Galaxy formation and evolution

<h2 id="commonly-observed-properties-of-galaxies">Commonly observed properties of galaxies</h2>
Because of the inability to conduct experiments in outer space, the only way to “test” theories and models of galaxy evolution is to compare them with observations. Explanations for how galaxies formed and evolved must be able to predict the observed properties and types of galaxies.
<a href="/facts/Edwin_Hubble/fpX3JlbJ">Edwin Hubble</a> created an early galaxy classification scheme, now known as the Hubble tuning-fork diagram. It partitioned galaxies into <a href="/facts/Elliptical_galaxy/1PUchrj1">ellipticals</a>, normal <a href="/facts/Spiral_galaxy/hRT2dtxJ">spirals</a>, <a href="/facts/Barred_spiral_galaxy/cntSCFX4">barred spirals</a> (such as the <a href="/facts/Milky_Way/ulF6lccN">Milky Way</a>), and <a href="/facts/Irregular_galaxy/P95rRpYR">irregulars</a>. These galaxy types exhibit the following properties which can be explained by current galaxy evolution theories:

<ul><li>Many of the properties of galaxies (including the <a href="/facts/Galaxy_color%E2%80%93magnitude_diagram/yVesL0pG">galaxy color–magnitude diagram</a>) indicate that there are fundamentally two types of galaxies. These groups divide into blue star-forming galaxies that are more like spiral types, and red non-star forming galaxies that are more like elliptical galaxies.</li>
<li>Spiral galaxies are quite thin, dense, and rotate relatively fast, while the stars in elliptical galaxies have randomly oriented orbits.</li>
<li>The majority of giant galaxies contain a <a href="/facts/Supermassive_black_hole/BcuTx8Q5">supermassive black hole</a> in their centers, ranging in mass from millions to billions of times the mass of the <a href="/facts/Sun/CadPCVHh">Sun</a>. The black hole mass is tied to the host galaxy bulge or spheroid mass.</li>
<li><a href="/facts/Metallicity/nhhPqbYF">Metallicity</a> has a positive correlation with the <a href="/facts/Absolute_magnitude/R8RVxkLx">absolute magnitude</a> (luminosity) of a galaxy.</li></ul>
Astronomers now believe that disk galaxies likely formed first, then evolved into elliptical galaxies through galaxy mergers.
Current models also predict that the majority of mass in galaxies is made up of <a href="/facts/Dark_matter/y5HgX55N">dark matter</a>, a substance which is not directly observable, and might not interact through any means except gravity. This observation arises because galaxies could not have formed as they have, or rotate as they are seen to, unless they contain far more mass than can be directly observed.

<h2 id="formation-of-disk-galaxies">Formation of disk galaxies</h2>
The earliest stage in the evolution of galaxies is their formation. When a galaxy forms, it has a disk shape and is called a spiral galaxy due to spiral-like "arm" structures located on the disk. There are different theories on how these disk-like distributions of stars develop from a cloud of matter: however, at present, none of them exactly predicts the results of observation.

<h3>Top-down theories</h3>
<a href="/facts/Olin_J._Eggen/EW77VQCE">Olin J. Eggen</a>, <a href="/facts/Donald_Lynden-Bell/vLGDqAXr">Donald Lynden-Bell</a>, and <a href="/facts/Allan_Sandage/Qk1kRoTm">Allan Sandage</a><a class="footnote-ref" id="fnref:1" href="#fn:1">1</a> in 1962, proposed a theory that disk galaxies form through a monolithic collapse of a large gas cloud. The distribution of matter in the early universe was in clumps that consisted mostly of dark matter. These clumps interacted gravitationally, putting tidal torques on each other that acted to give them some angular momentum. As the <a href="/facts/Baryon/QFwAUWK2">baryonic matter</a> cooled, it dissipated some energy and contracted toward the center. With angular momentum conserved, the matter near the center speeds up its rotation. Then, like a spinning ball of pizza dough, the matter forms into a tight disk. Once the disk cools, the gas is not gravitationally stable, so it cannot remain a singular homogeneous cloud. It breaks, and these smaller clouds of gas form stars. Since the dark matter does not dissipate as it only interacts gravitationally, it remains distributed outside the disk in what is known as the <a href="/facts/Dark_matter_halo/I6JEbRDm">dark halo</a>. Observations show that there are stars located outside the disk, which does not quite fit the "pizza dough" model. It was first proposed by <a href="/facts/Leonard_Searle/dBgDW2mW">Leonard Searle</a> and Robert Zinn <a class="footnote-ref" id="fnref:2" href="#fn:2">2</a> that galaxies form by the coalescence of smaller progenitors. Known as a top-down formation scenario, this theory is quite simple yet no longer widely accepted.

