Galaxy

A galaxy is a system of stars, stellar remnants, interstellar gas, dust, and dark matter bound together by gravity.<ref name="sparkegallagher2000" /><ref name=nasa060812 /> The word is derived from the Greek Template:Transliteration ({{#invoke:Lang|lang}}), literally 'milky', a reference to the Milky Way galaxy that contains the Solar System. Galaxies, averaging an estimated 100 million stars,<ref name="SPC-20220211"/> range in size from dwarfs with less than a thousand stars,<ref>Template:Cite journal</ref> to the largest galaxies known – supergiants with one hundred trillion stars, each orbiting its galaxy's centre of mass. Most of the mass in a typical galaxy is in the form of dark matter, with only a few per cent of that mass visible in the form of stars and nebulae. Supermassive black holes are a common feature at the centres of galaxies.

Galaxies are categorised according to their visual morphology as elliptical,<ref name=uf030616 /> spiral, or irregular.<ref name="IRatlas" /> The Milky Way is an example of a spiral galaxy. It is estimated that there are between 200 billion<ref name="jpost" /> (Template:Val) to 2 trillion<ref name="Saunders_2023" /> galaxies in the observable universe. Most galaxies are 1,000 to 100,000 parsecs in diameter (approximately 3,000 to 300,000 light years) and are separated by distances in the order of millions of parsecs (or megaparsecs). For comparison, the Milky Way has a diameter of at least 26,800 parsecs (87,400 ly)<ref name="MilkyWaySize">Template:Cite journal</ref>Template:Efn and is separated from the Andromeda Galaxy, its nearest large neighbour, by just over 750,000 parsecs (2.5 million ly).<ref>Template:Cite journal</ref>

The space between galaxies is filled with a tenuous gas (the intergalactic medium) with an average density of less than one atom per cubic metre. Most galaxies are gravitationally organised into groups, clusters and superclusters. The Milky Way is part of the Local Group, which it dominates along with the Andromeda Galaxy. The group is part of the Virgo Supercluster. At the largest scale, these associations are generally arranged into sheets and filaments surrounded by immense voids.<ref name="camb_lss" /> Both the Local Group and the Virgo Supercluster are contained in a much larger cosmic structure named Laniakea.<ref name=Gibney_2014/> Template:TOC limit

Etymology

The word galaxy was borrowed via French and Medieval Latin from the Greek term for the Milky Way, Template:Transliteration {{#invoke:Lang|lang}} ({{#invoke:Lang|lang}})<ref>Template:Cite book</ref><ref name=oed /> 'milky (circle)', named after its appearance as a milky band of light in the sky.<ref name=waller_hodge2003 /><ref name=konecny2006 /> In the astronomical literature, the capitalised word "Galaxy" is often used to refer to the Milky Way galaxy, to distinguish it from the other galaxies in the universe.Template:Cn

Galaxies were initially discovered telescopically and were known as spiral nebulae. Most 18th- to 19th-century astronomers considered them as either unresolved star clusters or extragalactic nebulae,Template:Rp but their true composition and natures remained a mystery. Observations using larger telescopes of a few nearby bright galaxies, like the Andromeda Galaxy, began resolving them into huge conglomerations of stars, but based simply on the apparent faintness and sheer population of stars, the true distances of these objects placed them well beyond the Milky Way. For this reason they were popularly called island universes. Harlow Shapley began to advocate for the term "galaxy" and against using "universes" and "nebula" for the objects but the very influential Edwin Hubble stuck to nebulae. The nomenclature did not fully change in until Hubble's death in 1953.<ref>Bartusiak, M. (2010). The Day We Found the Universe. United States: Knopf Doubleday Publishing Group.</ref>

Nomenclature

File:Probing the distant past SDSS J1152+3313.tif

Galaxy cluster SDSS J1152+3313. SDSS stands for Sloan Digital Sky Survey, J for Julian epoch, and 1152+3313 for right ascension and declination respectively.

Millions of galaxies have been catalogued, but only a few have well-established names, such as the Andromeda Galaxy, the Magellanic Clouds, the Whirlpool Galaxy, and the Sombrero Galaxy. Astronomers work with numbers from certain catalogues, such as the Messier catalogue, the NGC (New General Catalogue), the IC (Index Catalogue), the CGCG (Catalogue of Galaxies and of Clusters of Galaxies), the MCG (Morphological Catalogue of Galaxies), the UGC (Uppsala General Catalogue of Galaxies), and the PGC (Catalogue of Principal Galaxies, also known as LEDA). All the well-known galaxies appear in one or more of these catalogues but each time under a different number. For example, Messier 109 (or "M109") is a spiral galaxy having the number 109 in the catalogue of Messier. It also has the designations NGC 3992, UGC 6937, CGCG 269–023, MCG +09-20-044, and PGC 37617 (or LEDA 37617), among others.<ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref> Millions of fainter galaxies are known by their identifiers in sky surveys such as the Sloan Digital Sky Survey.<ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref>

Observation history

Milky Way

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Greek philosopher Democritus (450–370 BCE) proposed that the bright band on the night sky known as the Milky Way might consist of distant stars.<ref name="Plutarch"/> Aristotle (384–322 BCE), however, believed the Milky Way was caused by "the ignition of the fiery exhalation of some stars that were large, numerous and close together" and that the "ignition takes place in the upper part of the atmosphere, in the region of the World that is continuous with the heavenly motions."<ref name=Montada/> Neoplatonist philosopher Olympiodorus the Younger (Template:Circa–570 CE) was critical of this view, arguing that if the Milky Way was sublunary (situated between Earth and the Moon) it should appear different at different times and places on Earth, and that it should have parallax, which it did not. In his view, the Milky Way was celestial.<ref name=heidarzadeh23 />

According to Mohani Mohamed, Arabian astronomer Ibn al-Haytham (965–1037) made the first attempt at observing and measuring the Milky Way's parallax,<ref name=Mohamed /> and he thus "determined that because the Milky Way had no parallax, it must be remote from the Earth, not belonging to the atmosphere."<ref name=Bouali_et_al_2008/> Persian astronomer al-Biruni (973–1048) proposed the Milky Way galaxy was "a collection of countless fragments of the nature of nebulous stars."<ref name=al-Biruni/> Andalusian astronomer Avempace (Template:Abbr 1138) proposed that it was composed of many stars that almost touched one another, and appeared to be a continuous image due to the effect of refraction from sublunary material,<ref name=Montada /><ref name="heidarzadeh25" /> citing his observation of the conjunction of Jupiter and Mars as evidence of this occurring when two objects were near.<ref name=Montada /> In the 14th century, Syrian-born Ibn Qayyim al-Jawziyya proposed the Milky Way galaxy was "a myriad of tiny stars packed together in the sphere of the fixed stars."<ref name=Livingston/>

Actual proof of the Milky Way consisting of many stars came in 1610 when the Italian astronomer Galileo Galilei used a telescope to study it and discovered it was composed of a huge number of faint stars.<ref name=Galilei/><ref name="O'Connor_Robertson_2002"/> In 1750, English astronomer Thomas Wright, in his An Original Theory or New Hypothesis of the Universe, correctly speculated that it might be a rotating body of a huge number of stars held together by gravitational forces, akin to the Solar System but on a much larger scale, and that the resulting disk of stars could be seen as a band on the sky from a perspective inside it.Template:EfnTemplate:Sfn<ref name="our_galaxy" /> In his 1755 treatise, Immanuel Kant elaborated on Wright's idea about the Milky Way's structure.<ref name=Kant_1755/>

File:Herschel-Galaxy.png

The shape of the Milky Way as estimated from star counts by William Herschel in 1785; the Solar System was assumed to be near the center.

