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List of galaxy groups and clusters

Article Discussion

Template:Short description {{#invoke:Hatnote|hatnote}}{{#ifeq:||}}

File:Heic1401a-Abell2744-20140107.jpg
Abell 2744 galaxy cluster - Hubble Frontier Fields view (7 January 2014)<ref name="NASA-20140107">Template:Cite news</ref>

This article lists some galaxy groups and galaxy clusters.

Defining the limits of galaxy clusters is imprecise as many clusters are still forming. In particular, clusters close to the Milky Way tend to be classified as galaxy clusters even when they are much smaller than more distant clusters.

Clusters exhibiting strong evidence of dark matterEdit

Some clusters exhibiting strong evidence of dark matter.

Galaxy cluster Notes
Bullet Cluster citation CitationClass=web

}}</ref>

Abell 520 citation CitationClass=web

}}</ref>

Abell 2142 A collision between two massive, X-ray luminous galaxy clusters.
Cl 0024+17
(ClG 0024+16, ZwCl 0024+1652) 		citation CitationClass=web

}}</ref><ref>SIMBAD, "ClG 0024+17"</ref>

Named groups and clustersEdit

This is a list of galaxy groups and clusters that are well known by something other than an entry in a catalog or list, or a set of coordinates, or a systematic designation.

ClustersEdit

Galaxy cluster Origin of name Notes
Bullet Cluster The cluster is named for the merger of two clusters colliding like a bullet. Also has a systematic designation of 1E 0657-56
El Gordo Named for its size, El Gordo ("the fat one") is the biggest cluster found in the distant universe (at its distance and beyond), at the time of discovery in 2011, with a mass of 3 quadrillion suns. The second most massive galaxy cluster next to El Gordo is RCS2 J2327, a galaxy cluster with the mass of 2 quadrillion suns. Also has a systematic designation of ACT-CL J0102-4915.<ref>{{#invoke:citation/CS1|citation CitationClass=web

}}</ref><ref>Template:Cite journal</ref><ref>NASA, "El Gordo Galaxy Cluster", 10 January 2012 (accessed 7 July 2012)</ref>

Musket Ball Cluster Named in comparison to the Bullet Cluster, as this one is older and slower galaxy cluster merger than the Bullet Cluster. Also has a systematic designation of DLSCL J0916.2+2951.<ref>{{#invoke:citation/CS1|citation CitationClass=web

}}</ref>

Pandora's Cluster Named because the cluster resulted from a collision of clusters, which resulted in many different and strange phenomena. Also has a catalogue entry of Abell 2744.<ref>ESO, "A Galactic Crash Investigation", 22 June 2011 (accessed 7 July 2012)</ref>

GroupsEdit

Galaxy group Origin of name Notes
Local Group The galaxy group that includes the Milky Way.
Bullet Group Named in comparison with the Bullet Cluster, being of similar formation, except smaller. Also has a systematic catalogue name SL2S J08544-0121. As of 2014, it was the lowest mass object that showed separation between the concentrations of dark matter and baryonic matter in the object.<ref>{{#invoke:citation/CS1|citation CitationClass=web

