|Type||SBc (barred spiral galaxy)|
|Diameter||100–120 kly (31–37 kpc)|
|Thickness of thin stellar disk||≈2 kly (0.6 kpc)|
|Number of stars||200-400 billion (3×1011 ±1×1011)|
|Oldest known star||>13.6 Gyr|
|Sun's distance to Galactic Center||27.2 ± 1.1 kly (8.34 ± 0.34 kpc)|
|Sun's Galactic rotation period||240 Myr|
|Spiral pattern rotation period||220–360 Myr|
|Bar pattern rotation period||100–120 Myr|
|Speed relative to CMB rest frame||552 ± 6 km/s|
|See also: Galaxy, List of galaxies|
The Milky Way is the galaxy that contains our Solar System.[nb 1] Its name “milky” is derived from its appearance as a dim glowing band arching across the night sky in which the naked eye cannot distinguish individual stars. The term “Milky Way” is a translation of the Latin via lactea, from the Greek γαλαξίας κύκλος (galaxías kýklos, "milky circle"). From the Earth, the Milky Way appears as a band because its disk-shaped structure is viewed from within the Galaxy. Galileo Galilei first resolved the band of light into individual stars with his telescope in 1610. Up until the early 1920s, most astronomers thought that all of the stars in the universe were contained inside of the Milky Way. Following the 1920 Great Debate between the astronomers Harlow Shapley and Heber Curtis, observations by Edwin Hubble definitively showed that the Milky Way is just one of many billions of galaxies.
The Milky Way is a barred spiral galaxy some 100,000–120,000 light-years in diameter, which contains 100–400 billion stars. It may contain at least as many planets as well. The Solar System is located within the disk, about 27,000 light-years away from the Galactic Center, on the inner edge of one of the spiral-shaped concentrations of gas and dust called the Orion Arm. The stars in the inner ≈10,000 light-years form a bulge and one or more bars that radiate from the bulge. The very center is marked by an intense radio source, named Sagittarius A*, which is likely to be a supermassive black hole.
Stars and gases at a wide range of distances from the Galactic center orbit at approximately 220 kilometers per second. The constant rotation speed contradicts the laws of Keplerian dynamics and suggests that much of the mass of the Milky Way does not emit or absorb electromagnetic radiation. This mass has been given the name “dark matter”. The rotational period is about 240 million years at the position of the Sun. The Galaxy as a whole is moving at a velocity of approximately 600 km per second with respect to extragalactic frames of reference. The oldest known star in the Galaxy is at least 13.82  billion years old and thus must have formed shortly after the Big Bang.
Surrounded by several smaller satellite galaxies, the Milky Way is part of the Local Group of galaxies, which forms a subcomponent of the Virgo Supercluster, which again forms a subcomponent of the Laniakea supercluster.
- 1 Appearance
- 2 Size and mass
- 3 Stars and planets
- 4 Structure
- 5 Formation
- 6 Environment
- 7 Velocity
- 8 Etymology and mythology
- 9 Astronomical history
- 10 See also
- 11 Notes
- 12 References
- 13 Further reading
- 14 External links
When observing the night sky, the term “Milky Way” is limited to the hazy band of white light some 30 degrees wide arcing across the sky. Although all of the individual stars that can be seen in the entire sky with the naked eye are part of the Milky Way Galaxy, the light in this band originates from the accumulation of un-resolved stars and other material when viewed in the direction of the Galactic plane. Dark regions within the band, such as the Great Rift and the Coalsack, correspond to areas where light from distant stars is blocked by interstellar dust.
The Milky Way has a relatively low surface brightness. Its visibility can be greatly reduced by background light such as light pollution or stray light from the moon. It is readily visible when the limiting magnitude is +5.1 or better, while showing a great deal of detail at +6.1. This makes the Milky Way difficult to see from any brightly lit urban or suburban location, but very prominent when viewed from a rural area when the moon is below the horizon.[nb 2]
As viewed from Earth, the visible region of the Milky Way’s Galactic plane occupies an area of the sky that includes 30 constellations. The center of the Galaxy lies in the direction of the constellation Sagittarius; it is here that the Milky Way is brightest. From Sagittarius, the hazy band of white light appears to pass westward to the Galactic anticenter in Auriga. The band then continues westward the rest of the way around the sky, back to Sagittarius. The band divides the night sky into two roughly equal hemispheres.
The Galactic plane is inclined by about 60 degrees to the ecliptic (the plane of the Earth’s orbit). Relative to the celestial equator, it passes as far north as the constellation of Cassiopeia and as far south as the constellation of Crux, indicating the high inclination of Earth’s equatorial plane and the plane of the ecliptic, relative to the Galactic plane. The north Galactic pole is situated at right ascension 12h 49m, declination +27.4° (B1950) near β Comae Berenices, and the south Galactic pole is near α Sculptoris. Because of this high inclination, depending on the time of night and year, the arc of Milky Way may appear relatively low or relatively high in the sky. For observers from approximately 65 degrees north to 65 degrees south on the Earth's surface, the Milky Way passes directly overhead twice a day.
Size and mass
The stellar disk of the Milky Way Galaxy is approximately 100,000 ly (30 kpc) in diameter, and is, on average, about 1,000 ly (0.3 kpc) thick. As a guide to the relative physical scale of the Milky Way, if it were reduced to 100 m in diameter, the Solar System, including the hypothesized Oort cloud, would be no more than 1 mm in width, about the size of a grain of sand. The nearest star, Proxima Centauri, would be 4.2 mm distant.[nb 3] Alternatively visualized, if the Solar System out to Neptune were the size of a US quarter (25mm), the Milky Way would have a diameter of 4,000 kilometers, or approximately the breadth of the United States.
Estimates for the mass of the Milky Way vary, depending upon the method and data used. At the low end of the estimate range, the mass of the Milky Way is 5.8×1011 solar masses (M☉), somewhat smaller than the Andromeda Galaxy. Measurements using the Very Long Baseline Array in 2009 found velocities as large as 254 km/s for stars at the outer edge of the Milky Way. As the orbital velocity depends on the total mass inside the orbital radius, this suggests that the Milky Way is more massive, roughly equaling the mass of Andromeda Galaxy at 7×1011 M☉ within 160,000 ly (49 kpc) of its center. A 2010 measurement of the radial velocity of halo stars finds the mass enclosed within 80 kiloparsecs is 7×1011 M☉. Most of the mass of the Galaxy appears to be matter of unknown form which interacts with other matter through gravitational but not electromagnetic forces; this is dubbed dark matter. A dark matter halo is spread out relatively uniformly to a distance beyond one hundred kiloparsecs from the Galactic Center. Mathematical models of the Milky Way suggest that the total mass of the entire Galaxy lies in the range 1–1.5×1012 M☉. More recent studies indicate a mass as large as 4.5×1012 M☉  and as small as 0.8×1012 M☉.
Stars and planets
The Milky Way contains at least 100 billion planets and between 200 and 400 billion stars. The exact figure depends on the number of very low-mass, or dwarf stars, which are hard to detect, especially at distances of more than 300 ly (90 pc) from the Sun. As a comparison, the neighboring Andromeda Galaxy contains an estimated one trillion (1012) stars. Filling the space between the stars is a disk of gas and dust called the interstellar medium. This disk has at least a comparable extent in radius to the stars, while the thickness of the gas layer ranges from hundreds of light years for the colder gas to thousands of light years for warmer gas. Both gravitational microlensing and planetary transit observations indicate that there may be at least as many planets bound to stars as there are stars in the Milky Way, while microlensing measurements indicate that there are more rogue planets not bound to host stars than there are stars. The Milky Way Galaxy contains at least one planet per star, resulting in 100–400 billion planets, according to a January 2013 study of the five-planet star system Kepler-32 with the Kepler space observatory. A different January 2013 analysis of Kepler data estimated that at least 17 billion Earth-sized exoplanets reside in the Milky Way Galaxy. On November 4, 2013, astronomers reported, based on Kepler space mission data, that there could be as many as 40 billion Earth-sized planets orbiting in the habitable zones of sun-like stars and red dwarf stars within the Milky Way Galaxy. 11 billion of these estimated planets may be orbiting sun-like stars. The nearest such planet may be 12 light-years away, according to the scientists. Such Earth-sized planets may be more numerous than gas giants. Besides exoplanets, "exocomets", comets beyond the Solar System, have also been detected and may be common in the Milky Way Galaxy.
The disk of stars in the Milky Way does not have a sharp edge beyond which there are no stars. Rather, the concentration of stars decreases with distance from the center of the Galaxy. For reasons that are not understood, beyond a radius of roughly 40,000 ly (13 kpc) from the center, the number of stars per cubic parsec drops much faster with radius. Surrounding the Galactic disk is a spherical Galactic Halo of stars and globular clusters that extends further outward, but is limited in size by the orbits of two Milky Way satellites, the Large and the Small Magellanic Clouds, whose closest approach to the Galactic center is about 180,000 ly (55 kpc). At this distance or beyond, the orbits of most halo objects would be disrupted by the Magellanic Clouds. Hence, such objects would probably be ejected from the vicinity of the Milky Way. The integrated absolute visual magnitude of the Milky Way is estimated to be −20.9.
The Galaxy consists of a bar-shaped core region surrounded by a disk of gas, dust and stars. The gas, dust and stars are organized in roughly logarithmic spiral arm structures (see Spiral arms below). The mass distribution within the Galaxy closely resembles the type SBc in the Hubble classification, which represents spiral galaxies with relatively loosely wound arms. Astronomers first began to suspect that the Milky Way is a barred spiral galaxy, rather than an ordinary spiral galaxy, in the 1990s. Their suspicions were confirmed by the Spitzer Space Telescope observations in 2005 that showed the Galaxy's central bar to be larger than previously suspected.