The first project to describe the shape of the Milky Way and the position of the Sun was undertaken by William Herschel in 1785 by counting the number of stars in different regions of the sky. He produced a diagram of the shape of the galaxy with the Solar System close to the center.<ref name=Herschel_1785/><ref name=paul1993 /> Using a refined approach, Kapteyn in 1920 arrived at the picture of a small (diameter about 15 kiloparsecs) ellipsoid galaxy with the Sun close to the center. A different method by Harlow Shapley based on the cataloguing of globular clusters led to a radically different picture: a flat disk with diameter approximately 70 kiloparsecs and the Sun far from the centre.<ref name="our_galaxy" /> Both analyses failed to take into account the absorption of light by interstellar dust present in the galactic plane; but after Robert Julius Trumpler quantified this effect in 1930 by studying open clusters, the present picture of the Milky Way galaxy emerged.<ref name=Trimble_1999/>

Distinction from other nebulae

A few galaxies outside the Milky Way are visible on a dark night to the unaided eye, including the Andromeda Galaxy, Large Magellanic Cloud, Small Magellanic Cloud, and the Triangulum Galaxy. In the 10th century, Persian astronomer Abd al-Rahman al-Sufi made the earliest recorded identification of the Andromeda Galaxy, describing it as a "small cloud".<ref name="NSOG" /> In 964, he probably mentioned the Large Magellanic Cloud in his Book of Fixed Stars, referring to "Al Bakr of the southern Arabs",<ref name="obspm2"/> since at a declination of about 70° south it was not visible where he lived. It was not well known to Europeans until Magellan's voyage in the 16th century.<ref name="obspm"/><ref name="obspm2"/> The Andromeda Galaxy was later independently noted by Simon Marius in 1612.<ref name="NSOG" />

In 1734, philosopher Emanuel Swedenborg in his Principia speculated that there might be other galaxies outside that were formed into galactic clusters that were minuscule parts of the universe that extended far beyond what could be seen. Swedenborg's views "are remarkably close to the present-day views of the cosmos."<ref name="Gordon2002"/> In 1745, Pierre Louis Maupertuis conjectured that some nebula-like objects were collections of stars with unique properties, including a glow exceeding the light its stars produced on their own, and repeated Johannes Hevelius's view that the bright spots were massive and flattened due to their rotation.<ref name=Kant_1755/> In 1750, Thomas Wright correctly speculated that the Milky Way was a flattened disk of stars, and that some of the nebulae visible in the night sky might be separate Milky Ways.<ref name="our_galaxy"/><ref name=Dyson_1979/>

File:Pic iroberts1.jpg

Photograph of the "Great Andromeda Nebula" by Isaac Roberts, 1899, later identified as the Andromeda Galaxy

Toward the end of the 18th century, Charles Messier compiled a catalog containing the 109 brightest celestial objects having nebulous appearance. Subsequently, William Herschel assembled a catalog of 5,000 nebulae.<ref name="our_galaxy" /> In 1845, Lord Rosse examined the nebulae catalogued by Herschel and observed the spiral structure of Messier object M51, now known as the Whirlpool Galaxy.<ref>Template:Cite magazine</ref><ref>Template:Cite journal</ref>

In 1912, Vesto M. Slipher made spectrographic studies of the brightest spiral nebulae to determine their composition. Slipher discovered that the spiral nebulae have high Doppler shifts, indicating that they are moving at a rate exceeding the velocity of the stars he had measured. He found that the majority of these nebulae are moving away from us.<ref name=Slipher_1913/><ref name=Slipher_1915/>

In 1917, Heber Doust Curtis observed nova S Andromedae within the "Great Andromeda Nebula", as the Andromeda Galaxy, Messier object M31, was then known. Searching the photographic record, he found 11 more novae. Curtis noticed that these novae were, on average, 10 magnitudes fainter than those that occurred within this galaxy. As a result, he was able to come up with a distance estimate of 150,000 parsecs. He became a proponent of the so-called "island universes" hypothesis, which holds that spiral nebulae are actually independent galaxies.<ref>Template:Cite journal</ref>

In 1920 a debate took place between Harlow Shapley and Heber Curtis, the Great Debate, concerning the nature of the Milky Way, spiral nebulae, and the dimensions of the universe. To support his claim that the Great Andromeda Nebula is an external galaxy, Curtis noted the appearance of dark lanes resembling the dust clouds in the Milky Way, as well as the significant Doppler shift.<ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref>

In 1922, the Estonian astronomer Ernst Öpik gave a distance determination that supported the theory that the Andromeda Nebula is indeed a distant extra-galactic object.<ref>Template:Cite journal</ref> Using the new 100-inch Mt. Wilson telescope, Edwin Hubble was able to resolve the outer parts of some spiral nebulae as collections of individual stars and identified some Cepheid variables, thus allowing him to estimate the distance to the nebulae: they were far too distant to be part of the Milky Way.<ref>Template:Cite journal</ref> In 1926 Hubble produced a classification of galactic morphology that is used to this day.<ref>Template:Cite journal</ref><ref>Template:Cite journal</ref>

Multi-wavelength observation

Template:See also Template:Multiple image Advances in astronomy have always been driven by technology. After centuries of success in optical astronomy, recent decades have seen major progress in other regions of the electromagnetic spectrum.<ref>Template:Cite book</ref>

The dust present in the interstellar medium is opaque to visual light. It is more transparent to far-infrared, which can be used to observe the interior regions of giant molecular clouds and galactic cores in great detail.<ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref> Infrared is also used to observe distant, red-shifted galaxies that were formed much earlier. Water vapor and carbon dioxide absorb a number of useful portions of the infrared spectrum, so high-altitude or space-based telescopes are used for infrared astronomy.Template:Sfn

The first non-visual study of galaxies, particularly active galaxies, was made using radio frequencies. The Earth's atmosphere is nearly transparent to radio between 5 MHz and 30 GHz. The ionosphere blocks signals below this range.<ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref> Large radio interferometers have been used to map the active jets emitted from active nuclei.