<h3>Bottom-up theory</h3>
More recent theories include the clustering of dark matter halos in the bottom-up process. Instead of large gas clouds collapsing to form a galaxy in which the gas breaks up into smaller clouds, it is proposed that matter started out in these “smaller” clumps (mass on the order of <a href="/facts/Globular_cluster/FL0EERJU">globular clusters</a>), and then many of these clumps merged to form galaxies,<a class="footnote-ref" id="fnref:3" href="#fn:3">3</a> which then were drawn by gravitation to form <a href="/facts/Galaxy_cluster/BhIEgbx8">galaxy clusters</a>. This still results in disk-like distributions of baryonic matter with dark matter forming the halo for all the same reasons as in the top-down theory. Models using this sort of process predict more small galaxies than large ones, which matches observations.
Astronomers do not currently know what process stops the contraction. In fact, theories of disk galaxy formation are not successful at producing the rotation speed and size of disk galaxies. It has been suggested that the radiation from bright newly formed stars, or from an <a href="/facts/Active_galactic_nucleus/qT1owvXz">active galactic nucleus</a> can slow the contraction of a forming disk. It has also been suggested that the <a href="/facts/Dark_matter/y5HgX55N">dark matter</a> halo can pull the galaxy, thus stopping disk contraction.<a class="footnote-ref" id="fnref:4" href="#fn:4">4</a>
The <a href="/facts/Lambda-CDM_model/DmlhJHQU">Lambda-CDM model</a> is a cosmological model that explains the formation of the universe after the <a href="/facts/Big_Bang/I5T1vTnv">Big Bang</a>. It is a relatively simple model that predicts many properties observed in the universe, including the relative frequency of different galaxy types; however, it underestimates the number of thin disk galaxies in the universe.<a class="footnote-ref" id="fnref:5" href="#fn:5">5</a> The reason is that these galaxy formation models predict a large number of mergers. If disk galaxies merge with another galaxy of comparable mass (at least 15 percent of its mass) the merger will likely destroy, or at a minimum greatly disrupt the disk, and the resulting galaxy is not expected to be a disk galaxy (see next section). While this remains an unsolved problem for astronomers, it does not necessarily mean that the Lambda-CDM model is completely wrong, but rather that it requires further refinement to accurately reproduce the population of galaxies in the universe.

<h2 id="galaxy-mergers-and-the-formation-of-elliptical-galaxies">Galaxy mergers and the formation of elliptical galaxies</h2>