A galactic quadrant, or quadrant of the galaxy, refers to one of four circular sectors in the division of the Milky Way galaxy. In actual astronomical practice, the delineation of the galactic quadrants is based upon the galactic coordinate system, which places the Sun as the pole of the mapping system.
Quadrants are described using ordinals—for example, "1st galactic quadrant", "second galactic quadrant", or "third quadrant of the Galaxy". Viewing from the north galactic pole with 0 degrees (°) as the ray that runs starting from the Sun and through the galactic center, the quadrants are as follow:
- 1st galactic quadrant – 0° ≤ longitude (ℓ) ≤ 90°
- 2nd galactic quadrant – 90° ≤ ℓ ≤ 180°
- 3rd galactic quadrant – 180° ≤ ℓ ≤ 270°
- 4th galactic quadrant – 270° ≤ ℓ ≤ 360° (0°)
The Sun is 26,000–28,000 ly (8.0–8.6 kpc) from the Galactic Center. This value is estimated using geometric-based methods or by measuring selected astronomical objects that serve as standard candles, with different techniques yielding various values within this approximate range. In the inner few kpc (around 10,000 light-years radius) is a dense concentration of mostly old stars in a roughly spheroidal shape called the bulge. It has been proposed that our galaxy lacks a bulge formed due to a collision and merger between previous galaxies and that instead has a pseudobulge formed by its central bar.
The Galactic Center is marked by an intense radio source named Sagittarius A*. The motion of material around the center indicates that Sagittarius A* harbors a massive, compact object. This concentration of mass is best explained as a supermassive black hole[nb 4] with an estimated mass of 4.1–4.5 million times the mass of the Sun. Observations indicate that there are supermassive black holes located near the center of most normal galaxies.
The nature of the Galaxy's bar is actively debated, with estimates for its half-length and orientation spanning from 1–5 kpc (3,000–16,000 ly) and 10–50 degrees relative to the line of sight from Earth to the Galactic Center. Certain authors advocate that the Galaxy features two distinct bars, one nestled within the other. In most galaxies, Wang et al. report, the rate of accretion of the supermassive black hole is slow, but the Milky Way seems to be an important exception. X-ray emission is aligned with the massive stars surrounding the central bar. However, RR Lyr variables do not trace a prominent Galactic bar. The bar may be surrounded by a ring called the "5-kpc ring" that contains a large fraction of the molecular hydrogen present in the Galaxy, as well as most of the Milky Way's star-formation activity. Viewed from the Andromeda Galaxy, it would be the brightest feature of our own Galaxy.
In 2010, two gigantic spherical bubbles of high energy emission were detected to the north and the south of the Milky Way core, using data of the Fermi Gamma-ray Space Telescope. The diameter of each of the bubbles is about 25,000 light-years (7.7 kpc); they stretch up to Grus and to Virgo on the night-sky of the southern hemisphere. Subsequently, observations with the Parkes Telescope at radio frequencies identified polarized emission which is associated with the Fermi bubbles. These observations are best interpreted as a magnetized outflow driven by star formation in the central 640 ly (200 pc) of the Galaxy.
Outside the gravitational influence of the Galactic bars, astronomers generally organize the structure of the interstellar medium and stars in the disk of the Milky Way into four spiral arms. Spiral arms typically contain a higher density of interstellar gas and dust than the Galactic average as well as a greater concentration of star formation, as traced by H II regions and molecular clouds.
Maps of the Milky Way's spiral structure are notoriously uncertain and exhibit striking differences. Some 150 years after Alexander (1852) first suggested that the Milky Way was a spiral, there is currently no consensus on the nature of the Galaxy's spiral arms. Perfect logarithmic spiral patterns only crudely describe features near the Sun; namely since galaxies commonly exhibit arms that branch, merge, twist unexpectedly, and feature a degree of irregularity. The possible scenario of the Sun within a spur / Local arm emphasizes that point and indicates that such features are probably not unique, and exist elsewhere in the Galaxy.
As in most spiral galaxies, each spiral arm can be described as a logarithmic spiral. Estimates of the pitch angle of the arms range from about 7° to 25°. There are thought to be four spiral arms which all start near the Galaxy's center. These are named as follows, with the positions of the arms shown in the image at right:
|cyan||3-kpc Arm (Near 3 kpc Arm and Far 3 kpc Arm) and Perseus Arm|
|purple||Norma and Outer arm (Along with extension discovered in 2004)|
|There are at least two smaller arms or spurs, including:|
|orange||Orion–Cygnus Arm (which contains the Sun and Solar System)|
Two spiral arms, the Scutum–Centaurus arm and the Carina–Sagittarius arm, have tangent points inside the Sun's orbit about the center of the Milky Way. If these arms contain an overdensity of stars compared to the average density of stars in the Galactic disk, it would be detectable by counting the stars near the tangent point. Two surveys of near-infrared light, which is sensitive primarily to red giant stars and not affected by dust extinction, detected the predicted overabundance in the Scutum–Centaurus arm but not in the Carina–Sagittarius arm: the Scutum-Centaurus Arm contains approximately 30% more red giant stars than would be expected in the absence of a spiral arm. In 2008, Robert Benjamin of the University of Wisconsin–Whitewater used this observation to suggest that the Milky Way possesses only two major stellar arms: the Perseus arm and the Scutum–Centaurus arm. The rest of the arms contain excess gas but not excess old stars. In December 2013, astronomers found that the distribution of young stars and star-forming regions matches the four-arm spiral description of the Milky Way. Thus, the Galaxy appears to have two spiral arms as traced by old stars and four spiral arms as traced by gas and young stars. The explanation for this apparent discrepancy is unclear.
The Near 3 kpc Arm (also called Expanding 3 kpc Arm or simply 3 kpc Arm) was discovered in the 1950s by astronomer van Woerden and collaborators through 21-centimeter radio measurements of HI (atomic hydrogen). It was found to be expanding away from the center of the galaxy at more than 50 km/s. It is located in the fourth galactic quadrant at a distance of about 5.2 kpc from the Sun and 3.3 kpc from the galactic center. The Far 3 kpc Arm was discovered in 2008 by astronomer Tom Dame (Harvard-Smithsonian CfA). It's located in the first galactic quadrant at a distance of 3 kpc (about 10,000 ly) from the galactic center.
It has been suggested that the Milky Way contains two different spiral patterns: an inner one, formed by the Sagittarius arm, that rotates fast and an outer one, formed by the Carina and Perseus arms, whose rotation velocity is slower and whose arms are tightly wound. In this scenario, suggested by numerical simulations of the dynamics of the different spiral arms, the outer pattern would form an outer pseudoring and the two patterns would be connected by the Cygnus arm.
Outside of the major spiral arms is the Monoceros Ring (or Outer Ring), a ring of gas and stars torn from other galaxies billions of years ago.
The Galactic disk is surrounded by a spheroidal halo of old stars and globular clusters, of which 90% lie within 100,000 light-years (30 kpc) of the Galactic Center. However, a few globular clusters have been found farther, such as PAL 4 and AM1 at more than 200,000 light-years away from the Galactic Center. About 40% of the galaxy's clusters are on retrograde orbits, which means they move in the opposite direction from the Milky Way rotation. The globular clusters can follow rosette orbits about the Galaxy, in contrast to the elliptical orbit of a planet around a star.
While the disk contains dust which obscures the view in some wavelengths, the halo component does not. Active star formation takes place in the disk (especially in the spiral arms, which represent areas of high density), but does not take place in the halo, as there is little gas cool enough to collapse into stars. Open clusters are also located primarily in the disk.
Discoveries in the early 21st century have added dimension to the knowledge of the Milky Way's structure. With the discovery that the disk of the Andromeda Galaxy (M31) extends much further than previously thought, the possibility of the disk of the Milky Way Galaxy extending further is apparent, and this is supported by evidence from the 2004 discovery of the Outer Arm extension of the Cygnus Arm. With the discovery of the Sagittarius Dwarf Elliptical Galaxy came the discovery of a ribbon of galactic debris as the polar orbit of the dwarf and its interaction with the Milky Way tears it apart. Similarly, with the discovery of the Canis Major Dwarf Galaxy, it was found that a ring of galactic debris from its interaction with the Milky Way encircles the Galactic disk.
On January 9, 2006, Mario Jurić and others of Princeton University announced that the Sloan Digital Sky Survey of the northern sky found a huge and diffuse structure (spread out across an area around 5,000 times the size of a full moon) within the Milky Way that does not seem to fit within current models. The collection of stars rises close to perpendicular to the plane of the spiral arms of the Galaxy. The proposed likely interpretation is that a dwarf galaxy is merging with the Milky Way. This galaxy is tentatively named the Virgo Stellar Stream and is found in the direction of Virgo about 30,000 light-years (9 kpc) away.
In addition to the stellar halo, the Chandra X-ray Observatory, XMM-Newton, and Suzaku have provided evidence that there is a gaseous halo with a large amount of hot gas. The halo extends for hundreds of thousand of light years, much further than the stellar halo and close to the distance of the Large and Small Magellanic Clouds. The mass of this hot halo is nearly equivalent to the mass of the galaxy itself. The temperature of this halo gas is between 1 million and 2.5 million kelvin, a few hundred times hotter than the surface of the sun.
Observations of distant galaxies indicate that the Universe had about one-sixth as much baryonic (ordinary) matter as dark matter when it was just a few billion years old. However, only about half of those baryons are accounted for in the modern Universe based on observations of nearby galaxies like the Milky Way. If the finding that the mass of the halo is comparable to the mass of the galaxy is confirmed, it could be the identity of the missing baryons around the Milky Way.
