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{{About|the astronomical structure|our galaxy|Milky Way|other uses}}{{short description|Gravitationally bound astronomical structure}}{{pp-vand|small=yes}}{{Use mdy dates|date=February 2015}}{{Multiple image |direction=vertical |align=right |width=310|image1=NGC 4414 (NASA-med).jpg|caption1=NGC 4414, a typical spiral galaxy in the constellation Coma Berenices, is about 55,000 light-years in diameter and approximately 60 million light-years from Earth.}}A galaxy is a gravitationally bound system of stars, stellar remnants, interstellar gas, dust, and dark matter. The word galaxy is derived from the Greek {{transl|grc|galaxias}} (), literally "milky", a reference to the Milky Way. Galaxies range in size from dwarfs with just a few hundred million ({{10^|8}}) stars to giants with one hundred trillion ({{10^|14}}) stars, each orbiting its galaxy's center of mass.Galaxies are categorized according to their visual morphology as elliptical, spiral, or irregular. Many galaxies are thought to have supermassive black holes at their centers. The Milky Way's central black hole, known as Sagittarius A*, has a mass four million times greater than the Sun. As of March 2016, GN-z11 is the oldest and most distant observed galaxy with a comoving distance of 32 billion light-years from Earth, and observed as it existed just 400 million years after the Big Bang.Research released in 2016 revised the number of galaxies in the observable universe from a previous estimate of 200 billion ({{val|2e11}}) to a suggested 2 trillion ({{val|2e12}}) or moreNEWS, Fountain, Henry, Two Trillion Galaxies, at the Very Least,weblink 17 October 2016, The New York Times, 17 October 2016, and, overall, as many as an estimated {{val|1e24}} starsWEB, Staff, How Many Stars Are There In The Universe?,weblink 2019, European Space Agency, 21 September 2019, JOURNAL, The Structure of the Universe, 10.1007/978-1-4614-8730-2_10, (more stars than all the grains of sand on planet Earth).WEB, Mackie, Glen, To see the Universe in a Grain of Taranaki Sand,weblink 1 February 2002, Centre for Astrophysics and Supercomputing, 28 January 2017, Most of the galaxies are 1,000 to 100,000 parsecs in diameter (approximately 3000 to 300,000 light years) and separated by distances on the order of millions of parsecs (or megaparsecs). For comparison, the Milky Way has a diameter of at least 30,000 parsecs (100,000 ly) and is separated from the Andromeda Galaxy, its nearest large neighbor, by 780,000 parsecs (2.5 million ly.)The space between galaxies is filled with a tenuous gas (the intergalactic medium) having an average density of less than one atom per cubic meter. The majority of galaxies are gravitationally organized into groups, clusters, and superclusters. The Milky Way is part of the Local Group, which is dominated by it and the Andromeda Galaxy and is part of the Virgo Supercluster. At the largest scale, these associations are generally arranged into sheets and filaments surrounded by immense voids. The largest structure of galaxies yet recognised is a cluster of superclusters that has been named Laniakea, which contains the Virgo supercluster.JOURNAL, Gibney, Elizabeth, 2014, Earth's new address: 'Solar System, Milky Way, Laniakea', Nature, 10.1038/nature.2014.15819, {{TOC limit|3}}


The word galaxy was borrowed via French and Medieval Latin from the Greek term for the Milky Way, {{transl|grc|galaxías (kúklos)}} }} (}})C. T. Onions et al., The Oxford Dictionary of English Etymology, Oxford 1966, p. 385. ‘milky (circle)’, named after its appearance as a milky band of light in the sky. In Greek mythology, Zeus places his son born by a mortal woman, the infant Heracles, on Hera's breast while she is asleep so that the baby will drink her divine milk and will thus become immortal. Hera wakes up while breastfeeding and then realizes she is nursing an unknown baby: she pushes the baby away, some of her milk spills, and it produces the faint band of light known as the Milky Way.In the astronomical literature, the capitalized word "Galaxy" is often used to refer to our galaxy, the Milky Way, to distinguish it from the other galaxies in our universe. The English term Milky Way can be traced back to a story by Chaucer {{circa|1380}}:th the Milky Wey, For hit is whyt."|Geoffrey Chaucer|The House of Fame''}}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 anagalactic nebulae, and were just thought as a part of the Milky Way, 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, but this term quickly fell into disuse, as the word universe implied the entirety of existence. Instead, they became known simply as galaxies.


File:Probing the distant past SDSS J1152+3313.tif|thumb|Galaxy cluster SDSS J1152+3313. SDSS stands for Sloan Digital Sky Survey, J for Julian epoch, and 1152+3313 for the declination and right ascensionright ascensionTens of thousands 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) and UGC (Uppsala General Catalogue of Galaxies). All of the well-known galaxies appear in one or more of these catalogues but each time under a different number.For example, Messier 109 is a spiral galaxy having the number 109 in the catalogue of Messier, and also having the designations NGC 3992, UGC 6937, CGCG 269-023, MCG +09-20-044, and PGC 37617.

Observation history

The realization that we live in a galaxy which is one among many galaxies, parallels major discoveries that were made about the Milky Way and other nebulae.

