Virgo Cluster

{{Galaxy cluster

| name = Virgo Cluster

| image = ESO-M87.jpg

| caption = Virgo Cluster showing the diffuse light between member galaxies. Messier 87 is the largest galaxy (lower left).

| epoch = J2000

| ra = {{RA|12|27}}{{cite web

| title = NASA/IPAC Extragalactic Database

| work = Results for Virgo Cluster

| url = http://nedwww.ipac.caltech.edu/

| access-date = 2006-10-19}}

| dec = {{DEC|+12|43}}

| constellation = Virgo & Coma Berenices

| member_no = ~1,500

| parent = Virgo Supercluster

| bmtype = III

| brightest_member = Messier 49

| mass = 10¹⁵

| other_names =

}}

The Virgo Cluster is a cluster of galaxies whose center is 53.8 ± 0.3 Mly (16.5 ± 0.1 Mpc){{cite journal | author = Mei, Simona | author2 = Blakeslee, John P. | author3 = Côté, Patrick | author4 = Tonry, John L. | author5 = West, Michael J. | author6 = Ferrarese, Laura | author7 = Jordán, Andrés | author8 = Peng, Eric W. | author9 = Anthony, André | author10 = Merritt, Davi | title = The ACS Virgo Cluster Survey. XIII. SBF Distance Catalog and the Three-dimensional Structure of the Virgo Cluster | journal = The Astrophysical Journal | date = 2007 | volume = 655 | issue = 1 | pages = 144–162 | bibcode = 2007ApJ...655..144M | doi = 10.1086/509598 | arxiv = astro-ph/0702510 | s2cid = 16483538 }} away in the Virgo constellation. Comprising approximately 1,300 (and possibly up to 2,000) member galaxies,{{cite web |url=http://astronomy.swin.edu.au/cosmos/V/Virgo+Cluster |title=Virgo Cluster |website=Cosmos |publisher=Swinburne University of Technology}} the cluster forms the heart of the larger Virgo Supercluster, of which the Local Group (containing the Milky Way galaxy) is a 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{{e|15}} {{solar mass|link=y}} out to 8 degrees of the cluster's center or a radius of about 2.2 Mpc.{{cite journal | author = Fouqué, P. | author2 = Solanes, J. M. | author3 = Sanchis, T. | author4 = Balkowski, C. | title = Structure, mass and distance of the Virgo cluster from a Tolman-Bondi model | journal = Astronomy and Astrophysics | date = 2001 | volume = 375 | issue = 3 | pages = 770–780 | bibcode = 2001A&A...375..770F | doi = 10.1051/0004-6361:20010833 | arxiv = astro-ph/0106261 | s2cid = 10468717 }}

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.{{refn|group=upper-alpha|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.{{cite web |title=Messier 91 — Observations and Descriptions |url=http://messier.seds.org/Mdes/dm091.html |publisher=SEDS}}}}

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. Its brightest member is the elliptical galaxy Messier 49.{{Cite web|url=http://www.messier-objects.com/virgo-cluster/|title=Virgo Cluster {{!}} Messier Objects|website=www.messier-objects.com|date=9 August 2017|language=en-US|access-date=2018-06-24}}

Characteristics

The cluster is a fairly heterogeneous mixture of spiral and elliptical galaxies.{{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 }} {{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.{{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}} The elliptical galaxies are more centrally concentrated than the spiral galaxies.{{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}}

The cluster is an aggregate 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 Low Velocity Cloud (LVC) subclump, centered on the large spiral galaxy NGC 4216.{{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 }} The giant elliptical galaxy M87 contains a supermassive black hole, whose event horizon was observed by the Event Horizon Telescope Collaboration in 2019.{{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}}{{Cite web | title=Publications {{!}} Event Horizon Telescope| url=https://eventhorizontelescope.org/publications| access-date=2020-09-10| website=eventhorizontelescope.org| language=en}}

Virgo A is the dominant subclump; its mass of approximately 10¹⁴ {{solar mass|link=y}} is approximately ten times larger than the other two subclumps.[http://nedwww.ipac.caltech.edu/level5/Binggeli/frames.html The Virgo Super Cluster: home of M87] (with frames) It contains a mixture of elliptical, lenticular, and spiral galaxies which are generally gas-poor,{{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}}

File:14-296-GalaxyClusters-PerseusVirgo-ChandraXRay-20141027.jpg may prevent galaxy clusters from cooling (Chandra X-ray).]]