Sun’s location and neighborhood
The Sun is near the inner rim of the Galaxy's Orion Arm, within the Local Fluff of the Local Bubble, and in the Gould Belt, at a distance of 8.33 ± 0.35 kiloparsecs (27,200 ± 1,100 ly) from the Galactic Center. The Sun is currently 5–30 parsecs (16–98 ly) from the central plane of the Galactic disk. The distance between the local arm and the next arm out, the Perseus Arm, is about 2,000 parsecs (6,500 ly). The Sun, and thus the Solar System, is found in the Galactic habitable zone.
There are about 208 stars brighter than absolute magnitude 8.5 within a sphere with a radius of 15 parsecs (49 ly) from the Sun, giving a density of one star per 69 cubic parsec, or one star per 2,360 cubic light-year (from List of nearest bright stars). On the other hand, there are 64 known stars (of any magnitude, not counting 4 brown dwarfs) within 5 parsecs (16 ly) of the Sun, giving a density of about one star per 8.2 cubic parsec, or one per 284 cubic light-year (from List of nearest stars). This illustrates the fact that there are far more faint stars than bright stars: in the entire sky, there are about 500 stars brighter than apparent magnitude 4 but 15.5 million stars brighter than apparent magnitude 14.
The apex of the Sun's way, or the solar apex, is the direction that the Sun travels through space in the Milky Way. The general direction of the Sun's Galactic motion is towards the star Vega near the constellation of Hercules, at an angle of roughly 60 sky degrees to the direction of the Galactic Center. The Sun's orbit about the Galaxy is expected to be roughly elliptical with the addition of perturbations due to the Galactic spiral arms and non-uniform mass distributions. In addition, the Sun oscillates up and down relative to the Galactic plane approximately 2.7 times per orbit. This is very similar to how a simple harmonic oscillator works with no drag force (damping) term. These oscillations were until recently thought to coincide with mass lifeform extinction periods on Earth. However, a reanalysis of the effects of the Sun's transit through the spiral structure based on CO data has failed to find a correlation.
It takes the Solar System about 240 million years to complete one orbit of the Galaxy (a Galactic year), so the Sun is thought to have completed 18–20 orbits during its lifetime and 1/1250 of a revolution since the origin of humans. The orbital speed of the Solar System about the center of the Galaxy is approximately 220 km/s or 0.073% of the speed of light. At this speed, it takes around 1,400 years for the Solar System to travel a distance of 1 light-year, or 8 days to travel 1 AU (astronomical unit).
The stars and gas in the Galaxy rotate about its center differentially, meaning that the rotation period varies with location. As is typical for spiral galaxies, the orbital speed of most stars in the Galaxy does not depend strongly on their distance from the center. Away from the central bulge or outer rim, the typical stellar orbital speed is between 210 and 240 km/s. Hence the orbital period of the typical star is directly proportional only to the length of the path traveled. This is unlike the situation within the Solar System, where two-body gravitational dynamics dominate and different orbits have significantly different velocities associated with them. The rotation curve (shown in the figure) describes this rotation. Toward the center of the galaxy the orbit speeds are too low while beyond 7 kpcs the speeds are too high to match what would be expected from the universal law of gravitation.
If the Galaxy contained only the mass observed in stars, gas, and other baryonic (ordinary) matter, the rotation speed would decrease with distance from the center. However, the observed curve is relatively flat, indicating that there is additional mass that cannot be detected directly with electromagnetic radiation. This inconsistency is attributed to dark matter. Alternatively, a minority of astronomers propose that a modification of the law of gravity may explain the observed rotation curve.
The Milky Way began as one or several small overdensities in the mass distribution in the Universe shortly after the Big Bang. Some of these overdensities were the seeds of globular clusters in which the oldest remaining stars in what is now the Milky Way formed. These stars and clusters now comprise the stellar halo of the Galaxy. Within a few billion years of the birth of the first stars, the mass of the Milky Way was large enough so that it was spinning relatively quickly. Due to conservation of angular momentum, this led the gaseous interstellar medium to collapse from a roughly spheroidal shape to a disk. Therefore, later generations of stars formed in this spiral disk. Most younger stars, including the Sun, are observed to be in the disk.
Since the first stars began to form, the Milky Way has grown through both galaxy mergers (particularly early in the Galaxy's growth) and accretion of gas directly from the Galactic halo. The Milky Way is currently accreting material from two of its nearest satellite galaxies, the Large and Small Magellanic Clouds, through the Magellanic Stream. Direct accretion of gas is observed in high-velocity clouds like the Smith Cloud. However, properties of the Milky Way such as stellar mass, angular momentum, and metallicity in its outermost regions suggest it has undergone no mergers with large galaxies in the last 10 billion years. This lack of recent major mergers is unusual among similar spiral galaxies; its neighbour the Andromeda Galaxy appears to have a more typical history shaped by more recent mergers with relatively large galaxies.
According to recent studies, the Milky Way as well as Andromeda lie in what in the galaxy color–magnitude diagram is known as the green valley, a region populated by galaxies in transition from the blue cloud (galaxies actively forming new stars) to the red sequence (galaxies that lack star formation). Star-formation activity in green valley galaxies is slowing as they run out of star-forming gas in the interstellar medium. In simulated galaxies with similar properties, star formation will typically have been extinguished within about five billion years from now, even accounting for the expected, short-term increase in the rate of star formation due to the collision between both our galaxy and the Andromeda Galaxy. In fact, measurements of other galaxies similar to our own suggest it is among the reddest and brightest spiral galaxies that are still forming new stars and it is just slightly bluer than the bluest red sequence galaxies.
The ages of individual stars in the Milky Way can be estimated by measuring the abundance of long-lived radioactive elements such as thorium-232 and uranium-238, then comparing the results to estimates of their original abundance, a technique called nucleocosmochronology. These yield values of about 12.5 ± 3 billion years for CS 31082-001 and 13.8 ± 4 billion years for BD +17° 3248. Once a white dwarf star is formed, it begins to undergo radiative cooling and the surface temperature steadily drops. By measuring the temperatures of the coolest of these white dwarfs and comparing them to their expected initial temperature, an age estimate can be made. With this technique, the age of the globular cluster M4 was estimated as 12.7 ± 0.7 billion years. Globular clusters are among the oldest objects in the Milky Way Galaxy, which thus set a lower limit on the age of the galaxy. Age estimates of the oldest of these clusters gives a best fit estimate of 12.6 billion years, and a 95% confidence upper limit of 16 billion years.
In 2007, a star in the galactic halo, HE 1523-0901, was estimated to be about 13.2 billion years old, ≈0.5 billion years less than the age of the universe. As the oldest known object in the Milky Way at that time, this measurement placed a lower limit on the age of the Milky Way. This estimate was determined using the UV-Visual Echelle Spectrograph of the Very Large Telescope to measure the relative strengths of spectral lines caused by the presence of thorium and other elements created by the R-process. The line strengths yield abundances of different elemental isotopes, from which an estimate of the age of the star can be derived using nucleocosmochronology.
The age of stars in the galactic thin disk has also been estimated using nucleocosmochronology. Measurements of thin disk stars yield an estimate that the thin disk formed 8.8 ± 1.7 billion years ago. These measurements suggest there was a hiatus of almost 5 billion years between the formation of the galactic halo and the thin disk.
The Milky Way and the Andromeda Galaxy are a binary system of giant spiral galaxies belonging to a group of 50 closely bound galaxies known as the Local Group, itself being part of the Virgo Supercluster.
Two smaller galaxies and a number of dwarf galaxies in the Local Group orbit the Milky Way. The largest of these is the Large Magellanic Cloud with a diameter of 14,000 light-years. It has a close companion, the Small Magellanic Cloud. The Magellanic Stream is a stream of neutral hydrogen gas extending from these two small galaxies across 100° of the sky. The stream is thought to have been dragged from the Magellanic Clouds in tidal interactions with the Milky Way. Some of the dwarf galaxies orbiting the Milky Way are Canis Major Dwarf (the closest), Sagittarius Dwarf Elliptical Galaxy, Ursa Minor Dwarf, Sculptor Dwarf, Sextans Dwarf, Fornax Dwarf, and Leo I Dwarf. The smallest Milky Way dwarf galaxies are only 500 light-years in diameter. These include Carina Dwarf, Draco Dwarf, and Leo II Dwarf. There may still be undetected dwarf galaxies which are dynamically bound to the Milky Way, as well as some that have already been absorbed by the Milky Way, such as Omega Centauri.
In January 2006, researchers reported that the heretofore unexplained warp in the disk of the Milky Way has now been mapped and found to be a ripple or vibration set up by the Large and Small Magellanic Clouds as they circle the Galaxy, causing vibrations when they pass through its edges. Previously, these two galaxies, at around 2% of the mass of the Milky Way, were considered too small to influence the Milky Way. However, in a computer model, the movement of these two galaxies creates a dark matter wake that amplifies their influence on the larger Milky Way.
Current measurements suggest the Andromeda Galaxy is approaching us at 100 to 140 kilometers per second. In 3 to 4 billion years, there may be an Andromeda–Milky Way collision, depending on the importance of unknown lateral components to the galaxies' relative motion. If they collide, the chance of individual stars colliding with each other is extremely low, but instead the two galaxies will merge to form a single elliptical galaxy over the course of about a billion years.
Although special relativity states that there is no "preferred" inertial frame of reference in space with which to compare the Milky Way, the Galaxy does have a velocity with respect to cosmological frames of reference.
