A supercluster is a large group of smaller galaxy clusters or galaxy groups;[1] it is among the largest-known structures of the cosmos. The Milky Way is part of the Local Group galaxy group (which contains more than 54 galaxies), which in turn is part of the Laniakea Supercluster.[2] This supercluster spans over 500 million light-years, while the Local Group spans over 10 million light-years.[1] The large size and low density of superclusters means they, unlike clusters, expand with the Hubble expansion. The number of superclusters in the observable universe is estimated to be 10 million.[3]

A map of the Superclusters and voids nearest to Earth


An Intergalactic Heavyweight
The Abell 901/902 supercluster is located a little over two billion light-years from Earth.[4]

The existence of superclusters indicates that the galaxies in the Universe are not uniformly distributed; most of them are drawn together in groups and clusters, with groups containing up to some dozens of galaxies and clusters up to several thousand galaxies. Those groups and clusters and additional isolated galaxies in turn form even larger structures called superclusters.

Their existence was first postulated by George Abell in his 1958 Abell catalogue of galaxy clusters. He called them "second-order clusters", or clusters of clusters.[5]

Superclusters form massive structures of galaxies, called "filaments", "supercluster complexes", "walls" or "sheets", that may span between several hundred million light-years to 10 billion light-years, covering more than 5% of the observable universe. These are the largest known structures to date. Observations of superclusters can give information about the initial condition of the universe, when these superclusters were created. The directions of the rotational axes of galaxies within superclusters may also give insight and information into the early formation process of galaxies in the history of the Universe.[6]

Interspersed among superclusters are large voids of space where few galaxies exist. Superclusters are frequently subdivided into groups of clusters called galaxy groups and clusters.

List of superclusters

Galaxy supercluster Data Notes
Laniakea Supercluster
  • z = 0.000
  • Length = 153 Mpc (500 million light-years)
The Laniakea Supercluster is the supercluster that contains the Virgo Cluster, Local Group, and by extension on the latter, our galaxy; the Milky Way.[2]
Virgo Supercluster
  • z= 0.000
  • Length = 33 Mpc (110 million light-years)
It contains the Local Group with our galaxy, the Milky Way. It also contains the Virgo Cluster near its center, and is sometimes called the Local Supercluster. It is thought to contain over 47,000 galaxies.

In 2014, the newly announced Laniakea Supercluster subsumed the Virgo Supercluster, which became a component of the new supercluster.[7]

Hydra-Centaurus Supercluster It is composed of two lobes, sometimes also referred to as superclusters, or sometimes the entire supercluster is referred to by these other two names
  • Hydra Supercluster
  • Centaurus Supercluster

In 2014, the newly announced Laniakea Supercluster subsumed the Hydra-Centaurus Supercluster, which became a component of the new supercluster.[7]

Pavo-Indus Supercluster

In 2014, the newly announced Laniakea Supercluster subsumed the Pavo-Indus Supercluster, which became a component of the new supercluster.[7]

Southern Supercluster

Includes Fornax Cluster (S373), Dorado and Eridanus clouds.

Saraswati Supercluster Distance = 4000 Million light years (1.2 Gpc)

Length = 652 Million light-years

The Saraswati Supercluster consists of 43 massive galaxy clusters such as Abell 2361 and has a mass of about 2 x 1016 M and is seen in the Pisces constellation

Nearby superclusters

Galaxy supercluster Data Notes
Perseus-Pisces Supercluster
Coma Supercluster Forms most of the CfA Homunculus, the center of the CfA2 Great Wall galaxy filament
Sculptor Superclusters SCl 9
Hercules Superclusters SCl 160
Leo Supercluster SCl 93
Ophiuchus Supercluster
  •  17h 10m −22°
  • cz=8500–9000 km/s (centre)
  • 18 Mpc x 26 Mpc
Forming the far wall of the Ophiuchus Void, it may be connected in a filament, with the Pavo-Indus-Telescopium Supercluster and the Hercules Supercluster. This supercluster is centered on the cD cluster Ophiuchus Cluster, and has at least two more galaxy clusters, four more galaxy groups, several field galaxies, as members.[8]
Shapley Supercluster
  • z=0.046.(650 Mly away)
The second supercluster found, after the Local Supercluster.

