
''This article is about a celestial body. For alternate meanings, see galaxy (disambiguation).'' [[Image: NGC_4414_(NASA-med).jpg|right|thumb|280px|NGC 4414, a typical spiral galaxy in the constellation Coma Berenices, is about 56,000 light years in diameter and approximately 60 million light years distant.]] A galaxy is a large gravitation system of star, interstellar medium, unseen dark matter, and possibly dark energy. Typical galaxies contain 10 million to one trillion (scientific notation to scientific notation) or more stars, all orbiting a common center of gravity. In addition to single stars and a tenuous interstellar medium, most galaxies contain a large number of star system and star cluster as well as various types of nebula. Most galaxies are several thousand to several hundred thousand light year in diameter and are usually separated from one another by distances on the order of millions of light years. Although so called dark matter and dark energy appear to account for well over 90% of the mass of most galaxies, the nature of these unseen components is not well understood. There is some evidence that supermassive black hole may exist at the center of many, if not all, galaxies. Intergalactic space, the space between galaxies, is a near vacuum with an average density of less than one atom per cubic meter of gas or dust. There are probably more than scientific notation galaxies in the visible universe. == Types of galaxies == Galaxies come in three main types: Elliptical galaxy, Spiral galaxy, and irregular galaxy. A slightly more extensive description of galaxy types is given by the Hubble sequence which serves well for many purposes. While the Hubble sequence does encompass all galaxies, it is entirely based upon visual mophological type. Hence it may miss the importance of certain characteristics of galaxies such as star formation rate. Our own galaxy, the Milky Way, sometimes simply called ''the Galaxy'' (with uppercase), is a large disk-shaped barred spiral galaxy about 1 E20 m or 100,000 light years in diameter and 3,000 light years in thickness. It contains about 3x1011 stars and has a total mass of about 6x1011 times the mass of the Sun. In ''spiral galaxies'', the spiral arms 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 also rotate around the center, but they do so with constant angular velocity. That means that stars pass in and out of spiral arms. The spiral arms are thought to be areas of high density or density waves. As stars move into an arm, they slow down, thus creating a higher density; this 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 they therefore harbor many bright and young stars. A new type of galaxy, Ultra Compact Dwarf Galaxies was discovered in 2003 by Dr Michael Drinkwater of the University of Queensland et al. == Larger scale structures == Only few galaxies exist by themselves; these are known as ''field galaxies''. Most galaxies are gravitationally bound to a number of other galaxies. Structures containing up to about 50 galaxies are called groups and clusters of galaxies, and larger structures containing many thousands of galaxies packed into an area a few megaparsecs across are called groups and clusters of galaxies. Superclusters are giant collections containing tens of thousands of galaxies, found in clusters, groups and sometimes individually; as far as we can tell the universe is uniform at scales above this. Our galaxy is a member of the Local Group, and together with the Andromeda Galaxy dominates it; overall the Local Group contains about 30 galaxies in a space about 1 E22 m across. The Local Group is part of the Local Supercluster, also known as the Virgo Supercluster. == History == This account of the history of the investigation of our own and other galaxies is largely taken from [1]. In 1610, Galileo Galilei used a telescope to study the bright band on the night sky known as the Milky Way and discovered that it was composed of a huge number of faint stars. In a treatise in 1755, Immanuel Kant, drawing on earlier work by Thomas Wright (astronomer), 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 much larger scales. The resulting disk of stars would be seen as a band on the sky from our perspective inside the disk. Kant also conjectured that some of the nebulae visible in the night sky might be separate galaxies. Towards the end of the 18th century, Charles Messier compiled a catalog containing the 109 brightest nebulae, later followed by a catalog of 5000 nebulae assembled by William Herschel. In 1845, William Parsons, 3rd Earl of 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. However, the nebulae were not universally accepted as distant separate galaxies until the matter was