World Library  
Flag as Inappropriate
Email this Article

Virgo Cluster

Article Id: WHEBN0000214067
Reproduction Date:

Title: Virgo Cluster  
Author: World Heritage Encyclopedia
Language: English
Subject: Virgo (constellation), Supercluster, 100 zettametres, Paul L. Schechter, Adelaide Ames
Publisher: World Heritage Encyclopedia

Virgo Cluster

Virgo Cluster

Virgo Cluster showing the diffuse light between member galaxies. Messier 87 is the largest galaxy (lower left).
Observation data (Epoch J2000)
Constellation(s) Virgo & Coma Berenices
Right ascension 12h 27m[1]
Declination +12° 43′[1]
Bautz-Morgan classification III [1]
See also: Galaxy groups, Galaxy clusters, List of galaxy clusters

The Virgo Cluster (VC) is a cluster of galaxies whose center is 53.8 ± 0.3 Mly (16.5 ± 0.1 Mpc)[2] away in the constellation Virgo. Comprising approximately 1300 (and possibly up to 2000) member galaxies,[3] the cluster forms the heart of the larger Virgo Supercluster, of which the Local Group (LG) is an outlying member. However, the LG experiences the mass of the VC as the Virgocentric flow. It is estimated that the VC's mass is 1.2×1015 M out to 8 degrees of the cluster's center or a radius of about 2.2 Mpc.[4]

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.[5]

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 also elliptical galaxy Messier 87, that unlike the former is located in the center of the cluster.


The cluster is a fairly heterogeneous mixture of spirals and ellipticals.[6] As of 2004, it is believed that the spirals 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.[7] 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, that surrounds M49. Of the three, Virgo A, formed by a mixture of elliptical, lenticular, and -usually- gas-poor spiral galaxies,[8] is the dominant one, with a mass of approximately 1014 M, which is approximately an order of magnitude larger than the other two subclumps.[9]

Turbulence may prevent galaxy clusters from cooling (Chandra X-ray).

The three subgroups are in the process of merging to form a larger single cluster[9] 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,[10] 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.[11] This strongly suggests the Virgo cluster is a dynamically young cluster that is still forming.[10]

Other two nearby aggregations known as M Cloud and W Cloud seem to be background systems independent of the main cluster.[10]

The large mass of the cluster is indicated by the high peculiar velocities of many of its galaxies, sometimes as high as 1,600 km/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.

Intracluster medium

As with many other rich galaxy clusters, Virgo's intracluster medium is filled with a hot, rarefied plasma at temperatures of 30 million Kelvin that emits X-Rays,[12] and within it can be found a large number of intergalactic stars[13] (up to 10% of the stars in the cluster),[14] including some planetary nebulae,[15] that it's theorized were expelled from their home galaxies on interactions with other galaxies,[14] as well as some globular clusters,[16][17][18] possibly stripped off dwarf galaxies,[18] and even at least one star formation region.[19]

Bright or notable galaxies of the Virgo Cluster

Virgo Cluster of galaxies.

Below is given a table of bright or notable objects in the Virgo Cluster and the cluster's subunit where they're located. Note that in some cases a galaxy may be considered in one subunit or in another (sources:[10][20][21])

Column 1: The name of the galaxy.
Column 2: The Right Ascension for epoch 2000.
Column 3: The Declination for epoch 2000.
Column 4: The blue apparent magnitude of the galaxy.
Column 5: The galaxy type: E=Elliptical, S0=Lenticular, Sa,Sb,Sc,Sd=Spiral, SBa,SBb,SBc,SBd=Barred Spiral, Sm,SBm,Irr=Irregular.
Column 6: The angular diameter of the galaxy (arcminutes).
Column 7: The diameter of the galaxy (thousands of light years).
Column 8: The recessional velocity (km/s) of the galaxy relative to the cosmic microwave background.
Column 9: Subcluster where the galaxy is located.
Cluster Members
Designation Coordinates (Epoch 2000) Apparent Magnitude (blue) Type Angular Size Diameter
RA Dec
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 or N Cloud
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
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
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 or Virgo E
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