Distant superclusters

Galaxy supercluster Data Notes
Pisces-Cetus Supercluster
Boötes Supercluster SCl 138
Horologium Supercluster
z=0.063 (700 Mly)
Length = 550 Mly
The entire supercluster is referred to as the Horologium-Reticulum Supercluster
Corona Borealis Supercluster
Columba Supercluster
Aquarius Supercluster
Aquarius B Supercluster
Aquarius-Capricornus Supercluster
Aquarius-Cetus Supercluster
Bootes A Supercluster
Caelum Supercluster
z=0.126 (1.4 Gly)
Length = 910 Mly
The largest galaxy supercluster
Draco Supercluster
Draco-Ursa Major Supercluster
Fornax-Eridanus Supercluster
Grus Supercluster
Leo A Supercluster
Leo-Sextans Supercluster
Leo-Virgo Supercluster SCl 107
Microscopium Supercluster SCl 174
Pegasus-Pisces Supercluster SCl 3
Perseus-Pisces Supercluster SCl 40
Pisces-Aries Supercluster
Ursa Majoris Supercluster
Virgo-Coma Supercluster SCl 111

Incredibly distant superclusters

Galaxy supercluster Data Notes
Hyperion proto-supercluster z=2.45 This supercluster at the time of its discovery in 2018 was the earliest and largest proto-supercluster found to date.[10][11]
Lynx Supercluster z=1.27 Discovered in 1999[12] (as ClG J0848+4453, a name now used to describe the western cluster, with ClG J0849+4452 being the eastern one),[13] it contains at least two clusters RXJ 0848.9+4452 (z=1.26) and RXJ 0848.6+4453 (z=1.27) . At the time of discovery, it became the most distant known supercluster.[14] Additionally, seven smaller groups of galaxies are associated with the supercluster.[15]
SCL @ 1338+27 at z=1.1



A rich supercluster with several galaxy clusters was discovered around an unusual concentration of 23 QSOs at z=1.1 in 2001. The size of the complex of clusters may indicate a wall of galaxies exists there, instead of a single supercluster. The size discovered approaches the size of the CfA2 Great Wall filament. At the time of the discovery, it was the largest and most distant supercluster beyond z=0.5 [16][17]
SCL @ 1604+43 at z=0.9 z=0.91 This supercluster at the time of its discovery was the largest supercluster found so deep into space, in 2000. It consisted of two known rich clusters and one newly discovered cluster as a result of the study that discovered it. The then known clusters were Cl 1604+4304 (z=0.897) and Cl 1604+4321 (z=0.924), which then known to have 21 and 42 known galaxies respectively. The then newly discovered cluster was located at  16h 04m 25.7s, +43° 14′ 44.7″[18]
SCL @ 0018+16 at z=0.54 in SA26 z=0.54 This supercluster lies around radio galaxy 54W084C (z=0.544) and is composed of at least three large clusters, CL 0016+16 (z=0.5455), RX J0018.3+1618 (z=0.5506), RX J0018.8+1602 .[19]
MS 0302+17



This supercluster has at least three member clusters, the eastern cluster CL 0303+1706, southern cluster MS 0302+1659 and northern cluster MS 0302+1717.[20]


A diagram of Earth's location in the observable Universe and neighbouring superclusters of galaxies. (Alternative image.)
A diagram of Earth's location in the observable Universe and neighbouring superclusters of galaxies. (Alternative image.)