settled by Edwin Hubble in the early 1920s using a new telescope. He was able to resolve the outer parts of some spiral nebulae as collections of individual stars and identified some Cepheid variables, thus allowing to estimate the distance to the nebulae: they were far too distant to be part of the Milky Way. In 1936, Hubble produced a classification system for galaxies that is used to this day, the Hubble sequence. The first attempt to describe the shape of the Milky Way and the position of the Sun within it was carried out by William Herschel in 1785 by carefully counting the number of stars in different regions of the sky. Using a refined approach, Jacobus Kapteyn in 1920 arrived at the picture of a small (diameter ~15 kiloparsecs) ellipsoid galaxy with the Sun close to the center. A different method by Harlow Shapley based on the cataloging of globular clusters lead to a radically different picture: a flat disk with diameter ~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; once Robert Julius Trumpler had quantified this effect in 1930 by studying open clusters, the present picture of our galaxy as described above emerged. In 1944, Hendrik van de Hulst predicted microwave radiation at a wave length of 21 centimetres, resulting from interstellar atomic hydrogen gas; this radiation was observed in 1951. This radiation allowed for much improved study of the Galaxy, since it is not affected by dust absorption and its Doppler shift can be used to map the motion of the gas in the Galaxy. These observations led to the postulation of a rotating bar structure in the center of the Galaxy. With improved radio telescopes, hydrogen gas could also be traced in other galaxies. In the 1970s it was realized that the total visible mass of galaxies (from stars and gas) does not properly account for the speed of the rotating gas, thus leading to the postulation of dark matter. European_Southern_Observatory.">Image:Pr3 400galaxypix.jpg|225px|thumb|Galaxy Abell 1835 IR1916 is seen as a tiny dot in this photo of distant galaxies. Image courtesy of European Southern Observatory.Beginning in the 1990s, the Hubble Space Telescope yielded improved observations. Among other things, it established that the missing dark matter in our galaxy cannot solely consist of inherently faint and small stars. It photographed the Hubble Deep Field, providing evidence for hundreds of billions of galaxies in existence in the visible universe alone. In 2004, the galaxy Abell 1835 IR1916 became the most distant galaxy ever seen by humans. == Etymology == The word ''galaxy'' was derived from the Greek term for our own galaxy, ''kyklos galaktikos'' meaning "milky circle" for the system’s appearance in the sky. When astronomers speculated that certain objects previously classified as spiral nebulae were actually vast congeries of stars, this was called the "island universe theory"; but this was an obvious misnomer, since universe means everything there is. Consequently, this term fell into disuse, replaced by applying the term galaxy generically to all such bodies. == See also == * Timeline of galaxies, clusters of galaxies, and large scale structure * Galaxy formation and evolution * List of galaxies * List of nearest galaxies * Galaxy classification == References == * James Binney: ''Galactic astronomy'', Princeton University Press, 1998 == External links == *[http://www.seds.org/messier/galaxy.html Galaxies], SEDS Messier pages *[http://www.anzwers.org/free/universe/], An Atlas of The Universe Astronomy Galaxies Large-scale structure of the cosmos fa:کهکشان lv:Galaktika ms:Galaksi simple:Galaxy th:กาแล็กซี
Reason for reverting: in an article about a scientific subject ("galaxy" is a word invented by and for scientists, not some olden-days "spiritual" word), it's always possible to fill pages upon pages with "This is what the scientists think .... BUT, 'more advanced isoteric sources' say that ...", with a donzen alternate theories, but we should resits that "urge". The problem is that while thousands of scientists that study galaxies actually believe the kind of stuff written in the current article, the "esoteric" (spiritual, I'd call it) stuff you wrote about is hardly common belief, not even among any groups of spiritualists, astrologists, clerics of some religion, or anything. If you want to you explain how an esoteric school of thought called "Galaxism" (I'm just making this up, sorry) views galaxis, it would be much better if you added a "Galaxism's view on Galaxis" section in the Galaxism article, and in the Galaxy page add a link to that section, from the "Related Links". User:Nyh 07:39, 28 Apr 2004 (UTC) ::I believe the added stuff is just someone's joke and the material was not expected to stay!