}}</ref><ref>Template:Cite journal</ref>

Burbidge Chain
Copeland Septet Discovered by British astronomer Ralph Copeland in 1874.
Deer Lick Group Coined by Tom Lorenzin (author of "1000+ The Amateur Astronomers' Field Guide to Deep Sky Observing") to honor Deer Lick Gap in the mountains of North Carolina, from which he had especially fine views of the galaxy group. Also referred to as the NGC 7331 Group, after the brightest member of the group.<ref>Saratoga Skies, "NGC 7331 (Deer Lick Group and Stephan's Quintet)", Jim Solomon (accessed 7 May 2009)</ref>
Leo Triplet Named for the fact it contains only three galaxies. This small group of galaxies lies in the constellation Leo.
Markarian's Chain This stretch of galaxies forms part of the Virgo Cluster.
Robert's Quartet It was named by Halton Arp and Barry F. Madore, who compiled A Catalogue of Southern Peculiar Galaxies and Associations in 1987. This compact group of galaxies lies 160 million light-years away in the Phoenix constellation.
Seyfert's Sextet Named after its discoverer, Carl Seyfert. At the time it appeared to contain six external nebulae. It is also called the NGC 6027 Sextet, after its brightest member. There are actually only five galaxies in the sextet, and only four galaxies in the compact group. One of the galaxies is an ungravitationally bound background object. The other "galaxy" is instead an extension of the interacting system — a tidal stream caused by the merger. The group is, therefore, more properly called HCG 79; the name refers to the visual collection and not the group. HCG 79 lies 190 million light-years away in the Serpens Caput constellation.
Stephan's Quintet (Stephan's Quartet) Named after its discoverer, Édouard Stephan. There are actually only four galaxies in the compact group, the other galaxy is a foreground galaxy. The group is therefore more properly called HCG 92, because the name refers to a visual collection and not a group. Thus, the real group is also called Stephan's Quartet.
Wild's Triplet Named after the British-born and Australia-based astronomer Paul Wild (1923–2008), who studied the trio in the early 1950s.<ref>{{#invoke:citation/CS1|citation CitationClass=web

}}</ref>

Zwicky's Triplet

The major nearby groups and clusters are generally named after the constellation they lie in. Many groups are named after the leading galaxy in the group. This represents an ad hoc systematic naming system.

Groups and clusters visible to the unaided eyeEdit

The Local Group contains the largest number of visible galaxies with the naked eye. However, its galaxies are not visually grouped together in the sky, except for the two Magellanic Clouds. The IC342/Maffei Group, the nearest galaxy group, would be visible by the naked eye if it were not obscured by the stars and dust clouds in the Milky Way's spiral arms.

Galaxy group Visible galaxies Notes
Local Group 5 Apart from the Milky Way, only 4 galaxies are visible to the naked eye.<ref name=uitti />
Centaurus A/M83 Group 2 The Centaurus A galaxy has been spotted with the naked eye by Stephen James O'Meara <ref>{{#invoke:citation/CS1|citation CitationClass=web

}}</ref><ref>Template:Cite book</ref> and M83 has also reportedly been seen with the naked eye.<ref> Template:Cite book</ref>

M81 Group 1 Only Bode's Galaxy (M81, NGC 3031) is visible to the naked eye.<ref name=uitti>{{#invoke:citation/CS1|citation CitationClass=web

}}</ref><ref>SEDS, Messier 81</ref>

  • No galaxy cluster is visible to the unaided eye.<ref name=Arches-AIP-GalaxyClusters>{{#invoke:citation/CS1|citation

|CitationClass=web }}</ref>

FirstsEdit

First discovered Name Date Notes
Galaxy cluster Virgo Cluster 1784 Discovered by Charles Messier.<ref name=MA200>Template:Cite book</ref>
Galaxy group
Compact group The four brightest members of Stephan's Quintet 1877 Discovered by Edouard Stephan.
Proto-cluster
Double galaxy Magellanic Clouds antiquity

ExtremesEdit

{{safesubst:#invoke:Unsubst||date=__DATE__|$B= Template:Ambox }}

Title Name Data Notes time
Most distant galaxy cluster CL J1001+0220 redshift z=2.506 Announced August 2016. <ref name=AJ-828-1>Template:Cite journal</ref>
Nearest galaxy cluster Virgo Cluster The Virgo Cluster is at the core of the Virgo Supercluster. The Local Group is a member of the supercluster, but not the cluster.
Most distant galaxy group
Nearest galaxy group Local Group 0 distance This is the galaxy group that our galaxy belongs to.
Nearest neighbouring galaxy group IC 342/Maffei Group
Most distant proto-cluster A2744z7p9OD z=7.88 <ref name=arXiv-2211.09097>Template:Cite journal</ref>
Nearest proto-cluster
Most distant massive proto-cluster z66OD z=6.585 At time of discovery in 2019, the object had 12 members, including Himiko. <ref name=ScienceDaily-2019-09-27>Template:Cite news</ref><ref name=arXiv-1902.09555>Template:Cite journal</ref><ref name=UPI-2019-09-27>Template:Cite news</ref>
Least massive galaxy group
Most massive galaxy cluster RX J1347.5-1145 mass= 2.0 ± 0.4 × 1015 MSun
  • distance: z= 0.451
  • LX-ray = 6.0 ± 0.1 × 1045 erg/s Template:Small
  • temperature: kT = 10.0 ± 0.3 keV