Ultraviolet and X-ray telescopes can observe highly energetic galactic phenomena. Ultraviolet flares are sometimes observed when a star in a distant galaxy is torn apart from the tidal forces of a nearby black hole.<ref>Template:Cite news</ref> The distribution of hot gas in galactic clusters can be mapped by X-rays. The existence of supermassive black holes at the cores of galaxies was confirmed through X-ray astronomy.<ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref>

Modern research

File:Rotation curve of spiral galaxy Messier 33 (Triangulum).png

Rotation curve of spiral galaxy Messier 33 (yellow and blue points with error bars), and a predicted one from distribution of the visible matter (gray line). The discrepancy between the two curves can be accounted for by adding a dark matter halo surrounding the galaxy.<ref>Template:Cite journal</ref>

In 1944, Hendrik van de Hulst predicted that microwave radiation with wavelength of 21 cm would be detectable from interstellar atomic hydrogen gas;<ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref> and in 1951 it was observed. This radiation is not affected by dust absorption, and so its Doppler shift can be used to map the motion of the gas in this galaxy. These observations led to the hypothesis of a rotating bar structure in the center of this galaxy.<ref>Template:Cite journal</ref> With improved radio telescopes, hydrogen gas could also be traced in other galaxies. In the 1970s, Vera Rubin uncovered a discrepancy between observed galactic rotation speed and that predicted by the visible mass of stars and gas. Today, the galaxy rotation problem is thought to be explained by the presence of large quantities of unseen dark matter.<ref>Template:Cite magazine</ref><ref>Template:Cite journal</ref>

Beginning in the 1990s, the Hubble Space Telescope yielded improved observations. Among other things, its data helped establish that the missing dark matter in this galaxy could not consist solely of inherently faint and small stars.<ref>Template:Cite press release</ref> The Hubble Deep Field, an extremely long exposure of a relatively empty part of the sky, provided evidence that there are about 125 billion (Template:Val) galaxies in the observable universe.<ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref> Improved technology in detecting the spectra invisible to humans (radio telescopes, infrared cameras, and x-ray telescopes) allows detection of other galaxies that are not detected by Hubble. Particularly, surveys in the Zone of Avoidance (the region of sky blocked at visible-light wavelengths by the Milky Way) have revealed a number of new galaxies.<ref>Template:Cite journal</ref>

A 2016 study published in The Astrophysical Journal, led by Christopher Conselice of the University of Nottingham, analyzed many sources of data to estimate that the observable universe (up to z=8) contained at least two trillion (Template:Val) galaxies, a factor of 10 more than are directly observed in Hubble images.<ref name="Conselice">Template:Cite journal</ref>Template:Rp<ref name="NYT-20161017">Template:Cite news</ref> However, later observations with the New Horizons space probe from outside the zodiacal light observed less cosmic optical light than Conselice while still suggesting that direct observations are missing galaxies.<ref name="Lauer"/><ref>Template:Cite news</ref>

Types and morphology

File:Hubble sequence photo.png

Types of galaxies according to the Hubble classification scheme : an E indicates a type of elliptical galaxy; an S is a spiral; and SB is a barred spiral galaxy

Galaxies come in three main types: ellipticals, spirals, and irregulars. A slightly more extensive description of galaxy types based on their appearance is given by the Hubble sequence. Since the Hubble sequence is entirely based upon visual morphological type (shape), it may miss certain important characteristics of galaxies such as star formation rate in starburst galaxies and activity in the cores of active galaxies.<ref name="IRatlas" />

Template:AnchorMany galaxies are thought to contain a supermassive black hole at their center. This includes the Milky Way, whose core region is called the Galactic Center.Template:Sfn

Ellipticals

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The Hubble classification system rates elliptical galaxies on the basis of their ellipticity, ranging from E0, being nearly spherical, up to E7, which is highly elongated. These galaxies have an ellipsoidal profile, giving them an elliptical appearance regardless of the viewing angle. Their appearance shows little structure and they typically have relatively little interstellar matter. Consequently, these galaxies also have a low portion of open clusters and a reduced rate of new star formation. Instead, they are dominated by generally older, more evolved stars that are orbiting the common center of gravity in random directions. The stars contain low abundances of heavy elements because star formation ceases after the initial burst. In this sense they have some similarity to the much smaller globular clusters.<ref name="elliptical">{{#invoke:citation/CS1|citation |CitationClass=web }}</ref>

Type-cD galaxies

File:Galaxy Cluster Abell 1413.jpg

The galaxy cluster Abell 1413 is dominated by this cD elliptical galaxy designated Abell 1413 BCG. It has an isophotal diameter of over 800,000 light-years across. Note the gravitational lensing.

The largest galaxies are the type-cD galaxies. First described in 1964 by a paper by Thomas A. Matthews and others,<ref name=Matthews>Template:Cite journal</ref> they are a subtype of the more general class of D galaxies, which are giant elliptical galaxies, except that they are much larger. They are popularly known as the supergiant elliptical galaxies and constitute the largest and most luminous galaxies known. These galaxies feature a central elliptical nucleus with an extensive, faint halo of stars extending to megaparsec scales.<ref name="NASAVlog">{{#invoke:citation/CS1|citation |CitationClass=web }}</ref> The profile of their surface brightnesses as a function of their radius (or distance from their cores) falls off more slowly than their smaller counterparts.<ref name=Tonry>Template:Cite book</ref>

The formation of these cD galaxies remains an active area of research, but the leading model is that they are the result of the mergers of smaller galaxies in the environments of dense clusters, or even those outside of clusters with random overdensities.<ref>Template:Cite journal</ref> These processes are the mechanisms that drive the formation of fossil groups or fossil clusters, where a large, relatively isolated, supergiant elliptical resides in the middle of the cluster and are surrounded by an extensive cloud of X-rays as the residue of these galactic collisions. Another older model posits the phenomenon of cooling flow, where the heated gases in clusters collapses towards their centers as they cool, forming stars in the process,<ref>Template:Cite journal</ref> a phenomenon observed in clusters such as Perseus,<ref name=Fabian>Template:Cite journal</ref> and more recently in the Phoenix Cluster.<ref>Template:Cite journal</ref>

Shell galaxy

File:NGC 3923 Elliptical Shell Galaxy.jpg

NGC 3923 Elliptical Shell Galaxy (Hubble photograph)

A shell galaxy is a type of elliptical galaxy where the stars in its halo are arranged in concentric shells. About one-tenth of elliptical galaxies have a shell-like structure, which has never been observed in spiral galaxies. These structures are thought to develop when a larger galaxy absorbs a smaller companion galaxy—that as the two galaxy centers approach, they start to oscillate around a center point, and the oscillation creates gravitational ripples forming the shells of stars, similar to ripples spreading on water. For example, galaxy NGC 3923 has over 20 shells.<ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref>

Spirals

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File:M101 hires STScI-PRC2006-10a.jpg

The Pinwheel Galaxy, NGC 5457

Spiral galaxies resemble spiraling pinwheels. Though the stars and other visible material contained in such a galaxy lie mostly on a plane, the majority of mass in spiral galaxies exists in a roughly spherical halo of dark matter which extends beyond the visible component, as demonstrated by the universal rotation curve concept.<ref name="Williams2009">Template:Cite journal</ref>

