Large Magellanic Cloud
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The Large Magellanic Cloud (LMC) is a dwarf galaxy and satellite galaxy of the Milky Way.<ref>Template:Cite journal</ref> At a distance of around Template:Convert,<ref name="Nature" /><ref name="Macrietal2006"/><ref name=freedman2010>Template:Cite journal</ref><ref name="majaess2010">Template:Cite journal</ref> the LMC is the second- or third-closest galaxy to the Milky Way, after the Sagittarius Dwarf Spheroidal (Template:Circa away) and the possible dwarf irregular galaxy called the Canis Major Overdensity. Based on the D25 isophote at the B-band (445 nm wavelength of light), the Large Magellanic Cloud is about Template:Convert across.<ref name="ned" /><ref name=RC3 /> It is roughly one-hundredth the mass of the Milky Way<ref name="Britannica">Template:Cite encyclopedia</ref> and is the fourth-largest galaxy in the Local Group, after the Andromeda Galaxy (M31), the Milky Way, and the Triangulum Galaxy (M33).
The LMC is classified as a Magellanic spiral.<ref name="rydenpeterson">Template:Cite book</ref> It contains a stellar bar that is geometrically off-center, suggesting that it was once a barred dwarf spiral galaxy before its spiral arms were disrupted, likely by tidal interactions from the nearby Small Magellanic Cloud (SMC) and the Milky Way's gravity.<ref name=":0">Template:Cite journal</ref> The LMC is predicted to merge with the Milky Way in approximately 2.4 billion years.<ref>Template:Cite journal</ref>
With a declination of about −70°, the LMC is visible as a faint "cloud" from the southern hemisphere of the Earth and from as far north as 20° N. It straddles the constellations Dorado and Mensa and has an apparent length of about 10° to the naked eye, 20 times the Moon's diameter, from dark sites away from light pollution.<ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref>
History of observationEdit
Both the Large and Small Magellanic Clouds have been easily visible for southern nighttime observers well back into prehistory. It has been claimed that the first known written mention of the Large Magellanic Cloud was by the Persian astronomer 'Abd al-Rahman al-Sufi Shirazi (later known in Europe as "Azophi"), which he referred to as Al Bakr, the White Ox, in his Book of Fixed Stars around 964 AD.<ref name="obspm" >{{#invoke:citation/CS1|citation |CitationClass=web }}</ref><ref name="obspm2" >{{#invoke:citation/CS1|citation |CitationClass=web }}</ref> However, this seems to be a misunderstanding of a reference to some stars south of Canopus which he admits he had not seen.<ref>Hafez, Ihsan; Stephenson, Richard; Orchiston, Wayne (2011), Abdul-Rahman al-Sufi and his Book of the Fixed Stars, pp. 121–138, Template:ISBN, retrieved November 13, 2019</ref><ref name="ridpath">Template:Cite book</ref>
The first confirmed recorded observation was in 1503–1504 by Amerigo Vespucci in a letter about his third voyage. He mentioned "three CanopesTemplate:Sic, two bright and one obscure"; "bright" refers to the two Magellanic Clouds, and "obscure" refers to the Coalsack.<ref name="obspm3" >{{#invoke:citation/CS1|citation |CitationClass=web }}</ref>
Ferdinand Magellan sighted the LMC on his voyage in 1519 and his writings brought it into common Western knowledge. The galaxy now bears his name.<ref name="obspm2"/> The galaxy and southern end of Dorado are in the current epoch at opposition on about 5 December when thus visible from sunset to sunrise from equatorial points such as Ecuador, the Congos, Uganda, Kenya and Indonesia and for part of the night in nearby months. Above about 28° south, such as most of Australia and South Africa, the galaxy is always sufficiently above the horizon to be considered properly circumpolar, thus during spring and autumn the cloud is also visible much of the night, and the height of winter in June nearly coincides with closest proximity to the Sun's apparent position.
