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spiral density waves – they assumed that the stars travel in slightly elliptical orbits, and that the orientations of their orbits is correlated i.e. the ellipses vary in their orientation (one to another) in a smooth way with increasing distance from the galactic center. This is illustrated in the diagram to the right. It is clear that the elliptical orbits come close together in certain areas to give the effect of arms. Stars therefore do not remain forever in the position that we now see them in, but pass through the arms as they travel in their orbits.
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Spiral arms simply appear to pass through the older established stars as they travel in their galactic orbits, so they also do not necessarily follow the arms. As stars move through an arm, the space velocity of each stellar system is modified by the gravitational force of the local higher density.
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R. A. Benjamin; E. Churchwell; B. L. Babler; R. Indebetouw; M. R. Meade; B. A. Whitney; C. Watson; M. G. Wolfire; M. J. Wolff; R. Ignace; T. M. Bania; S. Bracker; D. P. Clemens; L. Chomiuk; M. Cohen; J. M. Dickey; J. M. Jackson; H. A. Kobulnicky; E. P. Mercer; J. S. Mathis; S. R. Stolovy; B. Uzpen
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Spiral arms appear visually brighter because they contain both young stars and more massive and luminous stars than the rest of the galaxy. As massive stars evolve far more quickly, their demise tends to leave a darker background of fainter stars immediately behind the density waves. This make the
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in 1925. He realized that the idea of stars arranged permanently in a spiral shape was untenable. Since the angular speed of rotation of the galactic disk varies with distance from the centre of the galaxy (via a standard solar system type of gravitational model), a radial arm (like a spoke) would
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in 1964, attempting to explain the large-scale structure of spirals in terms of a small-amplitude wave propagating with fixed angular velocity, that revolves around the galaxy at a speed different from that of the galaxy's gas and stars. They suggested that the spiral arms were manifestations of
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Bar-shaped elongations of stars are observed in roughly two-thirds of all spiral galaxies. Their presence may be either strong or weak. In edge-on spiral (and lenticular) galaxies, the presence of the bar can sometimes be discerned by the out-of-plane X-shaped or (peanut shell)-shaped structures
702:
Charles
Francis and Erik Anderson showed from observations of motions of over 20,000 local stars (within 300 parsecs) that stars do move along spiral arms, and described how mutual gravity between stars causes orbits to align on logarithmic spirals. When the theory is applied to gas, collisions
259:
have distinct arm-structures. Sc and SBc galaxies, for instance, have very "loose" arms, whereas Sa and SBa galaxies have tightly wrapped arms (with reference to the Hubble sequence). Either way, spiral arms contain many young, blue stars (due to the high mass density and the high rate of star
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in near- and mid-infrared light. Older stars appear blue here, and are clustered at the galaxies’ cores. Glowing dust, showing where it exists around and between stars – appearing in shades of red and orange. Stars that have not yet fully formed and are encased in gas and dust appear bright
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proposed that the arms represent regions of enhanced density (density waves) that rotate more slowly than the galaxy's stars and gas. As gas enters a density wave, it gets squeezed and makes new stars, some of which are short-lived blue stars that light the arms.
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is a large, tightly packed group of stars. The term refers to the central group of stars found in most spiral galaxies, often defined as the excess of stellar light above the inward extrapolation of the outer (exponential) disk
97:
Spiral galaxies are named by their spiral structures that extend from the center into the galactic disc. The spiral arms are sites of ongoing star formation and are brighter than the surrounding disc because of the young, hot
1300:
305:. Some bulges have similar properties to those of elliptical galaxies (scaled down to lower mass and luminosity); others simply appear as higher density centers of disks, with properties similar to disk galaxies.
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Roughly two-thirds of all spirals are observed to have an additional component in the form of a bar-like structure, extending from the central bulge, at the ends of which the spiral arms begin. The proportion of
301:, which are old, red stars with low metal content. Further, the bulge of Sa and SBa galaxies tends to be large. In contrast, the bulges of Sc and SBc galaxies are much smaller and are composed of young, blue
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Also the newly created stars do not remain forever fixed in the position within the spiral arms, where the average space velocity returns to normal after the stars depart on the other side of the arm.
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473:. At eleven billion years old, it is more than two billion years older than any previous discovery. Researchers believe the galaxy's shape is caused by the gravitational influence of a companion
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is a barred spiral, although the bar itself is difficult to observe from Earth's current position within the galactic disc. The most convincing evidence for the stars forming a bar in the
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Alexander, S. On the origin of the forms and the present condition of some of the clusters of stars, and several of the nebulae. Astronomical
Journal, vol. 2, iss. 37, p. 97-103 (1852)
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Animation of orbits as predicted by the density wave theory, which explains the existence of stable spiral arms. Stars move in and out of the spiral arms as they orbit the galaxy.
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quickly become curved as the galaxy rotates. The arm would, after a few galactic rotations, become increasingly curved and wind around the galaxy ever tighter. This is called the
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was once considered an ordinary spiral galaxy. Astronomers first began to suspect that the Milky Way is a barred spiral galaxy in the 1960s. Their suspicions were confirmed by
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Tiantian Yuan; Johan
Richard; Anshu Gupta; Christoph Federrath; Soniya Sharma; Brent A. Groves; Lisa J. Kewley; Renyue Cen; Yuval Birnboim; David B. Fisher (30 October 2017).
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Lin and Shu showed that this spiral pattern would persist more or less for ever, even though individual stars and gas clouds are always drifting into the arms and out again
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1008:, whose telescope Leviathan was the first to reveal the spiral structure of galaxies. In 1845 he discovered the spiral structure of M51, a galaxy nicknamed later as the "
148:, spiral galaxies make up approximately 60% of galaxies in today's universe. They are mostly found in low-density regions and are rare in the centers of galaxy clusters.
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118:, with only about 10% containing bars about 8 billion years ago, to roughly a quarter 2.5 billion years ago, until present, where over two-thirds of the
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1896:"Galaxy Zoo: unwinding the winding problem – observations of spiral bulge prominence and arm pitch angles suggest local spiral galaxies are winding"
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is a supermassive black hole. There are many lines of evidence for the existence of black holes in spiral galaxy centers, including the presence of
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is in the process of merging with the Milky Way and observations show that some stars in the halo of the Milky Way have been acquired from it.