Main article: <a href="/facts/Galaxy_merger/WRKsV7t2">Galaxy merger</a>
Elliptical galaxies (most notably <a href="/facts/Type-cD_galaxy/1n0mMurr">supergiant ellipticals</a>, such as <a href="/facts/ESO_306-17/y2PK4aTx">ESO 306-17</a>) are among some of the <a href="/facts/List_of_largest_galaxies/9PJtf6ld">largest known thus far</a>. Their stars are on orbits that are randomly oriented within the galaxy (i.e. they are not rotating like disk galaxies). A distinguishing feature of elliptical galaxies is that the velocity of the stars does not necessarily contribute to flattening of the galaxy, such as in spiral galaxies.<a class="footnote-ref" id="fnref:6" href="#fn:6">6</a> Elliptical galaxies have central <a href="/facts/Supermassive_black_hole/BcuTx8Q5">supermassive black holes</a>, and the masses of these black holes correlate with the galaxy's mass.
Elliptical galaxies have two main stages of evolution. The first is due to the supermassive black hole growing by accreting cooling gas. The second stage is marked by the black hole stabilizing by suppressing gas cooling, thus leaving the elliptical galaxy in a stable state.<a class="footnote-ref" id="fnref:7" href="#fn:7">7</a> The mass of the black hole is also correlated to a property called <a href="/facts/Velocity_dispersion/9FYB7pb9">sigma</a> which is the dispersion of the velocities of stars in their orbits. This relationship, known as the <a href="/facts/M%E2%80%93sigma_relation/CnU82b7D">M-sigma relation</a>, was discovered in 2000.<a class="footnote-ref" id="fnref:8" href="#fn:8">8</a> Elliptical galaxies mostly lack disks, although some <a href="/facts/Galaxy_bulge/cjJ0LFan">bulges</a> of disk galaxies resemble elliptical galaxies. Elliptical galaxies are more likely found in crowded regions of the universe (such as <a href="/facts/Galaxy_cluster/BhIEgbx8">galaxy clusters</a>).
Astronomers now see elliptical galaxies as some of the most evolved systems in the universe. It is widely accepted that the main driving force for the evolution of elliptical galaxies is <a href="/facts/Galaxy_merger/WRKsV7t2">mergers</a> of smaller galaxies. Many galaxies in the universe are gravitationally bound to other galaxies, which means that they will never escape their mutual pull. If those colliding galaxies are of similar size, the resultant galaxy will appear similar to neither of the progenitors,<a class="footnote-ref" id="fnref:9" href="#fn:9">9</a> but will instead be elliptical. There are many types of galaxy mergers, which do not necessarily result in elliptical galaxies, but result in a structural change. For example, a minor merger event is thought to be occurring between the Milky Way and the Magellanic Clouds.
Mergers between such large galaxies are regarded as violent, and the frictional interaction of the gas between the two galaxies can cause gravitational <a href="/facts/Shock_wave/CqrG1Xm5">shock waves</a>, which are capable of forming new stars in the new elliptical galaxy.<a class="footnote-ref" id="fnref:10" href="#fn:10">10</a> By sequencing several images of different galactic collisions, one can observe the timeline of two spiral galaxies merging into a single elliptical galaxy.<a class="footnote-ref" id="fnref:11" href="#fn:11">11</a>
In the <a href="/facts/Local_Group/kjUefCLr">Local Group</a>, the Milky Way and the <a href="/facts/Andromeda_Galaxy/MjmSLV6m">Andromeda Galaxy</a> are gravitationally bound, and currently approaching each other at high speed. Simulations show that the Milky Way and Andromeda are on a collision course, and are expected to collide in less than five billion years. During this collision, it is expected that the Sun and the rest of the Solar System will be ejected from its current path around the Milky Way. The remnant could be a giant elliptical galaxy.<a class="footnote-ref" id="fnref:12" href="#fn:12">12</a>