Milky Way

The 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.BOOK, The Complete Works Volume 3: Essays and Miscellanies, Echo Library, Plutarch, Plutarch, 2006, Chapter 3, 66, 978-1-4068-3224-2,weblink Aristotle (384–322 BCE), however, believed the Milky Way to be 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."WEB
, Montada, J. P.
, September 28, 2007
, Ibn Bâjja
, Stanford Encyclopedia of Philosophy
, July 11, 2008
, The Neoplatonist philosopher Olympiodorus the Younger ({{circa|495}}–570 CE) was critical of this view, arguing that if the Milky Way is 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 does not. In his view, the Milky Way is celestial.According to Mohani Mohamed, the Arabian astronomer Alhazen (965–1037) made the first attempt at observing and measuring the Milky Way's parallax, and he thus "determined that because the Milky Way had no parallax, it must be remote from the Earth, not belonging to the atmosphere."WEB
, Bouali, H.-E.
, Zghal, M.
, Lakhdar, Z. B.
, 2005
, Popularisation of Optical Phenomena: Establishing the First Ibn Al-Haytham Workshop on Photography
, The Education and Training in Optics and Photonics Conference
, July 8, 2008
, The Persian astronomer al-Bīrūnī (973–1048) proposed the Milky Way galaxy to be "a collection of countless fragments of the nature of nebulous stars."{{MacTutor Biography|id=Al-Biruni|title=Abu Arrayhan Muhammad ibn Ahmad al-Biruni}} The Andalusian astronomer Ibn Bâjjah ("Avempace", {{abbr|d.|died}} 1138) proposed that the Milky Way is made up of many stars that almost touch one another and appear to be a continuous image due to the effect of refraction from sublunary material, citing his observation of the conjunction of Jupiter and Mars as evidence of this occurring when two objects are near. In the 14th century, the Syrian-born Ibn Qayyim proposed the Milky Way galaxy to be "a myriad of tiny stars packed together in the sphere of the fixed stars."JOURNAL
, Livingston, J. W.
, 1971
, Ibn Qayyim al-Jawziyyah: A Fourteenth Century Defense against Astrological Divination and Alchemical Transmutation
, Journal of the American Oriental Society
, 91, 1, 96–103 [99]
, 10.2307/600445
, 600445
, File:Herschel-Galaxy.png|thumb|The shape of the Milky Way as estimated from star counts by William HerschelWilliam HerschelActual proof of the Milky Way consisting of many stars came in 1610 when the Italian astronomer Galileo Galilei used a telescope to study the Milky Way and discovered that it is composed of a huge number of faint stars.Galileo Galilei, Sidereus Nuncius (Venice, (Italy): Thomas Baglioni, 1610), pages 15 and 16.English translation: Galileo Galilei with Edward Stafford Carlos, trans., The Sidereal Messenger (London, England: Rivingtons, 1880), pages 42 and 43.WEB
, O'Connor, J. J.
, Robertson, E. F.
, November 2002
, Galileo Galilei
, University of St. Andrews
, January 8, 2007
, In 1750 the English astronomer Thomas Wright, in his An original theory or new hypothesis of the Universe, speculated (correctly) that the galaxy 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. The resulting disk of stars can be seen as a band on the sky from our perspective inside the disk.Thomas Wright, An Original Theory or New Hypothesis of the Universe … (London, England: H. Chapelle, 1750). From p.48: " … the stars are not infinitely dispersed and distributed in a promiscuous manner throughout all the mundane space, without order or design, … this phænomenon [is] no other than a certain effect arising from the observer's situation, … To a spectator placed in an indefinite space, … it [i.e., the Milky Way (Via Lactea)] [is] a vast ring of stars … "On page 73, Wright called the Milky Way the Vortex Magnus (the great whirlpool) and estimated its diameter at 8.64×1012 miles (13.9×1012 km). In a treatise in 1755, Immanuel Kant elaborated on Wright's idea about the structure of the Milky Way.Immanuel Kant, Allgemeine Naturgeschichte und Theorie des Himmels … [Universal Natural History and Theory of the Heavens … ], (Königsberg and Leipzig, (Germany): Johann Friederich Petersen, 1755).Available in English translation by Ian Johnston at: Vancouver Island University, British Columbia, Canada {{Webarchive|url= |date=August 29, 2014 }} 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.BOOK, William Herschel, Philosophical Transactions of the Royal Society of London, Giving Some Accounts of the Present Undertakings, Studies, and Labours, of the Ingenious, in Many Considerable Parts of the World,weblink XII. On the construction of the heavens,weblink vol. 75, 1785, London, 213–266, 10.1098/rstl.1785.0012, 0261-0523, Herschel's diagram of the galaxy appears immediately after the article's last page. 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 center. 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 our host galaxy, the Milky Way, emerged.JOURNAL
, Trimble, V.
, 1999
, Robert Trumpler and the (Non)transparency of Space
, Bulletin of the American Astronomical Society
, 31, 31, 1479
, 1999AAS...195.7409T
, File:Milky Way Arch.jpg|thumb|center|600px|A fish-eye mosaic of the Milky Way arching at a high inclination across the night sky, shot from a dark-sky location in Chile. The Magellanic CloudsMagellanic Clouds

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, the Small Magellanic Cloud, and the Triangulum Galaxy. In the 10th century, the Persian astronomer Al-Sufi made the earliest recorded identification of the Andromeda Galaxy, describing it as a "small cloud". In 964, Al-Sufi probably mentioned the Large Magellanic Cloud in his Book of Fixed Stars (referring to "Al Bakr of the southern Arabs", 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.WEB
, Abd-al-Rahman Al Sufi (December 7, 903 â€“ May 25, 986 A.D.)
, Observatoire de Paris
, April 19, 2007
, WEB, The Large Magellanic Cloud, LMC< 8 and its Implications, Christopher J. Conselice, etal, The Astrophysical Journal, 830, 2, 2016, 1607.03909v2, 2016ApJ...830...83C, 10.3847/0004-637X/830/2/83, 83, NEWS,weblink Universe has two trillion galaxies, astronomers say, The Guardian, 13 October 2016, 14 October 2016, WEB,weblink The Universe Has 10 Times More Galaxies Than Scientists Thought,, 13 October 2016, 14 October 2016,

Types and morphology

(File:Hubble sequence photo.png|thumb|360px|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 to the left side of the Hubble classification scheme are sometimes referred to as "early-type", while those to the right are "late-type".)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.


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.WEB
, Barstow, M. A.
, 2005
, Elliptical Galaxies
,weblink" title="">weblink
, 2012-07-29
, Leicester University Physics Department
, June 8, 2006
, The largest galaxies are giant ellipticals. Many elliptical galaxies are believed to form due to the interaction of galaxies, resulting in a collision and merger. They can grow to enormous sizes (compared to spiral galaxies, for example), and giant elliptical galaxies are often found near the core of large galaxy clusters.WEB
, October 20, 2005
, Galaxies
,weblink" title="">weblink
, 2014-06-29
, Cornell University
, August 10, 2006

Shell galaxy

File:NGC 3923 Elliptical Shell Galaxy.jpg|thumb|NGC 3923NGC 3923A shell galaxy is a type of elliptical galaxy where the stars in the galaxy's 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. The shell-like structures are thought to develop when a larger galaxy absorbs a smaller companion galaxy. As the two galaxy centers approach, the centers start to oscillate around a center point, the oscillation creates gravitational ripples forming the shells of stars, similar to ripples spreading on water. For example, galaxy NGC 3923 has over twenty shells.WEB, Galactic onion,weblink, 2015-05-11,


File:M101 hires STScI-PRC2006-10a.jpg|thumb|right|The Pinwheel GalaxyPinwheel GalaxySpiral 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 that extends beyond the visible component, as demonstrated by the universal rotation curve concept.JOURNAL, Williams, M. J., Bureau, M., Cappellari, M., 10.1111/j.1365-2966.2009.15582.x, Kinematic constraints on the stellar and dark matter content of spiral and S0 galaxies, Monthly Notices of the Royal Astronomical Society, 400, 4, 1665–1689, 2010, 0909.0680, 2009MNRAS.400.1665W, 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) that 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.WEB
, Smith
, G.
, March 6, 2000
, Galaxies â€” The Spiral Nebulae
, University of California, San Diego Center for Astrophysics & Space Sciences
, November 30, 2006
, dead
,weblink" title="">weblink
, July 10, 2012
, mdy-all
, 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. 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."Fat or flat: Getting galaxies into shape". February 2014File:Hubble2005-01-barred-spiral-galaxy-NGC1300.jpg|right|thumb|300px|NGC 1300, an example of a barred spiral galaxybarred spiral galaxyIn 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". 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.File:Hoag's object.jpg|thumb|right|Hoag's Object, an example of a ring galaxyring galaxy