Spiral galaxies consist of a rotating disk of stars and interstellar medium, along with a central bulge of generally older stars. Extending outward from the bulge are relatively bright arms. In the Hubble classification scheme, spiral galaxies are listed as type S, followed by a letter (a, b, or c) which indicates the degree of tightness of the spiral arms and the size of the central bulge. An Sa galaxy has tightly wound, poorly defined arms and possesses a relatively large core region. At the other extreme, an Sc galaxy has open, well-defined arms and a small core region.<ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref> A galaxy with poorly defined arms is sometimes referred to as a flocculent spiral galaxy; in contrast to the grand design spiral galaxy that has prominent and well-defined spiral arms.<ref name=bergh1998 /> The speed in which a galaxy rotates is thought to correlate with the flatness of the disc as some spiral galaxies have thick bulges, while others are thin and dense.<ref>Template:Cite journal</ref><ref>Template:Cite news4</ref>

File:Hubble2005-01-barred-spiral-galaxy-NGC1300.jpg

NGC 1300, an example of a barred spiral galaxy

In spiral galaxies, the spiral arms do have the shape of approximate logarithmic spirals, a pattern that can be theoretically shown to result from a disturbance in a uniformly rotating mass of stars. Like the stars, the spiral arms rotate around the center, but they do so with constant angular velocity. The spiral arms are thought to be areas of high-density matter, or "density waves".<ref name=bertin_lin1996 /> As stars move through an arm, the space velocity of each stellar system is modified by the gravitational force of the higher density. (The velocity returns to normal after the stars depart on the other side of the arm.) This effect is akin to a "wave" of slowdowns moving along a highway full of moving cars. The arms are visible because the high density facilitates star formation, and therefore they harbor many bright and young stars.<ref name=belkora355 />

File:Hoag's object.jpg

Hoag's Object, an example of a ring galaxy

Barred spiral galaxy

A majority of spiral galaxies, including the Milky Way galaxy, have a linear, bar-shaped band of stars that extends outward to either side of the core, then merges into the spiral arm structure.<ref>Template:Cite journal</ref> In the Hubble classification scheme, these are designated by an SB, followed by a lower-case letter (a, b or c) which indicates the form of the spiral arms (in the same manner as the categorization of normal spiral galaxies). Bars are thought to be temporary structures that can occur as a result of a density wave radiating outward from the core, or else due to a tidal interaction with another galaxy.<ref>Template:Cite journal</ref> Many barred spiral galaxies are active, possibly as a result of gas being channeled into the core along the arms.<ref>Template:Cite journal</ref>

Our own galaxy, the Milky Way, is a large disk-shaped barred-spiral galaxy<ref>Template:Cite journal</ref> about 30 kiloparsecs in diameter and a kiloparsec thick. It contains about two hundred billion (2×10¹¹)<ref>Template:Cite press release</ref> stars and has a total mass of about six hundred billion (6×10¹¹) times the mass of the Sun.<ref>Template:Cite journal</ref>

Super-luminous spiral

Recently, researchers described galaxies called super-luminous spirals. They are very large with an upward diameter of 437,000 light-years (compared to the Milky Way's 87,400 light-year diameter). With a mass of 340 billion solar masses, they generate a significant amount of ultraviolet and mid-infrared light. They are thought to have an increased star formation rate around 30 times faster than the Milky Way.<ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref><ref>Template:Cite journal</ref>

Other morphologies

• Peculiar galaxies are galactic formations that develop unusual properties due to tidal interactions with other galaxies.
  • A ring galaxy has a ring-like structure of stars and interstellar medium surrounding a bare core. A ring galaxy is thought to occur when a smaller galaxy passes through the core of a spiral galaxy.<ref>Template:Cite journal</ref> Such an event may have affected the Andromeda Galaxy, as it displays a multi-ring-like structure when viewed in infrared radiation.<ref>Template:Cite press release</ref>
• A lenticular galaxy is an intermediate form that has properties of both elliptical and spiral galaxies. These are categorized as Hubble type S0, and they possess ill-defined spiral arms with an elliptical halo of stars<ref>Template:Cite press release</ref> (barred lenticular galaxies receive Hubble classification SB0).
• Irregular galaxies are galaxies that can not be readily classified into an elliptical or spiral morphology.
  • An Irr-I galaxy has some structure but does not align cleanly with the Hubble classification scheme.
  • Irr-II galaxies do not possess any structure that resembles a Hubble classification, and may have been disrupted.<ref>{{#invoke:citation/CS1|citation

|CitationClass=web }}</ref> Nearby examples of (dwarf) irregular galaxies include the Magellanic Clouds.Template:Sfn

• A dark or "ultra diffuse" galaxy is an extremely-low-luminosity galaxy. It may be the same size as the Milky Way, but have a visible star count only one percent of the Milky Way's. Multiple mechanisms for producing this type of galaxy have been proposed, and it is possible that different dark galaxies formed by different means.<ref>Template:Cite journal</ref> One candidate explanation for the low luminosity is that the galaxy lost its star-forming gas at an early stage, resulting in old stellar populations.<ref name="NYT-20240126">Template:Cite news</ref><ref>Template:Cite journal</ref>

Dwarfs

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Despite the prominence of large elliptical and spiral galaxies, most galaxies are dwarf galaxies.<ref name=Mateo19989/> They are relatively small when compared with other galactic formations, being about one hundredth the size of the Milky Way, with only a few billion stars. Blue compact dwarf galaxies contains large clusters of young, hot, massive stars. Ultra-compact dwarf galaxies have been discovered that are only 100 parsecs across.<ref>Template:Cite journal</ref>

Many dwarf galaxies may orbit a single larger galaxy; the Milky Way has at least a dozen such satellites, with an estimated 300–500 yet to be discovered.<ref>Template:Cite magazine</ref> Most of the information we have about dwarf galaxies come from observations of the local group, containing two spiral galaxies, the Milky Way and Andromeda, and many dwarf galaxies. These dwarf galaxies are classified as either irregular or dwarf elliptical/dwarf spheroidal galaxies.<ref name=Mateo19989>Template:Cite journal</ref>

A study of 27 Milky Way neighbors found that in all dwarf galaxies, the central mass is approximately 10 million solar masses, regardless of whether it has thousands or millions of stars. This suggests that galaxies are largely formed by dark matter, and that the minimum size may indicate a form of warm dark matter incapable of gravitational coalescence on a smaller scale.<ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref>

Variants

Interacting

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File:Antennae galaxies xl.jpg

The Antennae Galaxies are undergoing a collision that will result in their eventual merger.