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,{{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

}} 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.{{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

}} This strongly suggests the Virgo cluster is a dynamically young cluster that is still forming.

Nearby aggregations known as M Cloud, W Cloud, and W' Cloud seem to be background systems independent of the main cluster.

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.

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.{{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 }}

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 kelvins that emits X-Rays.{{cite journal

| author=Lea, S. M.

| author2=Mushotzky, R.

| author3=Holt, S. S.

| title=Einstein Observatory solid state spectrometer observations of M87 and the Virgo cluster

| journal=Astrophysical Journal

| date=1982

| issue=1

| volume=262

| pages=24–32

|bibcode = 1982ApJ...262...24L |doi = 10.1086/160392 | hdl=2060/19820026438

| s2cid=120960432

| hdl-access=free

}} Within the intracluster medium (ICM) are found a large number of intergalactic stars{{cite journal

| author=Ferguson, H.

| title=Intergalactic Stars in the Virgo Cluster

| journal=HST Proposal

| date=1997

| bibcode=1997hst..prop.7411F| pages=7411

}}{{Cite journal|last1=Ferguson|first1=Henry C.|last2=Tanvir|first2=Nial R.|last3=von Hippel|first3=Ted|date=January 1998|title=Detection of intergalactic red-giant-branch stars in the Virgo cluster|journal=Nature|language=En|volume=391|issue=6666|pages=461–463|doi=10.1038/35087|issn=0028-0836|arxiv=astro-ph/9801228|bibcode=1998Natur.391..461F|s2cid=4390832}} (up to 10% of the stars in the cluster), including some planetary nebulae.{{cite journal

| author=Feldmeier, J.

| author2=Ciardullo, R.

| author3=Jacoby, G.

| title=Intracluster Planetary Nebulae in the Virgo Cluster. I. Initial Results

| journal=Astrophysical Journal

| date=1998

| volume=503

| issue=1

| pages=109–117

|arxiv = astro-ph/9803062 |bibcode = 1998ApJ...503..109F |doi = 10.1086/305981 | s2cid=9761241

}} It is theorized that these were expelled from their home galaxies by interactions with other galaxies.{{cite journal

| author=Ferguson, Henry C.

| author2=Tanvir, Nial R.

| author3=von Hippel, Ted

| title=Detection of intergalactic red-giant-branch stars in the Virgo cluster

| journal=Nature

| date=1998

| volume=391

| pages=461–463

|arxiv = astro-ph/9801228 |bibcode = 1998Natur.391..461F |doi = 10.1038/35087 | issue=6666

| s2cid=4390832

}} The ICM also contains some globular clusters,{{cite book

| author=Takamiya, Marianne

| author2=West, Michael

| author3=Côté, Patrick

| author4=Jordán, Andrés

| author5=Peng, Eric

| author6=Ferrarese, Laura

| title=Globular Clusters – Guides to Galaxies

| chapter=IGCs in the Virgo Cluster

| journal=Globular Clusters – Guides to Galaxies, Eso Astrophysics Symposia, Volume

| date=2009

| pages=361–365

| bibcode=2009gcgg.book..361T| doi=10.1007/978-3-540-76961-3_83

| series=Eso Astrophysics Symposia

| isbn=978-3-540-76960-6

}}{{cite journal

| author=Durrell, Patrick R.

| author2=Accetta, K.

| author3=Feldmeier, J. J.

| author4=Mihos, J. C.

| author5=Ciardullo, R.

| author6=Peng, E. W.