One such frame of reference is the Hubble flow, the apparent motions of galaxy clusters due to the expansion of space. Individual galaxies, including the Milky Way, have peculiar velocities relative to the average flow. Thus, to compare the Milky Way to the Hubble flow, one must consider a volume large enough so that the expansion of the Universe dominates over local, random motions. A large enough volume means that the mean motion of galaxies within this volume is equal to the Hubble flow. Astronomers believe the Milky Way is moving at approximately 630 km per second with respect to this local co-moving frame of reference. The Milky Way is moving in the general direction of the Great Attractor and other galaxy clusters, including the Shapley supercluster, behind it. The Local Group (a cluster of gravitationally bound galaxies containing, among others, the Milky Way and the Andromeda Galaxy) is part of a supercluster called the Local Supercluster, centered near the Virgo Cluster: although they are moving away from each other at 967 km/s as part of the Hubble flow, this velocity is less than would be expected given the 16.8 million pc distance due to the gravitational attraction between the Local Group and the Virgo Cluster.
Another reference frame is provided by the cosmic microwave background (CMB). The Milky Way is moving at 552 ± 6 km/s with respect to the photons of the CMB, toward 10.5 right ascension, −24° declination (J2000 epoch, near the center of Hydra). This motion is observed by satellites such as the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP) as a dipole contribution to the CMB, as photons in equilibrium in the CMB frame get blue-shifted in the direction of the motion and red-shifted in the opposite direction.
Etymology and mythology
In western culture the name "Milky Way" is derived from its appearance as a dim un-resolved "milky" glowing band arching across the night sky. The term is a translation of the Classical Latin via lactea, in turn derived from the Hellenistic Greek γαλαξίας, short for γαλαξίας κύκλος (pr. galaktikos kyklos, "milky circle"). The Ancient Greek γαλαξίας (galaxias), from root γαλακτ-, γάλα (milk) + -ίας (forming adjectives), is also the root of "galaxy", the name for our, and later all such, collections of stars. The Milky Way "milk circle" was just one of 11 circles the Greeks identified in the sky, others being the zodiac, the meridian, the horizon, the equator, the tropics of Cancer and Capricorn, Arctic and Antarctic circles, and two colure circles passing through both poles.
In Meteorologica (DK 59 A80), Aristotle (384–322 BC) wrote that the Greek philosophers Anaxagoras (ca. 500–428 BC) and Democritus (460–370 BC) proposed that the Milky Way might consist of distant stars. However, Aristotle himself believed the Milky Way to be caused by "the ignition of the fiery exhalation of some stars which 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 which is continuous with the heavenly motions." The Neoplatonist philosopher Olympiodorus the Younger (c. 495–570 A.D.) criticized this view, arguing that if the Milky Way were sublunary it should appear different at different times and places on the Earth, and that it should have parallax, which it does not. In his view, the Milky Way was celestial. This idea would be influential later in the Islamic world.
The Persian astronomer Abū Rayhān al-Bīrūnī (973–1048) proposed that the Milky Way is "a collection of countless fragments of the nature of nebulous stars". The Andalusian astronomer Avempace (d. 1138) proposed the Milky Way to be made up of many stars but appears to be a continuous image due to the effect of refraction in the Earth's atmosphere, citing his observation of a conjunction of Jupiter and Mars in 1106 or 1107 as evidence. Ibn Qayyim Al-Jawziyya (1292–1350) proposed that the Milky Way is "a myriad of tiny stars packed together in the sphere of the fixed stars" and that these stars are larger than planets.
According to Jamil Ragep, the Persian astronomer Naṣīr al-Dīn al-Ṭūsī (1201–1274) in his Tadhkira writes: "The Milky Way, i.e. the Galaxy, is made up of a very large number of small, tightly clustered stars, which, on account of their concentration and smallness, seem to be cloudy patches. Because of this, it was likened to milk in color."
Actual proof of the Milky Way consisting of many stars came in 1610 when Galileo Galilei used a telescope to study 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, speculated (correctly) that the Milky Way 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" themselves, similar to our own. Kant referred to both our Galaxy and the "extragalactic nebulae" as "island universes", a term still current up to the 1930s.
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 visible sky. He produced a diagram of the shape of the Galaxy with the Solar System close to the center.
In 1845, Lord Rosse constructed a new telescope and was able to distinguish between elliptical and spiral-shaped nebulae. He also managed to make out individual point sources in some of these nebulae, lending credence to Kant's earlier conjecture.
In 1917, Heber Curtis had observed the nova S Andromedae within the Great Andromeda Nebula (Messier object 31). 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 "island universes" hypothesis, which held that the spiral nebulae were actually independent galaxies. In 1920 the Great Debate took place between Harlow Shapley and Heber Curtis, concerning the nature of the Milky Way, spiral nebulae, and the dimensions of the universe. To support his claim that the Great Andromeda Nebula was 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.
The matter was conclusively settled by Edwin Hubble in the early 1920s using the Mount Wilson observatory 2.5 m Hooker telescope. With the light-gathering power of this new telescope he was able to produce astronomical photographs that resolved the outer parts of some spiral nebulae as collections of individual stars. He was also able to identify some Cepheid variables that he could use as a benchmark to estimate the distance to the nebulae. He found that the Andromeda Nebula is 275,000 parsecs from the Sun, far too distant to be part of the Milky Way.
- Baade's Window
- Galactic coordinate system
- MilkyWay@Home, a distributed computing project that attempts to generate highly accurate three-dimensional dynamic models of stellar streams in the immediate vicinity of our Milky Way Galaxy.
- NGC 6744, a galaxy thought to closely resemble the Milky Way
- Oort constants
- Jay M. Pasachoff in his textbook Astronomy: From the Earth to the Universe states the term Milky Way should refer exclusively to the band of light that the galaxy forms in the night sky, while the galaxy should receive the full name Milky Way Galaxy. See:
- See also Bortle Dark-Sky Scale.
- The scale is 1 mm equals 1 ly.
- For a photo see: "Sagittarius A*: Milky Way monster stars in cosmic reality show". Chandra X-ray Observatory. Harvard-Smithsonian Center for Astrophysics. January 6, 2003. Retrieved 2012-05-20.
- Gerhard, O. (2002). "Mass distribution in our Galaxy". Space Science Reviews 100 (1/4): 129–138. arXiv:astro-ph/0203110. Bibcode:2002astro.ph..3110G. doi:10.1023/A:1015818111633.
- Christian, Eric; Safi-Harb, Samar. "How large is the Milky Way?". NASA: Ask an Astrophysicist. Retrieved 2007-11-28.
- Rix, Hans-Walter and Bovy, Jo (2013). "The Milky Way's Stellar Disk". The Astronomy and Astrophysics Review. in press. arXiv:1301.3168. Bibcode:2013A&ARv..21...61R. doi:10.1007/s00159-013-0061-8.
- "NASA – Galaxy". NASA and World Book. Nasa.gov. November 29, 2007. Archived from the original on 2009-04-12. Retrieved 2012-12-06.
- Staff (December 16, 2008). "How Many Stars are in the Milky Way?". Universe Today. Retrieved 2010-08-10.
- Odenwald, S. (March 17, 2014). "Counting the Stars in the Milky Way". The Huffington Post. Retrieved 2014-06-09.
- H.E. Bond; E. P. Nelan; D. A. VandenBerg; G. H. Schaefer; D. Harmer (February 13, 2013). "HD 140283: A Star in the Solar Neighborhood that Formed Shortly After the Big Bang". The Astrophysical Journal 765 (1): L12. arXiv:1302.3180. Bibcode:2013ApJ...765L..12B. doi:10.1088/2041-8205/765/1/L12.
- McMillan, P. J. (July 2011). "Mass models of the Milky Way". Monthly Notices of the Royal Astronomical Society 414 (3): 2446–2457. arXiv:1102.4340. Bibcode:2011MNRAS.414.2446M. doi:10.1111/j.1365-2966.2011.18564.x.
- Kafle, P.R.; Sharma, S.; Lewis, G.F.; Bland-Hawthorn, J. (2012). "Kinematics of the Stellar Halo and the Mass Distribution of the Milky Way Using Blue Horizontal Branch Stars". The Astrophysical Journal 761 (2): 17. doi:10.1088/0004-637X/761/2/98.
- Gillessen, S. et al. (2009). "Monitoring stellar orbits around the massive black hole in the Galactic Center". Astrophysical Journal 692 (2): 1075–1109. arXiv:0810.4674. Bibcode:2009ApJ...692.1075G. doi:10.1088/0004-637X/692/2/1075.
- Sparke, Linda S.; Gallagher, John S. (2007). Galaxies in the Universe: An Introduction. p. 90. ISBN 9781139462389.
- Gerhard, O. Pattern speeds in the Milky Way. arXiv:1003.2489v1.
- Kogut, A. et al. (1993). "Dipole anisotropy in the COBE differential microwave radiometers first-year sky maps". The Astrophysical Journal 419: 1. arXiv:astro-ph/9312056. Bibcode:1993ApJ...419....1K. doi:10.1086/173453.
- "Milky Way". Oxford University Press. Retrieved 2012-10-31.
- "Milky Way Galaxy". Merriam-Webster Incorportated. Retrieved 2012-10-31.
- "Milky Way Galaxy". Encyclopædia Britannica, Inc. Retrieved 2012-10-31.
- Harper, Douglas. "galaxy". Online Etymology Dictionary. Retrieved 2012-05-20.
- Jankowski, Connie (2010). Pioneers of Light and Sound. Compass Point Books. p. 6. ISBN 0-7565-4306-1.