See also


  1. ^ a b c "NASA/IPAC Extragalactic Database". Results for Virgo Cluster. Retrieved 2006-10-19. 
  2. ^ Mei, Simona; Blakeslee, John P.; Côté, Patrick; Tonry, John L.; West, Michael J.; Ferrarese, Laura; Jordán, Andrés; Peng, Eric W.; Anthony, André; Merritt, Davi; Blakeslee; Côté; Tonry; West; Ferrarese; Jordán; Peng; Anthony; Merritt (2007). "The ACS Virgo Cluster Survey. XIII. SBF Distance Catalog and the Three-dimensional Structure of the Virgo Cluster". The Astrophysical Journal 655 (1): 144–162.  
  3. ^ See Virgo Cluster.
  4. ^ Fouqué, P.; Solanes, J. M.; Sanchis, T.; Balkowski, C.; Solanes; Sanchis; Balkowski (2001). "Structure, mass and distance of the Virgo cluster from a Tolman-Bondi model".  
  5. ^ Following the entry for M91 in the Connoissance des Temps for 1784, Messier added the following note:
    The constellation of Virgo, & especially the northern Wing is one of the constellations which encloses the most Nebulae: this Catalog contains thirteen which have been determined: viz. Nos. 49, 58, 59, 60, 61, 84, 85, 86, 87, 88, 89, 90, & 91. All these nebulae appear to be without stars: one can see them only in a very good sky, & near their meridian passage. Most of these nebulae have been pointed to me by Mr. Méchain. (see M91.)
  6. ^ Côté, Patrick; Blakeslee, John P.; Ferrarese, Laura; Jordán, Andrés; Mei, Simona;  
  7. ^ M. Fukugita, S. Okamura, N. Yasuda; Okamura; Yasuda (1993). "Spatial distribution of spiral galaxies in the Virgo Cluster from the Tully-Fisher relation".  
  8. ^ Chamaraux, P.; Balkowski, C.; Gerard, E. (1980). "The H I deficiency of the Virgo cluster spirals". Astronomy & Astrophysics 83 (1–2): 38–51.  
  9. ^ a b The Virgo Super Cluster: home of M87 (with frames)
  10. ^ a b c d Gavazzi, G.; Boselli, A.; Scodeggio, M.; Pierini, D.; Belsole, E.; Boselli; Scodeggio; Pierini; Belsole (1999). "The 3D structure of the Virgo cluster from H-band Fundamental Plane and Tully-Fisher distance determinations".  
  11. ^ Tully, R. B.; Shaya, E. J.; Shaya (1984). "Infall of galaxies into the Virgo cluster and some cosmological constraints". Astrophysical Journal 281: 31–55.  
  12. ^ Lea, S. M.; Mushotzky, R.; Holt, S. S.; Mushotzky; Holt (1982). "Einstein Observatory solid state spectrometer observations of M87 and the Virgo cluster". Astrophysical Journal 262 (1): 24–32.  
  13. ^ Ferguson, H. (1997). "Intergalactic Stars in the Virgo Cluster". HST proposal: 7411.  
  14. ^ a b Ferguson, Henry C.; Tanvir, Nial R.; von Hippel, Ted; Tanvir; von Hippel (1998). "Detection of intergalactic red-giant-branch stars in the Virgo cluster". Nature 391 (6666): 461.  
  15. ^ Feldmeier, J.; Ciardullo, R.; Jacoby, G.; Ciardullo; Jacoby (1998). "INTRACLUSTER PLANETARY NEBULAE IN THE VIRGO CLUSTER. I. INITIAL RESULTS". Astrophysical Journal 503: 109–117.  
  16. ^ Takamiya, Marianne; West, Michael; Côté, Patrick; Jordán, Andrés; Peng, Eric; Ferrarese, Laura; West; Côté; Jordán; Peng; Ferrarese (2009). "IGCs in the Virgo Cluster". Globular Clusters - Guides to Galaxies, Eso Astrophysics Symposia, Volume . Eso Astrophysics Symposia: 361.  
  17. ^ Durrell, Patrick R.; Accetta, K.; Feldmeier, J. J.; Mihos, J. C.; Ciardullo, R.; Peng, E. W.; Members of the NGVS team (2010). "Searching for Intracluster Globular Clusters in the Virgo Cluster". 
  18. ^ a b Lee, Myung Gyoon; Park, Hong Soo; Hwang, Ho Seong; Park; Hwang (2010). "Detection of a Large-Scale Structure of Intracluster Globular Clusters in the Virgo Cluster". Science 328 (5976): 334–.  
  19. ^ Gerhard, Ortwin; Arnaboldi, Magda; Freeman, Kenneth C.; Okamura, Sadanori; Arnaboldi; Freeman; Okamura (2002). "Isolated Star Formation: A Compact H II Region in the Virgo Cluster". The Astrophysical Journal 580 (2): L121–L124.  
  20. ^ "Galaxy On Line Database Milano Network (GOLDMine)". Retrieved 2012-08-06. 
  21. ^ "The Virgo Cluster". Retrieved 2013-04-06. 

External links

  • The Virgo Cluster at An Atlas of the Universe
  • California Institute of Technology site on Virgo cluster.
  • The Virgo Cluster of Galaxies, SEDS Messier pages
  • Partial Virgo cluster centered on M87 (Dark Atmospheres)

This article was sourced from Creative Commons Attribution-ShareAlike License; additional terms may apply. World Heritage Encyclopedia content is assembled from numerous content providers, Open Access Publishing, and in compliance with The Fair Access to Science and Technology Research Act (FASTR), Wikimedia Foundation, Inc., Public Library of Science, The Encyclopedia of Life, Open Book Publishers (OBP), PubMed, U.S. National Library of Medicine, National Center for Biotechnology Information, U.S. National Library of Medicine, National Institutes of Health (NIH), U.S. Department of Health & Human Services, and, which sources content from all federal, state, local, tribal, and territorial government publication portals (.gov, .mil, .edu). Funding for and content contributors is made possible from the U.S. Congress, E-Government Act of 2002.
Crowd sourced content that is contributed to World Heritage Encyclopedia is peer reviewed and edited by our editorial staff to ensure quality scholarly research articles.
By using this site, you agree to the Terms of Use and Privacy Policy. World Heritage Encyclopedia™ is a registered trademark of the World Public Library Association, a non-profit organization.

Copyright © World Library Foundation. All rights reserved. eBooks from Hawaii eBook Library are sponsored by the World Library Foundation,
a 501c(4) Member's Support Non-Profit Organization, and is NOT affiliated with any governmental agency or department.