Barred spiral galaxy

A majority of spiral galaxies, including our own 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.JOURNAL
, Eskridge, P. B.
, Frogel, J. A.
, 1999
, What is the True Fraction of Barred Spiral Galaxies?
, Astrophysics and Space Science
, 269/270, 427–430
, 1999Ap&SS.269..427E
, 10.1023/A:1017025820201
, In the Hubble classification scheme, these are designated by an SB, followed by a lower-case letter (a, b or c) that 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.JOURNAL
, Bournaud, F.
, Combes, F.
, 2002
, Gas accretion on spiral galaxies: Bar formation and renewal
, Astronomy and Astrophysics
, 392
, 1, 83–102
, 2002A&A...392...83B
, 10.1051/0004-6361:20020920, astro-ph/0206273, Many barred spiral galaxies are active, possibly as a result of gas being channeled into the core along the arms.JOURNAL
, Knapen, J. H.
, Perez-Ramirez, D.
, Laine, S.
, 2002
, Circumnuclear regions in barred spiral galaxies â€” II. Relations to host galaxies
, Monthly Notices of the Royal Astronomical Society
, 337, 3, 808–828
, 2002MNRAS.337..808K
, 10.1046/j.1365-8711.2002.05840.x, astro-ph/0207258,
Our own galaxy, the Milky Way, is a large disk-shaped barred-spiral galaxyJOURNAL
, Alard, C.
, 2001
, Another bar in the Bulge
, Astronomy and Astrophysics Letters
, 379, 2, L44–L47
, 2001A&A...379L..44A
, 10.1051/0004-6361:20011487, astro-ph/0110491, about 30 kiloparsecs in diameter and a kiloparsec thick. It contains about two hundred billion (2×1011)NEWS
, Sanders, R.
, January 9, 2006
, Milky Way galaxy is warped and vibrating like a drum
, UC Berkeley, UCBerkeley News
, May 24, 2006
, stars and has a total mass of about six hundred billion (6×1011) times the mass of the Sun.JOURNAL
, Bell, G. R.
, Levine, S. E.
, 1997
, Mass of the Milky Way and Dwarf Spheroidal Stream Membership
, Bulletin of the American Astronomical Society
, 29, 2, 1384
, 1997AAS...19110806B

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 100,000 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.WEB,weblink We Just Discovered a New Type of Colossal Galaxy, Futurism, en-US, 2016-03-21, 2016-03-21, JOURNAL, Ogle, Patrick M., Lanz, Lauranne, Nader, Cyril, Helou, George, 2016-01-01, Superluminous Spiral Galaxies,weblink The Astrophysical Journal, en, 817, 2, 109, 10.3847/0004-637X/817/2/109, 0004-637X, 1511.00659, 2016ApJ...817..109O,

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.JOURNAL

, Gerber, R. A.
, Lamb, S. A.
, Balsara, D. S.
, 1994
, Ring Galaxy Evolution as a Function of "Intruder" Mass
, Bulletin of the American Astronomical Society
, 26, 911
, 1994AAS...184.3204G
, Such an event may have affected the Andromeda Galaxy, as it displays a multi-ring-like structure when viewed in infrared radiation.PRESS RELEASE
, European Space Agency
, October 14, 1998
, ISO unveils the hidden rings of Andromeda
, May 24, 2006
, dead
,weblink" title="">weblink
, August 28, 1999
, mdy-all
  • 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 starsWEB

, May 31, 2004
, Spitzer Reveals What Edwin Hubble Missed
,weblink" title="">weblink
, 2006-09-07
, Harvard-Smithsonian Center for Astrophysics
, December 6, 2006
, (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.WEB

, Barstow, M. A.
, 2005
, Irregular Galaxies
,weblink" title="">weblink
, 2012-02-27
, University of Leicester
, December 5, 2006
, Nearby examples of (dwarf) irregular galaxies include the Magellanic Clouds.
  • An ultra diffuse galaxy (UDG) is an extremely-low-density galaxy. The galaxy may be the same size as the Milky Way but has a visible star count of only 1% of the Milky Way. The lack of luminosity is because there is a lack of star-forming gas in the galaxy which results in old stellar populations.


Despite the prominence of large elliptical and spiral galaxies, most galaxies in the Universe are dwarf galaxies. These galaxies are relatively small when compared with other galactic formations, being about one hundredth the size of the Milky Way, containing only a few billion stars. Ultra-compact dwarf galaxies have recently been discovered that are only 100 parsecs across.JOURNAL
, Phillipps, S.
, Drinkwater, M. J.
, Gregg, M. D.
, Jones, J. B.
, 2001
, Ultracompact Dwarf Galaxies in the Fornax Cluster
, The Astrophysical Journal
, 560, 1, 201–206
, 2001ApJ...560..201P
, 10.1086/322517, astro-ph/0106377,
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.MAGAZINE
, Groshong, K.
, April 24, 2006
, Strange satellite galaxies revealed around Milky Way
, New Scientist
, January 10, 2007
, Dwarf galaxies may also be classified as elliptical, spiral, or irregular. Since small dwarf ellipticals bear little resemblance to large ellipticals, they are often called dwarf spheroidal galaxies instead.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 the galaxy has thousands or millions of stars. This has led to the suggestion 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.WEB
, Schirber, M.
, August 27, 2008
, No Slimming Down for Dwarf Galaxies
, ScienceNOW
, August 27, 2008

Other types of galaxies


File:Antennae galaxies xl.jpg|thumb|right|200px|The Antennae GalaxiesAntennae GalaxiesInteractions 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.WEB
, Galaxy Interactions
, University of Maryland Department of Astronomy
, December 19, 2006
,weblink" title="">weblink
, May 9, 2006
, Interacting Galaxies
, Swinburne University
, December 19, 2006
, Collisions occur when two galaxies pass directly through each other and have sufficient relative momentum not to merge. The stars of interacting galaxies will usually not collide, but the gas and dust within the two forms will interact, sometimes triggering star formation. A collision can severely distort the shape of the galaxies, forming bars, rings or tail-like structures.At the extreme of interactions are galactic mergers. In this case the relative momentum of the two galaxies is insufficient to allow the galaxies to pass through each other. Instead, they gradually merge to form a single, larger galaxy. Mergers can result in significant changes to morphology, as compared to the original galaxies. If one of the merging galaxies is much more massive than the other merging galaxy then the result is known as cannibalism. The more massive larger galaxy will remain relatively undisturbed by the merger, while the smaller galaxy 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.