::User:Arpingstone 14:58, 28 Apr 2004 (UTC) Would "galactographic" be an appropriate adjective equivalent to "geographical"? (A neologism, but it might be useful) User:Jackiespeel 19:42, 22 Mar 2005 (UTC) There is no proof that galaxies evolve on their own - the Big Bang is a speculative theory and has quite a few problems. If anyone disagrees, let me know. User:Salva31 02:33, 28 Apr 2005 (UTC) :Salva, you know people disagree with that. -- User:Temtem 03:24, Apr 28, 2005 (UTC) ::Yes, thank you, "Temptem." Those that do disagree comprise a shrinking minority. One of the major problems with the Big Bang theory is that it violates several laws of physics. These include, but are not limited to: the first law of thermodynamics and second law of thermodynamics, the conservation of angular momentum, etc. Although the general relativity does show us that our galaxy and the universe are expanding, it does not prove the Big Bang actually happened. If you disagree, then I suggest that you consider relearning about these important laws. By the way - if the Big Bang is true, then where did the laws of physics come from?? User:Salva31 15:04, 28 Apr 2005 (UTC) == Protogalaxies == Wouldn't it be a good idea to restore the reference to protogalaxies? -- User:Temtem 16:53, Apr 28, 2005 (UTC) :Not much to say about them; I think a link in the See Also section would be sufficient. User:Ben Standeven 20:12, 12 Jun 2005 (UTC)
{| style="background-color: #FFFFF8; float: right; margin-left: 4em; margin-bottom: 2em; border: 1px solid #999; border-right-width: 2px; border-bottom-width: 2px; white-space: nowrap;" |+ {} |- ! style="background-color: #FFFFC0;" colspan="2" | Observation data
(Epoch (astronomy) {}) |- ! style="text-align: left; vertical-align: baseline;" | Hubble sequence | {} |- ! style="text-align: left; vertical-align: baseline;" | Right ascension | {} |- ! style="text-align: left; vertical-align: baseline;" | Declination | {} |- ! style="text-align: left; vertical-align: baseline;" | Distance | {} ({}) |- ! style="text-align: left; vertical-align: baseline;" | Apparent magnitude (V) | {} |- ! style="text-align: left; vertical-align: baseline;" | Apparent dimensions (V) | {} |- ! style="background-color: #FFFFC0;" colspan="2" | Physical characteristics |- ! style="text-align: left; vertical-align: baseline;" | Mass | {} ({} Solar mass) |- ! style="text-align: left; vertical-align: baseline;" | Radius | {} |- ! style="text-align: left; vertical-align: baseline;" | Colour (B-V) | {} |- ! style="text-align: left; vertical-align: baseline;" | Absolute magnitude (V) | {} |- ! style="text-align: left; vertical-align: baseline;" | Notable features | {} |- ! style="text-align: left; vertical-align: baseline;" | Other designations | {} |}
See other meanings of words starting from letter:
Words begining with Galaxy:
Galaxy
Galaxy
Galaxy
Galaxy
Galaxy-class_starship
Galaxy-stub
Galaxy07
Galaxy07
Galaxyland
Galaxy_(candy)
Galaxy_(disambiguation)
Galaxy_(ship)
Galaxy_(ship)
Galaxy_(Star_Wars)
Galaxy_102
Galaxy_102
Galaxy_102.2
Galaxy_105
Galaxy_105-106
Galaxy_4
Galaxy_4
Galaxy_Abell_1835_IR1916
Galaxy_Abell_1835_IR1916
Galaxy_Angel
Galaxy_bulge
Galaxy_Cauldron
Galaxy_Class
Galaxy_class
Galaxy_classification
Galaxy_classification
Galaxy_Class_starship
Galaxy_Class_starship
Galaxy_class_starship
Galaxy_class_starship
Galaxy_cloud
Galaxy_clouds
Galaxy_clouds
Galaxy_cluster
Galaxy_clusters
Galaxy_clusters
Galaxy_cluster_cloud
Galaxy_compact_groups
Galaxy_disk
Galaxy_Express_999
Galaxy_Express_999
Galaxy_Federation
Galaxy_Federation_Government
Galaxy_Fight
Galaxy_filament
Galaxy_filaments
Galaxy_filaments
Galaxy_FM
Galaxy_formation
Galaxy_Formation_and_Evolution
Galaxy_Formation_and_Evolution
Galaxy_formation_and_evolution
Galaxy_formation_and_evolution