| author7=Members of the NGVS team

| title=Searching for Intracluster Globular Clusters in the Virgo Cluster

| date=2010

| journal=Bulletin of the American Astronomical Society

| volume=42 |pages=567

| bibcode=2010AAS...21547814D

}}{{cite journal

| author=Lee, Myung Gyoon

| author2=Park, Hong Soo

| author3=Hwang, Ho Seong

| title=Detection of a Large-Scale Structure of Intracluster Globular Clusters in the Virgo Cluster

| journal=Science

| date=2010

| volume=328

| pages=334–

|arxiv = 1003.2499 |bibcode = 2010Sci...328..334L |doi = 10.1126/science.1186496 | issue=5976

| pmid=20223950

| s2cid=20743125

}} possibly stripped off dwarf galaxies, and even at least one star formation region.{{cite journal

| author=Gerhard, Ortwin

| author2=Arnaboldi, Magda

| author3=Freeman, Kenneth C.

| author4=Okamura, Sadanori

| title=Isolated Star Formation: A Compact H II Region in the Virgo Cluster

| journal=The Astrophysical Journal

| date=2002

| volume=580

| pages=L121–L124

|arxiv = astro-ph/0211341 |bibcode = 2002ApJ...580L.121G |doi = 10.1086/345657 | issue=2

| s2cid=8686119

}}

Galaxies

File:Virgosupercluster atlasoftheuniverse.gif (image diameter 200 Mly ≈ 60 Mpc). The Virgo Cluster is visible in the center right of the image, at about 50 Mly from the Local Group.]]

File:Virgo cluster 052012 overlay.jpg

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:{{cite web

| title = Galaxy On Line Database Milano Network |website = GOLDMine

| url = http://goldmine.mib.infn.it/

| access-date = 2012-08-06}}{{cite web

| title = The Virgo Cluster

| url = http://www.atlasoftheuniverse.com/galgrps/vir.html

| access-date = 2013-04-06}})

: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.