See also


  1. ^ a b Cain, Fraser (4 May 2009). "Local Group". Universe Today. Retrieved 6 December 2015.
  2. ^ a b Earth's new address: 'Solar System, Milky Way, Laniakea' / Nature
  3. ^ "The Universe within 14 billion Light Years". Atlas of the Universe. Retrieved 6 December 2015.
  4. ^ "An Intergalactic Heavyweight". ESO Picture of the Week. Retrieved 12 February 2013.
  5. ^ Abell, George O. (1958). "The distribution of rich clusters of galaxies. A catalogue of 2,712 rich clusters found on the National Geographic Society Palomar Observatory Sky Survey" (PDF). The Astrophysical Journal Supplement Series. 3: 211–88. Bibcode:1958ApJS....3..211A. doi:10.1086/190036.
  6. ^ Hu, F. X.; et al. (2006). "Orientation of Galaxies in the Local Supercluster: A Review". Astrophysics and Space Science. 302 (1–4): 43–59. arXiv:astro-ph/0508669. Bibcode:2006Ap&SS.302...43H. doi:10.1007/s10509-005-9006-7.
  7. ^ a b c R. Brent Tully; Helene Courtois; Yehuda Hoffman; Daniel Pomarède (2 September 2014). "The Laniakea supercluster of galaxies". Nature (published 4 September 2014). 513 (7516): 71. arXiv:1409.0880. Bibcode:2014Natur.513...71T. doi:10.1038/nature13674. PMID 25186900.
  8. ^ Hasegawa, T.; et al. (2000). "Large-scale structure of galaxies in the Ophiuchus region". Monthly Notices of the Royal Astronomical Society. 316 (2): 326–344. Bibcode:2000MNRAS.316..326H. doi:10.1046/j.1365-8711.2000.03531.x.
  9. ^ Postman, M.; Geller, M. J.; Huchra, J. P. (1988). "The dynamics of the Corona Borealis supercluster". Astronomical Journal. 95: 267–83. Bibcode:1988AJ.....95..267P. doi:10.1086/114635.
  10. ^ Natalia A. Ramos Miranda (October 17, 2018), Scientists in Chile unveil 'A Cosmic Titan' cluster of galaxies, Reuters
  11. ^ Cucciati, O.; Lemaux, B. C.; Zamorani, G.; Le Fevre, O.; Tasca, L. A. M.; Hathi, N. P.; Lee, K-G.; Bardelli, S.; Cassata, P.; Garilli, B.; Le Brun, V.; Maccagni, D.; Pentericci, L.; Thomas, R.; Vanzella, E.; Zucca, E.; Lubin, L. M.; Amorin, R.; Cassara', L. P.; Cimatti, A.; Talia, M.; Vergani, D.; Koekemoer, A.; Pforr, J.; Salvato, M. (2018). "The progeny of a Cosmic Titan: a massive multi-component proto-supercluster in formation at z=2.45 in VUDS". arXiv:1806.06073 [astro-ph.CO].
  12. ^ Rosati, P.; et al. (1999). "An X-Ray-Selected Galaxy Cluster at z = 1.26". The Astronomical Journal. 118 (1): 76–85. arXiv:astro-ph/9903381. Bibcode:1999AJ....118...76R. doi:10.1086/300934.
  13. ^ "Lynx Supercluster". SIMBAD.
  14. ^ Nakata, F.; et al. (2004). Discovery of a large-scale clumpy structure of the Lynx supercluster at z∼1.27. Proceedings of the International Astronomical Union. 2004. Cambridge University Press. pp. 29–33. Bibcode:2004ogci.conf...29N. doi:10.1017/S1743921304000080. ISBN 0-521-84908-X.
  15. ^ Ohta, K.; et al. (2003). "Optical Identification of the ASCA Lynx Deep Survey: An Association of Quasi-Stellar Objects and a Supercluster at z = 1.3?". The Astrophysical Journal. 598: 210–215. arXiv:astro-ph/0308066. Bibcode:2003ApJ...598..210O. doi:10.1086/378690.
  16. ^ Tanaka, I. (2004). "Subaru Observation of a Supercluster of Galaxies and QSOS at Z = 1.1". Studies of Galaxies in the Young Universe with New Generation Telescope, Proceedings of Japan-German Seminar, held in Sendai, Japan, July 24–28, 2001. pp. 61–64. Bibcode:2004sgyu.conf...61T.
  17. ^ Tanaka, I.; Yamada, T.; Turner, E. L.; Suto, Y. (2001). "Superclustering of Faint Galaxies in the Field of a QSO Concentration at z ~ 1.1". The Astrophysical Journal. 547 (2): 521–530. arXiv:astro-ph/0009229. Bibcode:2001ApJ...547..521T. doi:10.1086/318430.
  18. ^ Lubin, L. M.; et al. (2000). "A Definitive Optical Detection of a Supercluster at z ≈ 0.91". The Astrophysical Journal. 531 (1): L5–L8. arXiv:astro-ph/0001166. Bibcode:2000ApJ...531L...5L. doi:10.1086/312518. PMID 10673401.
  19. ^ Connolly, A. J.; et al. (1996). "Superclustering at Redshift z = 0.54". The Astrophysical Journal Letters. 473 (2): L67–L70. arXiv:astro-ph/9610047. Bibcode:1996ApJ...473L..67C. doi:10.1086/310395.
  20. ^ University of Hawaii, "The MS0302+17 Supercluster", Nick Kaiser. Retrieved 15 September 2009.
  • Freedman, Roger; Gellar, Robert M.; Kaufmann, William III (2015). "Galaxies". Universe (10th ed.). New York: W.H. Freedman. ISBN 978-1-319-04238-7.