Interactions between galaxies are relatively frequent, and they can play an important role in galactic evolution. Near misses between galaxies result in warping distortions due to tidal interactions, and may cause some exchange of gas and dust.<ref name="umda">{{#invoke:citation/CS1|citation |CitationClass=web }}</ref><ref name="suia">{{#invoke:citation/CS1|citation |CitationClass=web }}</ref> Collisions occur when two galaxies pass directly through each other and have sufficient relative momentum not to merge. The stars of interacting galaxies usually do not collide, but the gas and dust within the two forms interacts, sometimes triggering star formation. A collision can severely distort the galaxies' shapes, forming bars, rings or tail-like structures.<ref name="umda" /><ref name="suia" />

At the extreme of interactions are galactic mergers, where the galaxies' relative momentums are insufficient to allow them to pass through each other. Instead, they gradually merge to form a single, larger galaxy. Mergers can result in significant changes to the galaxies' original morphology. If one of the galaxies is much more massive than the other, the result is known as cannibalism, where the more massive larger galaxy remains relatively undisturbed, and the smaller one is torn apart. The Milky Way galaxy is currently in the process of cannibalizing the Sagittarius Dwarf Elliptical Galaxy and the Canis Major Dwarf Galaxy.<ref name="umda" /><ref name="suia" />

Starburst

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File:M82 HST ACS 2006-14-a-large web.jpg

M82, a starburst galaxy that has ten times the star formation of a "normal" galaxy<ref>Template:Cite press release</ref>

Stars are created within galaxies from a reserve of cold gas that forms giant molecular clouds. Some galaxies have been observed to form stars at an exceptional rate, which is known as a starburst. If they continue to do so, they would consume their reserve of gas in a time span less than the galaxy's lifespan. Hence starburst activity usually lasts only about ten million years, a relatively brief period in a galaxy's history. Starburst galaxies were more common during the universe's early history,<ref name="chandra">{{#invoke:citation/CS1|citation |CitationClass=web }}</ref> but still contribute an estimated 15% to total star production.<ref>Template:Cite conference</ref>

Starburst galaxies are characterized by dusty concentrations of gas and the appearance of newly formed stars, including massive stars that ionize the surrounding clouds to create H II regions.<ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref> These stars produce supernova explosions, creating expanding remnants that interact powerfully with the surrounding gas. These outbursts trigger a chain reaction of star-building that spreads throughout the gaseous region. Only when the available gas is nearly consumed or dispersed does the activity end.<ref name="chandra" />

Starbursts are often associated with merging or interacting galaxies. The prototype example of such a starburst-forming interaction is M82, which experienced a close encounter with the larger M81. Irregular galaxies often exhibit spaced knots of starburst activity.<ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref>

Radio galaxy

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File:A Multi-Wavelength View of Radio Galaxy Hercules A.jpg

Hercules A, supergiant elliptical radio galaxy

A radio galaxy is a galaxy with giant regions of radio emission extending well beyond its visible structure. These energetic radio lobes are powered by jets from its active galactic nucleus.<ref name="JonesAdamsLambourne20042">Template:Cite book</ref> Radio galaxies are classified according to their Fanaroff–Riley classification. The FR I class have lower radio luminosity and exhibit structures which are more elongated; the FR II class are higher radio luminosity. The correlation of radio luminosity and structure suggests that the sources in these two types of galaxies may differ.<ref>Template:Cite book</ref>

Radio galaxies can also be classified as giant radio galaxies (GRGs), whose radio emissions can extend to scales of megaparsecs (3.26 million light-years). Alcyoneus is an FR II class low-excitation radio galaxy which has the largest observed radio emission, with lobed structures spanning 5 megaparsecs (16×10⁶ ly). For comparison, another similarly sized giant radio galaxy is 3C 236, with lobes 15 million light-years across. It should however be noted that radio emissions are not always considered part of the main galaxy itself.<ref name="University_of_Maryland">{{#invoke:citation/CS1|citation |CitationClass=web }}</ref>

A giant radio galaxy is a special class of objects characterized by the presence of radio lobes generated by relativistic jets powered by the central galaxy's supermassive black hole. Giant radio galaxies are different from ordinary radio galaxies in that they can extend to much larger scales, reaching upwards to several megaparsecs across, far larger than the diameters of their host galaxies.<ref>Template:Cite journal</ref>

A "normal" radio galaxy do not have a source that is a supermassive black hole or monster neutron star; instead the source is synchrotron radiation from relativistic electrons accelerated by supernova. These sources are comparatively short lived, making the radio spectrum from normal radio galaxies an especially good way to study star formation.<ref>Template:Cite journal</ref>

Active galaxy

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File:M87 jet.jpg

A jet of particles is being emitted from the core of the elliptical radio galaxy M87.

Some observable galaxies are classified as "active" if they contain an active galactic nucleus (AGN).Template:Sfn A significant portion of the galaxy's total energy output is emitted by the active nucleus instead of its stars, dust and interstellar medium. There are multiple classification and naming schemes for AGNs, but those in the lower ranges of luminosity are called Seyfert galaxies, while those with luminosities much greater than that of the host galaxy are known as quasi-stellar objects or quasars. Models of AGNs suggest that a significant fraction of their light is shifted to far-infrared frequencies because optical and UV emission in the nucleus is absorbed and remitted by dust and gas surrounding it.<ref>Template:Cite journal</ref>

The standard model for an active galactic nucleus is based on an accretion disc that forms around a supermassive black hole (SMBH) at the galaxy's core region. The radiation from an active galactic nucleus results from the gravitational energy of matter as it falls toward the black hole from the disc.Template:Sfn<ref name="keel">{{#invoke:citation/CS1|citation |CitationClass=web }}</ref> The AGN's luminosity depends on the SMBH's mass and the rate at which matter falls onto it. In about 10% of these galaxies, a diametrically opposed pair of energetic jets ejects particles from the galaxy core at velocities close to the speed of light. The mechanism for producing these jets is not well understood.<ref name="monster">{{#invoke:citation/CS1|citation |CitationClass=web }}</ref>

Seyfert galaxy

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Seyfert galaxies are one of the two largest groups of active galaxies, along with quasars. They have quasar-like nuclei (very luminous, distant and bright sources of electromagnetic radiation) with very high surface brightnesses; but unlike quasars, their host galaxies are clearly detectable.<ref name=Peterson1997>Template:Cite book</ref> Seen through a telescope, a Seyfert galaxy appears like an ordinary galaxy with a bright star superimposed atop the core. Seyfert galaxies are divided into two principal subtypes based on the frequencies observed in their spectra.<ref>Template:Cite journal</ref>

Quasar

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Quasars are the most energetic and distant members of active galactic nuclei. Extremely luminous, they were first identified as high redshift sources of electromagnetic energy, including radio waves and visible light, that appeared more similar to stars than to extended sources similar to galaxies. Their luminosity can be 100 times that of the Milky Way.Template:Sfn The nearest known quasar, Markarian 231, is about 581 million light-years from Earth,<ref>Template:Cite journal</ref> while others have been discovered as far away as UHZ1, roughly 13.2 billion light-years distant.<ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref><ref>Template:Cite journal</ref> Quasars are noteworthy for providing the first demonstration of the phenomenon that gravity can act as a lens for light.<ref>Template:Cite journal</ref>

Other AGNs

Blazars are believed to be active galaxies with a relativistic jet pointed in the direction of Earth. A radio galaxy emits radio frequencies from relativistic jets. A unified model of these types of active galaxies explains their differences based on the observer's position.<ref name="monster" />