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galaxy cluster in the Virgo constellation. A1689B11 is 11 billion light years from the Earth, forming 2.6 billion years after the Big Bang.
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Giudice, G.F.; Mollerach, S.; Roulet, E. (1994). "Can EROS/MACHO be detecting the galactic spheroid instead of the galactic halo?".
2446:, an educational website about Spiral Galaxies and other spiral formations found in nature. For high school & general audience.
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cousins in the galactic disc (but similar to those in the galactic bulge). The galactic halo also contains many globular clusters.
1992:
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1012:", and his drawings of it closely resemble modern photographs. In 1846 and in 1849 Lord Rosse identified similar pattern in
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477:. Computer models based on that assumption indicate that BX442's spiral structure will last about 100 million years.
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The relative importance, in terms of mass, brightness and size, of the different components varies from galaxy to galaxy.
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As gas clouds move into the density wave, the local mass density increases. Since the criteria for cloud collapse (the
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Chen, W.; Gehrels, N.; Diehl, R.; Hartmann, D. (1996). "On the spiral arm interpretation of COMPTEL Al map features".
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Before it was understood that spiral galaxies existed outside of our Milky Way galaxy, they were often referred to as
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observations in 2005, which showed that the Milky Way's central bar is larger than what was previously suspected.
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orbits, or not move in regular orbits at all. Halo stars may be acquired from small galaxies which fall into and
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Exaggerated diagram illustrating Lin and Shu's explanation of spiral arms in terms of slightly elliptical orbits
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in some spiral galaxies, and dynamical measurements that find large compact central masses in galaxies such as
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These different hypotheses are not mutually exclusive, as they may explain different types of spiral arms.
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Studies of the
Magellanic Clouds. III. Surface brightness, colors and integrated magnitudes of the Clouds.
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Quantifying the (X/peanut)-shaped structure in edge-on disc galaxies: length, strength, and nested peanuts
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de
Vaucouleurs, G.; de Vaucouleurs, A.; Corwin, H. G., Jr.; Buta, R. J.; Paturel, G.; Fouqué, P. (2016),
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Since the 1970s, there have been two leading hypotheses or models for the spiral structures of galaxies:
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As the compression wave goes through, it triggers star formation on the leading edge of the spiral arms.
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The question of whether such objects were separate galaxies independent of the Milky Way, or a type of
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Inclination- and dust-corrected galaxy parameters: bulge-to-disc ratios and size-luminosity relations
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1548:"Galaxy morphology in rich clusters — Implications for the formation and evolution of galaxies"
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1024:'s spiral structure. In 1852 Stephen Alexander supposed that Milky Way is also a spiral nebula.
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The pioneer of studies of the rotation of the Galaxy and the formation of the spiral arms was
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The motion of halo stars does bring them through the disc on occasion, and a number of small
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The stars in spirals are distributed in thin disks radial with intensity profiles such that
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with respect to their distance from the galactic center is indeed higher than expected from
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1203: – Chart depicting the relationship between brightness and mass of large star systems
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The bulk of the stars in a spiral galaxy are located either close to a single plane (the
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Timeline of knowledge about galaxies, clusters of galaxies, and large-scale structure
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Proceedings of the Royal
Society A: Mathematical, Physical and Engineering Sciences
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1806:"The most ancient spiral galaxy: a 2.6-Gyr-old disk with a tranquil velocity field"
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As clouds get swept up by the spiral arms, they collide with one another and drive
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2008:
Lin, C. C.; Shu, F. H. (August 1964). "On the spiral structure of disk galaxies".
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1440:(September 2005). "First GLIMPSE Results on the Stellar Structure of the Galaxy".
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which typically have a maximum visibility at half the length of the in-plane bar.
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1215: – Galaxy type intermediate between a spiral galaxy and barred spiral galaxy
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Using the Hubble classification, the bulge of Sa galaxies is usually composed of
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is the oldest and most distant known spiral galaxy, as of 2024.The galaxy has a
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2418:"AEGIS survey reveals new principle governing galaxy formation and evolution"
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This article is about the class of galaxy. For the type of logic puzzle, see
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1932:
1895:
1063:, proving that they are, in fact, entire galaxies outside our own. The term
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form, and evolution towards grand-design bisymmetric spirals is explained.
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The following hypotheses exist for star formation caused by density waves:
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Interpretation of velocity distribution of the inner regions of the Galaxy
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1209: – Type of spiral galaxy with prominent and well-defined spiral arms
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through the gas, which in turn causes the gas to collapse and form stars.
677:
590:
421:
398:
393:. The orbital behaviour of these stars is disputed, but they may exhibit
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1221: – Class of galaxy between an elliptical galaxy and a spiral galaxy
332:
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1017:
1013:
500:
484:
222:
44:
1233: – Galaxy undergoing an exceptionally high rate of star formation
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27:
Class of galaxy that has spiral structures extending from their cores.
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GLIMPSE: the
Galactic Legacy Infrared Mid-Plane Survey Extraordinaire
1984:
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at their centers. In our own galaxy, for instance, the object called
234:
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The first acceptable theory for the spiral structure was devised by
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2277:
2215:
2188:
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1914:
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1603:
1587:
Salucci, P. (2019). "The distribution of dark matter in galaxies".
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of 4.4, meaning its light took 12.4 billion years to reach Earth.
282:
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1980:
Minding the
Heavens: the Story of our Discovery of the Milky Way
571:
but still cannot explain the stability of the spiral structure.
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2781:
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2256:(May 1926). "A spiral nebula as a stellar system: Messier 33".
2110:
Francis, C.; Anderson, E. (2009). "Galactic spiral structure".