External links

Media related to Superclusters of galaxies at Wikimedia Commons

3C 66B

3C 66B is an elliptical Fanaroff and Riley class 1 radio galaxy located in the constellation Andromeda. With an estimated redshift of 0.021258, the galaxy is about 300 million light-years away.The orbital motion of 3C 66B showed supposed evidence for a supermassive black hole binary (SMBHB) with a period of 1.05 ± 0.03 years,

but this claim was later proven wrong (at 95% certainty).Messier 87 (M87), about 55 million light years away, is the largest giant elliptical galaxy near the Earth, and also contains an active galactic nucleus. The smooth jet of 3C 66B rivals that of M87.3C 66B is an outlying member of Abell 347 which is part of the Perseus-Pisces Supercluster.

Abell 262

Abell 262 is a galaxy cluster in the Abell catalogue. It is part of the Perseus-Pisces Supercluster, one of the largest known structures in the universe. Although its central galaxy, NGC 708, is a giant cD galaxy, most of its bright galaxies are spirals, which is unusual for a galaxy cluster. With approximately 200 members it is a comparatively small cluster.

Galaxy filament

In physical cosmology, galaxy filaments (subtypes: supercluster complexes, galaxy walls, and galaxy sheets) are the largest known structures in the universe. They are massive, thread-like formations, with a typical length of 50 to 80 megaparsecs h−1 (163 to 261 million light-years) that form the boundaries between large voids in the universe. Filaments consist of gravitationally bound galaxies. Parts wherein many galaxies are very close to one another (in cosmic terms) are called superclusters.

Great Attractor

The Great Attractor is an apparent gravitational anomaly in intergalactic space at the center of the local Laniakea Supercluster, in which the Milky Way is located, in the so-called Zone of Avoidance that is very difficult to observe in visible wavelengths due to the obscuring effects of our own galactic plane. This anomaly suggests a localized concentration of mass thousands of times more massive than the Milky Way.

The anomaly is observable by its effect on the motion of galaxies and their associated clusters over a region hundreds of millions of light-years across. These galaxies are all redshifted, in accordance with the Hubble Flow, indicating that they are receding relative to us and to each other, but the variations in their redshift are sufficient to reveal the existence of the anomaly. The variations in their redshifts are known as peculiar velocities, and cover a range from about +700 km/s to −700 km/s, depending on the angular deviation from the direction to the Great Attractor.

The Great Attractor is moving towards the Shapley Supercluster. Recent astronomical studies by a team of South African astrophysicists revealed a supercluster of galaxies, termed the Vela Supercluster, in the Great Attractor's theorized location.

