Galaxy Cluster: Definition, Names and Examples, Supercluster, Facts

Galaxy clusters are the largest known structures in the universe, held together by gravity. These groupings contain hundreds to thousands of galaxies spanning millions of light-years. Cluster masses range from 10^14 to 10^15 solar masses, with dark matter comprising 85% of the total mass. Galaxy clusters form through the merging of galaxy groups, driven by gravitational forces.

Examples of galaxy clusters include the Coma Cluster, Virgo Cluster, and Norma Cluster. The Coma Cluster contains over 1,000 galaxies and is located 321 million light-years away. Virgo Cluster houses more than 2,000 galaxies at a distance of 54 million light-years. Norma Cluster features over 50 galaxies situated 220 million light-years from Earth.

 These complexes contain concentrations of galaxy clusters and individual galaxies. Laniakea, our supercluster, extends over 500 million light-years and includes the Milky Way galaxy. Superclusters form through gravitational collapse of regions of space and consist of multiple galaxy clusters and groups.

Clusters serve as laboratories for studying galaxy formation, cosmology, and physics. Hot intergalactic plasma within clusters reaches temperatures of up to 100 million degrees Celsius. Galaxies within clusters move at speeds of hundreds to over 1,000 km/s. Scientists use gravitational lensing to study galaxy clusters and estimate their mass.

Gravity holds galaxy clusters, with dark matter providing the invisible gravitational force. Dark matter outweighs visible matter by 5-10 times in clusters. ‘The combined gravitational pull of all components keeps clusters intact over billions of years. Galaxy clusters have a characteristic size called the virial radius, measuring 1-5 megaparsecs in diameter.

What is a galaxy cluster?

Galaxy clusters are the known structures in the universe. Gravity holds these groupings together. Clusters contain hundreds to thousands of galaxies. Clusters span millions of light-years. Cluster masses range from 10^14 to 10^15 solar masses. Plasma fills inter-galactic space. Dark matter comprises 85% of cluster mass.

Galaxy cluster formation occurs through the merging of galaxy groups. Gravity drives this process, with dark matter providing the gravitational scaffolding. Galaxy cluster structure includes a core, halo, and subclusters. The NFW profile measures galaxy cluster concentration, classifying them as regular, irregular, or merging.

Galaxy cluster mass ranges from 10^14 to 10^15 solar masses. Dark matter comprises 85% of this mass, with ordinary matter making up the remaining 15%. Galaxy cluster size ranges from 1 to 10 megaparsecs in diameter. Galaxy cluster matter includes dark matter, stars, gas, and dust.

Galaxy cluster groups contain elliptical, spiral, and dwarf galaxies. Galaxy clusters feature giant elliptical galaxies at their centers. Galaxy cluster galaxies interact and evolve compared to isolated galaxies due to the dense cluster environment.

Galaxy cluster properties include high temperatures and densities. Gas in galaxy clusters reaches temperatures of 10 to 100 million Kelvin. Galaxy cluster density ranges from 10^-3 to 10^-1 particles per cubic centimeter. Galaxy clusters exhibit gravitational lensing effects, providing insights into dark matter distribution.

What are examples and names of galaxy clusters?

Galaxy clusters include Coma, Virgo, Norma, Fornax, and Hydra. Groups comprise M81 Group, Triplet, and Quartet. Coma Cluster contains over 1,000 galaxies 321 million light-years away. Virgo Cluster houses 2,000+ galaxies 54 million light-years distant. Norma Cluster features 50+ galaxies 220 million light-years from Earth.

Examples and names of galaxy clusters are provided in the table below.

The Virgo Cluster is the closest large cluster to the Milky Way, located 54 million light-years away in the constellation Virgo. It contains over 2,000 galaxies. The Fornax Cluster is situated about 62 million light-years away in the constellation Fornax, containing 60 galaxies with a high concentration of dwarf galaxies.

The Local Group includes the Milky Way, Andromeda Galaxy, and several other galaxies. Baede’s Ursae Major Cluster is located about 30 million light-years away in the constellation Ursa Major, containing 20 galaxies with a compact structure. The Pegasus Group is situated about 40 million light-years away in the constellation Pegasus, containing 10 galaxies with a low velocity dispersion. The Cetus Group is located about 30 million light-years away in the constellation Cetus, containing 10 galaxies with a compact structure.

The Leo Triplet is found about 35 million light-years away in the constellation Leo, consisting of three galaxies: M65, M66, and NGC 3628. The Pisces Galaxy Cloud is located about 1 billion light-years in the constellation Pisces, containing over 100 galaxies with a high velocity dispersion. The Eridanus A Group is situated about 70 million light-years away in the constellation Eridanus, containing 10 galaxies with a compact structure. The Draco Trio is located about 30 million light-years away in the constellation Draco, consisting of three galaxies: NGC 5907, NGC 5905, and NGC 5904.