Galaxy_Four
Galaxy_Four
Galaxy_Group_HCG_87
Galaxy_Gun
Galaxy_Gun
Galaxy_halo
Galaxy_High
Galaxy_High
Galaxy_I
Galaxy_IV
Galaxy_listings
Galaxy_listings
Galaxy_M-33
Galaxy_M102
Galaxy_M33
Galaxy_Magazine
Galaxy_magazine
Galaxy_magazine
Galaxy_Manchester
Galaxy_Manchester
Galaxy_name_disambiguations
Galaxy_name_disambiguations
Galaxy_Network
Galaxy_NGC_3
Galaxy_NGC_3
Galaxy_NGC_7320
Galaxy_Power_Rangers
Galaxy_Press
Galaxy_Quest
Galaxy_Records
Galaxy_rotation_problem
Galaxy_rotation_problem
Galaxy_RXJ1242-11
Galaxy_Science_Fiction
Galaxy_Science_Fiction
Galaxy_science_fiction
Galaxy_science_fiction
Galaxy_science_fiction_magazine
Galaxy_song
Galaxy_stubs
Galaxy_subcluster
Galaxy_subclusters
Galaxy_subclusters
Galaxy_supercluster
Galaxy_superclusters
Galaxy_superclusters
Galaxy_survey
Galaxy_Trek
Galaxy
''This article is about a celestial body. For alternate meanings, see galaxy (disambiguation).'' [[Image: NGC_4414_(NASA-med).jpg|right|thumb|280px|NGC 4414, a typical spiral galaxy in the constellation Coma Berenices, is about 56,000 light years in diameter and approximately 60 million light years distant.]] A galaxy is a large gravitation system of star, interstellar medium, unseen dark matter, and possibly dark energy. Typical galaxies contain 10 million to one trillion (scientific notation to scientific notation) or more stars, all orbiting a common center of gravity. In addition to single stars and a tenuous interstellar medium, most galaxies contain a large number of star system and star cluster as well as various types of nebula. Most galaxies are several thousand to several hundred thousand light year in diameter and are usually separated from one another by distances on the order of millions of light years. Although so called dark matter and dark energy appear to account for well over 90% of the mass of most galaxies, the nature of these unseen components is not well understood. There is some evidence that supermassive black hole may exist at the center of many, if not all, galaxies. Intergalactic space, the space between galaxies, is a near vacuum with an average density of less than one atom per cubic meter of gas or dust. There are probably more than scientific notation galaxies in the visible universe. == Types of galaxies == Galaxies come in three main types: Elliptical galaxy, Spiral galaxy, and irregular galaxy. A slightly more extensive description of galaxy types is given by the Hubble sequence which serves well for many purposes. While the Hubble sequence does encompass all galaxies, it is entirely based upon visual mophological type. Hence it may miss the importance of certain characteristics of galaxies such as star formation rate. Our own galaxy, the Milky Way, sometimes simply called ''the Galaxy'' (with uppercase), is a large disk-shaped barred spiral galaxy about 1 E20 m or 100,000 light years in diameter and 3,000 light years in thickness. It contains about 3x1011 stars and has a total mass of about 6x1011 times the mass of the Sun. In ''spiral galaxies'', the spiral arms 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 also rotate around the center, but they do so with constant angular velocity. That means that stars pass in and out of spiral arms. The spiral arms are thought to be areas of high density or density waves. As stars move into an arm, they slow down, thus creating a higher density; this 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 they therefore harbor many bright and young stars. A new type of galaxy, Ultra Compact Dwarf Galaxies was discovered in 2003 by Dr Michael Drinkwater of the University of Queensland et al. == Larger scale structures == Only few galaxies exist by themselves; these are known as ''field galaxies''. Most galaxies are gravitationally