- Schiller, Jon (2010). Big Bang & Black Holes. CreateSpace. p. 163. ISBN 1-4528-6552-3.
- Shapley, H.; Curtis, H. D. (1921). "The Scale of the Universe". Bulletin of the National Research Council 2: 171–217. Bibcode:1921BuNRC...2..171S.
- Sandage, Allan (1989). "Edwin Hubble, 1889–1953". Journal of the Royal Astronomical Society of Canada 83 (6). Bibcode:1989JRASC..83..351S.
- Cassan, A. et al. (January 11, 2012). "One or more bound planets per Milky Way star from microlensing observations". Nature 481 (7380): 167–169. arXiv:1202.0903. Bibcode:2012Natur.481..167C. doi:10.1038/nature10684. PMID 22237108.
- Staff (January 2, 2013). "100 Billion Alien Planets Fill Our Milky Way Galaxy: Study". Space.com. Retrieved January 3, 2013.
- Koupelis, Theo; Kuhn, Karl F. (2007). In Quest of the Universe. Jones & Bartlett Publishers. p. 492; Figure 16-13. ISBN 0-7637-4387-9.
- youtube.com: Laniakea: Our home supercluster
- 4 September 2014, nature.com: The Laniakea supercluster of galaxies
- Pasachoff, Jay M. (1994). Astronomy: From the Earth to the Universe. Harcourt School. p. 500. ISBN 0-03-001667-3.
- H. A. Rey (1976). The Stars. Houghton Mifflin Harcourt. p. 145. ISBN 0395248302.
- Steinicke, Wolfgang; Jakiel, Richard (2007). Galaxies and how to observe them. Astronomers' observing guides. Springer. p. 94. ISBN 1-85233-752-4.
- "How Big is Our Universe: How far is it across the Milky Way?". NASA-Smithsonian Education Forum on the Structure and Evolution of the Universe, at the Harvard Smithsonian Center for Astrophysics. Retrieved March 13, 2013.
- Karachentsev, I. D.; Kashibadze, O. G. (2006). "Masses of the local group and of the M81 group estimated from distortions in the local velocity field". Astrophysics 49 (1): 3–18. Bibcode:2006Ap.....49....3K. doi:10.1007/s10511-006-0002-6.
- Vayntrub, Alina (2000). "Mass of the Milky Way". The Physics Factbook. Retrieved 2007-05-09.
- Battaglia, G. et al. (2005). "The radial velocity dispersion profile of the Galactic halo: Constraining the density profile of the dark halo of the Milky Way". Monthly Notices of the Royal Astronomical Society: 433–442. arXiv:astro-ph/0506102. Bibcode:2005MNRAS.364..433B. doi:10.1111/j.1365-2966.2005.09367.x.
- Finley, Dave; Aguilar, David (January 5, 2009). "Milky Way a Swifter Spinner, More Massive, New Measurements Show". National Radio Astronomy Observatory. Retrieved 2009-01-20.
- Reid, M. J. et al. (2009). "Trigonometric parallaxes of massive star-forming regions. VI. Galactic structure, fundamental parameters, and noncircular motions". The Astrophysical Journal 700: 137–148. arXiv:0902.3913. Bibcode:2009ApJ...700..137R. doi:10.1088/0004-637X/700/1/137.
- Gnedin, O. Y. et al. (2010). "The mass profile of the Galaxy to 80 kpc". The Astrophysical Journal 720: L108. arXiv:1005.2619. Bibcode:2010ApJ...720L.108G. doi:10.1088/2041-8205/720/1/L108.
- "The mass of the Milky Way and M31 using the method of least action". Retrieved February 6, 2014.
- "On the shoulders of Giants: Properties of the Stellar Halo and the Milky Way mass distribution". Retrieved August 8, 2014.
- Villard, Ray (January 11, 2012). "The Milky Way Contains at Least 100 Billion Planets According to Survey". HubbleSite.org. Retrieved 2012-01-11.
- Frommert, H.; Kronberg, C. (August 25, 2005). "The Milky Way Galaxy". SEDS. Retrieved 2007-05-09.
- Wethington, Nicholos. "How Many Stars are in the Milky Way?". Retrieved 2010-04-09.
- Young, Kelly (June 6, 2006). "Andromeda Galaxy hosts a trillion stars". NewScientist. Retrieved 2006-06-08.
- Levine, E. S.; Blitz, L.; Heiles, C. (2006). "The spiral structure of the outer Milky Way in hydrogen". Science 312 (5781): 1773–1777. arXiv:astro-ph/0605728. Bibcode:2006Sci...312.1773L. doi:10.1126/science.1128455. PMID 16741076.
- Dickey, J. M.; Lockman, F. J. (1990). "H I in the Galaxy". Annual Review of Astronomy and Astrophysics 28: 215. Bibcode:1990ARA&A..28..215D. doi:10.1146/annurev.aa.28.090190.001243.
- Savage, B. D.; Wakker, B. P. (2009). "The extension of the transition temperature plasma into the lower galactic halo". The Astrophysical Journal 702 (2): 1472. arXiv:0907.4955. Bibcode:2009ApJ...702.1472S. doi:10.1088/0004-637X/702/2/1472.
- Borenstein, Seth (February 19, 2011). "Cosmic census finds crowd of planets in our galaxy". The Washington Post. Associated Press. Archived from the original on 2011-02-21.
- Sumi, T. et al. (2011). "Unbound or distant planetary mass population detected by gravitational microlensing". Nature 473 (7347): 349–352. arXiv:1105.3544. Bibcode:2011Natur.473..349S. doi:10.1038/nature10092. PMID 21593867.
- "Free-Floating Planets May be More Common Than Stars". Pasadena, CA: NASA's Jet Propulsion Laboratory. February 18, 2011. Archived from the original on 2011-05-25. "The team estimates there are about twice as many of them as stars."
- Staff (January 7, 2013). "17 Billion Earth-Size Alien Planets Inhabit Milky Way". Space.com. Retrieved January 8, 2013.
- Overbye, Dennis (November 4, 2013). "Far-Off Planets Like the Earth Dot the Galaxy". New York Times. Retrieved November 5, 2013.
- Petigura, Eric A.; Howard, Andrew W.; Marcy, Geoffrey W. (October 31, 2013). "Prevalence of Earth-size planets orbiting Sun-like stars". Proceedings of the National Academy of Sciences of the United States of America. arXiv:1311.6806. Bibcode:2013PNAS..11019273P. doi:10.1073/pnas.1319909110. Retrieved November 5, 2013.
- Borenstein, Seth (2013-11-04). "8.8 billion habitable Earth-size planets exist in Milky Way alone". The Associated Press. NBC News.
- Khan, Amina (4 November 2013). "Milky Way may host billions of Earth-size planets". Los Angeles Times. Retrieved 5 November 2013.
- Sale, S. E. et al. (2010). "The structure of the outer Galactic disc as revealed by IPHAS early A stars". Monthly Notices of the Royal Astronomical Society 402 (2): 713–723. arXiv:0909.3857. Bibcode:2010MNRAS.402..713S. doi:10.1111/j.1365-2966.2009.15746.x.
- Connors, Tim W.; Kawata, Daisuke; Gibson, Brad K. (2006). "N-body simulations of the Magellanic stream". Monthly Notices of the Royal Astronomical Society 371 (1): 108–120. arXiv:astro-ph/0508390. Bibcode:2006MNRAS.371..108C. doi:10.1111/j.1365-2966.2006.10659.x.
- Coffey, Jerry. "Absolute Magnitude". Retrieved 2010-04-0.
- Benjamin, R. A. (2008). "The Spiral Structure of the Galaxy: Something Old, Something New...". In Beuther, H.; Linz, H.; Henning, T. (ed.). Massive Star Formation: Observations Confront Theory 387. Astronomical Society of the Pacific Conference Series. p. 375. Bibcode:2008ASPC..387..375B.
See also Bryner, Jeanna (June 3, 2008). "New Images: Milky Way Loses Two Arms". Space.com. Retrieved 2008-06-04.
- Chen, W.; Gehrels, N.; Diehl, R.; Hartmann, D. (1996). "On the spiral arm interpretation of COMPTEL ^26^Al map features". Space Science Reviews 120: 315–316. Bibcode:1996A&AS..120C.315C.
- McKee, Maggie (August 16, 2005). "Bar at Milky Way's heart revealed". New Scientist. Retrieved 2009-06-17.
- Thomas L. Wilson, Kristen Rohlfs, Susanne Hüttemeister Tools of radio astronomy
- "Far-infrared loops in the 2nd Galactic Quadrant". NASA Astrophysics Data. Adsabs.harvard.edu. Retrieved 2010-08-17.
- M. Lampton et al. An All-Sky Catalog of Faint Extreme Ultraviolet Sources The Astrophysical Journal Supplement Series . 1997
- THE BEGINNINGS OF RADIO ASTRONOMY IN THE NETHERLANDS. Journal of Astronomical History and Heritage. 2006
- Ghez, A. M. et al. (December 2008). "Measuring distance and properties of the Milky Way's central supermassive black hole with stellar orbits". The Astrophysical Journal 689 (2): 1044–1062. arXiv:0808.2870. Bibcode:2008ApJ...689.1044G. doi:10.1086/592738.
- Reid, M. J. et al. (November 2009). "A trigonometric parallax of Sgr B2". The Astrophysical Journal 705 (2): 1548–1553. arXiv:0908.3637. Bibcode:2009ApJ...705.1548R. doi:10.1088/0004-637X/705/2/1548.