<ref name=AN-2008-08-27>{{#invoke:citation/CS1|citation

CitationClass=web

}}</ref><ref>Template:Cite journal</ref>

Closest groupsEdit

Template:See also

Galaxy groups closer than the Virgo Cluster
Galaxy group Distance Redshift (z) Recession velocity (km/s) Notes
Local Group - - - Our Galaxy, the Milky Way, belongs to the Local Group.
LGG 104 (IC 342/Maffei Group, IC 342 / Maffei 1 Group, IC 342 Maffei 1-2 Group) 0.000868 {{#expr: 0.000868 * 299792.458 round0}} The IC 342/Maffei Group contains two subgroups, the IC 342 subgroup (IC 342 Group) and the Maffei 1 subgroup (Maffei subgroup, Maffei 1 Group, Maffei Group).
M81 Group (NGC 3031 Group) Template:Convert 0.001115 {{#expr: 0.001115 * 299792.458 round0}} <ref name=Hayden-ClG-SC>Hayden Planetarium, Galaxy Clusters and Superclusters Template:Webarchive</ref>
Centaurus A/M83 Group (Centaurus A Group, M83 Group) Template:Convert 0.000999 {{#expr: 0.000999 * 299792.458 round0}} The Centaurus A/M83 Group contains two subgroups, the Centaurus A subgroup (Centaurus A Group, NGC 5128 Group, LGG 344) and the M83 subgroup (M83 Group, NGC 5236 Group, LGG 355).
Sculptor Group (South Polar Group) Template:Convert
Canes Venatici Group (Canes Venatici I Group, Canes I Group, M94 Group, NGC 4736 Group, LGG 291) Template:Convert 0.001612 {{#expr: 0.001612 * 299792.458 round0}}
NGC 1023 Group (LGG 70) Template:Convert 0.002926 {{#expr: 0.002926 * 299792.458 round0}}
M101 Group (NGC 5457 Group, LGG 371) Template:Convert 0.001288 {{#expr: 0.001288 * 299792.458 round0}}
NGC 2997 Group (LGG 180) Template:Convert 0.002615 {{#expr: 0.002615 * 299792.458 round0}}
Canes Venatici II Group (Canes II Group) Template:Convert
M51 Group (NGC 5194 Group, LGG 347) Template:Convert 0.001850 {{#expr: 0.00185 * 299792.458 round0}} <ref name=Hayden-ClG-SC />
Leo Triplet (M66 Group, NGC 3627 Group, LGG 231) Template:Convert 0.002207 {{#expr: 0.002207 * 299792.458 round0}}
Leo Group (Leo I Group, M96 Group, NGC 3379 Group, LGG 217) Template:Convert 0.002267 {{#expr: 0.002267 * 299792.458 round0}}
Draco Group Template:Convert
LGG 396 (NGC 5866 Group, NGC 5907 Group) 0.003020 {{#expr: 0.00302 * 299792.458 round0}}
Ursa Major Group (Ursa Major I Group, M109 Group, NGC 3992 Group, NGC 3726 Group, LGG 258) Template:Convert 0.003388 {{#expr: 0.003388 * 299792.458 round0}} <ref name=Hayden-ClG-SC />
  • Mly represents millions of light-years, a measure of distance.
  • Mpc represents millions of parsecs, a measure of distance (1 Mpc = 3.26 Mly).
  • z represents redshift, a measure of recessional velocity and inferred distance due to cosmological expansion.
    In this very nearby context, however, the observed redshift and recessional velocity are due to the Doppler shifting of the light.
  • Distances are measured from Earth, with Earth being at zero.