File:M82 HST ACS 2006-14-a-large web.jpg|thumb|right|200px|M82, a starburst galaxy that has ten times the star formation of a "normal" galaxyWEB
, April 24, 2006
, Happy Sweet Sixteen, Hubble Telescope!
, August 10, 2006 NASAStars are created within galaxies from a reserve of cold gas that forms into 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, then they would consume their reserve of gas in a time span less than the lifespan of the galaxy. Hence starburst activity usually lasts for only about ten million years, a relatively brief period in the history of a galaxy. Starburst galaxies were more common during the early history of the Universe,WEB
, August 29, 2006
, Starburst Galaxies
, Harvard-Smithsonian Center for Astrophysics
, August 10, 2006
, and, at present, still contribute an estimated 15% to the total star production rate.CONFERENCE
, Kennicutt Jr., R. C.
, etal
, 2005
, Demographics and Host Galaxies of Starbursts
, Starbursts: From 30 Doradus to Lyman Break Galaxies
, 187
, Springer (publisher), Springer
, 2005ASSL..329..187K, 10.1007/1-4020-3539-X_33,
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.WEB
, Smith
, G.
, July 13, 2006
, Starbursts & Colliding Galaxies
, University of California, San Diego Center for Astrophysics & Space Sciences
, August 10, 2006
, dead
,weblink" title="">weblink
, July 7, 2012
, mdy-all
, These massive stars produce supernova explosions, resulting in 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 starburst activity end.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.WEB
, Keel, B.
, September 2006
, Starburst Galaxies
, University of Alabama
, December 11, 2006

Active galaxy

File:M87 jet.jpg|thumb|right|200px|A jet of particles is being emitted from the core of the elliptical radio galaxy M87.]]A portion of the observable galaxies are classified as active galaxies if the galaxy contains an active galactic nucleus (AGN). A significant portion of the total energy output from the galaxy is emitted by the active galactic nucleus, instead of the stars, dust and interstellar medium of the galaxy.The standard model for an active galactic nucleus is based upon an accretion disc that forms around a supermassive black hole (SMBH) at the core region of the galaxy. The radiation from an active galactic nucleus results from the gravitational energy of matter as it falls toward the black hole from the disc.WEB
, Keel, W. C.
, 2000
, Introducing Active Galactic Nuclei
, University of Alabama
, December 6, 2006
, 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.WEB
, Lochner, J.
, Gibb, M.
, A Monster in the Middle
, December 20, 2006
  • Seyfert galaxies or quasars, are classified depending on the luminosity, are active galaxies that emit high-energy radiation in the form of x-rays.


Blazars are believed to be an active galaxy with a relativistic jet that is 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 viewing angle of the observer.


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.JOURNAL
, Heckman, T. M.
, 1980
, An optical and radio survey of the nuclei of bright galaxies â€” Activity in normal galactic nuclei
, Astronomy and Astrophysics
, 87, 152–164
, 1980A&A....87..152H
, Approximately one-third of nearby galaxies are classified as containing LINER nuclei.JOURNAL
, Ho, L. C.
, Filippenko, A. V.
, Sargent, W. L. W.
, 1997
, A Search for "Dwarf" Seyfert Nuclei. V. Demographics of Nuclear Activity in Nearby Galaxies
, The Astrophysical Journal
, 487
, 2, 568–578
, 1997ApJ...487..568H
, 10.1086/304638, astro-ph/9704108,

Seyfert galaxy

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. Seyfert galaxies account for about 10% of all galaxies. Seen in visible light, most Seyfert galaxies look like normal spiral galaxies, but when studied under other wavelengths, the luminosity of their cores is equivalent to the luminosity of whole galaxies the size of the Milky Way.


Quasars (/ˈkweɪzɑr/) or quasi-stellar radio sources are the most energetic and distant members of active galactic nuclei. Quasars are extremely luminous and were first identified as being high redshift sources of electromagnetic energy, including radio waves and visible light, that appeared to be similar to stars, rather than extended sources similar to galaxies. Their luminosity can be 100 times greater than that of the Milky Way.

Luminous infrared galaxy

Luminous infrared galaxies or LIRGs are galaxies with luminosities, the measurement of brightness, above 1011 L☉. LIRGs are more abundant than starburst galaxies, Seyfert galaxies and quasi-stellar objects at comparable total luminosity. Infrared galaxies emit more energy in the infrared than at all other wavelengths combined. A LIRG's luminosity is 100 billion times that of our Sun.


Magnetic fields

Galaxies have magnetic fields of their own.ENCYCLOPEDIA, Galactic magnetic fields, Scholarpedia, 2, 8, 2411,weblink 2015-11-05, Beck, Rainer, 10.4249/scholarpedia.2411, 2007SchpJ...2.2411B, 2007, They are strong enough to be dynamically important: they drive mass inflow into the centers of galaxies, they modify the formation of spiral arms and they can affect the rotation of gas in the outer regions of galaxies. Magnetic fields provide the transport of angular momentum required for the collapse of gas clouds and hence the formation of new stars.The typical average equipartition strength for spiral galaxies is about 10 μG (microGauss) or 1 nT (nanoTesla). For 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 M 33, our Milky Way's neighbors, have weaker fields (about 5 μG), 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, for example in the centers of NGC 1097 and of other barred galaxies.

Formation and evolution

Galactic formation and evolution is an active area of research in astrophysics.


(File:Artist's impression of a protocluster forming in the early Universe.jpg|align=right|thumb|Artist's impression of a protocluster forming in the early UniverseWEB, Construction Secrets of a Galactic Metropolis,weblink, ESO Press Release, October 15, 2014, )Current cosmological models of the early Universe are based on the Big Bang theory. About 300,000 years after this event, 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.WEB
, November 18, 1999
, Protogalaxies
,weblink" title="">weblink
, 2008-03-25
, Harvard-Smithsonian Center for Astrophysics
, January 10, 2007
, These primordial structures would eventually become the galaxies we see today.(File:Young Galaxy Accreting Material.jpg|thumb|right|200px|Artist's impression of a young galaxy accreting material)