RA ! Dec
class="wikitable sortable" style="text-align: center" \|+ Cluster members ! rowspan="2" \| Designation ! colspan="2" \| Coordinates (Epoch 2000) ! rowspan="2" \| Apparent magnitude (blue) ! rowspan="2" \| Type ! rowspan="2" \| Angular size ! rowspan="2" \| Diameter (kly) ! rowspan="2" \| RV (km/s) ! rowspan="2" \| Subcluster
align=left\|Messier 98	12 13.8	14 54	10.9	SBb	9.8′	150	184	Virgo A or N Cloud
align=left\|NGC 4216	12 15.9	13 09	10.9	SBb	7.9′	120	459	Virgo A, N Cloud, or LVC.
align=left\|Messier 99	12 18.8	14 25	10.4	Sc	5.4′	80	2735	Virgo A or N Cloud
align=left\|NGC 4262	12 19.5	14 53	12.4	S0	1.9′	30	1683	Virgo A
align=left\|NGC 4388	12 25.5	12 39	11.8	SAb	6.2′	85	2845	Virgo A
align=left\|Messier 61	12 21.9	04 28	10.2	SBbc	6.2′	100	1911	S Cloud
align=left\|Messier 100	12 22.9	15 49	10.1	SBbc	7.6′	115	1899	Virgo A
align=left\|Messier 84	12 25.1	12 53	10.1	E₁	6.0′	90	1239	Virgo A Markarian's Chain
align=left\|Messier 85	12 25.4	18 11	10.0	S0	7.1′	105	1056	Virgo A
align=left\|Messier 86	12 26.2	12 57	9.9	E₃	10.2′	155	37	Virgo A or own subgroup. Markarian's Chain
align=left\|NGC 4435	12 27.7	13 05	11.7	S0	3.0′	45	1111	Virgo A
align=left\|NGC 4438	12 27.8	13 01	11.0	Sa	8.7′	130	404	Virgo A
align=left\|NGC 4450	12 28.5	17 05	10.9	Sab	5.1′	80	2273	Virgo A
align=left\|Messier 49	12 29.8	08 00	9.3	E₂	9.8′	150	1204	Virgo B
align=left\|Messier 87	12 30.8	12 23	9.6	E_0–1	9.8′	980	1204	Virgo A
align=left\|Messier 88	12 32.0	14 25	10.3	Sb	6.8′	100	2599	Virgo A
align=left\|NGC 4526	12 32.0	07 42	10.6	S0	7.1′	105	931	Virgo B
align=left\|NGC 4527	12 34.1	02 39	12.4	Sb	4.6′	69	1730	S Cloud
align=left\|NGC 4536	12 34.4	02 11	11.1	SBbc	7.2′	115	2140	S Cloud
align=left\|Messier 91	12 35.4	14 30	11.0	SBb	5.2′	80	803	Virgo A
align=left\|NGC 4546	12 35.5	−03 48	11.3	S0	2.3'	30	1054	S Cloud
align=left\|NGC 4550	12 35.5	12 13	12.5	S0	3.2′	50	704	Virgo A
align=left\|Messier 89	12 35.7	12 33	10.7	E₀	5.0′	75	628	Virgo A
align=left\|NGC 4567	12 36.5	11 15	12.1	Sbc	2.8′	40	2588	Virgo A
align=left\|NGC 4568	12 36.6	11 14	11.7	Sbc	4.4′	65	2578	Virgo A
align=left\|Messier 90	12 36.8	13 10	10.2	SBab	10.5′	160	87	Virgo A
align=left\|NGC 4571	12 36.9	14 13	11.9	Sc	3.7′	55	659	Virgo A
align=left\|Messier 58	12 37.7	11 49	10.6	SBb	5.6′	85	1839	Virgo A
align=left\|Messier 59	12 42.9	11 39	10.8	E₅	5.0′	75	751	Virgo A or Virgo E
align=left\|Messier 60	12 43.7	11 33	9.8	E₂	7.2′	110	1452	Virgo A, Virgo E, or Virgo C
align=left\|NGC 4651	12 43.7	16 24	11.4	Sc	4.0′	60	1113
align=left\|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.{{cite journal | last1 = Binggeli | first1 = Bruno | last2 = Sandage | first2 = Allan | author2-link = Allan Sandage | last3 = Tammann | first3 = Gustav | author3-link = Gustav Andreas Tammann | title = Studies of the Virgo Cluster. II – A Catalog of 2096 Galaxies in the Virgo Cluster Area | journal = Astronomical Journal | volume = 90 | pages = 1681–1759 | publisher = American Astronomical Society | date = 1985 | bibcode = 1985AJ.....90.1681B | doi = 10.1086/113874}}

Notes

References

External links

[http://www.atlasoftheuniverse.com/galgrps/vir.html The Virgo Cluster at An Atlas of the Universe], map (and table) of the 160 largest galaxies
[http://nedwww.ipac.caltech.edu/level5/Binggeli/Bin4.html California Institute of Technology site] on Virgo cluster.
[http://messier.seds.org/more/virgo.html The Virgo Cluster of Galaxies], SEDS Messier pages
[http://www.darkatmospheres.com/astro/gallery/galaxies/enlarge.php?fileBase=galaxies_6 Partial Virgo cluster centered on M87 (Dark Atmospheres)]
{{cite journal |last1=Binggeli |first1=B. |last2=Sandage |first2=A. |last3=Tammann |first3=G. A. |year=1985 |title=Studies of the Virgo cluster. II. A catalog of 2096 galaxies in the Virgo cluster area |journal=The Astronomical Journal |volume=90 |page=1681 |bibcode=1985AJ.....90.1681B |bibcode-access=free |doi=10.1086/113874 |doi-access=free}}

Category:Virgo Supercluster

Category:Virgo (constellation)

Category:Coma Berenices

Virgo Cluster

Characteristics

Intracluster medium

Galaxies

See also

Notes

References

External links