Hyperion proto-supercluster

The Hyperion proto-supercluster is the largest and earliest known proto-supercluster, 5,000 times the mass of the Milky Way and seen at 20% of the current age of the universe. It was discovered in 2018 by analysing the redshifts of 10,000 objects observed with the Very Large Telescope in Chile.

Laniakea Supercluster

The Laniakea Supercluster (Laniakea, Hawaiian for open skies or immense heaven; also called Local Supercluster or Local SCl or sometimes Lenakaeia) is the galaxy supercluster that is home to the Milky Way and approximately 100,000 other nearby galaxies. It was defined in September 2014, when a group of astronomers including R. Brent Tully of the University of Hawaii, Hélène Courtois of the University of Lyon, Yehuda Hoffman of the Hebrew University of Jerusalem, and Daniel Pomarède of CEA Université Paris-Saclay published a new way of defining superclusters according to the relative velocities of galaxies. The new definition of the local supercluster subsumes the prior defined local supercluster, the Virgo Supercluster, as an appendage.Follow-up studies suggest that Laniakea is not gravitationally bound; it will disperse rather than continue to maintain itself as an overdensity relative to surrounding areas.

List of voids

This is a list of voids. Voids are particularly galaxy-poor volumes of space between filaments, making up the large-scale structure of the universe. Some voids are known as supervoids.

Local Group

The Local Group is the galaxy group that includes the Milky Way. The Local Group comprises more than 54 galaxies, most of them dwarf galaxies. Its gravitational center is located somewhere between the Milky Way and the Andromeda Galaxy. The Local Group has a diameter of 10 Mly (3.1 Mpc) (about 1023 meters) and has a binary (dumbbell)

distribution. The group itself is a part of the larger Virgo Supercluster, which may be a part of the Laniakea Supercluster.

The three largest members of the group (in descending order) are the Andromeda Galaxy, the Milky Way and the significantly smaller Triangulum Galaxy. The larger two of these spiral galaxies each have their own system of satellite galaxies.

The Andromeda Galaxy's satellite system consists of Messier 32 (M32), Messier 110 (M110), NGC 147, NGC 185, Andromeda I (And I), And II, And III, And V, And VI (also known as Pegasus Dwarf Spheroidal Galaxy, or Pegasus DSph), And VII (also known as Cassiopeia Dwarf Galaxy), And VIII, And IX, And X, And XI, And XIX, And XXI and And XXII, plus several additional ultra-faint dwarf spheroidal galaxies.

The Milky Way's satellite galaxies system comprises Sagittarius Dwarf Galaxy, Large Magellanic Cloud, Small Magellanic Cloud, Canis Major Dwarf Galaxy (disputed, considered by some not a galaxy), Ursa Minor Dwarf Galaxy, Draco Dwarf Galaxy, Carina Dwarf Galaxy, Sextans Dwarf Galaxy, Sculptor Dwarf Galaxy, Fornax Dwarf Galaxy, Leo I (a dwarf galaxy), Leo II (a dwarf galaxy), and Ursa Major I Dwarf Galaxy and Ursa Major II Dwarf Galaxy, plus several additional ultra-faint dwarf spheroidal galaxies.

The Triangulum Galaxy may or may not be a companion to the Andromeda Galaxy. Pisces Dwarf Galaxy is equidistant from the Andromeda Galaxy and the Triangulum Galaxy, so it may be a satellite of either.

The membership of NGC 3109, with its companions Sextans A and the Antlia Dwarf Galaxy, is uncertain due to extreme distances from the center of the Local Group.

The other members of the group are likely gravitationally secluded from these large subgroups: IC 10, IC 1613, Phoenix Dwarf Galaxy, Leo A, Tucana Dwarf Galaxy, Cetus Dwarf Galaxy, Pegasus Dwarf Irregular Galaxy, Wolf–Lundmark–Melotte, Aquarius Dwarf Galaxy, and Sagittarius Dwarf Irregular Galaxy.