<h2 id="galaxy-quenching">Galaxy quenching</h2>
Main article: <a href="/facts/Quenching_(astronomy)/9KeWD1vU">Quenching (astronomy)</a>
One observation that must be explained by a successful theory of galaxy evolution is the existence of two different populations of galaxies on the galaxy color-magnitude diagram. Most galaxies tend to fall into two separate locations on this diagram: a "red sequence" and a "blue cloud". Red sequence galaxies are generally non-star-forming elliptical galaxies with little gas and dust, while blue cloud galaxies tend to be dusty star-forming spiral galaxies.<a class="footnote-ref" id="fnref:13" href="#fn:13">13</a><a class="footnote-ref" id="fnref:14" href="#fn:14">14</a>
As described in previous sections, galaxies tend to evolve from spiral to elliptical structure via mergers. However, the current rate of galaxy mergers does not explain how all galaxies move from the "blue cloud" to the "red sequence". It also does not explain how star formation ceases in galaxies. Theories of galaxy evolution must therefore be able to explain how star formation turns off in galaxies. This phenomenon is called galaxy "quenching".<a class="footnote-ref" id="fnref:15" href="#fn:15">15</a>
<a href="/facts/Star_formation/SMyfVDY6">Stars form</a> out of cold gas (see also the <a href="/facts/Kennicutt%E2%80%93Schmidt_law/PmrUSNt7">Kennicutt–Schmidt law</a>), so a galaxy is quenched when it has no more cold gas. However, it is thought that quenching occurs relatively quickly (within 1 billion years), which is much shorter than the time it would take for a galaxy to simply use up its reservoir of cold gas.<a class="footnote-ref" id="fnref:16" href="#fn:16">16</a><a class="footnote-ref" id="fnref:17" href="#fn:17">17</a> Galaxy evolution models explain this by hypothesizing other physical mechanisms that remove or shut off the supply of cold gas in a galaxy. These mechanisms can be broadly classified into two categories: (1) preventive feedback mechanisms that stop cold gas from entering a galaxy or stop it from producing stars, and (2) ejective feedback mechanisms that remove gas so that it cannot form stars.<a class="footnote-ref" id="fnref:18" href="#fn:18">18</a>
One theorized preventive mechanism called “strangulation” keeps cold gas from entering the galaxy. Strangulation is likely the main mechanism for quenching star formation in nearby low-mass galaxies.<a class="footnote-ref" id="fnref:19" href="#fn:19">19</a> The exact physical explanation for strangulation is still unknown, but it may have to do with a galaxy's interactions with other galaxies. As a galaxy falls into a galaxy cluster, gravitational interactions with other galaxies can strangle it by preventing it from accreting more gas.<a class="footnote-ref" id="fnref:20" href="#fn:20">20</a> For galaxies with massive <a href="/facts/Dark_matter_halo/I6JEbRDm">dark matter halos</a>, another preventive mechanism called “virial <a href="/facts/Shock_wave/CqrG1Xm5">shock</a> heating” may also prevent gas from becoming cool enough to form stars.<a class="footnote-ref" id="fnref:21" href="#fn:21">21</a>
Ejective processes, which expel cold gas from galaxies, may explain how more massive galaxies are quenched.<a class="footnote-ref" id="fnref:22" href="#fn:22">22</a> One ejective mechanism is caused by supermassive black holes found in the centers of galaxies. Simulations have shown that gas accreting onto supermassive black holes in galactic centers produces high-energy <a href="/facts/Astrophysical_jet/QYerB8R3">jets</a>; the released energy can expel enough cold gas to quench star formation.<a class="footnote-ref" id="fnref:23" href="#fn:23">23</a>
Our own Milky Way and the nearby Andromeda Galaxy currently appear to be undergoing the quenching transition from star-forming blue galaxies to passive red galaxies.<a class="footnote-ref" id="fnref:24" href="#fn:24">24</a>

<h2 id="hydrodynamics-simulation">Hydrodynamics Simulation</h2>
Dark energy and dark matter account for most of the Universe's energy, so it is valid to ignore baryons when simulating large-scale structure formation (using methods such as <a href="/facts/N-body_simulation/xrHwX7j3">N-body simulation</a>). However, since the visible components of galaxies consist of baryons, it is crucial to include baryons in the simulation to study the detailed structures of galaxies. At first, the baryon component consists of mostly hydrogen and helium gas, which later transforms into stars during the formation of structures. From observations, models used in simulations can be tested and the understanding of different stages of galaxy formation can be improved.

<h3>Euler equations</h3>
In cosmological simulations, astrophysical gases are typically modeled as inviscid ideal gases that follow the <a href="/facts/Euler_equations_(fluid_dynamics)/EYW5lerl">Euler equations</a>, which can be expressed mainly in three different ways: Lagrangian, Eulerian, or arbitrary Lagrange-Eulerian methods. Different methods give specific forms of hydrodynamical equations.<a class="footnote-ref" id="fnref:25" href="#fn:25">25</a> When using the Lagrangian approach to specify the field, it is assumed that the observer tracks a specific fluid parcel with its unique characteristics during its movement through space and time. In contrast, the Eulerian approach emphasizes particular locations in space that the fluid passes through as time progresses.

<h3>Baryonic Physics</h3>
To shape the population of galaxies, the hydrodynamical equations must be supplemented by a variety of astrophysical processes mainly governed by baryonic physics.