Early galaxies

Evidence for the early appearance of galaxies was found in 2006, when it was discovered that the galaxy IOK-1 has an unusually high redshift of 6.96, corresponding to just 750 million years after the Big Bang and making it the most distant and primordial galaxy yet seen.JOURNAL
, McMahon, R.
, 2006
, Astronomy: Dawn after the dark age
, Nature (journal), Nature
, 443, 7108, 151–2
, 10.1038/443151a
, 16971933, 2006Natur.443..151M,
While some scientists have claimed other objects (such as Abell 1835 IR1916) have higher redshifts (and therefore are seen in an earlier stage of the Universe's evolution), IOK-1's age and composition have been more reliably established. In December 2012, astronomers reported that UDFj-39546284 is the most distant object known and has a redshift value of 11.9. The object, estimated to have existed around "380 million years"WEB, Wall, Mike, Ancient Galaxy May Be Most Distant Ever Seen,weblink December 12, 2012,, December 12, 2012, after the Big Bang (which was about 13.8 billion years ago),WEB, Cosmic Detectives,weblink The European Space Agency (ESA), April 2, 2013,
publisher=Observatoire de Paris
,weblink" title="">weblink
url-status=live, Mar 11, 2004, The Andromeda Galaxy was later independently noted by Simon Marius in 1612.In 1734, philosopher Emanuel Swedenborg in his Principia speculated that there may be galaxies outside our own that are formed into galactic clusters that are minuscule parts of the universe which extends far beyond what we can see. These views "are remarkably close to the present-day views of the cosmos."WEB, Gordon, Kurtiss J., History of our Understanding of a Spiral Galaxy: Messier 33,weblink, 11 June 2018, In 1745, Pierre Louis Maupertuis conjectured that some nebula-like objects are collections of stars with unique properties, including a glow exceeding the light its stars produce on their own, and repeated Johannes Hevelius's view that the bright spots are massive and flattened due to their rotation.Kant, Immanuel, Universal Natural History and Theory of the Heavens (1755)In 1750, Thomas Wright speculated (correctly) that the Milky Way is a flattened disk of stars, and that some of the nebulae visible in the night sky might be separate Milky Ways.EVANS >FIRST1=J. C., November 24, 1998, Our Galaxy,weblink George Mason University, January 4, 2007, dead,weblink" title="">weblink June 30, 2012, mdy-all, See text quoted from Wright's An original theory or new hypothesis of the Universe in BOOK
, Dyson, F.
, 1979
, Disturbing the Universe
, 245
, Pan Books
, 978-0-330-26324-5,weblink
File:Pic iroberts1.jpg|thumb|right|Photograph of the "Great Andromeda Nebula" from 1899, later identified as the Andromeda GalaxyAndromeda GalaxyToward 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. In 1845, Lord Rosse constructed a new telescope and was able to distinguish between elliptical and spiral nebulae. He also managed to make out individual point sources in some of these nebulae, lending credence to Kant's earlier conjecture."Parsonstown | The genius of the Parsons family | William Rosse". 1912, Vesto 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.JOURNAL
, Slipher, V. M.
, 1913
, The radial velocity of the Andromeda Nebula
, Lowell Observatory Bulletin
, 1, 56–57
, 1913LowOB...2...56S
, Slipher, V. M.
, 1915
, Spectrographic Observations of Nebulae
, Popular Astronomy (US magazine), Popular Astronomy
, 23, 21–24
, 1915PA.....23...21S
, In 1917, Heber 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 our 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.JOURNAL
, Curtis, H. D.
, 1988
, Novae in Spiral Nebulae and the Island Universe Theory
, Publications of the Astronomical Society of the Pacific
, 100, 6
, 1988PASP..100....6C
, 10.1086/132128
, 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.WEB
, Weaver, H. F.
, Robert Julius Trumpler
, United States National Academy of Sciences, US National Academy of Sciences
, January 5, 2007
, 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.JOURNAL
, Öpik, E.
, 1922
, An estimate of the distance of the Andromeda Nebula
, The Astrophysical Journal
, 55, 406
, 1922ApJ....55..406O
, 10.1086/142680
, 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.JOURNAL
, Hubble, E. P.
, 1929
, A spiral nebula as a stellar system, Messier 31
, The Astrophysical Journal
, 69, 103–158
, 1929ApJ....69..103H
, 10.1086/143167
, In 1936 Hubble produced a classification of galactic morphology that is used to this day.JOURNAL
, Sandage, A.
, 1989
, Edwin Hubble, 1889–1953
, Journal of the Royal Astronomical Society of Canada
, 83, 6, 351–362
, January 8, 2007, 1989JRASC..83..351S,

Modern research

File:GalacticRotation2.svg|thumb|right|200px|Rotation curve of a typical spiral galaxy: predicted based on the visible matter (A) and observed (B). The distance is from the galactic core.]]In 1944, Hendrik van de Hulst predicted that microwave radiation with wavelength of 21 cm would be detectable from interstellar atomic hydrogen gas;WEB
, Tenn, J.
, Hendrik Christoffel van de Hulst
, Sonoma State University
, January 5, 2007
, 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 our galaxy. These observations led to the hypothesis of a rotating bar structure in the center of our galaxy.JOURNAL
, López-Corredoira, M.
, etal
, 2001
, Searching for the in-plane Galactic bar and ring in DENIS
, Astronomy and Astrophysics
, 373
, 1, 139–152
, 2001A&A...373..139L
, 10.1051/0004-6361:20010560, astro-ph/0104307, 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.MAGAZINE
, Rubin, V. C.
, 1983
, Dark matter in spiral galaxies
, Scientific American
, 248
, 6, 96–106
, 1983SciAm.248f..96R
, 10.1038/scientificamerican0683-96
, Rubin, V. C.
, 2000
, One Hundred Years of Rotating Galaxies
, Publications of the Astronomical Society of the Pacific
, 112, 772, 747–750
, 2000PASP..112..747R
, 10.1086/316573
, File:GOODS South field.jpg|left|thumb|Scientists used the galaxies visible in the GOODS survey to recalculate the total number of galaxies.WEB, Observable Universe contains ten times more galaxies than previously thought,weblink, 17 October 2016, ]]Beginning in the 1990s, the Hubble Space Telescope yielded improved observations. Among other things, Hubble data helped establish that the missing dark matter in our galaxy cannot solely consist of inherently faint and small stars.NEWS
, Hubble Rules Out a Leading Explanation for Dark Matter
, Hubble News Desk
, October 17, 1994
, January 8, 2007
, The Hubble Deep Field, an extremely long exposure of a relatively empty part of the sky, provided evidence that there are about 125 billion ({{val|1.25|e=11}}) galaxies in the observable universe.WEB
, November 27, 2002
, How many galaxies are there?
, January 8, 2007
, Improved technology in detecting the spectra invisible to humans (radio telescopes, infrared cameras, and x-ray telescopes) allow detection of other galaxies that are not detected by Hubble. Particularly, galaxy surveys in the Zone of Avoidance (the region of the sky blocked at visible-light wavelengths by the Milky Way) have revealed a number of new galaxies.JOURNAL
, Kraan-Korteweg, R. C.
, Juraszek, S.
, 2000
, Mapping the hidden Universe: The galaxy distribution in the Zone of Avoidance
, Publications of the Astronomical Society of Australia
, 17, 1, 6–12
, 2000PASA...17....6K, astro-ph/9910572
, 10.1071/AS00006,
In 2016, a study published in The Astrophysical Journal and led by Christopher Conselice of the University of Nottingham using 3D modeling of images collected over 20 years by the Hubble Space Telescope concluded that there are over 2 trillion ({{val|2|e=12}}) galaxies in the observable universe.JOURNAL, The Evolution of Galaxy Number Density at z
Distance measures (cosmology)>light travel distance years away. The existence of such early protogalaxy suggests that they must have grown in the so-called "dark ages". As of May 5, 2015, the galaxy EGS-zs8-1 is the most distant and earliest galaxy measured, forming 670 million years after the Big Bang. The light from EGS-zs8-1 has taken 13 billion years to reach Earth, and is now 30 billion light-years away, because of the expansion of the universe during 13 billion years.HUBBLESITE – NEWSCENTER – ASTRONOMERS SET A NEW GALAXY DISTANCE RECORD (05/05/2015) – INTRODUCTIONWEBSITE = HUBBLESITE.ORGACCESSDATE = 2015-05-07, ASTRONOMERS UNVEIL THE FARTHEST GALAXY>URL = HTTP://PHYS.ORG/NEWS/2015-05-ASTRONOMERS-UNVEIL-FARTHEST-GALAXY.HTMLNEWSPAPER = THE NEW YORK TIMESACCESS-DATE = 2015-05-07FIRST = DENNIS ARXIV = 1502.05399 FIRST = P. A.FIRST2 = P. G.FIRST3 = G. D.FIRST4 = R. J.FIRST5 = I.FIRST6 = B.FIRST7 = G. W.FIRST8 = R.FIRST9 = M.BIBCODE = 2015APJ...804L..30OISSUE = 2 PAGES=L30,

