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Supercluster
Supercluster
Supercluster
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A map of the superclusters and voids nearest to Earth

A supercluster is a large group of smaller galaxy clusters or galaxy groups;[1] they are among the largest known structures in the universe. The Milky Way is part of the Local Group galaxy group (which contains more than 54 galaxies), which in turn is part of the Virgo Supercluster, which is part of the Laniakea Supercluster, which is part of the Pisces–Cetus Supercluster Complex.[2] The large size and low density of superclusters means that most of them, unlike clusters, expand with the Hubble expansion. The number of superclusters in the observable universe is estimated to be 10 million.[3]

Existence

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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.

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

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 structures known 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 are studied by those who believe that they may 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.

Although superclusters are supposed to be the largest structures in the universe according to the cosmological principle, larger structures have been observed in surveys, including the Sloan Great Wall.[7]

List of superclusters

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Galaxy supercluster Data Notes
Einasto Supercluster
  • z = ~0.25 (3 billion light years )
  • Length = 360 million light years
  • Mass = 2.6 × 1016 solar masses
 Discovered in 2023 by analyzing Sloan Digital Sky Survey images. Claimed to be the most massive galaxy supercluster discovered so far.[8][9]
King Ghidorah Supercluster
  • z = 0.50-0.64
  • Mass = 1 × 1016 solar masses
 The most massive galaxy supercluster discovered until 2023.[10]
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.

A 2014 study indicates that the Virgo Supercluster is only a lobe of an even greater supercluster, Laniakea.[11]

Hydra–Centaurus Supercluster SCl 128 - 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.[11]

Pavo–Indus Supercluster

In 2014, the newly announced Laniakea Supercluster subsumed the Pavo-Indus Supercluster, which became a component of the new supercluster.[11]

Southern Supercluster

Includes Fornax Cluster (S373), Dorado and Eridanus clouds.[12]

Saraswati Supercluster Distance = 4 billion 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

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Galaxy supercluster Data Notes
Perseus–Pisces Supercluster SCl 40
Coma Supercluster SCl 117 - 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
 (no SCl number) - 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.[13]
Shapley Supercluster
  • z=0.046.(650 Mly away)
 SCl 124 - The second supercluster found, after the Local Supercluster.

Distant superclusters

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Galaxy supercluster Data Notes
Pisces–Cetus Supercluster SCl 10
Boötes Supercluster SCl 138
Horologium–Reticulum Supercluster
z=0.063 (700 Mly)
Length = 550 Mly
 SCl 48 + SCl 49
Corona Borealis Supercluster
z=0.07[14]
 SCl 158
Columba Supercluster (no SCl number)
Aquarius Supercluster SCl 4
Aquarius B Supercluster SCl 193
Aquarius–Capricornus Supercluster SCl 189
Aquarius–Cetus Supercluster SCl 188
Bootes A Supercluster SCl 150
Caelum Supercluster
z=0.126 (1.4 Gly)
 SCl 59
Draco Supercluster SCl 114
Draco–Ursa Major Supercluster SCl 257
Fornax–Eridanus Supercluster SCl 53
Grus Supercluster SCl 197
Leo A Supercluster SCl 100
Leo–Sextans Supercluster SCl 91
Leo–Virgo Supercluster SCl 107
Microscopium Supercluster SCl 174
Pegasus–Pisces Supercluster SCl 3
Perseus–Pisces Supercluster SCl 40
Pisces–Aries Supercluster SCl 30
Ursa Majoris Supercluster SCl 109
Virgo-Coma Supercluster SCl 111

Extremely distant superclusters

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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.[15][16]
Lynx Supercluster z=1.27 Discovered in 1999[17] (as ClG J0848+4453, a name now used to describe the western cluster, with ClG J0849+4452 being the eastern one),[18] 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.[19] Additionally, seven smaller groups of galaxies are associated with the supercluster.[20]
SCL @ 1338+27 at z=1.1

z=1.1

Length=70Mpc

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[21][22]
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″[23]
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 .[24]
MS 0302+17

z=0.42

Length=6Mpc

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.[25]

Diagram

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

See also

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References

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Revisions and contributorsEdit on WikipediaRead on Wikipedia

Supercluster

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A supercluster is a large-scale structure in the observable universe consisting of numerous galaxy clusters, galaxy groups, and isolated galaxies that are associated through weak gravitational influences but are typically not bound together as a single entity. These structures represent the largest known density enhancements beyond individual galaxy clusters, often defined as collections of two or more galaxy clusters exhibiting significant spatial overdensities relative to the cosmic average. Superclusters span typical diameters of 100 to 500 million light-years (roughly 30 to 160 megaparsecs) and contain total masses ranging from 101510^{15} to 101710^{17} solar masses, depending on the specific definition and boundaries used. Unlike gravitationally bound galaxy clusters, superclusters exist in a quasi-linear of cosmic evolution and are not virialized, meaning their components are slowly drifting apart due to the universe's accelerating expansion driven by . They form part of the cosmic web, connecting filaments, walls, and voids, and their identification relies on mapping distributions through surveys and peculiar velocity analyses. While some central regions of superclusters may exhibit sufficient overdensity to potentially collapse in the distant future (termed "superstes-clusters"), most, including our own, will ultimately disperse. The resides in the , a prominent example identified in 2014 through analysis of galaxy flows toward the , encompassing over 100,000 across a volume of about 500 million light-years in diameter and a total mass equivalent to 101710^{17} solar masses. Other notable superclusters include the , one of the most massive known with a central collapsing region of approximately 101610^{16} solar masses, and the Einasto Supercluster, identified in 2023 with a mass of about 2.6×10162.6 \times 10^{16} solar masses. Vast filamentary structures like the extend up to 1.4 billion light-years. The study of superclusters provides critical insights into the initial conditions of the , the role of in , and the large-scale geometry of cosmology.