Possibly related to active galactic nuclei (as well as starburst regions) are low-ionization nuclear emission-line regions (LINERs). The emission from LINER-type galaxies is dominated by weakly ionized elements. The excitation sources for the weakly ionized lines include post-AGB stars, AGN, and shocks.<ref name="heckman1980">Template:Cite journal</ref> Approximately one-third of nearby galaxies are classified as containing LINER nuclei.<ref name="keel" /><ref name="heckman1980" /><ref name="hoetal1997b">Template:Cite journal</ref>

Luminous infrared galaxy

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Luminous infrared galaxies (LIRGs) are galaxies with luminosities—the measurement of electromagnetic power output—above 10¹¹ L☉ (solar luminosities). In most cases, most of their energy comes from large numbers of young stars which heat surrounding dust, which reradiates the energy in the infrared. Luminosity high enough to be a LIRG requires a star formation rate of at least 18 M☉ yr⁻¹. Ultra-luminous infrared galaxies (ULIRGs) are at least ten times more luminous still and form stars at rates >180 M☉ yr⁻¹. Many LIRGs also emit radiation from an AGN.<ref>Template:Cite journal</ref><ref name=":0">Template:Cite journal</ref> Infrared galaxies emit more energy in the infrared than all other wavelengths combined, with peak emission typically at wavelengths of 60 to 100 microns. LIRGs are believed to be created from the strong interaction and merger of spiral galaxies.<ref>Template:Cite journal</ref> While uncommon in the local universe, LIRGs and ULIRGS were more prevalent when the universe was younger.<ref name=":0" />

Physical diameters

Galaxies do not have a definite boundary by their nature, and are characterized by a gradually decreasing stellar density as a function of increasing distance from their center, making measurements of their true extents difficult. Nevertheless, astronomers over the past few decades have made several criteria in defining the sizes of galaxies.

Angular diameter

As early as the time of Edwin Hubble in 1936, there have been attempts to characterize the diameters of galaxies. The earliest efforts were based on the observed angle subtended by the galaxy and its estimated distance, leading to an angular diameter (also called "metric diameter").Template:Sfn

Isophotal diameter

The isophotal diameter is introduced as a conventional way of measuring a galaxy's size based on its apparent surface brightness.<ref name=Chamba>Template:Cite journal</ref> Isophotes are curves in a diagram - such as a picture of a galaxy - that adjoins points of equal brightnesses, and are useful in defining the extent of the galaxy. The apparent brightness flux of a galaxy is measured in units of magnitudes per square arcsecond (mag/arcsec²; sometimes expressed as mag arcsec⁻²), which defines the brightness depth of the isophote. To illustrate how this unit works, a typical galaxy has a brightness flux of 18 mag/arcsec² at its central region. This brightness is equivalent to the light of an 18th magnitude hypothetical point object (like a star) being spread out evenly in a one square arcsecond area of the sky.<ref name="UMD_Week_6">{{#invoke:citation/CS1|citation |CitationClass=web }}</ref> The isophotal diameter is typically defined as the region enclosing all the light down to 25 mag/arcsec² in the blue B-band,<ref name="sparkegallagher2000_131"/> which is then referred to as the D₂₅ standard.<ref>Template:Cite journal</ref>

Examples of isophotal diameters (25.0 B-mag/arcsec² isophote)

galaxy	diameter	reference
Large Magellanic Cloud	Template:Convert	citation	CitationClass=web }}</ref>
Milky Way	Template:Convert	<ref name="MilkyWaySize"/>
Messier 87	Template:Convert	<ref>{{#invoke:citation/CS1|citation	CitationClass=web }}</ref>
Andromeda Galaxy	Template:Convert	citation	CitationClass=web }}</ref>

Effective radius (half-light) and its variations

The half-light radius (also known as effective radius; R_e) is a measure that is based on the galaxy's overall brightness flux. This is the radius upon which half, or 50%, of the total brightness flux of the galaxy was emitted. This was first proposed by Gérard de Vaucouleurs in 1948.<ref name=Vaucouleurs>Template:Cite journal</ref> The choice of using 50% was arbitrary, but proved to be useful in further works by R. A. Fish in 1963,<ref name=Fish>Template:Cite journal</ref> where he established a luminosity concentration law that relates the brightnesses of elliptical galaxies and their respective R_e, and by José Luis Sérsic in 1968<ref name=Sersic>Template:Cite journal</ref> that defined a mass-radius relation in galaxies.<ref name=Chamba/>

In defining R_e, it is necessary that the overall brightness flux galaxy should be captured, with a method employed by Bershady in 2000 suggesting to measure twice the size where the brightness flux of an arbitrarily chosen radius, defined as the local flux, divided by the overall average flux equals to 0.2.<ref name=Bershady>Template:Cite journal</ref> Using half-light radius allows a rough estimate of a galaxy's size, but is not particularly helpful in determining its morphology.<ref name=SpiralDisks>Template:Cite journal</ref>

Variations of this method exist. In particular, in the ESO-Uppsala Catalogue of Galaxies values of 50%, 70%, and 90% of the total blue light (the light detected through a B-band specific filter) had been used to calculate a galaxy's diameter.<ref name=ESO>Template:Cite book</ref>

Petrosian magnitude

First described by Vahe Petrosian in 1976,<ref name=Petrosian>Template:Cite journal</ref> a modified version of this method has been used by the Sloan Digital Sky Survey (SDSS). This method employs a mathematical model on a galaxy whose radius is determined by the azimuthally (horizontal) averaged profile of its brightness flux. In particular, the SDSS employed the Petrosian magnitude in the R-band (658 nm, in the red part of the visible spectrum) to ensure that the brightness flux of a galaxy would be captured as much as possible while counteracting the effects of background noise. For a galaxy whose brightness profile is exponential, it is expected to capture all of its brightness flux, and 80% for galaxies that follow a profile that follows de Vaucouleurs's law.<ref name="sdss">{{#invoke:citation/CS1|citation |CitationClass=web }}</ref>

Petrosian magnitudes have the advantage of being redshift and distance independent, allowing the measurement of the galaxy's apparent size since the Petrosian radius is defined in terms of the galaxy's overall luminous flux.<ref name="Graham" />

A critique of an earlier version of this method has been issued by the Infrared Processing and Analysis Center,<ref name=ipac1>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref> with the method causing a magnitude of error (upwards to 10%) of the values than using isophotal diameter. The use of Petrosian magnitudes also have the disadvantage of missing most of the light outside the Petrosian aperture, which is defined relative to the galaxy's overall brightness profile, especially for elliptical galaxies, with higher signal-to-noise ratios on higher distances and redshifts.<ref name=Ned2>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref> A correction for this method has been issued by Graham et al. in 2005, based on the assumption that galaxies follow Sérsic's law.<ref name=Graham>Template:Cite journal</ref>