Measurements with the Hubble Space Telescope, announced in 2006, suggest the Large and Small Magellanic Clouds may be moving too quickly to be orbiting the Milky Way.<ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref>
Astronomers discovered a new black hole inside the Large Magellanic Cloud in November 2021 using the European Southern Observatory's Very Large Telescope in Chile. Astronomers claim its gravity is influenced by a nearby star, which is about five times the mass of the Sun.<ref>Template:Cite journal</ref>
In March 2025, the Center for Astrophysics announced the discovery of strong evidence for the closest supermassive black hole outside of the Milky Way galaxy. This supermassive black hole is located in the Large Magellanic Cloud, which is considered to be one of the nearest galactic neighbors to our own, and its estimated mass is about 600,000 times the mass of the Sun.<ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref>
GeometryEdit
The Large Magellanic Cloud has a prominent central bar and spiral arm.<ref name="Nicolson">Template:Cite book</ref> The central bar, with a radius of 6,900 light-years (2.13 kpc) and a position angle of about 121°,<ref>Template:Cite journal</ref> seems to be warped so that the east and west ends are nearer the Milky Way than the middle.<ref name="Subramaniam">Template:Cite journal</ref> In 2014, measurements from the Hubble Space Telescope made it possible to determine a rotation period of 250 million years.<ref>Template:Cite journal</ref>
The LMC was long considered to be a planar galaxy that could be assumed to lie at a single distance from the Solar System. However, in 1986, Caldwell and Coulson<ref>Template:Cite journal</ref> found that field Cepheid variables in the northeast lie closer to the Milky Way than those in the southwest. From 2001 to 2002 this inclined geometry was confirmed by the same means,<ref>Template:Cite journal</ref> by core helium-burning red clump stars,<ref>Template:Cite journal</ref> and by the tip of the red giant branch.<ref name="Marel2001">Template:Cite journal</ref> All three papers find an inclination of Template:Abbreviation35°, where a face-on galaxy has an inclination of 0°. Further work on the structure of the LMC using the kinematics of carbon stars showed that the LMC's disk is both thick<ref name="Marel2001" /> and flared,<ref>Template:Cite journal</ref><ref name=Ripepi>Template:Cite journal</ref> likely due to interactions with the SMC.<ref name=Ripepi/> Regarding the distribution of star clusters in the LMC, Schommer et al.<ref>Template:Cite journal</ref> measured velocities for Template:Abbreviation80 clusters and found that the LMC's cluster system has kinematics consistent with the clusters moving in a disk-like distribution. These results were confirmed by Grocholski et al.,<ref>Template:Cite journal</ref> who calculated distances to a sample of clusters and showed that the cluster system is distributed in the same plane as the field stars.
DistanceEdit
The distance to the LMC has been calculated using standard candles; Cepheid variables are one of the most popular. These have been shown to have a relationship between their absolute luminosity and the period over which their brightness varies. However the variable of metallicity may also need to be taken as a component of this as consensus is this likely affects their period-luminosity relations. Cepheid variables in the Milky Way typically used to calibrate the relation are more metal-rich than those found in the LMC.<ref name="mottini2006">Template:Cite journal</ref>
Modern 8-meter-class optical telescopes have discovered eclipsing binaries throughout the Local Group. Parameters of these systems can be measured without mass or compositional assumptions. The light echoes of supernova 1987A are also geometric measurements, without any stellar models or assumptions.<ref>Template:Cite journal</ref>
In 2006, the Cepheid absolute luminosity was re-calibrated using Cepheid variables in the galaxy Messier 106 that cover a range of metallicities.<ref name="Macrietal2006" >Template:Cite journal</ref> Using this improved calibration, they find an absolute distance modulus of <math>(m - M)_0 = 18.41</math>, or Template:Convert. This distance has been confirmed by other authors.<ref name="freedman2010"/><ref name="majaess2010" />
By cross-correlating different measurement methods, one can bound the distance; the residual errors are now less than the estimated size parameters of the LMC.
The results of a study using late-type eclipsing binaries to determine the distance more accurately was published in the scientific journal Nature in March 2013. A distance of Template:Convert with an accuracy of 2.2% was obtained.<ref name="Nature" />
FeaturesEdit
Like many irregular galaxies, the LMC is rich in gas and dust, and is currently undergoing vigorous star formation activity.<ref>Template:Cite book</ref> It holds the Tarantula Nebula, the most active star-forming region in the Local Group.