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The spiral galaxies light profiles, in terms of the coordinate
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255:
and thus give spiral galaxies their name. Naturally, different
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are regions of stars that extend from the center of barred and
119:
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1398:"Hubble and Galaxy Zoo Find Bars and Baby Galaxies Don't Mix"
1277: – All of space observable from the Earth at the present
470:
416:, and in further contrast, stars in the galactic halo are of
367:
3295:
1335:. Mrs. Hepsa Ely Silliman memorial lectures, 25. New Haven:
1260: – Hot, ionised, gaseous component in the Galactic halo
1191: – Low-luminosity galaxy of old stars & little dust
988:
227:
164:
Spiral galaxies may consist of several distinct components:
2480:
1868:"Citizen scientists re-tune Hubble's galaxy classification"
1755:"Hubble Has Spotted an Ancient Galaxy That Shouldn't Exist"
1742:
http://www.zmescience.com/space/oldest-spiral-galaxy-31321/
1720:"ALMA Spots Candidate for Most Distant Known Spiral Galaxy"
75:
3901:
1862:
1079:
Milky Way Galaxy's spiral arms and barred core – based on
1159: – Spiral galaxy in the constellation Coma Berenices
1153: – Spiral galaxy in the constellation Coma Berenices
1132: – Spiral galaxy in the constellation Canes Venatici
657:
436:
2240:"NASA - Hubble Views the Star That Changed the Universe"
1271: – Observed discrepancy in galactic angular momenta
1239: – Class of active galaxies with very bright nuclei
439:
are thought to belong to the galactic halo, for example
1134:
Pages displaying short descriptions of redirect targets
1031:
existing within our own galaxy, was the subject of the
412:
Unlike the galactic disc, the halo seems to be free of
589:
the stochastic self-propagating star formation model (
3878:
1141: – Spiral galaxy in the constellation Triangulum
958:
893:
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as the size of the stellar disk, whose luminosity is
849:
822:
802:
736:
1197: – Patchy galaxy with discontinuous spiral arms
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respectively. In 1850 he made the first drawing of
82:, and a central concentration of stars known as the
1059:in several spiral nebulae, including the so-called
714:
632:
70:. Most spiral galaxies consist of a flat, rotating
1659:Galaxy Zoo: CANDELS barred discs and bar fractions
1185: – Elliptical galaxy smaller than normal ones
1147: – Galaxy in the constellation Canes Venatici
972:
941:
877:
835:
808:
785:
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192:A near-spherical halo of stars, including many in
1901:Monthly Notices of the Royal Astronomical Society
1893:
1671:Astronomers detect double ‘peanut shell’ galaxies
1500:Monthly Notices of the Royal Astronomical Society
697:
563:. Measurements in the late 1960s showed that the
514:
483:is an extremely old spiral galaxy located in the
469:The oldest grand design spiral galaxy on file is
137:comes from several recent surveys, including the
3926:
1894:Masters, Karen L.; et al. (30 April 2019).
1681:Bogdan C. Ciambur and Alister W. Graham (2016),
160:Tuning-fork-style diagram of the Hubble sequence
2109:
1114: – Barred spiral galaxy in the Local Group
511:, may not be supported, and may need updating.
86:. These are often surrounded by a much fainter
2186:
2041:
2039:
1972:
1970:
1968:
1887:
1695:"Webb reveals structure in 19 spiral galaxies"
1633:Alister W. Graham and C. Clare Worley (2008),
1126: – Galaxy in the constellation Ursa Major
843:is the central value; it is useful to define:
3311:
3137:List of the most distant astronomical objects
2496:
2252:
2007:
176:of which spiral arms are prominent components
1647:Third Reference Catalogue of Bright Galaxies
1545:
723:The similar distribution of stars in spirals
565:orbital velocity of stars in spiral galaxies
2074:
2036:
1965:
1856:
1492:
260:formation), which make the arms so bright.
114:has likely changed over the history of the
3318:
3304:
2503:
2489:
2001:
1791:"The most ancient spiral galaxy confirmed"
1740:Oldest spiral galaxy is a freak of cosmos
1580:
1371:
1365:
1319:
1120: – Galaxy containing the Solar System
183:of mainly older stars, which resembles an
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2214:
2123:
1931:
1913:
1839:
1821:
1602:
1571:
1530:
1512:
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1227: – Galaxy with an annular appearance
454:
378:galactic bulge around the galactic core.
2415:
2189:"On the Disks of Spiral and so Galaxies"
1752:
1074:
987:
718:
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610:
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405:with the spiral galaxy—for example, the
366:) in more or less conventional circular
348:
331:
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155:
38:
3400:) may be read as "within" or "part of".
2045:
1976:
1777:"[BBC2005] Source 11 -- Galaxy"
1586:
942:{\displaystyle L_{tot}=2\pi I_{0}h^{2}}
14:
3927:
2459:
1325:
980:, do not depend on galaxy luminosity.
658:Star formation caused by density waves
251:. These long, thin regions resemble a
3299:
2484:
2329:
2180:
2164:The Luminosity Gradient of Messier 33
1590:The Astronomy and Astrophysics Review
600:
370:around the center of the galaxy (the
2437:Spiral Galaxies @ SEDS Messier pages
1797:
1753:Gonzalez, Robert T. (19 July 2012).
353:19 face-on spiral galaxies from the
2462:"Spiral Galaxies and Pattern Speed"
2332:"Bar at Milky Way's heart revealed"
2323:
690:density waves much more prominent.
407:Sagittarius Dwarf Spheroidal Galaxy
43:An example of a spiral galaxy, the
24:
3406:
2090:Swinburne University of Technology
1948:"A spiral home to exploding stars"
1098:
786:{\displaystyle I(R)=I_{0}e^{-R/h}}
308:Many bulges are thought to host a
257:classifications of spiral galaxies
189:A bar-shaped distribution of stars
90:of stars, many of which reside in
25:
3961:
2354:
1495:"The APM Bright Galaxy Catalogue"
1442:The Astrophysical Journal Letters
1169:
420:, much older and with much lower
3912:
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3863:
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3852:
3277:
3266:
3265:
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2330:McKee, Maggie (16 August 2005).
983:
715:Distribution of stars in spirals
703:between gas clouds generate the
633:Historical theory of Lin and Shu
2420:. UC Santa Cruz. Archived from
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1746:
1734:
1722:. www.sci-news.com. 20 May 2021
1712:
1687:
1675:
1663:
1651:
1639:
1275:Groups and clusters of galaxies
685:More young stars in spiral arms
202:at the very center of the bulge
66:and, as such, form part of the
3208:Galaxy formation and evolution
3203:Galaxy color–magnitude diagram
2416:Stephens, Tim (6 March 2007).