Closest clustersEdit

Template:See also

Closest clusters
Galaxy cluster Distance Redshift (z) Recession velocity (km/s) Notes
Virgo Cluster Template:Convert 0.0038 {{#expr: 0.0038 * 299792.458 round0}} The Virgo Cluster is at the core of the Virgo Supercluster. The Local Group is a member of the supercluster, but not the cluster.<ref name=Hayden-2MASS>Hayden Planetarium, The 2MASS Galaxies Template:Webarchive</ref>
Fornax Cluster (Abell S 373, AM 0336-353, MCL 52) Template:Convert 0.0046 {{#expr: 0.0046 * 299792.458 round0}} <ref name=Hayden-2MASS />
Antlia Cluster (Abell S 636) Template:Convert 0.0087 {{#expr: 0.0087 * 299792.458 round0}} Also called the Antlia Group.
Centaurus Cluster (Abell 3526, Cl 1247-4102) 52.4 Mpc 0.0110 {{#expr: 0.0110 * 299792.458 round0}} <ref name=Hayden-2MASS />
Hydra Cluster (Hydra I Cluster, Abell 1060, Cl 1034-2716) 58.3 Mpc 0.0114 {{#expr: 0.0114 * 299792.458 round0}} <ref name=Hayden-2MASS />
  • Mly represents millions of light-years, a measure of distance.
  • Mpc represents millions of parsecs, a measure of distance.
  • z represents redshift, a measure of recessional velocity and inferred distance due to cosmological expansion.
  • Distances are measured from Earth, with Earth being at zero.

Farthest clustersEdit

Farthest clusters
Galaxy cluster Distance Notes
No entries yet
  • Mly represents millions of light-years, a measure of distance.
  • Mpc represents millions of parsecs, a measure of distance.
  • z represents redshift, a measure of recessional velocity and inferred distance due to cosmological expansion.
  • Distances are measured from Earth, with Earth being at zero.
Most remote cluster titleholder
Galaxy cluster Date Redshift (z) Recession Velocity
(km/s) 		Notes
CL J1001+0220 2016 −  2.506 <ref name=AJ-828-1/>
CL J1449+0856
(ClG J1449+0856) 		2011–2016 2.07 <ref name=AnA-526a-133g>Template:Cite journal</ref><ref name=ABC-2011-03-10>ABC News (Australia), "Astronomers find old heads in a young crowd", Stuart Gary, 10 March 2011</ref><ref name="SIMBAD-ClG_J1449+0856">SIMBAD, "ClG J1449+0856"</ref>
JKCS 041 2009–2011 1.9
XMMXCS 2215-1738 (XMMXCS 2215.9-1738) 2006–2009 1.45 XMM-XCS 2215-1738 was also the most massive early cluster so far discovered.<ref>XCS, {{#invoke:citation/CS1|citation CitationClass=web

}}Template:Dead link, April 2006</ref><ref>University of Portsmith - Institute of Cosmology and Gravitation; ICG in team that detects the most distant galaxy cluster Template:Webarchive, 15 June 2006</ref>