bound to a number of other galaxies. Structures containing up to about 50 galaxies are called groups and clusters of galaxies, and larger structures containing many thousands of galaxies packed into an area a few megaparsecs across are called groups and clusters of galaxies. Superclusters are giant collections containing tens of thousands of galaxies, found in clusters, groups and sometimes individually; as far as we can tell the universe is uniform at scales above this. Our galaxy is a member of the Local Group, and together with the Andromeda Galaxy dominates it; overall the Local Group contains about 30 galaxies in a space about 1 E22 m across. The Local Group is part of the Local Supercluster, also known as the Virgo Supercluster. == History == This account of the history of the investigation of our own and other galaxies is largely taken from [1]. In 1610, Galileo Galilei used a telescope to study the bright band on the night sky known as the Milky Way and discovered that it was composed of a huge number of faint stars. In a treatise in 1755, Immanuel Kant, drawing on earlier work by Thomas Wright (astronomer), 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 much larger scales. The resulting disk of stars would be seen as a band on the sky from our perspective inside the disk. Kant also conjectured that some of the nebulae visible in the night sky might be separate galaxies. Towards the end of the 18th century, Charles Messier compiled a catalog containing the 109 brightest nebulae, later followed by a catalog of 5000 nebulae assembled by William Herschel. In 1845, William Parsons, 3rd Earl of 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. However, the nebulae were not universally accepted as distant separate galaxies until the matter was settled by Edwin Hubble in the early 1920s using a new telescope. He was able to resolve the outer parts of some spiral nebulae as collections of individual stars and identified some Cepheid variables, thus allowing to estimate the distance to the nebulae: they were far too distant to be part of the Milky Way. In 1936, Hubble produced a classification system for galaxies that is used to this day, the Hubble sequence. The first attempt to describe the shape of the Milky Way and the position of the Sun within it was carried out by William Herschel in 1785 by carefully counting the number of stars in different regions of the sky. Using a refined approach, Jacobus Kapteyn in 1920 arrived at the picture of a small (diameter ~15 kiloparsecs) ellipsoid galaxy with the Sun close to the center. A different method by Harlow Shapley based on the cataloging of globular clusters lead to a radically different picture: a flat disk with diameter ~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; once Robert Julius Trumpler had quantified this effect in 1930 by studying open clusters, the present picture of our galaxy as described above emerged. In 1944, Hendrik van de Hulst predicted microwave radiation at a wave length of 21 centimetres, resulting from interstellar atomic hydrogen gas; this radiation was observed in 1951. This radiation allowed for much improved study of the Galaxy, since it is not affected by dust absorption and its Doppler shift can be used to map the motion of the gas in the Galaxy. These observations led to the postulation of a rotating bar structure in the center of the Galaxy. With improved radio telescopes, hydrogen gas could also be traced in other galaxies. In the 1970s it was realized that the total visible mass of galaxies (from stars and gas) does not properly account for the speed of the rotating gas, thus leading to the postulation of dark matter. European_Southern_Observatory.">Image:Pr3 400galaxypix.jpg|225px|thumb|Galaxy Abell 