2290:Gerard de Vaucouleurs (1964),
2174:Gerard de Vaucouleurs (1957),
1627:
1539:
1486:
1432:
1424:. October 2005. Archived from
1410:
1390:
1264:Galaxy formation and evolution
1201:Galaxy color–magnitude diagram
746:
740:
698:Gravitationally aligned orbits
515:Origin of the spiral structure
381:However, some stars inhabit a
216:
13:
1:
3825:Andromeda–Milky Way collision
3325:
2162:F. Shirley Patterson (1940),
1669:Astronomy Now (8 May 2016),
1493:Loveday, J. (February 1996).
1313:
1179: – Type of galactic form
1067:has since fallen out of use.
816:being the disk scale-length;
2510:
1657:B.D. Simmons et al. (2014),
1418:"Ripples in a Galactic Pond"
1070:
878:{\displaystyle R_{opt}=3.2h}
151:
7:
3090:Galaxies named after people
1793:. PhysOrg. 3 November 2017.
1546:Dressler, A. (March 1980).
1164:
505:usual Hubble classification
344:
10:
3966:
3940:Galaxy morphological types
3223:Gravitational microlensing
3178:Galactic coordinate system
2450:Spiral Structure explained
2086:Swinburne Astronomy Online
2054:Cambridge University Press
1864:Royal Astronomical Society
1308: – Trend in astronomy
1252:Galactic coordinate system
1213:Intermediate spiral galaxy
1207:Grand design spiral galaxy
1102:
604:
549:
507:, particularly concerning
490:
355:James Webb Space Telescope
267:
220:
29:
3848:
3812:
3620:
3592:
3581:
3513:
3465:
3457:Galactic Center filaments
3425:
3418:
3404:
3333:
3261:
3160:
3075:
2968:
2927:
2837:
2772:
2663:
2518:
2258:The Astrophysical Journal
2010:The Astrophysical Journal
1810:The Astrophysical Journal
1621:10.1007/s00159-018-0113-1
1552:The Astrophysical Journal
578:star formation caused by
122:in the visible universe (
3188:Galactic magnetic fields
3001:Brightest cluster galaxy
2897:Luminous infrared galaxy
2474:University of Nottingham
2393:10.1103/PhysRevD.50.2406
2082:"Main Sequence Lifetime"
1841:10.3847/1538-4357/aa951d
1532:10.1093/mnras/278.4.1025
1332:The realm of the nebulae
1286:List of nearest galaxies
1244:
1195:Flocculent spiral galaxy
1049:Mount Wilson Observatory
263:
64:The Realm of the Nebulae
58:originally described by
47:(also known as NGC 1068)
32:Spiral Galaxies (puzzle)
3452:Supermassive black hole
3183:Galactic habitable zone
3168:Extragalactic astronomy
2757:Supermassive black hole
2671:Active galactic nucleus
2317:1996A&AS..120C.315C
2187:Freeman, K. C. (1970).
2049:The Guide to the Galaxy
2046:Henbest, Nigel (1994),
1613:2019A&ARv..27....2S
1291:List of spiral galaxies
1189:Dwarf spheroidal galaxy
1183:Dwarf elliptical galaxy
1105:List of spiral galaxies
1093:Spitzer Space Telescope
310:supermassive black hole
200:supermassive black hole
139:Spitzer Space Telescope
3745:Sagittarius Spheroidal
3607:Small Magellanic Cloud
3602:Large Magellanic Cloud
3559:Pisces-Eridanus stream
3412:
2935:Low surface brightness
2686:Central massive object
2142:10.1098/rspa.2009.0036
1084:
997:
974:
943:
879:
837:
810:
787:
724:
642:
622:
546:
531:
529:Hubble Space Telescope
455:Oldest spiral galaxies
359:
337:
336:Spiral galaxy NGC 2008
327:
294:
237:
161:
48:
3410:
3371:Laniakea Supercluster
3213:Galaxy rotation curve
2305:Space Science Reviews
2194:Astrophysical Journal
1933:10.1093/mnras/stz1153
1337:Yale University Press
1306:Tully–Fisher relation
1269:Galaxy rotation curve
1103:Further information:
1078:
1051:. Beginning in 1923,
991:
975:
944:
880:
838:
836:{\displaystyle I_{0}}
811:
788:
722:
640:
620:
537:
522:
352:
335:
285:
230:
159:
42:
3411:The Milky Way Galaxy
3248:Population III stars
3243:Intergalactic travel
3193:Galactic orientation
3060:Voids and supervoids
1977:Belkora, L. (2003).
1428:on 6 September 2013.
956:
891:
847:
820:
800:
734:
232:Barred spiral galaxy
3385:Observable universe
3238:Intergalactic stars
3127:Large quasar groups
3122:Groups and clusters
2986:Groups and clusters
2845:Lyman-alpha emitter
2737:Interstellar medium
2385:1994PhRvD..50.2406G
2270:1926ApJ....63..236H
2207:1970ApJ...160..811F
2134:2009RSPSA.465.3425F
2118:(2111): 3425–3446.
2022:1964ApJ...140..646L
1924:2019MNRAS.487.1808M
1832:2017ApJ...850...61Y
1564:1980ApJ...236..351D
1523:1996MNRAS.278.1025L
1464:2005ApJ...630L.149B
1422:Scientific American
1372:D. Mihalas (1968).
973:{\displaystyle R/h}
607:Density wave theory
299:Population II stars
174:interstellar matter
102:that inhabit them.
3730:Pisces Overdensity
3564:Sagittarius Stream
3475:Carina–Sagittarius
3413:
3365:Virgo Supercluster
3346:Milky Way subgroup
3233:Intergalactic dust
3218:Gravitational lens
3173:Galactic astronomy
3142:Starburst galaxies
2882:blue compact dwarf
2838:Energetic galaxies
2802:BL Lacertae object
2460:Merrifield, M. R.
1406:. 16 January 2014.
1374:Galactic Astronomy
1362:(pp. 124–151)
1085:
1061:"Andromeda Nebula"
998:
970:
939:
875:
833:
806:
783:
725:
643:
623:
601:Density wave model
569:Newtonian dynamics
547:
538:The spiral galaxy
532:
503:reported that the
497:citizen scientists
360:
338:
303:Population I stars
295:
238:
179:A central stellar
162:
146:irregular galaxies
49:
3876:
3875:
3840:Zone of Avoidance
3808:
3807:
3655:Canes Venatici II
3612:Magellanic Bridge
3594:Magellanic Clouds
3577:
3576:
3543:Magellanic Stream
3528:Fimbulthul stream
3293:
3292:
3253:Galaxy X (galaxy)
3228:Illustris project
3198:Galactic quadrant
2919:Wolf-Rayet galaxy
2909:Green bean galaxy
2904:Hot dust-obscured
2855:Luminous infrared
2619:Elliptical galaxy
2363:Physical Review D
1994:978-0-7503-0730-7
1383:978-0-7167-0326-6
1376:. W. H. Freeman.