Among the clusters, the Hercules Cluster is located 500 million light-years away in the constellation Hercules. It contains over 200 galaxies and has a structure. The Coma Cluster is situated about 320 million light-years away in the constellation Coma Berenices, containing over 1,000 galaxies and is one of the galaxy clusters in the universe.

The Great Attractor is pulling our galaxy and others towards it, located about 250 million light-years away. It is thought to be a large galaxy cluster. The Norma Cluster is located 220 million light-years away in the constellation Norma, containing over 200 galaxies with a velocity dispersion.

Abell 370 is situated 4.2 billion light-years away in the constellation Cetus, containing over 100 galaxies and is known for its gravitational lensing effects. Markarian’s Chain is located 300 million light-years away in the constellation Virgo, containing 10 galaxies with a structure. Abell 2199 is found 1.2 billion light-years in the constellation Hercules, containing over 100 galaxies with a high velocity dispersion.

What is the cluster of galaxies that our own galaxy belongs to called?

The Milky Way galaxy belongs to the Local Group. Local Group contains over 50 galaxies, including spirals like Andromeda (M31) and Triangulum (M33). Membership comprises galaxy types – spirals, ellipticals, and irregulars. Local Group demonstrates a variety of galactic structures within our neighborhood.

The Local Group spans 10 million light-years in diameter. It has a mass of around 1.29 x 10^12 solar masses, with the Milky Way contributing 1.5 x 10^12 solar masses. The Andromeda Galaxy, the largest member of the Local Group, has a diameter of 220,000 light-years, while the Milky Way measures 100,000 light-years.

The Local Group is part of the Laniakea Supercluster. Laniakea stretches over 500 million light-years and contains thousands of galaxies.

What is a supercluster of galaxies?

Superclusters are the largest known structures in the universe, spanning distances over 100 million light-years.  Superclusters form through gravitational collapse of large space regions. Laniakea, our local supercluster, extends over 500 million light-years and includes the Milky Way.

Examples of superclusters include the Laniakea Supercluster, Virgo Supercluster, and Shapley Supercluster. Superclusters form part of the large-scale structure of the universe, referred to as the “cosmic web.” Voids of empty space separate these structures, creating a network of matter distribution throughout the cosmos.

What is the difference between galaxy clusters and superclusters?

Galaxy clusters contain 100-1,000 galaxies, measuring 2-10 megaparsecs in diameter. Superclusters encompass multiple clusters and groups, stretching hundreds of megaparsecs. Clusters have masses of 10^14-10^15 solar masses. Superclusters comprise thousands of galaxies. Size and scale constitute the difference. Gravitational forces hold both structures together.

Gravitational properties distinguish galaxy clusters from superclusters. Galaxy clusters are gravitationally bound systems, with galaxies held by mutual gravitational attraction. Superclusters are not gravitationally bound, as the clusters and groups within them lack a common gravitational potential.

Galaxy clusters are components of supercluster structures. Superclusters form through the aggregation of multiple galaxy clusters and groups, connected by filaments of galaxies. The Sloan Great Wall, a supercluster discovered in 2003, contains thousands of galaxy clusters and groups and extends over 1.3 billion light-years.

Prevalence and scale differ between galaxy clusters and superclusters. Galaxy clusters are common, with an estimated 10^5 to 10^6 clusters in the observable universe. Superclusters are less common, with only 10^3 to 10^4 estimated to exist. Superclusters represent some of the largest known structures in the universe, rivaling the size of cosmic web voids and filaments.

What are fun facts about galaxy clusters?

Galaxy clusters are the largest structures in the universe. Gravity binds hundreds to thousands of galaxies. Clusters contain amounts of dark matter, comprising 85% of their mass. Coma Cluster, a known galaxy cluster, spans 20 million light-years and weighs 7 x 10^14 solar masses. Scientists study clusters using gravitational lensing.

Fun facts about galaxy clusters are listed below:

• Galaxies in galaxy clusters: Galaxy clusters contain hundreds to thousands of galaxies: These vast structures are bound by gravity over distances of up to 10 million light-years.
• Galaxy clusters’ hot intergalactic plasma: This plasma reaches temperatures of up to 100 million degrees Celsius between galaxies.
• Dark matter in galaxy clusters: Comprising about 85% of a cluster’s mass, dark matter acts as the gravitational glue.
• Galaxy motions in clusters: Galaxies move at speeds of hundreds to over 1,000 km/s within clusters.
• Coma galaxy cluster: Contains over 1,000 galaxies and is located about 320 million light-years from Earth.
• Hot plasma in galaxy clusters: X-ray telescopes like NASA’s Chandra X-ray Observatory observe emissions from clusters.
• Virgo Cluster: The nearest large galaxy cluster to the Milky Way covering 54 million light-years.
• Galaxy clusters as cosmic laboratories: These structures are crucial for studying galaxy formation, cosmology, and physics.
• Mass estimation of galaxy clusters: Scientists measure galaxy motion to estimate cluster mass.
• Galaxy distribution in clusters: Provides insights into galaxy evolution across billions of years.
• Feedback mechanisms in galaxy clusters: Supernovae and active galactic nuclei heat the surrounding gas.