1835 IR1916 is seen as a tiny dot in this photo of distant galaxies. Image courtesy of European Southern Observatory.Beginning in the 1990s, the Hubble Space Telescope yielded improved observations. Among other things, it established that the missing dark matter in our galaxy cannot solely consist of inherently faint and small stars. It photographed the Hubble Deep Field, providing evidence for hundreds of billions of galaxies in existence in the visible universe alone. In 2004, the galaxy Abell 1835 IR1916 became the most distant galaxy ever seen by humans. == Etymology == The word ''galaxy'' was derived from the Greek term for our own galaxy, ''kyklos galaktikos'' meaning "milky circle" for the system’s appearance in the sky. When astronomers speculated that certain objects previously classified as spiral nebulae were actually vast congeries of stars, this was called the "island universe theory"; but this was an obvious misnomer, since universe means everything there is. Consequently, this term fell into disuse, replaced by applying the term galaxy generically to all such bodies. == See also == * Timeline of galaxies, clusters of galaxies, and large scale structure * Galaxy formation and evolution * List of galaxies * List of nearest galaxies * Galaxy classification == References == * James Binney: ''Galactic astronomy'', Princeton University Press, 1998 == External links == *[http://www.seds.org/messier/galaxy.html Galaxies], SEDS Messier pages *[http://www.anzwers.org/free/universe/], An Atlas of The Universe Astronomy Galaxies Large-scale structure of the cosmos fa:کهکشان lv:Galaktika ms:Galaksi simple:Galaxy th:กาแล็กซี
Galaxy
Reason for reverting: in an article about a scientific subject ("galaxy" is a word invented by and for scientists, not some olden-days "spiritual" word), it's always possible to fill pages upon pages with "This is what the scientists think .... BUT, 'more advanced isoteric sources' say that ...", with a donzen alternate theories, but we should resits that "urge". The problem is that while thousands of scientists that study galaxies actually believe the kind of stuff written in the current article, the "esoteric" (spiritual, I'd call it) stuff you wrote about is hardly common belief, not even among any groups of spiritualists, astrologists, clerics of some religion, or anything. If you want to you explain how an esoteric school of thought called "Galaxism" (I'm just making this up, sorry) views galaxis, it would be much better if you added a "Galaxism's view on Galaxis" section in the Galaxism article, and in the Galaxy page add a link to that section, from the "Related Links". User:Nyh 07:39, 28 Apr 2004 (UTC) ::I believe the added stuff is just someone's joke and the material was not expected to stay!
::User:Arpingstone 14:58, 28 Apr 2004 (UTC) Would "galactographic" be an appropriate adjective equivalent to "geographical"? (A neologism, but it might be useful) User:Jackiespeel 19:42, 22 Mar 2005 (UTC) There is no proof that galaxies evolve on their own - the Big Bang is a speculative theory and has quite a few problems. If anyone disagrees, let me know. User:Salva31 02:33, 28 Apr 2005 (UTC) :Salva, you know people disagree with that. -- User:Temtem 03:24, Apr 28, 2005 (UTC) ::Yes, thank you, "Temptem." Those that do disagree comprise a shrinking minority. One of the major problems with the Big Bang theory is that it violates several laws of physics. These include, but are not limited to: the first law of thermodynamics and second law of thermodynamics, the conservation of angular momentum, etc. Although the general relativity does show us that our galaxy and the universe are expanding, it does not prove the Big Bang actually happened. If you disagree, then I suggest that you consider relearning about these important laws. By the way - if the Big Bang is true, then where did the laws of physics come from?? User:Salva31 15:04, 28 Apr 2005 (UTC) == Protogalaxies == Wouldn't it be a good idea to restore the reference to protogalaxies? -- User:Temtem 16:53, Apr 28, 2005 (UTC) :Not much to say about them; I think a link in the See Also section would be sufficient. User:Ben Standeven 20:12, 12 Jun 2005 (UTC)