1219:Lenticular galaxy
1139:Triangulum Galaxy
1057:Cepheid variables
1035:of 1920, between
809:{\displaystyle h}
668:Jeans instability
618:
387:galactic spheroid
205:A near-spherical
194:globular clusters
185:elliptical galaxy
168:A flat, rotating
92:globular clusters
62:in his 1936 work
16:(Redirected from
3957:
3917:
3916:
3915:
3905:
3904:
3893:
3892:
3891:
3884:
3866:
3865:
3858:Astronomy portal
3856:
3650:Canes Venatici I
3590:
3589:
3495:Scutum–Centaurus
3423:
3422:
3401:
3399:
3390:
3383:
3376:
3369:
3363:
3357:
3351:
3344:
3320:
3313:
3306:
3297:
3296:
3281:
3269:
3268:
2914:Hanny's Voorwerp
2824:Relativistic jet
2698:Dark matter halo
2505:
2498:
2491:
2482:
2481:
2477:
2433:
2431:
2429:
2424:on 11 March 2007
2412:
2378:
2376:astro-ph/9312047
2369:(4): 2406–2413.
2349:
2348:
2346:
2344:
2327:
2321:
2320:
2300:
2294:
2288:
2282:
2281:
2250:
2244:
2243:
2236:
2230:
2227:
2221:
2220:
2218:
2184:
2178:
2172:
2166:
2160:
2154:
2153:
2127:
2107:
2101:
2100:
2098:
2096:
2078:
2072:
2070:
2043:
2034:
2033:
2005:
1999:
1998:
1974:
1963:
1962:
1960:
1958:
1944:
1938:
1937:
1935:
1917:
1908:(2): 1808–1820.
1891:
1885:
1884:
1882:
1880:
1866:(11 June 2019).
1860:
1854:
1853:
1843:
1825:
1801:
1795:
1794:
1787:
1781:
1780:
1773:
1767:
1766:
1764:
1762:
1750:
1744:
1738:
1732:
1731:
1729:
1727:
1716:
1710:
1709:
1707:
1705:
1691:
1685:
1679:
1673:
1667:
1661:
1655:
1649:
1643:
1637:
1631:
1625:
1624:
1606:
1584:
1578:
1577:
1575:
1543:
1537:
1536:
1534:
1516:
1514:astro-ph/9603040
1507:(4): 1025–1048.
1490:
1484:
1483:
1457:
1455:astro-ph/0508325
1448:(2): L149–L152.
1436:
1430:
1429:
1414:
1408:
1407:
1394:
1388:
1387:
1369:
1363:
1358:
1323:
1281:List of galaxies
1231:Starburst galaxy
1151:Black Eye Galaxy
1145:Whirlpool Galaxy
1135:
1130:Sunflower Galaxy
1112:Andromeda Galaxy
1041:Lick Observatory
1022:Andromeda Galaxy
1010:Whirlpool Galaxy
996:by Rosse in 1845
994:Whirlpool Galaxy
979:
977:
976:
971:
966:
948:
946:
945:
940:
938:
937:
928:
927:
909:
908:
884:
882:
881:
876:
865:
864:
842:
840:
839:
834:
832:
831:
815:
813:
812:
807:
792:
790:
789:
784:
782:
781:
777:
761:
760:
705:molecular clouds
619:
445:Groombridge 1830
21:
3965:
3964:
3960:
3959:
3958:
3956:
3955:
3954:
3935:Spiral galaxies
3925:
3924:
3923:
3913:
3911:
3899:
3889:
3887:
3879:
3877:
3872:
3844:
3820:Alternate names
3804:
3616:
3584:
3573:
3523:Aquarius Stream
3509:
3461:
3427:Galactic Center
3414:
3402:
3397:
3395:
3394:
3388:
3381:
3374:
3367:
3361:
3355:
3349:
3342:
3329:
3324:
3294:
3289:
3257:
3156:
3071:
2964:
2923:
2833:
2768:
2747:Galaxy filament
2691:Galactic Center
2659:
2514:
2509:
2427:
2425:
2357:
2352:
2342:
2340:
2328:
2324:
2301:
2297:
2289:
2285:
2251:
2247:
2238:
2237:
2233:
2228:
2224:
2185:
2181:
2173:
2169:
2161:
2157:
2108:
2104:
2094:
2092:
2080:
2079:
2075:
2064:
2044:
2037:
2006:
2002:
1995:
1987:. p. 355.
1975:
1966:
1956:
1954:
1946:
1945:
1941:
1892:
1888:
1878:
1876:
1861:
1857:
1802:
1798:
1789:
1788:
1784:
1779:. 24 June 2018.