<h4>Gas cooling</h4>
Processes, such as collisional excitation, ionization, and inverse <a href="/facts/Compton_scattering/Q98Ty8rz">Compton scattering</a>, can cause the internal energy of the gas to be dissipated. In the simulation, cooling processes are realized by coupling cooling functions to energy equations. Besides the primordial cooling, at high temperature,
 
 
 
  
 
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, the fine structure and molecular cooling also need to be considered to simulate the cold phase of the <a href="/facts/Interstellar_medium/mokU0WEz">interstellar medium</a>.

<h4>Interstellar medium</h4>
Complex multi-phase structure, including relativistic particles and magnetic field, makes simulation of interstellar medium difficult. In particular, modeling the cold phase of the interstellar medium poses technical difficulties due to the short timescales associated with the dense gas. In the early simulations, the dense gas phase is frequently not modeled directly but rather characterized by an effective polytropic equation of state.<a class="footnote-ref" id="fnref:27" href="#fn:27">27</a> More recent simulations use a <a href="/facts/Multimodal_distribution/wYBCJ67S">multimodal distribution</a><a class="footnote-ref" id="fnref:28" href="#fn:28">28</a><a class="footnote-ref" id="fnref:29" href="#fn:29">29</a> to describe 
the gas density and temperature distributions, which directly model the multi-phase structure. However, more detailed physics processes needed to be considered in future simulations, since the structure of the interstellar medium directly affects <a href="/facts/Star_formation/SMyfVDY6">star formation</a>.

<h4>Star formation</h4>
As cold and dense gas accumulates, it undergoes gravitational collapse and eventually forms stars. To simulate this process, a portion of the gas is transformed into collisionless star particles, which represent coeval, single-metallicity stellar populations and are described by an initial underlying mass function. Observations suggest that star formation efficiency in molecular gas is almost universal, with around 1% of the gas being converted into stars per free fall time.<a class="footnote-ref" id="fnref:30" href="#fn:30">30</a> In simulations, the gas is typically converted into star particles using a probabilistic sampling scheme based on the calculated star formation rate. Some simulations seek an alternative to the probabilistic sampling scheme and aim to better capture the clustered nature of star formation by treating star clusters as the fundamental unit of star formation. This approach permits the growth of star particles by accreting material from the surrounding medium.<a class="footnote-ref" id="fnref:31" href="#fn:31">31</a> In addition to this, modern models of galaxy formation track the evolution of these stars and the mass they return to the gas component, leading to an enrichment of the gas with metals.<a class="footnote-ref" id="fnref:32" href="#fn:32">32</a>

<h4>Stellar feedback</h4>
Stars have an influence on their surrounding gas by injecting energy and momentum. This creates a feedback loop that regulates the process of star formation. To effectively control star formation, stellar feedback must generate galactic-scale outflows that expel gas from galaxies. Various methods are utilized to couple energy and momentum, particularly through supernova explosions, to the surrounding gas. These methods differ in how the energy is deposited, either thermally or kinetically. However, excessive radiative gas cooling must be avoided in the former case. Cooling is expected in dense and cold gas, but it cannot be reliably modeled in cosmological simulations due to low resolution. This leads to artificial and excessive cooling of the gas, causing the supernova feedback energy to be lost via radiation and significantly reducing its effectiveness. In the latter case, kinetic energy cannot be radiated away until it thermalizes. However, using hydrodynamically decoupled wind particles to inject momentum non-locally into the gas surrounding active star-forming regions may still be necessary to achieve large-scale galactic outflows.<a class="footnote-ref" id="fnref:33" href="#fn:33">33</a> Recent models explicitly model stellar feedback.<a class="footnote-ref" id="fnref:34" href="#fn:34">34</a> These models not only incorporate supernova feedback but also consider other feedback channels such as energy and momentum injection from stellar winds, photoionization, and radiation pressure resulting from radiation emitted by young, massive stars.<a class="footnote-ref" id="fnref:35" href="#fn:35">35</a> During the <a href="/facts/Cosmic_Dawn/tfqf1Ny9">Cosmic Dawn</a>, galaxy formation occurred in short bursts of 5 to 30 Myr due to stellar feedbacks.<a class="footnote-ref" id="fnref:36" href="#fn:36">36</a>

<h4>Supermassive black holes</h4>
Simulation of supermassive black holes is also considered, numerically seeding them in dark matter haloes, due to their observation in many galaxies<a class="footnote-ref" id="fnref:37" href="#fn:37">37</a> and the impact of their mass on the mass density distribution. Their mass accretion rate is frequently modeled by the Bondi-Hoyle model.