The LMC has a wide range of galactic objects and phenomena that make it known as an "astronomical treasure-house, a great celestial laboratory for the study of the growth and evolution of the stars", per Robert Burnham Jr.<ref>Template:Cite book</ref> Surveys of the galaxy have found roughly 60 globular clusters, 400 planetary nebulae and 700 open clusters, along with hundreds of thousands of giant and supergiant stars.<ref>Burnham (1978), 840–848.</ref> Supernova 1987A—the nearest supernova in recent years—was in the Large Magellanic Cloud. The Lionel-Murphy SNR (N86) nitrogen-abundant supernova remnant was named by astronomers at the Australian National University's Mount Stromlo Observatory, acknowledging Australian High Court Justice Lionel Murphy's interest in science and its perceived resemblance to his large nose.<ref name="DopitaMathewson1977">Template:Cite journal</ref>
A bridge of gas connects the Small Magellanic Cloud (SMC) with the LMC, which evinces tidal interaction between the galaxies.<ref name="Mathewson">Template:Cite journal</ref> The Magellanic Clouds have a common envelope of neutral hydrogen, indicating that they have been gravitationally bound for a long time. This bridge of gas is a star-forming site.<ref name=Heydari>Template:Cite journal</ref>
The Large Magellanic Cloud has a supermassive black hole at its center, estimated to have Template:Val times the mass of the Sun. 21 hypervelocity stars have been discovered within the Milky Way's halo, which are thought to have been ejected from the Large Magellanic Cloud after gravitational interaction with this black hole via the Hills mechanism.<ref name=Han2025>Template:Cite journal</ref>
X-ray sourcesEdit
No X-rays above background were detected from either cloud during the September 20, 1966, Nike-Tomahawk rocket flight nor that of two days later.<ref name=Chodil >Template:Cite journal</ref> The second took off from Johnston Atoll at 17:13 UTC and reached an apogee of Template:Cvt, with spin-stabilization at 5.6 rps.<ref name=Seward >Template:Cite journal</ref> The LMC was not detected in the X-ray range 8–80 keV.<ref name="Seward"/>
Another was launched from same atoll at 11:32 UTC on October 29, 1968, to scan the LMC for X-rays.<ref name=Mark/> The first discrete X-ray source in Dorado was at RA Template:RA Dec Template:Dec,<ref name=Mark >Template:Cite journal</ref><ref name=Lewin >Template:Cite journal</ref> and it was the Large Magellanic Cloud.<ref name="Dolan">Template:Cite journal</ref> This X-ray source extended over about 12° and is consistent with the Cloud. Its emission rate between 1.5–10.5 keV for a distance of 50 kpc is Template:Val/s.<ref name=Mark/> An X-ray astronomy instrument was carried aboard a Thor missile launched from the same atoll on September 24, 1970, at 12:54 UTC and altitudes above Template:Cvt, to search for the Small Magellanic Cloud and to extend observation of the LMC.<ref name=PriceThor>Template:Cite journal</ref> The source in the LMC appeared extended and contained star ε Dor. The X-ray luminosity (Lx) over the range 1.5–12 keV was Template:Val (Template:Val).<ref name="PriceThor"/>
The Large Magellanic Cloud (LMC) appears in the constellations Mensa and Dorado. LMC X-1 (the first X-ray source in the LMC) is at RA Template:RA Dec Template:Dec, and is a high-mass X-ray binary (star system) source (HMXB).<ref name="Rapley">Template:Cite journal</ref> Of the first five luminous LMC X-ray binaries: LMC X-1, X-2, X-3, X-4 and A 0538–66 (detected by Ariel 5 at A 0538–66), LMC X-2 is the one that is a bright low-mass X-ray binary system (LMXB) in the LMC.<ref name=Bonnet>Template:Cite journal</ref>
DEM L316 in the Cloud consists of two supernova remnants.<ref name=Williams>Template:Cite journal</ref> Chandra X-ray spectra show that the hot gas shell on the upper left has an abundance of iron. This implies that the upper-left SNR is the product of a Type Ia supernova; much lower such abundance in the lower remnant belies a Type II supernova.<ref name="Williams"/>
A 16 ms X-ray pulsar is associated with SNR 0538-69.1.<ref name="MarshallGotthelf1998">Template:Cite journal</ref> SNR 0540-697 was resolved using ROSAT.<ref name="ChuKennicutt1997">Template:Cite journal</ref>
GalleryEdit
- Deepest, widest view of the Large Magellanic Cloud from SMASH.jpg
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- Large Magellanic Cloud.png
Large Magellanic Cloud as photographed by an amateur astronomer. Unrelated stars have been edited out.
- Large Magellanic Cloud rendered from Gaia EDR3.png
Large Magellanic Cloud rendered from Gaia EDR3
- Large Magellanic Cloud rendered from Gaia EDR3 without foreground stars.png
Large Magellanic Cloud rendered from Gaia EDR3 without foreground stars
- Revisiting a Celestial Fireworks Display (potw2248a).jpg
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- Hubble views a spectacular supernova with interstellar material over 160,000 light-years away (28629479145).jpg
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