1775:
1774:
1770:
1760:
1758:
1751:
1747:
1739:
1735:
1725:
1723:
1718:
1717:
1713:
1703:
1701:
1693:
1692:
1688:
1680:
1676:
1668:
1664:
1656:
1652:
1644:
1640:
1632:
1628:
1585:
1581:
1544:
1540:
1491:
1487:
1437:
1433:
1416:
1415:
1411:
1396:
1395:
1391:
1384:
1370:
1366:
1347:
1324:
1320:
1316:
1311:
1258:Galactic corona
1247:
1242:
1172:
1167:
1162:
1133:
1124:Pinwheel Galaxy
1107:
1101:
1099:Famous examples
1073:
992:Drawing of the
986:
962:
957:
954:
953:
933:
929:
923:
919:
898:
894:
892:
889:
888:
854:
850:
848:
845:
844:
827:
823:
821:
818:
817:
801:
798:
797:
773:
766:
762:
756:
752:
735:
732:
731:
717:
700:
687:
660:
635:
626:Bertil Lindblad
611:
609:
603:
561:winding problem
556:Bertil Lindblad
552:
542:, home of five
517:
509:spiral galaxies
493:
457:
383:spheroidal halo
372:Galactic Center
347:
330:
272:
266:
225:
219:
154:
135:Galactic Center
112:barless spirals
68:Hubble sequence
56:class of galaxy
52:Spiral galaxies
35:
28:
23:
22:
18:Spiral galaxies
15:
12:
11:
5:
3963:
3953:
3952:
3947:
3942:
3937:
3922:
3921:
3909:
3897:
3874:
3873:
3871:
3870:
3860:
3849:
3846:
3845:
3843:
3842:
3837:
3832:
3830:Baade's Window
3827:
3822:
3816:
3814:
3810:
3809:
3806:
3805:
3803:
3802:
3797:
3792:
3787:
3785:Ursa Major III
3782:
3777:
3772:
3767:
3762:
3757:
3752:
3747:
3742:
3737:
3732:
3727:
3722:
3717:
3712:
3707:
3702:
3697:
3692:
3687:
3682:
3677:
3672:
3670:Coma Berenices
3667:
3662:
3657:
3652:
3647:
3642:
3637:
3632:
3626:
3624:
3618:
3617:
3615:
3614:
3609:
3604:
3598:
3596:
3587:
3579:
3578:
3575:
3574:
3572:
3571:
3566:
3561:
3556:
3550:
3548:Monoceros Ring
3545:
3540:
3535:
3530:
3525:
3519:
3517:
3511:
3510:
3508:
3507:
3502:
3500:Near 3 kpc Arm
3497:
3492:
3487:
3482:
3477:
3471:
3469:
3463:
3462:
3460:
3459:
3454:
3449:
3448:
3447:
3440:Sagittarius A*
3437:
3431:
3429:
3420:
3416:
3415:
3405:
3403:
3337:
3335:
3331:
3330:
3323:
3322:
3315:
3308:
3300:
3291:
3290:
3288:
3287:
3275:
3262:
3259:
3258:
3256:
3255:
3250:
3245:
3240:
3235:
3230:
3225:
3220:
3215:
3210:
3205:
3200:
3195:
3190:
3185:
3180:
3175:
3170:
3164:
3162:
3158:
3157:
3155:
3154:
3149:
3144:
3139:
3134:
3129:
3124:
3119:
3118:
3117:
3112:
3107:
3102:
3097:
3092:
3081:
3079:
3073:
3072:
3070:
3069:
3068:
3067:
3057:
3052:
3047:
3045:Stellar stream
3042:
3037:
3032:
3031:
3030:
3025:
3020:
3010:
3009:
3008:
3003:
2998:
2993:
2983:
2978:
2972:
2970:
2966:
2965:
2963:
2962:
2957:
2952:
2947:
2942:
2937:
2931:
2929:
2925:
2924:
2922:
2921:
2916:
2911:
2906:
2901:
2900:
2899:
2894:
2889:
2884:
2874:
2873:
2872:
2867:
2862:
2852:
2847:
2841:
2839:
2835:
2834:
2832:
2831:
2826:
2821:
2820:
2819:
2814:
2804:
2799:
2794:
2789:
2784:
2778:
2776:
2770:
2769:
2767:
2766:
2765:
2764:
2754:
2749:
2744:
2739:
2734:
2732:Galactic ridge
2729:
2727:Galactic plane
2724:
2723:
2722:
2712:
2711:
2710:
2700:
2695:
2694:
2693:
2683:
2678:
2673:
2667:
2665:
2661:
2660:
2658:
2657:
2656:
2655:
2645:
2640:
2639:
2638:
2628:
2627:
2626:
2616:
2615:
2614:
2609:
2604:
2599:
2589:
2588:
2587:
2582:
2577:
2572:
2567:
2562:
2557:
2547:
2546:
2545:
2540:
2530:
2524:
2522:
2516:
2515:
2508:
2507:
2500:
2493:
2485:
2479:
2478:
2457:
2452:
2447:
2443:SpiralZoom.com
2439:
2434:
2413:
2356:
2355:External links
2353:
2351:
2350:
2322:
2295:
2283:
2278:10.1086/142976
2245:
2231:
2222:
2216:10.1086/150474
2179:
2167:
2155:
2102:
2073:
2062:
2056:, p. 74,
2035:
2030:10.1086/147955
2000:
1993:
1964:
1939:
1886:
1855:
1796:
1782:
1768:
1745:
1733:
1711:
1686:
1674:
1662:
1650:
1638:
1626:
1579:
1573:10.1086/157753
1538:
1485:
1472:10.1086/491785
1431:
1409:
1389:
1382:
1364:
1345:
1317:
1315:
1312:
1310:
1309:
1303:
1298:
1293:
1288:
1283:
1278:
1272:
1266:
1261:
1255:
1248:
1246:
1243:
1241:
1240:
1237:Seyfert galaxy
1234:
1228:
1222:
1216:
1210:
1204:
1198:
1192:
1186:
1180:
1173:
1171:
1170:Classification
1168:
1166:
1163:
1161:
1160:
1154:
1148:
1142:
1136:
1127:
1121:
1115:
1108:
1100:
1097:
1072:
1069:
1045:Harlow Shapley
1002:spiral nebulae
985:
982:
969:
965:
961:
936:
932:
926:
922:
918:
915:
912:
907:
904:
901:
897:
874:
871:
868:
863:
860:
857:
853:
830:
826:
805:
794:
793:
780:
776:
772:
769:
765:
759:
755:
751:
748:
745:
742:
739:
716:
713:
699:
696:
686:
683:
682:
681:
674:
671:
659:
656:
634:
631:
605:Main article:
602:
599:
595:
594:
587:
586:of the galaxy.