- Vanhollebeke, E.; Groenewegen, M. A. T.; Girardi, L. (April 2009). "Stellar populations in the Galactic bulge. Modelling the Galactic bulge with TRILEGAL". Astronomy and Astrophysics 498: 95–107. Bibcode:2009A&A...498...95V. doi:10.1051/0004-6361/20078472.
- Majaess, D. (March 2010). "Concerning the Distance to the Center of the Milky Way and Its Structure". Acta Astronomica 60 (1): 55. arXiv:1002.2743. Bibcode:2010AcA....60...55M.
- Grant, J.; Lin, B. (2000). "The Stars of the Milky Way". Fairfax Public Access Corporation. Retrieved 2007-05-09.
- Shen, J.; Rich, R. M.; Kormendy, J.; Howard, C. D.; De Propris, R.; Kunder, A. (2010). "Our Milky Way As a Pure-Disk Galaxy—A Challenge for Galaxy Formation". The Astrophysical Journal 720: L72. arXiv:1005.0385. Bibcode:2010ApJ...720L..72S. doi:10.1088/2041-8205/720/1/L72.
- Jones, Mark H.; Lambourne, Robert J.; Adams, David John (2004). An Introduction to Galaxies and Cosmology. Cambridge University Press. pp. 50–51. ISBN 0-521-54623-0.
- Blandford, R. D. (1999). "Origin and Evolution of Massive Black Holes in Galactic Nuclei". Galaxy Dynamics, proceedings of a conference held at Rutgers University, 8–12 August 1998, ASP Conference Series vol. 182. Bibcode:1999ASPC..182...87B.
- Frolov, Valeri P.; Zelnikov, Andrei (2011). Introduction to Black Hole Physics. Oxford University Press. pp. 11, 36. ISBN 0199692297.
- Cabrera-Lavers, A. et al. (December 2008). "The long Galactic bar as seen by UKIDSS Galactic plane survey". Astronomy and Astrophysics 491 (3): 781–787. arXiv:0809.3174. Bibcode:2008A&A...491..781C. doi:10.1051/0004-6361:200810720.
- Nishiyama, S. et al. (2005). "A distinct structure inside the Galactic bar". The Astrophysical Journal 621 (2): L105. arXiv:astro-ph/0502058. Bibcode:2005ApJ...621L.105N. doi:10.1086/429291.
- Wang, Q. D.; Nowak, M. A.; Markoff, S. B.; Baganoff, F. K.; Nayakshin, S.; Yuan, F.; Cuadra, J.; Davis, J.; Dexter, J.; Fabian, A. C.; Grosso, N.; Haggard, D.; Houck, J.; Ji, L.; Li, Z.; Neilsen, J.; Porquet, D.; Ripple, F.; Shcherbakov, R. V. (2013). "Dissecting X-ray-Emitting Gas Around the Center of Our Galaxy". Science 341 (6149): 981–983. doi:10.1126/science.1240755. PMID 23990554.
- Alcock, C. et al. (1998). "The RR Lyrae population of the Galactic Bulge from the MACHO database: mean colors and magnitudes". The Astrophysical Journal 492 (2): 190. arXiv:astro-ph/0502058. Bibcode:2005ApJ...621L.105N. doi:10.1086/305017.
- Kunder, A.; Chaboyer, B. (2008). "Metallicity analysis of Macho Galactic Bulge RR0 Lyrae stars from their light curves". The Astronomical Journal 136 (6): 2441. arXiv:0809.1645. Bibcode:2008AJ....136.2441K. doi:10.1088/0004-6256/136/6/2441.
- Staff (September 12, 2005). "Introduction: Galactic Ring Survey". Boston University. Retrieved 2007-05-10.
- Overbye, Dennis (November 9, 2010). "Bubbles of Energy Are Found in Galaxy". The New York Times.
- "Rätselhafte Blasen im All". Süddeutsche Zeitung. Retrieved 2010-11-10.
- Carretti, E.; Crocker, R. M.; Staveley-Smith, L.; Haverkorn, M.; Purcell, C.; Gaensler, B. M.; Bernardi, G.; Kesteven, M. J.; Poppi, S. (2013). "Giant magnetized outflows from the centre of the Milky Way". Nature 493 (7430): 66–69. doi:10.1038/nature11734. PMID 23282363.
- Churchwell, E. et al. (2009). "The Spitzer/GLIMPSE surveys: a new view of the Milky Way". Publications of the Astronomical Society of the Pacific 121 (877): 213. Bibcode:2009PASP..121..213C. doi:10.1086/597811.
- Taylor, J. H.; Cordes, J. M. (1993). "Pulsar distances and the galactic distribution of free electrons". The Astrophysical Journal 411: 674. Bibcode:1993ApJ...411..674T. doi:10.1086/172870.
- Russeil, D. (2003). "Star-forming complexes and the spiral structure of our Galaxy". Astronomy and Astrophysics 397: 133–146. Bibcode:2003A&A...397..133R. doi:10.1051/0004-6361:20021504.
- Dame, T. M.; Hartmann, D.; Thaddeus, P. (2001). "The Milky Way in Molecular Clouds: A New Complete CO Survey". The Astrophysical Journal 547 (2): 792. arXiv:astro-ph/0009217. Bibcode:2001ApJ...547..792D. doi:10.1086/318388.
- Nakanishi, Hiroyuki; Sofue, Yoshiaki (2003). "Three-Dimensional Distribution of the ISM in the Milky Way Galaxy: I. The H I Disk". Publications of the Astronomical Society of Japan 55: 191. arXiv:astro-ph/0304338. Bibcode:2003PASJ...55..191N. doi:10.1093/pasj/55.1.191.
- Vallée, J. P. (2008). "New velocimetry and revised cartography of the spiral arms in the Milky Way—a consistent symbiosis". The Astronomical Journal 135 (4): 1301. Bibcode:2008AJ....135.1301V. doi:10.1088/0004-6256/135/4/1301.
- Hou, L. G.; Han, J. L.; Shi, W. B. (2009). "The spiral structure of our Milky Way Galaxy". Astronomy and Astrophysics 499 (2): 473. arXiv:0903.0721. Bibcode:2009A&A...499..473H. doi:10.1051/0004-6361/200809692.
- Majaess, D. J.; Turner, D. J.; Lane (2009). "Searching Beyond the Obscuring Dust Between the Cygnus-Aquila Rifts for Cepheid Tracers of the Galaxy's Spiral Arms". The Journal of the American Association of Variable Star Observers 37: 179. arXiv:0909.0897. Bibcode:2009JAVSO..37..179M.
- Lépine, J. R. D. et al. (2011). "The spiral structure of the Galaxy revealed by CS sources and evidence for the 4:1 resonance". Monthly Notices of the Royal Astronomical Society 414 (2): 1607. arXiv:1010.1790. Bibcode:2011MNRAS.414.1607L. doi:10.1111/j.1365-2966.2011.18492.x.
- Alexander, S. (1852). "On the origin of the forms and the present condition of some of the clusters of stars, and several of the nebulae". The Astronomical Journal 2: 97. Bibcode:1852AJ......2...97A. doi:10.1086/100231.
- Drimmel, R. (2000). "Evidence for a two-armed spiral in the Milky Way". Astronomy & Astrophysics 358: L13–L16. arXiv:astro-ph/0005241. Bibcode:2000A&A...358L..13D.
- Levine, E. S.; Blitz, L.; Heiles, C. (2006). "The spiral structure of the outer Milky Way in hydrogen". Science 312 (5781): 1773–1777. arXiv:astro-ph/0605728. Bibcode:2006Sci...312.1773L. doi:10.1126/science.1128455. PMID 16741076.
- McClure-Griffiths, N. M.; Dickey, J. M.; Gaensler, B. M.; Green, A. J. (2004). "A Distant Extended Spiral Arm in the Fourth Quadrant of the Milky Way". The Astrophysical Journal 607 (2): L127. arXiv:astro-ph/0404448. Bibcode:2004ApJ...607L.127M. doi:10.1086/422031.
- Benjamin, R. A. et al. (2005). "First GLIMPSE results on the stellar structure of the Galaxy". The Astrophysical Journal 630 (2): L149–L152. arXiv:astro-ph/0508325. Bibcode:2005ApJ...630L.149B. doi:10.1086/491785.
- "Massive stars mark out Milky Way's 'missing' arms", University of Leeds. 17 Dec 2013. Retrieved 18 Dec 2013.
- Russell Westerholm, "Milky Way Galaxy Has Four Arms, Reaffirming Old Data and Contradicting Recent Research", University Herald. 18 Dec 2013. Retrieved 18 Dec 2013.
- J. S. Urquhart, C. C. Figura, T. J. T., Moore, M. G. Hoare, S. L. Lumsde, J. C. Mottram, M. A. Thompson, R. D. Oudmaijer (2013). "The RMS Survey: Galactic distribution of massive star formation". Monthly Notices of the Royal Astronomical Society. in press. arXiv:1310.4758. Bibcode:2014MNRAS.437.1791U. doi:10.1093/mnras/stt2006.
- Expansion d'une structure spirale dans le noyau du Système Galactique, et position de la radiosource Sagittarius A, Comptes Rendus l'Academie des Sciences, Vol. 244, p. 1691-1695, 1957
- A New Spiral Arm of the Galaxy: The Far 3-Kpc Arm, T. M. Dame, P. Thaddeus, ApJ Letters, 2008
- Milky Way's Inner Beauty Revealed, Press Release Harvard-Smithsonian Center for Astrophysics, 2008
- "Star-Crossed: Milky Way's Spiral Shape May Result from a Smaller Galaxy's Impact". Scientific American. 14 September 2011.
- Mel'Nik, A.; Rautiainen, A. (2005). "Kinematics of the outer pseudorings and the spiral structure of the Galaxy". Astronomy Letters 35 (9): 609–624.