ISCS J143809+341419 2005–2006 1.41 <ref>NASA - Spitzer Space Telescope, Great Galactic Buddies Template:Webarchive</ref><ref>Template:Cite journal</ref>
XMMU J2235.3-2557 2005 1.393 <ref name=NS-2005-03-02>New Scientist, Most distant galaxy cluster yet is revealed, 08:00 02 March 2005</ref><ref>The Most Distant X-ray Massive Galaxy Cluster XMMU J2235.3-2557 z=1.4 Template:Webarchive</ref><ref name=ClArchae /><ref>ESO Press Release 04/05; Surprise Discovery of Highly Developed Structure in the Young Universe Template:Webarchive; 2 March 2005</ref>
RDCS 0848+4453 ( RDCS0848.6+4453, RX J0848+4453, ClG 0848+4453 ) 1997– 1.276 ClG 0848+4453 forms a double-cluster supercluster with RDCS J0849+4452<ref name="z=1.24" /><ref name=XGlGz1.11 /><ref>Template:Cite journal</ref><ref>Template:Cite journal</ref><ref name="z=1.26" />
galaxy cluster around 3C 324 (3C 234 Cluster) 1984– 1.206 At the time, the BCG, 3C324 was the most distant non-quasar galaxy.<ref>Template:Cite journal</ref>
Cl 1409+524 1960–1975 0.461 The measurement of 3C295's redshift in 1960 also defined its cluster's position. 3C 295 was also the most distant galaxy of the time.<ref name=200in>Template:Cite journal</ref><ref>Palomar Skies, Pushing the limit, Saturday, March 29, 2008</ref>
Abell 732 (fainter Hydra Cluster Cl 0855+0321) 1951–1960 0.2 61 000  Attempts at measuring the redshift of the brightest cluster galaxy of this Hydra Cluster had been attempted for years before it had been successfully achieved. The BCG was also the most distant galaxy of the time.<ref name=200in /><ref>Template:Cite journal</ref><ref name=Sandage01Sept>Annu. Rev. Astron. Astrophys. 1988. 26: 561-630; OBSERVATIONAL TESTS OF WORLD MODELS - 6. THE m(z) HUBBLE DIAGRAM; Allan Sandage</ref><ref>Template:Cite journal</ref>
Abell 1930 (Bootes Cluster) 1936–1951 0.13 39 000  The BCG of this cluster was also the most distant galaxy of the time.<ref name=Sandage01Sept /><ref name=z1936>Template:Cite journal</ref>
Gemini Cluster (Abell 568) 1932 − 1936 0.075 23 000  The BCG of this cluster was the most distant galaxy at the time.<ref name=z1936 /><ref name=RASC-26>Template:Cite journal</ref>
WH Christie's Leo Cluster 1931–1932 19 700  The BCG of this cluster was the most distant galaxy known at the time.<ref name=Sandage01Sept /><ref name=RASC-26 /><ref>Template:Cite journal</ref><ref>Template:Cite journal</ref><ref name=ASPL-1>Template:Cite journal</ref>
Baede's Ursa Major Cluster 1930–1931 11 700  The BCG of this cluster was the highest redshift galaxy of the time.<ref name=ASPL-1 /><ref name=Rayton>Template:Cite journal</ref>
Coma Cluster 1929–1930 0.026 7 800  This cluster's distance was determined by one of the NGC objects lying in it, NGC4860.<ref name=Rayton /><ref>Template:Cite journal</ref>
Pegasus Group (LGG 473, NGC 7619 Group) 1929 0.012 3 779  The BCG for this group was used to measure its redshift. Shortly after this was publicized, it was accepted that redshifts were an acceptable measure of inferred distance.<ref name=Humason-1929-03-15>From the Proceedings of the National Academy of Sciences; Volume 15 : March 15, 1929 : Number 3; THE LARGE RADIAL VELOCITY OF N. G. C. 7619; January 17, 1929</ref>
Cetus Group (Holmberg 45, LGG 27) 1921–1929 0.006 1 800  NGC 584 (Dreyer 584) was measured for the redshift to this galaxy group.<ref name=Humason-1929-03-15 /><ref>Template:Cite journal</ref><ref>New York Times, DREYER NEBULA NO. 584 INCONCEIVABLY DISTANT; Dr. Slipher Says the Celestial Speed Champion Is 'Many Millions of Light Years' Away.; January 19, 1921, Wednesday</ref><ref name=NYT-1921-01-18>New York Times, NEBULA DREYER BREAKS ALL SKY SPEED RECORDS; Portion of the Constellation of Cetus Is Rushing Along at Rate of 1,240 Miles a Second.; January 18, 1921, Tuesday</ref>
Virgo Cluster 1784–1921 59 Mly (18 Mpc)
z=0.003 		1 200  This was the first noted cluster of "nebulae" that would become galaxies. The first redshifts to galaxies in the cluster were measured in the 1910s. Galaxies were not identified as such until the 1920s. The distance to the Virgo Cluster would have to wait until the 1930s.<ref name=MA200 />
  • Mly represents millions of light-years, a measure of distance.
  • Mpc represents millions of parsecs, a measure of distance.
  • z represents redshift, a measure of recessional velocity and inferred distance due to cosmological expansion.
  • Distances are measured from Earth, with Earth being at zero.
  • In 2003 RDCS 1252-29 (RDCS1252.9–2927) at z=1.237, was found to be the most distant rich cluster, which lasted until 2005.<ref name=NS-2005-03-02 /><ref name=ClArchae>MAX-PLANCK-INSTITUT FÜR EXTRATERRESTRISCHE PHYSIK, GARCHING, GERMANY; DEPARTMENT OF ASTRONOMY, UNIVERSITY OF MICHIGAN, ANN ARBOR, USA; ESO, ASTROPHYSIKALISCHES INSTITUT, POTSDAM, GERMANY; {{#invoke:citation/CS1|citation