551:
548:
523:Spiral galaxy
516:
513:
495:In June 2019,
492:
489:
456:
453:
441:Kapteyn's Star
397:and/or highly
364:galactic plane
346:
343:
329:
326:
314:Sagittarius A*
270:Galactic bulge
268:Main article:
265:
262:
221:Main article:
218:
215:
211:
210:
203:
196:
190:
187:
177:
153:
150:
144:Together with
108:barred spirals
26:
9:
6:
4:
3:
2:
3962:
3951:
3948:
3946:
3943:
3941:
3938:
3936:
3933:
3932:
3930:
3920:
3910:
3908:
3903:
3898:
3896:
3886:
3885:
3882:
3869:
3861:
3859:
3855:
3851:
3850:
3847:
3841:
3838:
3836:
3833:
3831:
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3815:
3811:
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3798:
3796:
3793:
3791:
3788:
3786:
3783:
3781:
3780:Ursa Major II
3778:
3776:
3773:
3771:
3770:Triangulum II
3768:
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3761:
3758:
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3506:
3505:Far 3 kpc Arm
3503:
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3481:
3478:
3476:
3473:
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3464:
3458:
3455:
3453:
3450:
3446:
3445:Fermi bubbles
3443:
3442:
3441:
3438:
3436:
3435:Sagittarius A
3433:
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3430:
3428:
3424:
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3176:
3174:
3171:
3169:
3166:
3165:
3163:
3159:
3153:
3150:
3148:
3147:Superclusters
3145:
3143:
3140:
3138:
3135:
3133:
3130:
3128:
3125:
3123:
3120:
3116:
3113:
3111:
3108:
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3101:
3098:
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3088:
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3080:
3078:
3074:
3066:
3063:
3062:
3061:
3058:
3056:
3053:
3051:
3050:Superclusters
3048:
3046:
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3041:
3038:
3036:
3033:
3029:
3026:
3024:
3021:
3019:
3016:
3015:
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3011:
3007:
3004:
3002:
2999:
2997:
2994:
2992:
2989:
2988:
2987:
2984:
2982:
2981:Galactic tide
2979:
2977:
2974:
2973:
2971:
2967:
2961:
2958:
2956:
2953:
2951:
2948:
2946:
2943:
2941:
2940:Ultra diffuse
2938:
2936:
2933:
2932:
2930:
2926:
2920:
2917:
2915:
2912:
2910:
2907:
2905:
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2800:
2798:
2795:
2793:
2790:
2788:
2785:
2783:
2780:
2779:
2777:
2775:
2774:Active nuclei
2771:
2763:
2760:
2759:
2758:
2755:
2753:
2750:
2748:
2745:
2743:
2740:
2738:
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2466:Sixty Symbols
2463:
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2337:New Scientist
2333:
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2310:
2306:
2299:
2293:
2287:
2279:
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2271:
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2259:
2255:
2254:Hubble, E. P.
2249:
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2235:
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2196:
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2063:9780521458825
2059:
2055:
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2027:
2023:
2019:
2015:
2011:
2004:
1996:
1990:
1986:
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1981:
1973:
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1953:
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1934:
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1925:
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1404:
1403:Science Daily
1399:
1393:
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1379:
1375:
1368:
1361:
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1352:
1348:
1346:9780300025002
1342:
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1119:
1116:
1113:
1110:
1109:
1106:
1096:
1094:
1090:
1082:
1077:
1068:
1066:
1065:spiral nebula
1062:
1058:
1054:
1050:
1046:
1042:
1038:
1034:
1030:
1025:
1023:
1019:
1015:
1011:
1007:
1003:
995:
990:
984:Spiral nebula
981:
967:
963:
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934:
930:
924:
920:
916:
913:
910:
905:
902:
899:
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861:
858:
855:
851:
828:
824:
803:
778:
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749:
743:
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729:
728:
721:
712:
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679:
675:
672:
669:
665:
664:
663:
655:
652:
648:
639:
630:
627:
608:
598:
592:
588:
585:
584:galactic disk
581:
580:density waves
577:
576:
575:
572:
570:
566:
562:
557:
545:
541:
536:
530:
526:
521:
512:
510:
506:
502:
498:
488:
486:
482:
478:
476:
472:
467:
465:
461:
460:BRI 1335-0417
452:
450:
449:proper motion
446:
442:
438:
435:close to the
434:
429:
427:
423:
419:
418:Population II
415:
410:
408:
404:
400:
396:
392:
391:galactic halo
388:
384:
379:
377:
373:
369:
365:
356:
351:
342:
334:
325:
323:
319:
318:active nuclei
315:
311:
306:
304:
300:
292:
288:
284:
280:
277:
271:
261:
258:
254:
250:
246:
242:
236:
233:
229:
224:
214:
208:
204:
201:
197:
195:
191:
188:
186:
182:
178:
175:
172:of stars and
171:
167:
166:
165:
158:
149:
147:
142:
140:
136:
132:
127:
126:) have bars.
125:
124:Hubble volume
121:
117:
113:
109:
103:
101:
95:
93:
89:
85:
81:
77:
73:
69:
65:
61:
57:
53:
46:
41:
37:
33:
19:
3950:Edwin Hubble
3835:In mythology
3775:Ursa Major I
3740:Reticulum II
3569:Virgo Stream
3538:Helmi stream
3533:Gaia Sausage
3485:Orion–Cygnus
3480:Norma–Cygnus
3396:Each arrow (
3283:
3271:
3006:fossil group
2928:Low activity
2762:Ultramassive
2592:Dwarf galaxy
2575:intermediate
2570:grand design
2549:
2465:
2442:
2426:. Retrieved
2422:the original
2366:
2362:
2341:. Retrieved
2335:
2325:
2308:
2304:
2298:
2286:
2261:
2257:
2248:
2234:
2225:
2198:
2192:
2182:
2170:
2158:
2115:
2111:
2105:
2093:. Retrieved
2085:
2076:
2067:
2048:
2013:
2009:
2003:
1979:
1955:. Retrieved
1952:ESA / Hubble
1951:
1942:
1905:
1899:
1889:
1877:. Retrieved
1871:
1858:
1813:
1809:
1799:
1785:
1771:
1761:10 September
1759:. Retrieved
1748:
1736:
1724:. Retrieved
1714:
1702:. Retrieved
1698:
1689:
1677:
1665:
1653:
1641:
1629:
1594:
1588:
1582:
1555:
1551:
1541:
1504:
1498:
1488:
1445:
1441:
1434:
1426:the original
1421:
1412:
1401:
1392:
1373:
1367:
1331:
1327:Hubble, E.P.