Local Sheet

The Local Sheet in astronomy is a nearby extragalactic region of space where the Milky Way, the members of the Local Group and other galaxies share a similar peculiar velocity. This region lies within a radius of about 7 Mpc (23 Mly), 0.46 Mpc (1.5 Mly) thick, and galaxies beyond that distance show markedly different velocities. The Local Group has only a relatively small peculiar velocity of 66 km⋅s−1 with respect to the Local Sheet. Typical velocity dispersion of galaxies is only 40 km⋅s−1 in the radial direction. Nearly all nearby bright galaxies belong to the Local Sheet. The Local Sheet is part of the Local Volume and is in the Virgo Supercluster (Local Supercluster). The Local Sheet forms a wall of galaxies delineating one boundary of the Local Void.A significant component of the mean velocity of the galaxies in the Local Sheet appears as the result of the gravitational attraction of the Virgo Cluster of galaxies, resulting in a peculiar motion ~185 km⋅s−1 toward the cluster. A second component is directed away from the center of the Local Void; an expanding region of space spanning an estimated 45 Mpc (150 Mly) that is only sparsely populated with galaxies. This component has a velocity of 259 km⋅s−1. The Local Sheet is inclined 8° from the Local Supercluster (Virgo Supercluster).The so-called Council of Giants is a ring of twelve large galaxies surrounding the Local Group in the Local Sheet, with a radius of 3.75 Mpc (12.2 Mly). Ten of these are spirals, while the remaining two are ellipticals. The two ellipticals (Maffei 1 and Centaurus A) lie on opposite sides of the Local Group, and their formation may have prompted the development of the Local Group. The Local Sheet's own development outlines a concentration of dark matter in a filament.

* The mass is given as the logarithm of the mass in solar masses.

NGC 3626

NGC 3626, also Caldwell 40, is a medium-tightness spiral galaxy and Caldwell object in the constellation Leo. It was discovered by William Herschel, on 14 March 1784. It shines at magnitude +10.6/+10.9. Its celestial coordinates are RA 11h 20.1m, dec +18° 21′. It is located near the naked-eye class A4 star Zosma, as well as galaxies NGC 3608, NGC 3607, NGC 3659, NGC 3686, NGC 3684, NGC 3691, NGC 3681, and NGC 3655. Its dimensions are 2′.7 × 1′.9. The galaxy belongs to the NGC 3607 group some 70 million light-years distant, itself one of the many Leo II groups.

NGC 4084

NGC 4084 is an elliptical galaxy located 315 million light-years away in the constellation Coma Berenices. NGC 4084 was discovered by astronomer Heinrich d'Arrest on April 26, 1865. NGC 4084 is an isolated member of the Coma Supercluster and is classified as a LINER galaxy.

NGC 498

NGC 498 is a lenticular galaxy located about 260 million light-years away from Earth, in the constellation Pisces. NGC 498 was discovered by astronomer R. J. Mitchell on October 23, 1856.NGC 498 is a member of the NGC 507 Group which is part of the Perseus-Pisces Supercluster.

NGC 6744

NGC 6744 is an intermediate spiral galaxy about 30 million light-years away in the constellation Pavo. It is considered as a Milky Way mimic in our immediate vicinity, displaying flocculent (fluffy) arms and an elongated core. It also has at least one distorted companion galaxy (NGC 6744A) superficially similar to one of the Magellanic Clouds. It was discovered from Parramatta in Australia by Scottish astronomer James Dunlop on 30 June 1826.NGC 6744 lies within the Virgo Supercluster.

NGC 6946

NGC 6946 is a face-on intermediate spiral galaxy with a small bright nucleus, whose location in the sky straddles the boundary between the northern constellations of Cepheus and Cygnus. Its distance from Earth is about 22.5 million light-years or 6.8 megaparsecs, similar to the distance of M101 (NGC 5457) in the constellation Ursa Major. Both were once considered to be part of the Local Group. but are now known to be among the dozen bright spiral galaxies near the Milky Way but beyond the confines of the Local Group. NGC 6946 lies within the Virgo Supercluster.Discovered by William Herschel on 9 September 1798, this well-studied galaxy has a diameter of approximately 40,000 light-years

