of the cluster in which they are located. Note that in some cases a galaxy may be considered in a different subunit by other researchers (sources:)
|Designation||Coordinates (Epoch 2000)||Apparent magnitude (blue)||Type||Angular size||Diameter
|Messier 98||12 13.8||14 54||10.9||SBb||9.8′||150||184||Virgo A or N Cloud|
|NGC 4216||12 15.9||13 09||10.9||SBb||7.9′||120||459||Virgo A, N Cloud, or LVC.|
|Messier 99||12 18.8||14 25||10.4||Sc||5.4′||80||2735||Virgo A or N Cloud|
|NGC 4262||12 19.5||14 53||12.4||S0||1.9′||30||1683||Virgo A|
|NGC 4388||12 25.5||12 39||11.8||SAb||6.2′||85||2845||Virgo A|
|Messier 61||12 21.9||04 28||10.2||SBbc||6.2′||100||1911||S Cloud|
|Messier 100||12 22.9||15 49||10.1||SBbc||7.6′||115||1899||Virgo A|
|Messier 84||12 25.1||12 53||10.1||E1||6.0′||90||1239||Virgo A|
|Messier 85||12 25.4||18 11||10.0||S0||7.1′||105||1056||Virgo A|
|Messier 86||12 26.2||12 57||9.9||E3||10.2′||155||37||Virgo A or own subgroup.|
|NGC 4435||12 27.7||13 05||11.7||S0||3.0′||45||1111||Virgo A|
|NGC 4438||12 27.8||13 01||11.0||Sa||8.7′||130||404||Virgo A|
|NGC 4450||12 28.5||17 05||10.9||Sab||5.1′||80||2273||Virgo A|
|Messier 49||12 29.8||08 00||9.3||E2||9.8′||150||1204||Virgo B|
|Messier 87||12 30.8||12 23||9.6||E0-1||9.8′||150||1204||Virgo A|
|Messier 88||12 32.0||14 25||10.3||Sb||6.8′||100||2599||Virgo A|
|NGC 4526||12 32.0||07 42||10.6||S0||7.1′||105||931||Virgo B|
|NGC 4527||12 34.1||02 39||12.4||Sb||4.6′||69||1730||S Cloud|
|NGC 4536||12 34.4||02 11||11.1||SBbc||7.2′||115||2140||S Cloud|
|Messier 91||12 35.4||14 30||11.0||SBb||5.2′||80||803||Virgo A|
|NGC 4550||12 35.5||12 13||12.5||S0||3.2′||50||704||Virgo A|
|Messier 89||12 35.7||12 33||10.7||E0||5.0′||75||628||Virgo A|
|NGC 4567||12 36.5||11 15||12.1||Sbc||2.8′||40||2588||Virgo A|
|NGC 4568||12 36.6||11 14||11.7||Sbc||4.4′||65||2578||Virgo A|
|Messier 90||12 36.8||13 10||10.2||SBab||10.5′||160||87||Virgo A|
|NGC 4571||12 36.9||14 13||11.9||Sc||3.7′||55||659||Virgo A|
|Messier 58||12 37.7||11 49||10.6||SBb||5.6′||85||1839||Virgo A|
|Messier 59||12 42.9||11 39||10.8||E5||5.0′||75||751||Virgo A or Virgo E|
|Messier 60||12 43.7||11 33||9.8||E2||7.2′||110||1452||Virgo A, Virgo E, or Virgo C|
|NGC 4651||12 43.7||16 24||11.4||Sc||4.0′||60||1113|
|NGC 4654||12 43.9||13 08||11.1||SBc||5.0′||75||1349||Virgo A|
Fainter galaxies within the cluster are usually known by their numbers in the Virgo Cluster Catalog, particularly members of the numerous dwarf galaxy population.