Galaxy
Galaxy
{| style="background-color: #FFFFF8; float: right; margin-left: 4em; margin-bottom: 2em; border: 1px solid #999; border-right-width: 2px; border-bottom-width: 2px; white-space: nowrap;" |+ {} |- ! style="background-color: #FFFFC0;" colspan="2" | Observation data
(Epoch (astronomy) {}) |- ! style="text-align: left; vertical-align: baseline;" | Hubble sequence | {} |- ! style="text-align: left; vertical-align: baseline;" | Right ascension | {} |- ! style="text-align: left; vertical-align: baseline;" | Declination | {} |- ! style="text-align: left; vertical-align: baseline;" | Distance | {} ({}) |- ! style="text-align: left; vertical-align: baseline;" | Apparent magnitude (V) | {} |- ! style="text-align: left; vertical-align: baseline;" | Apparent dimensions (V) | {} |- ! style="background-color: #FFFFC0;" colspan="2" | Physical characteristics |- ! style="text-align: left; vertical-align: baseline;" | Mass | {} ({} Solar mass) |- ! style="text-align: left; vertical-align: baseline;" | Radius | {} |- ! style="text-align: left; vertical-align: baseline;" | Colour (B-V) | {} |- ! style="text-align: left; vertical-align: baseline;" | Absolute magnitude (V) | {} |- ! style="text-align: left; vertical-align: baseline;" | Notable features | {} |- ! style="text-align: left; vertical-align: baseline;" | Other designations | {} |}
See other meanings of words starting from letter:
G
GA | GB | GC | GD | GE | GF | GH | GI | GJ | GK | GL | GM | GN | GO | GP | GR | GS | GT | GU | GW | GX | GY | GZ |Words begining with Galaxy:
Galaxy
Galaxy
Galaxy
Galaxy
Galaxy-class_starship
Galaxy-stub
Galaxy07
Galaxy07
Galaxyland
Galaxy_(candy)
Galaxy_(disambiguation)
Galaxy_(ship)
Galaxy_(ship)
Galaxy_(Star_Wars)
Galaxy_102
Galaxy_102
Galaxy_102.2
Galaxy_105
Galaxy_105-106
Galaxy_4
Galaxy_4
Galaxy_Abell_1835_IR1916
Galaxy_Abell_1835_IR1916
Galaxy_Angel
Galaxy_bulge
Galaxy_Cauldron
Galaxy_Class
Galaxy_class
Galaxy_classification
Galaxy_classification
Galaxy_Class_starship
Galaxy_Class_starship
Galaxy_class_starship
Galaxy_class_starship
Galaxy_cloud
Galaxy_clouds
Galaxy_clouds
Galaxy_cluster
Galaxy_clusters
Galaxy_clusters
Galaxy_cluster_cloud
Galaxy_compact_groups
Galaxy_disk
Galaxy_Express_999
Galaxy_Express_999
Galaxy_Federation
Galaxy_Federation_Government
Galaxy_Fight
Galaxy_filament
Galaxy_filaments
Galaxy_filaments
Galaxy_FM
Galaxy_formation
Galaxy_Formation_and_Evolution
Galaxy_Formation_and_Evolution
Galaxy_formation_and_evolution
Galaxy_formation_and_evolution
Galaxy_Four
Galaxy_Four
Galaxy_Group_HCG_87
Galaxy_Gun
Galaxy_Gun
Galaxy_halo
Galaxy_High
Galaxy_High
Galaxy_I
Galaxy_IV
Galaxy_listings
Galaxy_listings
Galaxy_M-33
Galaxy_M102
Galaxy_M33
Galaxy_Magazine
Galaxy_magazine
Galaxy_magazine
Galaxy_Manchester
Galaxy_Manchester
Galaxy_name_disambiguations
Galaxy_name_disambiguations
Galaxy_Network
Galaxy_NGC_3
Galaxy_NGC_3
Galaxy_NGC_7320
Galaxy_Power_Rangers
Galaxy_Press
Galaxy_Quest
Galaxy_Records
Galaxy_rotation_problem
Galaxy_rotation_problem
Galaxy_RXJ1242-11
Galaxy_Science_Fiction
Galaxy_Science_Fiction
Galaxy_science_fiction
Galaxy_science_fiction
Galaxy_science_fiction_magazine
Galaxy_song
Galaxy_stubs
Galaxy_subcluster
Galaxy_subclusters
Galaxy_subclusters
Galaxy_supercluster
Galaxy_superclusters
Galaxy_superclusters
Galaxy_survey
Galaxy_Trek
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