<h4>Active galactic nuclei</h4>
<a href="/facts/Active_galactic_nuclei/qT1owvXz">Active galactic nuclei</a> (AGN) have an impact on the observational phenomena of supermassive black holes, and further have a regulation of black hole growth and star formation. In simulations, AGN feedback is usually classified into two modes, namely quasar and radio mode. Quasar mode feedback is linked to the radiatively efficient mode of black hole growth and is frequently incorporated through energy or momentum injection.<a class="footnote-ref" id="fnref:38" href="#fn:38">38</a> The regulation of star formation in massive galaxies is believed to be significantly influenced by radio mode feedback, which occurs due to the presence of highly collimated jets of relativistic particles. These jets are typically linked to X-ray bubbles that possess enough energy to counterbalance cooling losses.<a class="footnote-ref" id="fnref:39" href="#fn:39">39</a>

<h4>Magnetic fields</h4>
The ideal <a href="/facts/Magnetohydrodynamics/7mQbJPPD">magnetohydrodynamics</a> approach is commonly utilized in cosmological simulations since it provides a good approximation for cosmological magnetic fields. The effect of magnetic fields on the dynamics of gas is generally negligible on large cosmological scales. Nevertheless, magnetic fields are a critical component of the interstellar medium since they provide pressure support against gravity<a class="footnote-ref" id="fnref:40" href="#fn:40">40</a> and affect the propagation of cosmic rays.<a class="footnote-ref" id="fnref:41" href="#fn:41">41</a>

<h4>Cosmic rays</h4>
Cosmic rays play a significant role in the interstellar medium by contributing to its pressure,<a class="footnote-ref" id="fnref:42" href="#fn:42">42</a> serving as a crucial heating channel,<a class="footnote-ref" id="fnref:43" href="#fn:43">43</a> and potentially driving galactic gas outflows.<a class="footnote-ref" id="fnref:44" href="#fn:44">44</a> The propagation of cosmic rays is highly affected by magnetic fields. So in the simulation, equations describing the cosmic ray energy and flux are coupled to <a href="/facts/Magnetohydrodynamics/7mQbJPPD">magnetohydrodynamics</a> equations.<a class="footnote-ref" id="fnref:45" href="#fn:45">45</a>

<h4>Radiation Hydrodynamics</h4>
Radiation hydrodynamics simulations are computational methods used to study the interaction of radiation with matter. In astrophysical contexts, radiation hydrodynamics is used to study the epoch of reionization when the Universe had high redshift. There are several numerical methods used for radiation hydrodynamics simulations, including ray-tracing, <a href="/facts/Monte_Carlo/uGorqC7k">Monte Carlo</a>, and moment-based methods. Ray-tracing involves tracing the paths of individual photons through the simulation and computing their interactions with matter at each step. This method is computationally expensive but can produce very accurate results.