The Coma galaxy cluster contains over 1,000 galaxies and lies about 320 million light-years from Earth. X-ray telescopes like NASA’s Chandra X-ray Observatory detect X-ray emissions from hot plasma in clusters. The Virgo Cluster, the nearest large galaxy cluster to the Milky Way, spans a distance of 54 million light-years.

Galaxy clusters serve as cosmic laboratories for studying galaxy formation, cosmology, and physics. Scientists estimate cluster mass by measuring galaxy motions within clusters. The distribution of galaxies in clusters provides clues about galaxy evolution over billions of years. Clusters exhibit feedback mechanisms where supernovae and active galactic nuclei heat surrounding gas.

What holds the galaxy clusters together?

Gravity holds galaxy clusters together. Dark matter provides the invisible gravitational force binding these structures.   Gravitational scaffolding maintains cluster structure over billions of years. Galaxy clusters are the known objects in the universe.

Galaxy clusters have masses ranging from 10^14 to 10^15 solar masses. Galaxy clusters are the largest gravitationally bound objects in the universe.  The combined gravitational pull of all components keeps clusters intact.

The force of gravity keeps galaxies in equilibrium within clusters. Inward gravitational attraction balances the outward pressure of galaxy motions and gas.  Within this radius, the cluster density is 200 times the critical density of the universe.

Gravitational attraction binds galaxies, gas, and dark matter in a complex network. Gas temperatures in clusters reach 10-100 million Kelvin. Galaxy clusters have a velocity dispersion of 500-1,000 kilometers per second. The gravitational potential energy of clusters is 10-100 times the total kinetic energy of their components.

How does gravitational lensing tell us about the mass of a galaxy cluster?

Gravitational lensing determines galaxy cluster mass through light distortion analysis. Cluster gravitational fields bend light from distant galaxies. Astronomers observe these distortions to map mass distribution. Lensing effects reveal cluster mass. Orbital velocities of galaxies within clusters contribute to mass determination. Stronger gravitational fields produce pronounced lensing effects, indicating higher cluster mass.

Gravitational lensing allows astronomers to calculate the mass of galaxy clusters. Researchers study how clusters’ gravitational fields distort and bend light from background galaxies. Clusters with greater lensing distortion have more mass. Einstein’s general theory of relativity predicts this lensing effect. Massive objects like galaxy clusters warp spacetime and deflect light paths.

Gravitational lensing occurs when light from distant sources passes massive clusters. Clusters’ mass warps surrounding space, causing light to bend and change direction. The bending of light results in magnification, distortion, and multiple imaging of background sources. Astronomers study these distortions to map the mass distribution of galaxy clusters. The amount of light bending depends on cluster mass, allowing calculation of total cluster mass.

Gravitational lensing determines orbital speeds of galaxies in clusters. Astronomers measure distortion of background light to infer velocity dispersion of clusters. Velocity dispersion measures average galaxy velocity in clusters, in kilometers per second. This velocity dispersion relates to cluster mass. Gravitational lensing detects dark matter presence in galaxy clusters. Dark matter does not interact with electromagnetic radiation, remaining invisible to telescopes. The gravitational effects of dark matter on light are inferred through lensing observations.

Astronomers determine cluster mass by studying background light distortion. Clusters create Einstein rings, which calculate cluster mass. Researchers analyze Einstein ring shape and size to measure cluster mass in solar masses. The Einstein radius is proportional to cluster mass, allowing for mass calculations. For example, gravitational lensing observations estimate the Abell 1689 galaxy cluster has a mass of 1.2 x 10^15 solar masses, distributed over a 2 megaparsec diameter.

How many galaxies are in a typical cluster of galaxies?

Galaxy clusters contain hundreds to thousands of galaxies. Clusters have between 100 to 1,000 galaxies. Abell catalogue clusters contain up to 2,000 galaxies or more. The Abell 2744 cluster has an estimated 1,500 galaxies. Clusters like Coma (Abell 1656) have over 1,000 galaxies. Clusters contain a few dozen galaxies.

The range for galaxies in clusters spans from 100 to 2,000. Astronomers provide an estimate of a few hundred to a few thousand galaxies in clusters. The number of galaxies in a cluster depends on definition criteria and observational sensitivity. Galaxy clusters represent the largest gravitationally-bound structures in the universe. The total mass of clusters ranges from 100 trillion to 1 quadrillion solar masses.