Near-infrared method

This method has been used by 2MASS as an adaptation from the previously used methods of isophotal measurement. Since 2MASS operates in the near infrared, which has the advantage of being able to recognize dimmer, cooler, and older stars, it has a different form of approach compared to other methods that normally use B-filter. The detail of the method used by 2MASS has been described thoroughly in a document by Jarrett et al., with the survey measuring several parameters.<ref name=Jarrett>Template:Cite journal</ref>

The standard aperture ellipse (area of detection) is defined by the infrared isophote at the K_s band (roughly 2.2 μm wavelength) of 20 mag/arcsec². Gathering the overall luminous flux of the galaxy has been employed by at least four methods: the first being a circular aperture extending 7 arcseconds from the center, an isophote at 20 mag/arcsec², a "total" aperture defined by the radial light distribution that covers the supposed extent of the galaxy, and the Kron aperture (defined as 2.5 times the first-moment radius, an integration of the flux of the "total" aperture).<ref name=Jarrett />

Larger-scale structures

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Deep-sky surveys show that galaxies are often found in groups and clusters. Solitary galaxies that have not significantly interacted with other galaxies of comparable mass in the past few billion years are relatively scarce.<ref>Template:Cite journal</ref> Only about 5% of the galaxies surveyed are isolated in this sense.<ref>Template:Cite journal</ref><ref>Template:Cite journal</ref> However, they may have interacted and even merged with other galaxies in the past,<ref>Template:Cite journal</ref> and may still be orbited by smaller satellite galaxies.<ref>Template:Cite journal</ref>

On the largest scale, the universe is continually expanding, resulting in an average increase in the separation between individual galaxies (see Hubble's law). Associations of galaxies can overcome this expansion on a local scale through their mutual gravitational attraction. These associations formed early, as clumps of dark matter pulled their respective galaxies together. Nearby groups later merged to form larger-scale clusters. This ongoing merging process, as well as an influx of infalling gas, heats the intergalactic gas in a cluster to very high temperatures of 30–100 megakelvins.<ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref> About 70–80% of a cluster's mass is in the form of dark matter, with 10–30% consisting of this heated gas and the remaining few percent in the form of galaxies.<ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref>

Most galaxies are gravitationally bound to a number of other galaxies. These form a fractal-like hierarchical distribution of clustered structures, with the smallest such associations being termed groups. A group of galaxies is the most common type of galactic cluster; these formations contain the majority of galaxies (as well as most of the baryonic mass) in the universe.<ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref><ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref> To remain gravitationally bound to such a group, each member galaxy must have a sufficiently low velocity to prevent it from escaping (see Virial theorem). If there is insufficient kinetic energy, however, the group may evolve into a smaller number of galaxies through mergers.<ref>Template:Cite journal</ref>

Clusters of galaxies consist of hundreds to thousands of galaxies bound together by gravity.<ref name="Hubble protocluster">Template:Cite press release</ref> Clusters of galaxies are often dominated by a single giant elliptical galaxy, known as the brightest cluster galaxy, which, over time, tidally destroys its satellite galaxies and adds their mass to its own.<ref>Template:Cite journal</ref>

File:The southern plane of the Milky Way from the ATLASGAL survey.jpg

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Superclusters contain tens of thousands of galaxies, which are found in clusters, groups and sometimes individually. At the supercluster scale, galaxies are arranged into sheets and filaments surrounding vast empty voids.<ref>Template:Cite journal</ref> Above this scale, the universe appears to be the same in all directions (isotropic and homogeneous),<ref>Template:Cite journal</ref> though this notion has been challenged in recent years by numerous findings of large-scale structures that appear to be exceeding this scale. The Hercules–Corona Borealis Great Wall, currently the largest structure in the universe found so far, is 10 billion light-years (three gigaparsecs) in length.<ref name=HBHT2>Template:Cite journal</ref><ref name=HBHT>Template:Cite journal</ref><ref name=cookie>Template:Cite journal</ref>

The Milky Way galaxy is a member of an association named the Local Group, a relatively small group of galaxies that has a diameter of approximately one megaparsec. The Milky Way and the Andromeda Galaxy are the two brightest galaxies within the group; many of the other member galaxies are dwarf companions of these two.<ref>Template:Cite journal</ref> The Local Group itself is a part of a cloud-like structure within the Virgo Supercluster, a large, extended structure of groups and clusters of galaxies centered on the Virgo Cluster.<ref name="tully1982">Template:Cite journal</ref> In turn, the Virgo Supercluster is a portion of the Laniakea Supercluster.<ref>Template:Cite journal</ref>

Magnetic fields

Galaxies have magnetic fields of their own. A galaxy's magnetic field influences its dynamics in multiple ways, including affecting the formation of spiral arms and transporting angular momentum in gas clouds. The latter effect is particularly important, as it is a necessary factor for the gravitational collapse of those clouds, and thus for star formation.<ref name="galactic_magnetic_fields">Template:Cite journal</ref>

The typical average equipartition strength for spiral galaxies is about 10 μG (microgauss) or 1Template:NbspnT (nanotesla). By comparison, the Earth's magnetic field has an average strength of about 0.3 G (Gauss) or 30 μT (microtesla). Radio-faint galaxies like M 31 and M33, the Milky Way's neighbors, have weaker fields (about 5Template:NbspμG), while gas-rich galaxies with high star-formation rates, like M 51, M 83 and NGC 6946, have 15 μG on average. In prominent spiral arms, the field strength can be up to 25 μG, in regions where cold gas and dust are also concentrated. The strongest total equipartition fields (50–100 μG) were found in starburst galaxies—for example, in M 82 and the Antennae; and in nuclear starburst regions, such as the centers of NGC 1097 and other barred galaxies.<ref name="galactic_magnetic_fields"/>

Formation and evolution

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Formation

File:Artist's impression of a protocluster forming in the early Universe.jpg

Artist's impression of a protocluster forming in the early universe<ref>Template:Cite press release</ref>

Current models of the formation of galaxies in the early universe are based on the ΛCDM model. About 300,000 years after the Big Bang, atoms of hydrogen and helium began to form, in an event called recombination. Nearly all the hydrogen was neutral (non-ionized) and readily absorbed light, and no stars had yet formed. As a result, this period has been called the "dark ages". It was from density fluctuations (or anisotropic irregularities) in this primordial matter that larger structures began to appear. As a result, masses of baryonic matter started to condense within cold dark matter halos.<ref name="hqrdvj">{{#invoke:citation/CS1|citation |CitationClass=web }}</ref><ref name=rmaa17_107 /> These primordial structures allowed gasses to condense in to protogalaxies, large scale gas clouds that were precursors to the first galaxies.<ref name=DayalFerrara2018>Template:Cite journal</ref>Template:Rp

As gas falls in to the gravity of the dark matter halos, its pressure and temperature rise. To condense further, the gas must radiate energy. This process was slow in the early universe dominated by hydrogen atoms and molecules which are inefficient radiators compared to heavier elements. As clumps of gas aggregate forming rotating disks, temperatures and pressures continue to increase. Some places within the disk reach high enough density to form stars.