Early galaxy formation

File:Signatures of the Earliest Galaxies.jpg|thumb|Different components of near-infrared background light detected by the Hubble Space TelescopeHubble Space TelescopeThe detailed process by which early galaxies formed is an open question in astrophysics. Theories can be divided into two categories: top-down and bottom-up. In top-down correlations (such as the Eggen–Lynden-Bell–Sandage [ELS] model), protogalaxies form in a large-scale simultaneous collapse lasting about one hundred million years.JOURNAL
, Eggen, O. J.
, Lynden-Bell, D.
, Sandage, A. R.
, 1962
, Evidence from the motions of old stars that the Galaxy collapsed
, The Astrophysical Journal
, 136, 748
, 1962ApJ...136..748E
, 10.1086/147433
, In bottom-up theories (such as the Searle-Zinn [SZ] model), small structures such as globular clusters form first, and then a number of such bodies accrete to form a larger galaxy.JOURNAL
, Searle, L.
, Zinn, R.
, 1978
, Compositions of halo clusters and the formation of the galactic halo
, The Astrophysical Journal
, 225, 1, 357–379
, 1978ApJ...225..357S
, 10.1086/156499
, Once protogalaxies began to form and contract, the first halo stars (called Population III stars) appeared within them. These were composed almost entirely of hydrogen and helium, and may have been massive. If so, these huge stars would have quickly consumed their supply of fuel and became supernovae, releasing heavy elements into the interstellar medium.JOURNAL
, Heger, A.
, Woosley, S. E.
, 2002
, The Nucleosynthetic Signature of Population III
, The Astrophysical Journal
, 567, 1, 532–543
, 2002ApJ...567..532H
, 10.1086/338487, astro-ph/0107037, This first generation of stars re-ionized the surrounding neutral hydrogen, creating expanding bubbles of space through which light could readily travel.JOURNAL
, Barkana, R.
, Loeb, A.
, 2001
, In the beginning: the first sources of light and the reionization of the Universe
, Physics Reports
, 349, 2, 125–238
, 2001PhR...349..125B
, astro-ph/0010468
, 10.1016/S0370-1573(01)00019-9,weblink
, Submitted manuscript
In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at {{math|z {{=}} 6.60}}. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.JOURNAL, Sobral, David, Matthee, Jorryt, Darvish, Behnam, Schaerer, Daniel, Mobasher, Bahram, Röttgering, Huub J. A., Santos, Sérgio, Hemmati, Shoubaneh, Evidence for POPIII-like Stellar Populations in the Most Luminous LYMAN-α Emitters at the Epoch of Re-ionisation: Spectroscopic Confirmation, 4 June 2015, The Astrophysical Journal, 10.1088/0004-637x/808/2/139, 2015ApJ...808..139S, 808, 2, 139, 1504.01734, NEWS, Overbye, Dennis, Dennis Overbye, Traces of Earliest Stars That Enriched Cosmos Are Spied,weblink 17 June 2015, The New York Times, 17 June 2015,


Within a billion years of a galaxy's formation, key structures begin to appear. 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.NEWS
, February 9, 2005
, Simulations Show How Growing Black Holes Regulate Galaxy Formation
, Carnegie Mellon University
, January 7, 2007
, dead
,weblink" title="">weblink
, June 4, 2012
, mdy-all
, During this early epoch, galaxies undergo a major burst of star formation.NEWS
, Massey, R.
, April 21, 2007
, Caught in the act; forming galaxies captured in the young Universe
,weblink" title="">weblink
, 2013-11-15
, Royal Astronomical Society
, April 20, 2007
, During the following two billion years, the accumulated matter settles into a galactic disc.JOURNAL
, Noguchi, M.
, 1999
, Early Evolution of Disk Galaxies: Formation of Bulges in Clumpy Young Galactic Disks
, The Astrophysical Journal
, 514, 1, 77–95
, 1999ApJ...514...77N
, 10.1086/306932
high-velocity clouds and dwarf galaxy>dwarf galaxies throughout its life.WEB
, Baugh, C.
, Frenk, C.
, May 1999
,weblink" title="">weblink
, 2007-04-26
, How are galaxies made?
, PhysicsWeb
, January 16, 2007
, 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.CONFERENCE
, Gonzalez, G.
, 1998
, The Stellar Metallicity â€” Planet Connection
, Brown dwarfs and extrasolar planets: Proceedings of a workshop ...
, 431
, 1998ASPC..134..431G
, {{Multiple image |direction=vertical |align=right |width=200 |image1=XDF-scale.jpg|image2=Constellation Fornax, EXtreme Deep Field.jpg |image3=XDF-separated.jpg |caption1=XDF view field compared to the angular size of the Moon. Several thousand galaxies, each consisting of billions of stars, are in this small view. |caption2=XDF (2012) view: Each light speck is a galaxy, some of which are as old as 13.2 billion yearsWEB, Moskowitz, Clara, Hubble Telescope Reveals Farthest View Into Universe Ever,weblink September 25, 2012,, September 26, 2012,  â€“ the observable universe is estimated to contain 200 billion to 2 trillion galaxies. |caption3=XDF image shows (from left) fully mature galaxies, nearly mature galaxies (from 5 to 9 billion years ago), and protogalaxies, blazing with young stars (beyond 9 billion years). |header=Hubble eXtreme Deep Field (XDF) }}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.MAGAZINE
, Conselice, C. J.
, February 2007
, The Universe's Invisible Hand
, Scientific American
, 296, 2, 35–41
, 10.1038/scientificamerican0207-34, 2007SciAm.296b..34C, 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 4676NEWS
, Ford, H.
, etal
, April 30, 2002
, The Mice (NGC 4676): Colliding Galaxies With Tails of Stars and Gas
, Hubble News Desk
, May 8, 2007
, or the Antennae Galaxies.JOURNAL
, Struck, C.
, 1999
, Galaxy Collisions
, 10.1016/S0370-1573(99)00030-7
, Physics Reports
, 321
, 1–3
, 1–137
, astro-ph/9908269, 1999PhR...321....1S,
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, evidence of past collisions of the Milky Way with smaller dwarf galaxies is increasing.NEWS
, Wong, J.
, April 14, 2000
, Astrophysicist maps out our own galaxy's end
, University of Toronto
, January 11, 2007
,weblink" title="">weblink
, January 8, 2007
, 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 approximately ten billion years ago.JOURNAL
, Panter, B.
, Jimenez, R.
, Heavens, A. F.
, Charlot, S.
, 2007
, The star formation histories of galaxies in the Sloan Digital Sky Survey
, Monthly Notices of the Royal Astronomical Society
, 378, 4, 1550–1564
, astro-ph/0608531
, 10.1111/j.1365-2966.2007.11909.x, 2007MNRAS.378.1550P