Definition and Characteristics

Definition

A supercluster is a vast aggregation of galaxy clusters, groups, and isolated galaxies within the cosmic web, representing one of the largest known structures in the observable universe. These structures typically span diameters of 30 to 200 megaparsecs (Mpc), encompassing regions where gravitational influences have gathered matter on scales far exceeding those of individual clusters. The exact definition of superclusters varies, often based on overdensity criteria relative to the cosmic mean or algorithmic clustering methods, as reviewed in recent studies. Unlike smaller cosmic entities, superclusters are not tightly gravitationally bound and instead participate in the overall expansion of the universe driven by the Hubble flow. In the hierarchical framework of cosmic , superclusters serve as intermediate-scale features between galaxy clusters—which range from 1 to 10 Mpc in diameter and contain hundreds to thousands of —and the expansive filamentary networks and sheets that trace the large-scale structure over hundreds of Mpc. Galaxy clusters form the primary building blocks of superclusters, linking together through weak gravitational ties to create these extended assemblies. This positioning highlights superclusters' role in bridging local dynamics with the broader distribution of matter in the . Key properties of superclusters include their loose gravitational cohesion, which prevents full virialization—the state of dynamic equilibrium seen in galaxy clusters where member galaxies a common center. Instead, the expansion of space dominates on these scales, causing superclusters to elongate and disperse over , though dark matter halos and tidal interactions can maintain some coherence. This non-bound nature distinguishes them from denser, self-gravitating systems and underscores their sensitivity to the 's accelerating expansion. The concept of superclusters emerged in the mid-20th century through early surveys of galaxy distributions. George Abell's 1958 catalog of 2712 rich galaxy clusters provided the first systematic evidence for "second-order clustering," describing large aggregates of clusters beyond isolated groupings. Building on this, Gérard de Vaucouleurs formalized the term "Local Supercluster" in 1953 and 1958 to denote the extended structure encompassing the and nearby groups, marking a pivotal recognition of these immense cosmic architectures.

Scale and Composition

Superclusters represent the largest gravitationally influenced structures in the , typically encompassing diameters ranging from 20 to 350 megaparsecs (Mpc) and total masses on the order of 101510^{15} to 101710^{17} solar masses (M⊙M_\odot). These immense scales highlight their role as extended aggregates of smaller components within the cosmic web, far surpassing the dimensions of individual clusters, which are limited to a few megaparsecs. The variation in size and mass depends on the richness of the supercluster, with poorer examples around 20–50 Mpc and 1015M⊙10^{15} M_\odot, while richer ones approach the upper limits, influenced by the Hubble parameter h≈0.7h \approx 0.7. In terms of composition, superclusters consist primarily of 10 to 100 galaxy clusters, which account for the majority of their bound mass, supplemented by intergalactic gas, extensive halos, and vast voids that occupy much of the intervening space. Galaxy clusters form the nodal points, containing hundreds to thousands of galaxies each, while the intergalactic medium includes hot, diffuse gas detectable via emissions and inferred from gravitational lensing and dynamics. Voids, comprising low-density regions, separate these components and contribute to the overall filamentary network, with the baryonic gas fraction estimated at around 10% of the total mass. Density profiles within superclusters exhibit lower overall densities compared to galaxy clusters, with average overdensities of approximately 2 to 5 relative to the cosmic , reflecting their marginally bound nature. These profiles feature high- cores around central massive clusters, where the contrast can reach Δρ≈30–40\Delta \rho \approx 30–40 at the borders of collapsing subregions, transitioning outward to near-critical thresholds for future . Such gradients underscore the hierarchical assembly of matter, with the density remaining close to the universal average across the supercluster volume. Morphologically, superclusters often appear as irregular aggregates aligned along cosmic filaments, with central concentrations dominated by one or more massive clusters that anchor the structure. Common types include filamentary forms with linear extensions and spider-like configurations featuring multiple branching filaments radiating from a dense core, as observed in surveys like the . These shapes arise from the anisotropic distribution of matter in the large-scale structure, emphasizing elongated rather than spherical geometries.

Formation and Evolution

Theoretical Formation

The formation of superclusters originates from quantum fluctuations in the density of the early , generated during cosmic . These primordial perturbations, initially on subatomic scales, are exponentially stretched to macroscopic sizes by the rapid expansion of the inflationary epoch and imprinted as Gaussian random-phase density fluctuations in the . As the universe cools and expands, these fluctuations grow through gravitational instability, where overdense regions decelerate relative to the background expansion, eventually leading to the collapse and coalescence into larger structures like superclusters. Unlike bound clusters, superclusters represent unbound overdensities that grow through gravitational infall but are ultimately dispersing due to expansion. Within the , (CDM) is essential for seeding and amplifying these overdensities, as it clusters efficiently without the pressure support that inhibits baryonic matter on small scales. halos form first around the primordial peaks, attracting baryons and facilitating the hierarchical merging of smaller structures—such as dwarf galaxies, groups, and clusters—into extended filaments, sheets, and voids that define superclusters. This bottom-up assembly process, a of Lambda-CDM cosmology, emerges naturally from N-body simulations of gravitational dynamics starting from initial conditions set by the power of fluctuations. The characteristic scale for the onset of gravitational instability in cosmological perturbations is described by the Jeans length, λJ≈csGρ,\lambda_J \approx \frac{c_s}{\sqrt{G \rho}},
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