- Mel'Nik, A. (2005). "Outer pseudoring in the galaxy". Astronomische Nachrichten 326: 599.
- Harris, William E. (February 2003). "Catalog of Parameters for Milky Way Globular Clusters: The Database" (text). SEDS. Retrieved 2007-05-10.
- Dauphole, B. et al. (September 1996). "The kinematics of globular clusters, apocentric distances and a halo metallicity gradient". Astronomy and Astrophysics 313: 119–128. Bibcode:1996A&A...313..119D.
- Gnedin, O. Y.; Lee, H. M.; Ostriker, J. P. (1999). "Effects of Tidal Shocks on the Evolution of Globular Clusters". The Astrophysical Journal 522 (2): 935–949. arXiv:astro-ph/9806245. Bibcode:1999ApJ...522..935G. doi:10.1086/307659.
- Janes, K.A.; Phelps, R.L. (1980). "The galactic system of old star clusters: The development of the galactic disk". The Astronomical Journal 108: 1773–1785. Bibcode:1994AJ....108.1773J. doi:10.1086/117192.
- Ibata, R. et al. (2005). "On the accretion origin of a vast extended stellar disk around the Andromeda Galaxy". The Astrophysical Journal 634 (1): 287–313. arXiv:astro-ph/0504164. Bibcode:2005ApJ...634..287I. doi:10.1086/491727.
- "Outer Disk Ring?". SolStation. Retrieved 2007-05-10.
- Jurić, M. et al. (February 2008). "The Milky Way Tomography with SDSS. I. Stellar Number Density Distribution". The Astrophysical Journal 673 (2): 864–914. arXiv:astro-ph/0510520. Bibcode:2008ApJ...673..864J. doi:10.1086/523619.
- Boen, Brooke. "NASA's Chandra Shows Milky Way is Surrounded by Halo of Hot Gas09.24.12". Brooke Boen. Retrieved October 28, 2012.
- Gupta, A.; Mathur, S.; Krongold, Y.; Nicastro, F.; Galeazzi, M. (2012). "A Huge Reservoir of Ionized Gas Around the Milky Way: Accounting for the Missing Mass?". The Astrophysical Journal 756: L8. arXiv:1205.5037. Bibcode:2012ApJ...756L...8G. doi:10.1088/2041-8205/756/1/L8.
- "Galactic Halo: Milky Way is Surrounded by Huge Halo of Hot Gas". Smithsonian Astrophysical Observatory. September 24, 2012.
- Communications, Discovery. "OUR GALAXY SWIMS INSIDE A GIANT POOL OF HOT GAS". Discovery Communications. Retrieved October 28, 2012.
- J.D. Harrington, Janet Anderson, and Peter Edmonds (September 24, 2012). "NASA's Chandra Shows Milky Way is Surrounded by Halo of Hot Gas". NASA.
- Reid, M. J. (1993). "The distance to the center of the Galaxy". Annual Review of Astronomy and Astrophysics 31: 345–372. Bibcode:1993ARA&A..31..345R. doi:10.1146/annurev.aa.31.090193.002021.
- Majaess, D. J.; Turner, D. G.; Lane, D. J. (2009). "Characteristics of the Galaxy according to Cepheids". Monthly Notices of the Royal Astronomical Society 398 (1): 263–270. arXiv:0903.4206. Bibcode:2009MNRAS.398..263M. doi:10.1111/j.1365-2966.2009.15096.x.
- English, Jayanne (January 14, 2000). "Exposing the Stuff Between the Stars". Hubble News Desk. Retrieved 2007-05-10.
- "Magnitude". National Solar Observatory—Sacramento Peak. Archived from the original on 2008-02-06. Retrieved 2013-08-09.
- Gillman, M.; Erenler, H. (2008). "The galactic cycle of extinction". International Journal of Astrobiology 7. Bibcode:2008IJAsB...7...17G. doi:10.1017/S1473550408004047.
- Overholt, A. C.; Melott, A. L.; Pohl, M. (2009). "Testing the link between terrestrial climate change and galactic spiral arm transit". The Astrophysical Journal 705 (2): L101–L103. arXiv:0906.2777. Bibcode:2009ApJ...705L.101O. doi:10.1088/0004-637X/705/2/L101.
- Garlick, Mark Antony (2002). The Story of the Solar System. Cambridge University. p. 46. ISBN 0-521-80336-5.
- Peter Schneider (2006). Extragalactic Astronomy and Cosmology. Springer. p. 4, Figure 1.4. ISBN 3-540-33174-3.
- Jones, Mark H.; Lambourne, Robert J.; Adams, David John (2004). An Introduction to Galaxies and Cosmology. Cambridge University Press. p. 21; Figure 1.13. ISBN 0-521-54623-0.
- Imamura, Jim (August 10, 2006). "Mass of the Milky Way Galaxy". University of Oregon. Archived from the original on 2007-03-01. Retrieved 2007-05-10.
- Peter Schneider (2006). Extragalactic Astronomy and Cosmology. Springer. p. 413. ISBN 3-540-33174-3.
- Wethington, Nicholas (May 27, 2009). "Formation of the Milky Way". Universe Today.
- Buser, R. (2000). "The Formation and Early Evolution of the Milky Way Galaxy". Science 287 (5450): 69–74. Bibcode:2000Sci...287...69B. doi:10.1126/science.287.5450.69. PMID 10615051.
- Wakker, B. P.; Van Woerden, H. (1997). "High-Velocity Clouds". Annual Review of Astronomy and Astrophysics 35: 217. Bibcode:1997ARA&A..35..217W. doi:10.1146/annurev.astro.35.1.217.
- Lockman, F. J. et al. (2008). "The Smith Cloud: A High-Velocity Cloud Colliding with the Milky Way". The Astrophysical Journal 679: L21–L24. arXiv:0804.4155. Bibcode:2008ApJ...679L..21L. doi:10.1086/588838.
- Yin, J.; Hou, J.L; Prantzos, N.; Boissier, S.; Chang, R. X.; Shen, S. Y.; Zhang, B. (2009). "Milky Way versus Andromeda: a tale of two disks". Astronomy and Astrophysics 505 (2): 497–508. arXiv:0906.4821. Bibcode:2009A&A...505..497Y. doi:10.1051/0004-6361/200912316.
- Hammer, F.; Puech, M.; Chemin, L.; Flores, H.; Lehnert, M. D. (2007). "The Milky Way, an Exceptionally Quiet Galaxy: Implications for the Formation of Spiral Galaxies". The Astrophysical Journal 662 (1): 322–334. arXiv:astro-ph/0702585. Bibcode:2007ApJ...662..322H. doi:10.1086/516727.
- Mutch, S.J.; Croton, D.J.; Poole, G.B. (2011). "The Mid-life Crisis of the Milky Way and M31". The Astrophysical Journal 736 (2). arXiv:1105.2564. Bibcode:2011ApJ...736...84M. doi:10.1088/0004-637X/736/2/84.
- Licquia, T.; Newman, J.A.; Poole, G.B. (2012). "What Is The Color Of The Milky Way?". American Astronomical Society. Bibcode:2012AAS...21925208L.
- Cayrel et al (2001). "Measurement of stellar age from uranium decay". Nature 409: 691. arXiv:astro-ph/0104357. Bibcode:2001Natur.409..691C.
- Cowan, J. J.; Sneden, C.; Burles, S.; Ivans, I. I.; Beers, T. C.; Truran, J. W.; Lawler, J. E.; Primas, F.; Fuller, G. M. et al. (2002). "The Chemical Composition and Age of the Metal‐poor Halo Star BD +17o3248". The Astrophysical Journal 572 (2): 861. doi:10.1086/340347.
- Krauss, L. M.; Chaboyer, B. (2003). "Age Estimates of Globular Clusters in the Milky Way: Constraints on Cosmology". Science 299 (5603): 65–69. Bibcode:2003Sci...299...65K. doi:10.1126/science.1075631. PMID 12511641.
- Frebel, A. et al. (2007). "Discovery of HE 1523-0901, a strongly r-process-enhanced metal-poor star with detected uranium". The Astrophysical Journal 660 (2): L117. arXiv:astro-ph/0703414. Bibcode:2007ApJ...660L.117F. doi:10.1086/518122.
- Del Peloso, E. F. (2005). "The age of the Galactic thin disk from Th/Eu nucleocosmochronology". Astronomy and Astrophysics 440 (3): 1153. arXiv:astro-ph/0506458. Bibcode:2005A&A...440.1153D. doi:10.1051/0004-6361:20053307.
- Putman, M. E.; Staveley‐Smith, L.; Freeman, K. C.; Gibson, B. K.; Barnes, D. G. (2003). "The Magellanic Stream, High‐Velocity Clouds, and the Sculptor Group". The Astrophysical Journal 586: 170. doi:10.1086/344477.
- "Milky Way Galaxy is warped and vibrating like a drum" (Press release). University of California, Berkeley. January 9, 2006. Retrieved 2007-10-18.
- Wong, Janet (April 14, 2000). "Astrophysicist maps out our own galaxy's end". University of Toronto. Archived from the original on 2007-01-08. Retrieved 2007-01-11.
- Mark H. Jones, Robert J. Lambourne, David John Adams (2004). An Introduction to Galaxies and Cosmology. Cambridge University Press. p. 298. ISBN 0-521-54623-0.
- Kocevski, D. D.; Ebeling, H. (2006). "On the origin of the Local Group's peculiar velocity". The Astrophysical Journal 645 (2): 1043–1053. arXiv:astro-ph/0510106. Bibcode:2006ApJ...645.1043K. doi:10.1086/503666.