File:Young Galaxy Accreting Material.jpg

Artist impression of a young galaxy accreting material

Once protogalaxies began to form and contract, the first halo stars, called Population III stars, appeared within them.<ref name=KlessenGlover2023>Template:Cite journal</ref> These were composed of primordial gas, almost entirely of hydrogen and helium. Emission from the first stars heats the remaining gas helping to trigger additional star formation; the ultraviolet light emission from the first generation of stars re-ionized the surrounding neutral hydrogen in expanding spheres eventually reaching the entire universe, an event called reionization.<ref>Template:Cite journal</ref> The most massive stars collapse in violent supernova explosions releasing heavy elements ("metals") into the interstellar medium.<ref name="NYT-20150617">Template:Cite news</ref><ref name=DayalFerrara2018/>Template:Rp This metal content is incorporated into population II stars.

Theoretical models for early galaxy formation have been verified and informed by a large number and variety of sophisticated astronomical observations.<ref name=DayalFerrara2018/>Template:Rp The photometric observations generally need spectroscopic confirmation due the large number mechanisms that can introduce systematic errors. For example, a high redshift (z ~ 16) photometric observation by James Webb Space Telescope (JWST) was later corrected to be closer to z ~ 5.<ref name=ConfirmRefute>Template:Cite journal</ref> Nevertheless, confirmed observations from the JWST and other observatories are accumulating, allowing systematic comparison of early galaxies to predictions of theory.<ref>Template:Cite journal</ref>

Evidence for individual Population III stars in early galaxies is even more challenging. Even seemingly confirmed spectroscopic evidence may turn out to have other origins. For example, astronomers reported He_II emission evidence for Population III stars in the Cosmos Redshift 7 galaxy, with a redshift value of 6.60.<ref name="AJ-20150604">Template:Cite journal</ref> Subsequent observations<ref>Template:Cite journal</ref> found metallic emission lines, O_III, inconsistent with an early-galaxy star.<ref name=KlessenGlover2023/>Template:Rp

File:Signatures of the Earliest Galaxies.jpg

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Evolution

Once stars begin to form, emit radiation, and in some cases explode, the process of galaxy formation becomes very complex, involving interactions between the forces of gravity, radiation, and thermal energy. Many details are still poorly understood.Template:Sfn

Within a billion years of a galaxy's formation, key structures begin to appear.<ref name="SA-20221206">Template:Cite news</ref> Globular clusters, the central supermassive black hole, and a galactic bulge of metal-poor Population II stars form. The creation of a supermassive black hole appears to play a key role in actively regulating the growth of galaxies by limiting the total amount of additional matter added.<ref>Template:Cite press release</ref> During this early epoch, galaxies undergo a major burst of star formation.<ref>Template:Cite news</ref>

During the following two billion years, the accumulated matter settles into a galactic disc.<ref>Template:Cite journal</ref> A galaxy will continue to absorb infalling material from high-velocity clouds and dwarf galaxies throughout its life.<ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref> This matter is mostly hydrogen and helium. The cycle of stellar birth and death slowly increases the abundance of heavy elements, eventually allowing the formation of planets.<ref>Template:Cite conference</ref> Template:Multiple image

Star formation rates in galaxies depend upon their local environment. Isolated 'void' galaxies have highest rate per stellar mass, with 'field' galaxies associated with spiral galaxies having lower rates and galaxies in dense cluster having the lowest rates.<ref>Template:Cite journal</ref>

The evolution of galaxies can be significantly affected by interactions and collisions. Mergers of galaxies were common during the early epoch, and the majority of galaxies were peculiar in morphology.<ref name="sa296">Template:Cite magazine</ref> Given the distances between the stars, the great majority of stellar systems in colliding galaxies will be unaffected. However, gravitational stripping of the interstellar gas and dust that makes up the spiral arms produces a long train of stars known as tidal tails. Examples of these formations can be seen in NGC 4676<ref>Template:Cite press release</ref> or the Antennae Galaxies.<ref>Template:Cite journal</ref>

The Milky Way galaxy and the nearby Andromeda Galaxy are moving toward each other at about 130 km/s, and—depending upon the lateral movements—the two might collide in about five to six billion years. Although the Milky Way has never collided with a galaxy as large as Andromeda before, it has collided and merged with other galaxies in the past.<ref name="Buser">Template:Cite journal</ref> Cosmological simulations indicate that, 11 billion years ago, it merged with a particularly large galaxy that has been labeled the Kraken.<ref>Template:Cite journal</ref><ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref>

Such large-scale interactions are rare. As time passes, mergers of two systems of equal size become less common. Most bright galaxies have remained fundamentally unchanged for the last few billion years, and the net rate of star formation probably also peaked about ten billion years ago.<ref>Template:Cite journal</ref>

Future trends

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Spiral galaxies, like the Milky Way, produce new generations of stars as long as they have dense molecular clouds of interstellar hydrogen in their spiral arms.<ref>Template:Cite journal</ref> Elliptical galaxies are largely devoid of this gas, and so form few new stars.<ref>Template:Cite book</ref> The supply of star-forming material is finite; once stars have converted the available supply of hydrogen into heavier elements, new star formation will come to an end.<ref name="cosmic_battle">{{#invoke:citation/CS1|citation |CitationClass=web }}</ref><ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref>

The current era of star formation is expected to continue for up to one hundred billion years, and then the "stellar age" will wind down after about ten trillion to one hundred trillion years (10¹³–10¹⁴ years), as the smallest, longest-lived stars in the visible universe, tiny red dwarfs, begin to fade. At the end of the stellar age, galaxies will be composed of compact objects: brown dwarfs, white dwarfs that are cooling or cold ("black dwarfs"), neutron stars, and black holes. Eventually, as a result of gravitational relaxation, all stars will either fall into central supermassive black holes or be flung into intergalactic space as a result of collisions.<ref name="cosmic_battle" /><ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref>

Gallery

• Hubble-Space-Telescope-Galaxy-Collection.jpg

  Galaxies (left/top, right/bottom): Template:Small

• PHANGS image mosaic.jpg

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• Andromeda Galaxy M31 - Heic1502a Full resolution.jpg

  Zooming In on the Andromeda Galaxy – A mosaic of the Andromeda Galaxy and the largest image ever released by the Hubble Space Telescope

See also

• Bright early galaxies
• Dark galaxy
• Galactic orientation
• Galaxy formation and evolution
• Illustris project
• List of galaxies
• List of the most distant astronomical objects
• List of nearest galaxies
• List of largest galaxies
• Low surface brightness galaxy
• Outline of galaxies
• Timeline of knowledge about galaxies, clusters of galaxies, and large-scale structure

Bibliography

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External links

• NASA/IPAC Extragalactic Database (NED)
• NED Redshift-Independent Distances
• Template:In Our Time
• An Atlas of The Universe
• Galaxies – Information and amateur observations
• Galaxy Zoo – citizen science galaxy classification project
• "A Flight Through the Universe, by the Sloan Digital Sky Survey" – animated video from Berkeley Lab