<h2 id="gallery">Gallery</h2>

<ul><li><a href="/facts/Big_Bang/I5T1vTnv">Big Bang</a> – Physical theory</li>
<li><a href="/facts/Bulge_(astronomy)/cjJ0LFan">Bulge (astronomy)</a> – Tightly packed group of stars within a larger formationPages displaying short descriptions of redirect targets</li>
<li><a href="/facts/Chronology_of_the_universe/ezBKAdjy">Chronology of the universe</a> – History and future of the universe</li>
<li><a href="/facts/Cosmology/yM19zM7Y">Cosmology</a> – Scientific study of the origin, evolution, and eventual fate of the universe</li>
<li><a href="/facts/Galactic_disc/D7GeqnFf">Galactic disc</a> – Component of disc galaxies comprising gas and stars</li>
<li><a href="/facts/Formation_and_evolution_of_the_Solar_System/cgElXHpM">Formation and evolution of the Solar System</a></li>
<li><a href="/facts/Galactic_coordinate_system/Un6BambN">Galactic coordinate system</a> – Celestial coordinate system in spherical coordinates, with the Sun as its center</li>
<li><a href="/facts/Galactic_corona/6PS8BuXm">Galactic corona</a> – Hot, ionised, gaseous component in the Galactic halo</li>
<li><a href="/facts/Galactic_halo/A6jsautY">Galactic halo</a> – Spherical component of a galaxy which extends beyond the main, visible component</li>
<li><a href="/facts/Galactic_orientation/WPDTAuHw">Galactic orientation</a></li>
<li><a href="/facts/Galaxy_rotation_curve/YJyb1Jy3">Galaxy rotation curve</a> – Observed discrepancy in galactic angular momenta</li>
<li><a href="/facts/Illustris_project/6QbkyNgt">Illustris project</a> – Computer-simulated universes</li>
<li><a href="/facts/List_of_galaxies/9PJtf6ld">List of galaxies</a></li>
<li><a href="/facts/Mass_segregation_(astronomy)/e9RDXonL">Mass segregation (astronomy)</a> – Gravitational process, eg in star clusters</li>
<li><a href="/facts/Metallicity_distribution_function/JJ1tBSBv">Metallicity distribution function</a> – Distribution within a group of stars of the ratio of iron to hydrogen in a star</li>
<li><a href="/facts/Pea_galaxy/TeeCcNIk">Pea galaxy</a> – Possible type of luminous blue compact galaxy</li>
<li><a href="/facts/Dark_matter/y5HgX55N">Recent development (2018): Galaxies with little or no dark matter</a> – Concept in cosmology</li>
<li><a href="/facts/Red_nugget/oB58qm1u">Red nugget</a>, small galaxies packed with large amounts of red stars</li>
<li><a href="/facts/Star_formation/SMyfVDY6">Star formation</a> – Process by which dense regions of molecular clouds in interstellar space collapse to form stars</li>
<li><a href="/facts/Structure_formation/1wnrpsKz">Structure formation</a> – Formation of galaxies, galaxy clusters and larger structures from small early density fluctuations</li>
<li><a href="/facts/UniverseMachine/Vk9Ijg42">UniverseMachine</a> – Computer simulated universes</li>
<li><a href="/facts/Zeldovich_pancake/uduwGn5R">Zeldovich pancake</a> – Theoretical condensation of gas out of a primordial density fluctuation following the Big Bang</li></ul>

<h2 id="further-reading">Further reading</h2>
<ul><li>Mo, Houjun; van den Bosch, Frank; <a href="/facts/Simon_White/vs1GKLlI">White, Simon</a> (June 2010), Galaxy Formation and Evolution (1 ed.), <a href="/facts/Cambridge_University_Press/fgEBSSRq">Cambridge University Press</a>, <a href="/facts/ISBN_(identifier)/15AdSPa9">ISBN</a> 978-0521857932</li></ul>

<h2 id="external-links">External links</h2>
<ul><li><a href="http://www.noao.edu/image_gallery/galaxies.html">NOAO gallery of galaxy images</a> <a href="https://web.archive.org/web/20020802193225/http://www.noao.edu/image_gallery/galaxies.html">Archived</a> 2 August 2002 at the <a href="/facts/Wayback_Machine/nmQ3a6JC">Wayback Machine</a>
<ul><li><a href="http://www.noao.edu/image_gallery/html/im0685.html">Image of Andromeda galaxy (M31)</a> <a href="https://web.archive.org/web/20021021025020/http://www.noao.edu/image_gallery/html/im0685.html">Archived</a> 21 October 2002 at the <a href="/facts/Wayback_Machine/nmQ3a6JC">Wayback Machine</a></li></ul></li>
<li><a href="http://www.astro.yale.edu/dokkum/evocalc/">Javascript passive evolution calculator</a> for early type (elliptical) galaxies</li>
<li><a href="http://spacegeek.org/ep4_flash.shtml">Video on the evolution of galaxies by Canadian astrophysicist Doctor P</a></li></ul>

<h2 id="references">References</h2>

<ol>
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</ol>

Galaxy formation and evolution open-in-new

Galaxy formation and evolution