- Peirani, S; Defreitaspacheco, J (2006). "Mass determination of groups of galaxies: Effects of the cosmological constant". New Astronomy 11 (4): 325. arXiv:astro-ph/0508614. Bibcode:2006NewA...11..325P. doi:10.1016/j.newast.2005.08.008.
- Jankowski, Connie (2010). Pioneers of Light and Sound. Compass Point Books. p. 6. ISBN 0-7565-4306-1.
- Schiller, Jon (2010). Big Bang & Black Holes. CreateSpace. p. 163. ISBN 1-4528-6552-3.
- Simpson, John; Weiner, Edmund, eds. (March 30, 1989). The Oxford English Dictionary (2nd ed.). Oxford University Press. ISBN 0198611862. See the entries for "Milky Way" and "galaxy".
- Eratosthenes (1997). Condos, Theony, ed. Star Myths of the Greeks and Romans: A Sourcebook Containing the Constellations of Pseudo-Eratosthenes and the Poetic Astronomy of Hyginus. Red Wheel/Weiser. ISBN 1890482935.
- Montada, Josep Puig (September 28, 2007). "Ibn Bajja". Stanford Encyclopedia of Philosophy. Retrieved 2008-07-11.
- Heidarzadeh, Tofigh (2008). A history of physical theories of comets, from Aristotle to Whipple. Springer. pp. 23–25. ISBN 1-4020-8322-X.
- O'Connor, John J.; Robertson, Edmund F., "Abu Rayhan Muhammad ibn Ahmad al-Biruni", MacTutor History of Mathematics archive, University of St Andrews.[unreliable source?]
- Livingston, John W. (1971). "Ibn Qayyim al-Jawziyyah: A Fourteenth Century Defense against Astrological Divination and Alchemical Transmutation". Journal of the American Oriental Society (American Oriental Society) 91 (1): 96–103 . doi:10.2307/600445. JSTOR 600445.
- Ragep, Jamil (1993). Nasir al-Din al-Tusi’s Memoir on Astronomy (al-Tadhkira fi `ilm al-hay’ a). New York: Springer-Verlag. p. 129.
- 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.
- O'Connor, J. J.; Robertson, E. F. (November 2002). "Galileo Galilei". University of St. Andrews. Retrieved 2007-01-08.
- Thomas Wright, An Original Theory or New Hypothesis of the Universe … (London, England: H. Chapelle, 1750).
- On page 57, Wright stated that despite their mutual gravitational attraction, the stars in the constellations don't collide because they are in orbit, so centrifugal force keeps them separated: " … centrifugal force, which not only preserves them in their orbits, but prevents them from rushing all together, by the common universal law of gravity, … "
- On page 48, Wright stated that the form of the Milky Way is a ring: " … 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 65, Wright speculated that the central body of the Milky Way, around which the rest of the galaxy revolves, might not be visible to us: " ... the central body A, being supposed as incognitum [i.e., an unknown], without [i.e., outside of] the finite view; ... "
- On page 73, Wright called the Milky Way the Vortex Magnus (the great whirlpool) and estimated its diameter to be 8.64×1012 miles (13.9×1012 km).
- On page 33, Wright speculated that there are a vast number of inhabited planets in the galaxy: " … ; therefore we may justly suppose, that so many radiant bodies [i.e., stars] were not created barely to enlighten an infinite void, but to … display an infinite shapeless universe, crowded with myriads of glorious worlds, all variously revolving round them; and … with an inconceivable variety of beings and states, animate … "
- Immanuel Kant, Allgemeine Naturgeschichte und Theorie des Himmels … [Universal Natural History and Theory of Heaven … ], (Koenigsberg and Leipzig, (Germany): Johann Friederich Petersen, 1755). On pages 2-3, Kant acknowledged his debt to Thomas Wright: "Dem Herrn Wright von Durham, einen Engeländer, war es vorbehalten, einen glücklichen Schritt zu einer Bemerkung zu thun, welche von ihm selber zu keiner gar zu tüchtigen Absicht gebraucht zu seyn scheinet, und deren nützliche Anwendung er nicht genugsam beobachtet hat. Er betrachtete die Fixsterne nicht als ein ungeordnetes und ohne Absicht zerstreutes Gewimmel, sondern er fand eine systematische Verfassung im Ganzen, und eine allgemeine Beziehung dieser Gestirne gegen einen Hauptplan der Raume, die sie einnehmen." (To Mr. Wright of Durham, an Englishman, it was reserved to take a happy step towards an observation, which seemed, to him and to no one else, to be needed for a clever idea, the exploitation of which he hasn't studied sufficiently. He regarded the fixed stars not as a disorganized swarm that was scattered without a design; rather, he found a systematic shape in the whole, and a general relation between these stars and the principal plane of the space that they occupy.)
- Kant (1755), pages xxxiii-xxxvi of the Preface (Vorrede): "Ich betrachtete die Art neblichter Sterne, deren Herr von Maupertuis in der Abhandlung von der Figur der Gestirne gedenket, und die die Figur von mehr oder weniger offenen Ellipsen vorstellen, und versicherte mich leicht, daß sie nichts anders als eine Häufung vieler Fixsterne seyn können. Die jederzeit abgemessene Rundung dieser Figuren belehrte mich, daß hier ein unbegreiflich zahlreiches Sternenheer, und zwar um einen gemeinschaftlichen Mittelpunkt, müste geordnet seyn, weil sonst ihre freye Stellungen gegen einander, wohl irreguläre Gestalten, aber nicht abgemessene Figuren vorstellen würden. Ich sahe auch ein: daß sie in dem System, darinn sie sich vereinigt befinden, vornemlich auf eine Fläche beschränkt seyn müßten, weil sie nicht zirkelrunde, sondern elliptische Figuren abbilden, und daß sie wegen ihres blassen Lichts unbegreiflich weit von uns abstehen." (I considered the type of nebulous stars, which Mr. de Maupertuis considered in his treatise on the shape of stars, and which present the figures of more or less open ellipses, and I readily assured myself, that they could be nothing else than a cluster of fixed stars. That these figures always measured round informed me that here an inconceivably numerous host of stars, [which were clustered] around a common center, must be orderly, because otherwise their free positions among each other would likely present irregular forms, not measurable figures. I also realized: that in the system in which they find themselves bound, they must be restricted primarily to a plane, because they display not circular, but elliptical figures, and that on account of their faint light, they are located inconceivably far from us.)
- Evans, J. C. (November 24, 1998). "Our Galaxy". George Mason University. Retrieved 2007-01-04.
- The term Weltinsel (island universe) appears nowhere in Kant's book of 1755. The term first appeared in 1850, in the third volume of von Humboldt's Kosmos: Alexander von Humboldt, Kosmos … , vol. 3 (Stuttgart & Tübingen, (Germany): J.G. Cotta, 1850), pages 187, 189. From page 187: "Thomas Wright von Durham, Kant, Lambert und zuerst auch William Herschel waren geneigt die Gestalt der Milchstraße und die scheinbare Anhäufung der Sterne in derselben als eine Folge der abgeplatteten Gestalt und ungleichen Dimensionen der Weltinsel (Sternschict) zu betrachten, in welche unser Sonnensystem eingeschlossen ist." (Thomas Wright of Durham, Kant, Lambert and first of all also William Herschel were inclined to regard the shape of the Milky Way and the apparent clustering of stars in it as a consequence of the oblate shape and unequal dimensions of the world island (star stratum), in which our solar system is included.)
In the English translation — Alexander von Humboldt with E.C. Otté, trans., Cosmos … (New York, New York: Harper & Brothers, 1897), vols. 3-5 — see page 147.
- William Herschel (1785) "On the Construction of the Heavens," Philosophical Transactions of the Royal Society of London, 75 : 213-266. Herschel's diagram of the galaxy appears immediately after the article's last page. See:
- Abbey, Lenny. "The Earl of Rosse and the Leviathan of Parsontown". The Compleat Amateur Astronomer. Retrieved 2007-01-04.
- Curtis, H. D. (1988). "Novae in spiral nebulae and the Island Universe Theory". Publications of the Astronomical Society of the Pacific 100: 6–2. Bibcode:1988PASP..100....6C. doi:10.1086/132128.
- Weaver, Harold F. "Robert Julius Trumpler". National Academy of Sciences. Retrieved 2007-01-05.
- Hubble, E. P. (1929). "A spiral nebula as a stellar system, Messier 31". The Astrophysical Journal 69: 103–158. Bibcode:1929ApJ....69..103H. doi:10.1086/143167.
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- Thorsten Dambeck in Sky and Telescope, "Gaia's Mission to the Milky Way", March 2008, p. 36–39.
- Cristina Chiappini, The Formation and Evolution of the Milky Way, American Scientist, November/December 2001, pp. 506–515
|Wikimedia Commons has media related to Milky Way Galaxy.|
- 3D Galaxy Map - a 3D representation of the Milky Way galaxy
- Basic Milky Way plan map - includes spiral arms and Orion spur
- Milky Way – IRAS (infrared) survey - wikisky.org
- Milky Way – H-Alpha survey - wikisky.org
- The Milky Way Galaxy - SEDS Messier website
- MultiWavelength Milky Way - NASA site with images and VRML models
- Milky Way Explorer - images in infrared with radio, microwave and hydrogen-alpha.
- Milky Way Panorama (9 billion pixels).
- Milky Way Video (02:37) - VISTA IR Telescope Image (October 24, 2012)
- Animated tour of the Milky Way, University of South Wales
- all-sky map of microwave radiation (Planck (spacecraft) one-year all-sky survey)