|CitationClass=web }} ; HANS BÖHRINGER, CHRISTOPHER MULIS, PIERO ROSATI, GEORG LAMER, RENE FASSBENDER, AXEL SCHWOPE, PETER SCHUECKER</ref><ref name="z=1.24">Template:Cite journal</ref>

Farthest protoclustersEdit

5 Farthest protoclusters
Galaxy protocluster Distance Notes
No entries yet
  • Mly represents millions of light-years, a measure of distance.
  • Mpc represents millions of parsecs, a measure of distance.
  • z represents redshift, a measure of recessional velocity and inferred distance due to cosmological expansion.
  • Distances are measured from Earth, with Earth being at zero.
Most remote protocluster titleholder
Galaxy protocluster Date Redshift (z) Notes
BoRG-58 2012 ~ 8 <ref name=STorg-2012-01-10>SpaceTelescope.org (ESA), "Hubble Spies Building Blocks of Most Distant Galaxy Cluster", 10 January 2012 (accessed March 2012)</ref>
COSMOS-AzTEC3 2011– 5.3 Located in Sextans, the cluster appears to contain 11 young small galaxies.<ref name=SkyAndTelescope-2011-01-13>{{#invoke:citation/CS1|citation CitationClass=web

}}</ref><ref name=BBC-2011-01-13>BBC News, "Galaxy clusters' ancient light shows young cosmic city", Jason Palmer, 13 January 2011</ref>

Protocluster around radio-galaxy TN J1338-1942 2002– 4.11 It was described as the most distant cluster.<ref>Associated Press, Oldest, most distant galaxy clusters found, 4:37 p.m. ET, Mon., Jan. 5, 2004</ref><ref>Template:Cite journal</ref><ref>Science, Oldest Galaxy Cluster Found, 12 April 2002</ref><ref name=ESOpr0702>ESO Press Release 07/02; Most Distant Group of Galaxies Known in the Universe Template:Webarchive; 9 April 2002</ref>
Protocluster around 3C 368 1982– 1.13 <ref>Publications of the Astronomical Society of the Pacific, vol. 94, June–July 1982, p. 397-403. Redshifts and spectroscopy of very distant radio galaxies with strong emission lines 1982PASP...94..397S</ref>
  • z represents redshift, a measure of recessional velocity and inferred distance due to cosmological expansion.
  • Distances are measured from Earth, with Earth being at zero.

False clustersEdit

Sometimes clusters are put forward that are not genuine clusters or superclusters. Through the researching of member positions, distances, peculiar velocities, and binding mass, former clusters are sometimes found to be the product of a chance line-of-sight superposition.

Former cluster Notes
Cancer Cluster The Cancer Cluster was found to be a random assortment of galaxy groups, and not a true cluster.<ref name=MA200 />
Coma-Virgo Cloud The early identification of the Coma-Virgo Cloud of Nebulae was actually a mistaken identification due to the superposition of the Virgo Supercluster and Coma Supercluster, and not a Coma-Virgo Supercluster

See alsoEdit

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Lists of groups and clustersEdit

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ReferencesEdit

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External linksEdit

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