|This article is outdated. (July 2012)|
Superclusters are large groups of smaller galaxy clusters or galaxy groups and are among the largest known structures of the cosmos. The Milky Way is in the Local Group of galaxies, which in turn is in the Laniakea Supercluster. This supercluster spans over 500 million light years, while the Local Group spans over 10 million light years.
Galaxies are grouped into clusters instead of being dispersed randomly. Clusters of galaxies are grouped together to form superclusters. Typically, superclusters contain dozens of individual clusters throughout an area of space about 150 million lightyears across. Unlike clusters, superclusters are not bound together by gravity. They are all shifting away from each other due to the Hubble flow.
Our galaxy falls within the Local Group, which is a poor and irregular cluster of galaxies. Poor clusters may contain only a few dozen galaxies as compared to rich clusters that can contain hundreds or even thousands. The Local Group is near the Local Supercluster (also known as the Virgo Supercluster) which has a diameter of 100 million lightyears. The Local Supercluster contains a total of about 1015 times the mass of the Sun.
The biggest cluster in the local universe is called the Great Attractor. Its gravity is so strong that the Local Supercluster, including the Milky Way, is moving in a direction towards it at a rate of several hundred kilometers per second. The biggest supercluster outside of the local universe is the Purseus-Pegasus Filament. It contains the Perseus supercluster and it spans about a billion light years. From what we currently know, it is the largest structure in the universe. This supercluster was discovered by David Batuski and Jack Burns of New Mexico State University.
Distribution: cosmic voids and sheets
Research has been done to try to understand the way in which superclusters are arranged in space. Maps are used to display the positions of 1.6 million galaxies. Three-dimensional maps are used to further understand the positions of these superclusters. In order to map them three-dimensionally, the position of the galaxy in the sky as well as the galaxy's redshift are used for calculation. The galaxy's redshift is used with the Hubble Law in order to determine its position in three-dimensional space.
It was discovered from those maps that superclusters of galaxies are not spread uniformly across the universe but they seem to lie along filaments. Maps reveal huge voids where there are extremely few galaxies. Some dim galaxies or hydrogen clouds can be found in some voids, but most galaxies are found in sheets between the voids. The voids themselves are often spherical but the superclusters are not. They can range from being 100 million to 400 million lightyears in diameter.The pattern of sheets and voids contains information about how galaxy clusters formed in the early universe.
There is a sponge analogy used often that compares a sponge to the pattern of clusters of galaxies in the universe – the holes are the voids and the other parts are the locations of the superclusters.
The existence of superclusters indicates that the galaxies in our 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.
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. Observations of superclusters likely tell us something 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 us insight and information into the early formation process of galaxies in the history of the Universe.
List of superclusters
||The Laniakea Supercluster is the supercluster that contains the Virgo Cluster, Local Group, and by extension on the latter, our galaxy; the Milky Way.|
||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.|
|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
|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|
||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.|
||The second supercluster found, after the Local Supercluster.|
|Boötes Supercluster||SCl 138|
||The entire supercluster is referred to as the Horologium-Reticulum Supercluster|
|Corona Borealis Supercluster|
|Aquarius B Supercluster|
|Bootes A Supercluster|
|Caelum Supercluster||SCl 59|
|Draco-Ursa Major Supercluster|
|Leo A Supercluster|
|Leo-Virgo Supercluster||SCl 107|
|Microscopium Supercluster||SCl 174|
|Pegasus-Pisces Supercluster||SCl 3|
|Perseus-Pisces Supercluster||SCl 40|
|Ursa Majoris Supercluster|
|Virgo-Coma Supercluster||SCl 111|
Far distant superclusters
|Lynx Supercluster||z=1.27||Discovered in 1999 (as ClG J0848+4453, a name now used to describe the western cluster, with ClG J0849+4452 being the eastern one), 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. Additionally, seven smaller groups of galaxies are associated with the supercluster.|
|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 |
|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″|
|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 .|
|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.|
- Earth's new address: 'Solar System, Milky Way, Laniakea' / Nature
- "An Intergalactic Heavyweight". ESO Picture of the Week. Retrieved 12 February 2013.
- Abell, George O. (1958). "The distribution of rich clusters of galaxies. A catalogue of 2712 rich clusters found on the National Geographic Society Palomar Observatory Sky Survey". The Astrophysical Journal Supplement Series, 3 3: 211–88. Bibcode:1958ApJS....3..211A. doi:10.1086/190036.
- 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.
- R. Brent Tully; Helene Courtois; Yehuda Hoffman; Daniel Pomarède (2 September 2014). "The Laniakea supercluster of galaxies". Nature (4 September 2014) 513 (7516): 71. arXiv:1409.0880. Bibcode:2014Natur.513...71T. doi:10.1038/nature13674.
- 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.
- 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.
- 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.
- "Lynx Supercluster". SIMBAD.
- 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): 29–33. Bibcode:2004ogci.conf...29N. doi:10.1017/S1743921304000080. ISBN 0-521-84908-X.
- 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.
- 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.
- 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.
- Lubin, L. M.; et al. (2000). "A Definitive Optical Detection of a Supercluster at [CLC][ITAL]z[/ITAL][/CLC] ≈ 0.91". The Astrophysical Journal 531 (1): L5–L8. arXiv:astro-ph/0001166. Bibcode:2000ApJ...531L...5L. doi:10.1086/312518. PMID 10673401.
- Connolly, A. J.; et al. (1996). "Superclustering at Redshift [CLC][ITAL]z[/ITAL] = 0.54[/CLC]". The Astrophysical Journal Letters 473 (2): L67–L70. arXiv:astro-ph/9610047. Bibcode:1996ApJ...473L..67C. doi:10.1086/310395.
- University of Hawaii, "The MS0302+17 Supercluster", Nick Kaiser. Retrieved 15 September 2009.
- Overview of local superclusters
- The Nearest Superclusters
- Universe family tree: Supercluster
- Superclusters - Large Scale Structures