Future trends

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.JOURNAL
, Kennicutt Jr., R. C.
, Tamblyn, P.
, Congdon, C. E.
, 1994
, Past and future star formation in disk galaxies
, The Astrophysical Journal
, 435, 1, 22–36
, 1994ApJ...435...22K
, 10.1086/174790
, Elliptical galaxies are largely devoid of this gas, and so form few new stars.BOOK
, Knapp, G. R.
, 1999
, Star Formation in Early Type Galaxies
, Star Formation in Early Type Galaxies
, 163
, 119
, Astronomical Society of the Pacific
, 1999ASPC..163..119K
, 41302839
, 978-1-886733-84-8
, 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.WEB
, Adams, Fred
, Laughlin, Greg
, July 13, 2006
, The Great Cosmic Battle
, Astronomical Society of the Pacific
, January 16, 2007
, WEB, Cosmic 'Murder Mystery' Solved: Galaxies Are 'Strangled to Death',weblink 2015-05-14, 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 our 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.WEB
, Pobojewski, S.
, January 21, 1997
, Physics offers glimpse into the dark side of the Universe
, University of Michigan
, January 13, 2007

Larger-scale structures

Deep sky surveys show that galaxies are often found in groups and clusters. Solitary galaxies that have not significantly interacted with another galaxy of comparable mass during the past billion years are relatively scarce. Only about 5% of the galaxies surveyed have been found to be truly isolated; however, these isolated formations may have interacted and even merged with other galaxies in the past, and may still be orbited by smaller, satellite galaxies. Isolated galaxiesThe term "field galaxy" is sometimes used to mean an isolated galaxy, although the same term is also used to describe galaxies that do not belong to a cluster but may be a member of a group of galaxies. can produce stars at a higher rate than normal, as their gas is not being stripped by other nearby galaxies.MAGAZINE
, McKee, M.
, June 7, 2005
, Galactic loners produce more stars
, New Scientist
, January 15, 2007
, 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 in the Universe, as clumps of dark matter pulled their respective galaxies together. Nearby groups later merged to form larger-scale clusters. This on-going merger process (as well as an influx of infalling gas) heats the inter-galactic gas within a cluster to very high temperatures, reaching 30–100 megakelvins.WEB
, Groups & Clusters of Galaxies
, NASA/Chandra
, January 15, 2007
, About 70–80% of the mass in a cluster is in the form of dark matter, with 10–30% consisting of this heated gas and the remaining few percent of the matter in the form of galaxies.WEB
, Ricker, P.
, When Galaxy Clusters Collide
, San Diego Supercomputer Center
, August 27, 2008
, {{multiple image| align = right| direction = vertical| width = 230| image1 = Seyfert Sextet full.jpg| width1 =| alt1 =| caption1 = Seyfert's Sextet is an example of a compact galaxy group.| image2 =| width2 =| alt2 =| caption2 = Millennium Simulation showing large-scale structure of the Cosmos. The image spans about 400 million light years across.}}Most galaxies in the Universe 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, and these formations contain a majority of the galaxies (as well as most of the baryonic mass) in the Universe.WEB
, Dahlem, M.
, November 24, 2006
, Optical and radio survey of Southern Compact Groups of galaxies
, University of Birmingham Astrophysics and Space Research Group
, January 15, 2007
,weblink" title="">weblink
, June 13, 2007
, Ponman, T.
, February 25, 2005
, Galaxy Systems: Groups
,weblink" title="">weblink
, 2009-02-15
, University of Birmingham Astrophysics and Space Research Group
, January 15, 2007
, 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.JOURNAL
, Girardi, M.
, Giuricin, G.
, 2000
, The Observational Mass Function of Loose Galaxy Groups
, The Astrophysical Journal
, 540, 1, 45–56
, 2000ApJ...540...45G
, 10.1086/309314, astro-ph/0004149,
Clusters of galaxies consist of hundreds to thousands of galaxies bound together by gravity.NEWS, Hubble Pinpoints Furthest Protocluster of Galaxies Ever Seen,weblink January 22, 2015, ESA/Hubble Press Release, 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.JOURNAL
, Dubinski
, J.
, 1998
, The Origin of the Brightest Cluster Galaxies
, The Astrophysical Journal
, 502
, 2
, 141–149
, 10.1086/305901
, 1998ApJ...502..141D
, astro-ph/9709102
, January 16, 2007
,weblink" title="">weblink
, May 14, 2011
, dead
, mdy-all
, 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.JOURNAL
, Bahcall, N. A.
, 1988
, Large-scale structure in the Universe indicated by galaxy clusters
, Annual Review of Astronomy and Astrophysics
, 26
, 1, 631–686
, 1988ARA&A..26..631B
, 10.1146/annurev.aa.26.090188.003215
, Above this scale, the Universe appears to be the same in all directions (isotropic and (wikt:Homogeneity|homogeneous)).JOURNAL
, Mandolesi, N.
, etal
, 1986
, Large-scale homogeneity of the Universe measured by the microwave background
, Letters to Nature
, 319
, 6056, 751–753
, 10.1038/319751a0, 1986Natur.319..751M,
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 galaxies.JOURNAL
, van den Bergh, S.
, 2000
, Updated Information on the Local Group
, Publications of the Astronomical Society of the Pacific
, 112, 770, 529–536
, 2000PASP..112..529V
, 10.1086/316548, astro-ph/0001040, 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.JOURNAL
, Tully, R. B.
, 1982
, The Local Supercluster
, The Astrophysical Journal
, 257, 389–422
, 1982ApJ...257..389T
, 10.1086/159999
, And the Virgo Supercluster itself is a part of the Pisces-Cetus Supercluster Complex, a giant galaxy filament.File:NASA-HubbleLegacyFieldZoomOut-20190502.webm|thumb|225px|right|Hubble Space Telescope - Ultra deep field galaxies to Legacy field zoom out (video 00:50; 2 May 2019)NEWS, NASA, Hubble astronomers assemble wide view of the evolving universe,weblink May 2, 2019, EurekAlert!EurekAlert!(File:The southern plane of the Milky Way from the ATLASGAL survey.jpg|left|thumb|The southern plane of the Milky Way from submillimeter wavelengthsWEB, ATLASGAL Survey of Milky Way Completed,weblink 7 March 2016, )