1321:
1296:Stellar halo
1086:
1064:
1053:Edwin Hubble
1037:Heber Curtis
1033:Great Debate
1026:
1001:
999:
951:
887:
795:
726:
701:
692:
688:
661:
644:
624:
596:
573:
560:
553:
494:
479:
475:dwarf galaxy
468:
458:
430:
426:Population I
411:
389:, a type of
386:
382:
380:
361:
339:
307:
296:
275:
273:
240:
239:
212:
163:
143:
128:
110:relative to
104:
96:
80:gas and dust
63:
60:Edwin Hubble
51:
50:
36:
3919:Outer space
3685:Eridanus II
3660:Canis Major
3359:Local Sheet
3353:Local Group
3065:void galaxy
3028:cannibalism
3013:Interacting
2969:Interaction
2955:Blue Nugget
2945:Dark galaxy
2850:Lyman-break
2742:Protogalaxy
2708:Disc galaxy
2470:Brady Haran
2311:: 315–316.
2264:: 236–274.
2016:: 646–655.
1873:EurekAlert!
1699:www.esa.int
1558:: 351–365.
1225:Ring galaxy
1177:Disc galaxy
678:shock waves
591:SSPSF model
424:than their
422:metallicity
374:), or in a
322:Messier 106
241:Spiral arms
217:Spiral arms
207:dark matter
74:containing
3929:Categories
3790:Ursa Minor
3645:Boötes III
3378:Local Hole
3105:Polar-ring
2950:Red nugget
2892:faint blue
2752:Spiral arm
2607:spheroidal
2597:elliptical
2580:Magellanic
2565:flocculent
2533:Lenticular
2520:Morphology
1915:1904.11436
1823:1710.11130
1704:30 January
1604:1811.08843
1314:References
1018:Messier 33
1014:Messier 99
1006:Lord Rosse
544:supernovae
501:Galaxy Zoo
485:Abell 1689
433:red dwarfs
395:retrograde
376:spheroidal
223:Spiral arm
45:Messier 77
3895:Astronomy
3800:Willman 1
3735:Pisces II
3640:Boötes II
3630:Antlia II
3583:Satellite
3553:Palomar 5
3419:Structure
3339:Milky Way
3327:Milky Way
3040:Satellite
3035:Jellyfish
3023:collision
2960:Dead disk
2877:Starburst
2792:Markarian
2664:Structure
2631:Irregular
2602:irregular
2125:0901.3503
1985:CRC Press
1850:119267114
1816:(1): 61.
1355:611263346
1118:Milky Way
1089:Milky Way
1071:Milky Way
1055:observed
1004:, due to
917:π
768:−
709:new stars
707:in which
651:Frank Shu
647:C. C. Lin
527:taken by
235:UGC 12158
152:Structure
131:Milky Way
3868:Category
3760:Sculptor
3695:Hercules
3675:Crater 2
3635:Boötes I
3585:galaxies
3392:Universe
3334:Location
3272:Category
3161:See also
3085:Galaxies
2812:X-shaped
2643:Peculiar
2585:unbarred
2543:unbarred
2512:Galaxies
2472:for the
2409:14500715
2401:10017873
2150:12461073
1597:(1): 2.
1480:14782284
1329:(1936).
1165:See also
540:NGC 1084
525:NGC 6384
499:through
481:A1689B11
464:redshift
399:inclined
345:Spheroid
291:infrared
287:NGC 1300
249:galaxies
245:unbarred
120:galaxies
116:universe
100:OB stars
3945:Spirals
3881:Portals
3813:Related
3795:Virgo I
3765:Sextans
3755:Segue 2
3750:Segue 1
3725:Phoenix
3490:Perseus
3132:Quasars
3100:Nearest
3095:Largest
2996:cluster
2829:Seyfert
2381:Bibcode
2343:17 June
2313:Bibcode
2266:Bibcode
2203:Bibcode
2201:: 811.
2130:Bibcode
2018:Bibcode
1957:2 April
1920:Bibcode
1879:11 June
1828:Bibcode
1609:Bibcode
1560:Bibcode
1519:Bibcode
1460:Bibcode
1360:Alt URL
1157:Malin 1
582:in the
550:History
491:Related
247:spiral
54:form a
3710:Leo IV
3705:Leo II
3690:Fornax
3665:Carina
3622:Dwarfs
3555:stream
3387:
3380:
3373:
3348:
3341:
3284:Portal
3115:Spiral
3018:merger
2797:Quasar
2782:Blazar
2720:corona
2636:barred
2612:spiral
2560:barred
2555:anemic
2550:Spiral
2538:barred
2428:24 May
2407:
2399:
2148:
2095:8 June
2060:
1991:
1848:
1726:20 May
1478:
1380:
1353:
1343:
1029:nebula
368:orbits
279:light.
253:spiral
3907:Stars
3720:Leo T
3715:Leo V
3700:Leo I
3680:Draco
3152:Voids
3077:Lists
3055:Walls
2991:group
2976:Field
2870:ELIRG
2865:HLIRG
2860:ULIRG
2817:DRAGN
2807:Radio
2787:LINER
2681:Bulge
2653:Polar
2405:S2CID
2371:arXiv
2146:S2CID
2120:arXiv
1910:arXiv
1846:S2CID
1818:arXiv
1757:. io9
1599:arXiv
1509:arXiv
1476:S2CID
1450:arXiv
1245:Other
796:with
471:BX442
403:merge
293:light
276:bulge
264:Bulge
181:bulge
84:bulge
76:stars
3515:Halo
3467:Disk
3110:Ring
2715:Halo
2703:Disc
2648:Ring
2528:Disc
2430:2006
2397:PMID
2345:2009
2097:2019
2058:ISBN
1989:ISBN
1959:2014
1881:2019
1763:2012
1728:2021
1706:2024
1378:ISBN
1351:OCLC
1341:ISBN
1087:The
1083:data
1081:WISE
1043:and
1016:and
649:and
443:and
414:dust
358:red.
209:halo
170:disc
129:The
88:halo
72:disk
2887:pea
2676:Bar
2389:doi
2309:120
2274:doi
2211:doi
2199:160
2138:doi
2116:465
2026:doi
2014:140
1928:doi
1906:487
1836:doi
1814:850
1617:doi
1568:doi
1556:236
1527:doi
1505:278
1468:doi
1446:630
1047:of
1039:of
870:3.2
437:Sun
385:or
328:Bar
289:in
3931::
2624:cD
2468:.
2464:.
2403:.
2395:.
2387:.
2379:.
2367:50
2365:.
2334:.
2307:.
2272:.
2262:63
2260:.
2209:.
2197:.
2191:.
2144:.
2136:.
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