| Virgo Cluster | |
|---|---|
.jpg) The southern portion of the Virgo Cluster as imaged by theVera C. Rubin Observatory in very high resolution, taken on June 5, 2025.[1][a] | |
| Observation data (EpochJ2000) | |
| Constellation(s) | Virgo &Coma Berenices |
| Right ascension | 12h 27m[3] |
| Declination | +12° 43′[3] |
| Brightest member | Messier 49 |
| Number of galaxies | ~1,500[3] |
| Parent structure | Virgo Supercluster |
| Bautz–Morgan classification | III[3] |
| Distance | 53.8 ± 0.3Mly (16.5 ± 0.1Mpc) |
| Binding mass | 1015 M☉ |
TheVirgo Cluster is acluster of galaxies whose center is53.8 ± 0.3Mly (16.5 ± 0.1Mpc)[4] away in theVirgo constellation. Comprising approximately 1,300 (and possibly up to 2,000) member galaxies,[5] the cluster forms the heart of the largerVirgo Supercluster, of which theLocal Group (containing theMilky Way galaxy) is a member. The Local Group actually experiences the mass of the Virgo Supercluster as theVirgocentric flow. It is estimated that the Virgo Cluster's mass is 1.2×1015M☉ out to 8 degrees of the cluster's center or a radius of about 2.2 Mpc.[6]
Many of the brighter galaxies in this cluster, including the giantelliptical galaxyMessier 87, were discovered in the late 1770s and early 1780s and subsequently included inCharles Messier's catalogue of non-cometary fuzzy objects. Described by Messier asnebulae without stars, their true nature was not recognized until the 1920s.[A]
The cluster extends across approximately 8 degrees centered in the constellation Virgo. Some of its most prominent members can be seen with binoculars and small telescopes, while a 6-inch telescope will reveal about 160 of the cluster's galaxies on a clear night. Itsbrightest member is theelliptical galaxyMessier 49.[8]
The cluster is a fairlyheterogeneous mixture ofspiral andelliptical galaxies.[9] As of 2004[update], it is believed that the spiral galaxies of the cluster are distributed in an oblongprolatefilament, approximately four times as long as it is wide, stretching along the line of sight from theMilky Way.[10] The elliptical galaxies are more centrally concentrated than the spiral galaxies.[11] The first example of anultra-diffuse galaxy was also found in the central core of the cluster in 1984.
The cluster is an aggregate of at least three separatesubclumps: Virgo A, centered onM87, a second centered on the galaxyM86, and Virgo B, centered onM49, with some authors including a Virgo C subcluster, centered on the galaxyM60 as well as a Low Velocity Cloud (LVC) subclump, centered on the large spiral galaxyNGC 4216.[12] The giantelliptical galaxy M87 contains asupermassive black hole, whoseevent horizon was observed by theEvent Horizon Telescope Collaboration in 2019.[13][14]
Virgo A is the dominant subclump; its mass of approximately 1014M☉ is approximately ten times larger than the other two subclumps.[15] It contains a mixture ofelliptical,lenticular, andspiral galaxies which are generally gas-poor,[16]
The three subgroups are in the process of merging to form a larger single cluster,[15] and are surrounded by other smallergalaxy 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,[17] plus other farther isolated galaxies and galaxy groups (like the galaxy cloudComa I) that are also attracted by the gravity of Virgo to merge with it in the future.[18] This strongly suggests the Virgo cluster is a dynamically young cluster that is still forming.[17]
Nearby aggregations known as M Cloud, W Cloud, and W' Cloud seem to be background systems independent of the main cluster.[12][17]
The large mass of the cluster is indicated by the highpeculiar velocities of many of its galaxies, sometimes as high as 1,600km/s with respect to the cluster's center.
The Virgo cluster lies within theVirgo 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 inastrophysics. According to scientists, it occurs because of the extreme environment of the Virgo Cluster.[19]
As with many other rich galaxy clusters, Virgo'sintracluster medium is filled with a hot, rarefiedplasma at temperatures of 30 millionkelvins that emitsX-Rays.[20] Within the intracluster medium (ICM) are found a large number ofintergalactic stars[21][22] (up to 10% of the stars in the cluster),[23] including someplanetary nebulae.[24] It is theorized that these were expelled from their home galaxies byinteractions with other galaxies.[23] The ICM also contains someglobular clusters,[25][26][27] possibly stripped offdwarf galaxies,[27] and even at least onestar formationregion.[28]
Below is a table of bright or notable objects in the cluster and their subcluster. In some cases a galaxy may be considered to be in a different subcluster by other researchers (sources:[12][17][29][30])
| Designation | Coordinates (Epoch 2000) | Apparent magnitude (blue) | Type | Angular size | Diameter (kly) | RV (km/s) | Subcluster | |
|---|---|---|---|---|---|---|---|---|
| RA | Dec | |||||||
| Messier 98 | 12 13.8 | 14 54 | 10.9 | SBb | 9.8′ | 150 | 184 | Virgo A orN Cloud |
| NGC 4216 | 12 15.9 | 13 09 | 10.9 | SBb | 7.9′ | 120 | 459 | Virgo A,N Cloud, orLVC. |
| Messier 99 | 12 18.8 | 14 25 | 10.4 | Sc | 5.4′ | 80 | 2735 | Virgo A orN 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 Markarian's Chain |
| 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. Markarian's Chain |
| 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′ | 980 | 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 4546 | 12 35.5 | −03 48 | 11.3 | S0 | 2.3' | 30 | 1054 | S Cloud |
| 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 orVirgo E |
| Messier 60 | 12 43.7 | 11 33 | 9.8 | E2 | 7.2′ | 110 | 1452 | Virgo A,Virgo E, orVirgo 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.[31]
{{cite book}}:|journal= ignored (help)| Local Sheet |  | |
|---|---|---|
| Others | ||
| Included | Earth →Solar System →Local Interstellar Cloud →Local Bubble →Gould Belt →Orion Arm →Milky Way →Milky Way subgroup →Local Group→Local Sheet→Local Volume→Virgo Supercluster→Laniakea Supercluster →Pisces–Cetus Supercluster Complex →Local Hole →Observable universe →Universe Each arrow (→) may be read as "within" or "part of". |
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| Related | |