Multi-wavelength observation

{{See also|Observational astronomy}}{{multiple image| align = right| direction = vertical| width = 220| image1 =| caption1 = A visual light image of Andromeda Galaxy shows the emission of ordinary stars and the light reflected by dust.| image2 = Andromeda galaxy.jpg
Andromeda Galaxy>Andromeda shows blue regions containing young, massive stars.}}The peak radiation of most stars lies in the visible spectrum, so the observation of the stars that form galaxies has been a major component of optical astronomy. It is also a favorable portion of the spectrum for observing ionized H II regions, and for examining the distribution of dusty arms.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.WEB
, Near, Mid & Far Infrared
, Infrared Processing and Analysis Center, IPAC/NASA
, January 2, 2007
, dead
,weblink" title="">weblink
, December 30, 2006
, Infrared is also used to observe distant, red-shifted galaxies that were formed much earlier in the history of the Universe. 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.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.)WEB
, The Effects of Earth's Upper Atmosphere on Radio Signals
, August 10, 2006
, Large radio interferometers have been used to map the active jets emitted from active nuclei. Radio telescopes can also be used to observe neutral hydrogen (via 21 cm radiation), including, potentially, the non-ionized matter in the early Universe that later collapsed to form galaxies.WEB
, Giant Radio Telescope Imaging Could Make Dark Matter Visible
, ScienceDaily
, December 14, 2006
, January 2, 2007
, 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.NEWS
, NASA Telescope Sees Black Hole Munch on a Star
, December 5, 2006
, January 2, 2007
, 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.WEB
, Dunn, R.
, An Introduction to X-ray Astronomy
, Institute of Astronomy, Cambridge, Institute of Astronomy X-Ray Group
, January 2, 2007

See also

{{Wikipedia books|Galaxies}}{{div col|colwidth=30em}} {{div col end}}




{{Reflist|30em|refs={{harvnb|Sparke|Gallagher III|2000|p=i}}{{harvnb|Heidarzadeh|2008|pp=23–25}}{{harvnb|Heidarzadeh|2008|p=25, Table 2.1}}{{harvnb|Paul|1993|pp=16–18}}{{harvnb|Al-Biruni|2004|p=87}}{{harvnb|Mohamed|2000|pp=49–50}}{{harvnb|Kepple|Sanner|1998|p=18}}{{harvnb|Van den Bergh|1998|p=17}}{{harvnb|Waller|Hodge|2003|p=91}}{{harvnb|Bertin|Lin|1996|pp=65–85}}{{harvnb|Belkora|2003|p=355}}WEB
, Hupp, E.
, Roy, S.
, Watzke, M.
, August 12, 2006
, NASA Finds Direct Proof of Dark Matter
, April 17, 2007
, Uson, J. M.
, Boughn, S. P.
, Kuhn, J. R.
, 1990
, The central galaxy in Abell 2029 â€“ An old supergiant
, Science (journal), Science
, 250, 4980, 539–540
, 1990Sci...250..539U
, 10.1126/science.250.4980.539, 17751483
, Hoover
, A.
, June 16, 2003
, UF Astronomers: Universe Slightly Simpler Than Expected
, Hubble News Desk
, March 4, 2011
, dead
,weblink" title="">weblink
, July 20, 2011
, mdy-all,
  • Based upon: JOURNAL

, Graham, A. W.
, Guzman, R.
, 2003
, HST Photometry of Dwarf Elliptical Galaxies in Coma, and an Explanation for the Alleged Structural Dichotomy between Dwarf and Bright Elliptical Galaxies
, The Astronomical Journal
, 125, 6, 2936–2950
, 2003AJ....125.2936G
, 10.1086/374992, astro-ph/0303391,
, Jarrett, T. H.
, Near-Infrared Galaxy Morphology Atlas
, California Institute of Technology
, January 9, 2007
, Galaxy Clusters and Large-Scale Structure
, University of Cambridge
, January 15, 2007
, Finley, D.
, Aguilar, D.
, November 2, 2005
, Astronomers Get Closest Look Yet At Milky Way's Mysterious Core
, National Radio Astronomy Observatory
, August 10, 2006
, Gott III, J. R.
, 2005
, etal
, A Map of the Universe
, The Astrophysical Journal
, 624, 2, 463–484
, 2005ApJ...624..463G
, 10.1086/428890
, astro-ph/0310571,
, Firmani, C.
, Avila-Reese, V.
, 2003
, Physical processes behind the morphological Hubble sequence
, Revista Mexicana de Astronomía y Astrofísica
, 17, 107–120
, 2003RMxAC..17..107F, astro-ph/0303543
, Konečný, Lubomír
, Emblematics, Agriculture, and Mythography in The Origin of the Milky Way
, Academy of Sciences of the Czech Republic
, January 5, 2007
,weblink" title="">weblink
, July 20, 2006
, Harper, D.
, galaxy, Online Etymology Dictionary
, November 11, 2011
, Rao, J.
, September 2, 2005
, Explore the Archer's Realm
, January 3, 2007
, }}


  • WEB

, May 3, 2000
, Unveiling the Secret of a Virgo Dwarf Galaxy
,weblink" title="">weblink
, 2009-01-09
, January 3, 2007


  • BOOK, harv

, Belkora, L.
, 2003
, Minding the Heavens: the Story of our Discovery of the Milky Way
, CRC Press
, 978-0-7503-0730-7,weblink
  • BOOK, harv

, Bertin, G.
, Lin, C.-C.
, 1996
, Spiral Structure in Galaxies: a Density Wave Theory
, MIT Press
, 978-0-262-02396-2,weblink
  • BOOK

, Binney, J.
, Merrifield, M.
, 1998
, Galactic Astronomy
, Princeton University Press
, 978-0-691-00402-0
, 39108765,weblink
  • BOOK

, Dickinson, T.
, 2004
, The Universe and Beyond
, 4th
, Firefly Books
, 978-1-55297-901-3
, 55596414
  • BOOK, harv

, Heidarzadeh, T.
, 2008
, A History of Physical Theories of Comets, from Aristotle to Whipple
, Springer
, 978-1-4020-8322-8,weblink
  • BOOK, harv

, Mo, Houjun
, van den Bosch, Frank
, White, Simon
, Simon White
, 2010
, Galaxy Formation and Evolution
, Cambridge University Press
, 1
, 978-0-521-85793-2,weblink
  • BOOK, harv

, Kepple, G. R.
, Sanner, G. W.
, 1998
, The Night Sky Observer's Guide, Volume 1
, Willmann-Bell
, 978-0-943396-58-3,weblink
  • BOOK, harv

, Merritt, D.
, David Merritt
, 2013
, Dynamics and Evolution of Galactic Nuclei
, Princeton University Press
, 978-1-4008-4612-2,weblink
  • BOOK, harv

, Mohamed, M.
, 2000
, Great Muslim Mathematicians
, Penerbit UTM
, 978-983-52-0157-8
, 48759017,weblink
  • BOOK, harv

, Paul, E. R.
, 1993
, The Milky Way Galaxy and Statistical Cosmology, 1890–1924
, Cambridge University Press
, 978-0-521-35363-2,weblink
  • BOOK, harv

, Sparke, L. S.
, Gallagher III, J. S.
, 2000
, Galaxies in the Universe: An Introduction
, Cambridge University Press
, 978-0-521-59740-1,weblink
  • BOOK, harv

, Van den Bergh, S.
, 1998
, Galaxy Morphology and Classification
, Cambridge University Press
, 978-0-521-62335-3,weblink
  • BOOK, harv

, Waller, W. H.
, Hodge, P. W.
, 2003
, Galaxies and the Cosmic Frontier
, Harvard University Press
, 978-0-674-01079-6,weblink

External links

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