, about one-third of the Milky Way's size, and it contains roughly half the number of stars as the Milky Way. The galaxy is heavily obscured by interstellar matter as it lies quite close to the galactic plane of the Milky Way. Due to its prodigious star formation it has been classified as an active starburst galaxy.Various unusual celestial objects have been observed within NGC 6964. This includes the so-called 'Red Ellipse' along one of the northern arms that looks like a super-bubble or very large supernova remnant, and which may have been formed by an open cluster containing massive stars. There are also two regions of unusual dark lanes of nebulosity, while within the spiral arms several regions appear devoid of stars and gaseous hydrogen, some spanning up to two kiloparsecs across. A third peculiar object, discovered in 1967, is now known as "Hodge's Complex". This was once thought to be a young supergiant cluster, but in 2017 it was conjectured to be an interacting dwarf galaxy superimposed on NGC 6964.

Pisces–Cetus Supercluster Complex

The Pisces–Cetus Supercluster Complex is a galaxy filament. It includes the Virgo Supercluster which in turn contains the Local Group, the galaxy cluster that includes the Milky Way.

This filament is adjacent to the Perseus–Pegasus Filament.

However, a 2014 study indicates that the Virgo Supercluster is only a lobe of a greater supercluster, Laniakea.

Shapley Supercluster

The Shapley Supercluster or Shapley Concentration (SCl 124) is the largest concentration of galaxies in our nearby universe that forms a gravitationally interacting unit, thereby pulling itself together instead of expanding with the universe. It appears as a striking overdensity in the distribution of galaxies in the constellation of Centaurus. It is 650 million light years away (z=0.046).

Supercluster (band)

Supercluster is a recording project that formed during 2007 in Athens, Georgia. It includes musicians from the Athens, Georgia bands New Sound Of Numbers, Bob Hay & the Jolly Beggars, Casper & the Cookies, Of Montreal, Circulatory System and Pylon, along with Elephant 6 recording artist John Fernandes. Members presently include Hannah M. Jones, Bob Hay, Bill David, Kay Stanton, Bryan Poole, Vanessa Briscoe Hay, Jason NeSmith and John Fernandes. Alumni include Randy Bewley (deceased), Heather McIntosh, Will Cullen Hart and Peter Erchick. Supercluster play what they term "Appalachian Wave." For a brief period they were known as FFFM.

On February 23, 2009, Randy Bewley was driving on Barber Street in Athens when he suffered a heart attack. According to the band Pylon's statement, his van drifted off the road and overturned. He was admitted to Athens Regional Medical Center and lapsed into a coma; he died two days later on February 25 when he was removed from life support.Bradford Cox from the group Deerhunter came into Bel*Air studio and helped Supercluster finish the last couple of tracks that needed to be recorded for Waves which was released October 6, 2009 on Cloud Recordings Live performance guitar duties are now handled by Jason NeSmith and Bryan Poole.

Supercluster have continued to record singles since this release and perform locally in Athens, Georgia. They plan on releasing a full length project at some point composed of these singles.

Virgo Cluster

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 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 1.2×1015 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. Although some of the cluster's most prominent members can be seen with smaller instruments, 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; however its most famous member is the elliptical galaxy Messier 87, which is located in the center of the cluster.

Virgo Supercluster

The Virgo Supercluster (Virgo SC) or the Local Supercluster (LSC or LS) is a mass concentration of galaxies containing the Virgo Cluster and Local Group, which in turn contains the Milky Way and Andromeda galaxies. At least 100 galaxy groups and clusters are located within its diameter of 33 megaparsecs (110 million light-years). The Virgo SC is one of about 10 million superclusters in the observable universe and is in the Pisces–Cetus Supercluster Complex, a galaxy filament.

A 2014 study indicates that the Virgo Supercluster is only a lobe of an even greater supercluster, Laniakea, a larger, competing referent of Local Supercluster centered on the Great Attractor.

Active nuclei
Energetic galaxies
Low activity
See also

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