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| {{Infobox galaxy
| | I mean if you actually were weird enough to consider this a nice perfume, you'd want it to last long right. These can include: sidewalk chalk, bubble soap with cool bubble wands, new crayons and coloring books, new books, funky shoelaces to re-lace shoes, squirt guns, water balloons, etc. I didn't realize the price until I got home and looked at the receipt.<br><br> |
| | name = Large Magellanic Cloud
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| | image = [[Image:large.mc.arp.750pix.jpg|340px]]
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| |caption= The Large Magellanic Cloud
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| | epoch = [[J2000]]
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| | type = SB(s)m<ref name="ned" >{{cite web
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| | title=NASA/IPAC Extragalactic Database
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| | work=Results for Large Magellanic Cloud
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| | url=http://nedwww.ipac.caltech.edu/
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| | accessdate=2006-10-29 }}</ref>
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| | ra = {{RA|05|23|34.5}}<ref name="ned" />
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| | dec = {{DEC|-69|45|22}}<ref name="ned" />
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| | dist_ly = [[1 E20 m|162.98]] [[light-year|kly]] (49.97 [[parsec|kpc]])<ref name="Macrietal2006" /><ref name=freedman2010/><ref name=majaess2010/><ref name=Nature>{{cite journal|last=Pietrzyński|first=G|coauthors=D. Graczyk, W. Gieren, I. B. Thompson, B. Pilecki, A. Udalski, I. Soszyński, et al|title=An eclipsing-binary distance to the Large Magellanic Cloud accurate to two per cent|journal=Nature|date=7 March 2013|volume=495|pages=76–79|doi=10.1038/nature11878|url=http://www.nature.com/nature/journal/v495/n7439/full/nature11878.html|accessdate=7 March 2013|arxiv = 1303.2063 |bibcode = 2013Natur.495...76P }}</ref>
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| | Radial Velocity = 278 ± 3 [[kilometer|km]]/[[second|s]]<ref name="ned" />
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| | appmag_v = 0.9<ref name="ned" />
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| | size_v = 10.75[[degree (angle)|°]] × 9.17°<ref name="ned" />
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| | constellation name = [[Dorado]]/[[Mensa (constellation)|Mensa]]
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| | names = LMC, ESO 56- G 115, [[Principal Galaxies Catalogue|PGC]] 17223,<ref name="ned" /> [[Nubecula Major]]<ref>Astronomical Society of the Pacific Leaflets, "The Magellanic Clouds", Buscombe, William, v.7, p.9, ''1954'', {{bibcode|1954ASPL....7....9B}}</ref>
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| The '''Large Magellanic Cloud''' (LMC) is a nearby [[galaxy]], and a [[satellite galaxy|satellite]] of the [[Milky Way]].<ref>[http://adsabs.harvard.edu/abs/2009MNRAS.392L..21S Implications of recent measurements of the Milky Way rotation for the orbit of t<!-- Bot generated title -->]</ref> At a distance of slightly less than 50 [[kiloparsec]]s (≈163,000 [[light-year]]s),<ref name="Macrietal2006" /><ref name=freedman2010>Freedman, Wendy L.; Madore, Barry F. [http://adsabs.harvard.edu/abs/2010ARA%26A..48..673F "The Hubble Constant"], ''Annual Review of Astronomy and Astrophysics'', 2010</ref><ref name=majaess2010>Majaess, Daniel J.; Turner, David G.; Lane, David J.; Henden, Arne; Krajci, Tom [http://adsabs.harvard.edu/abs/2010arXiv1007.2300M "Anchoring the Universal Distance Scale via a Wesenheit Template"], ''JAAVSO'', 2010</ref><ref name="Nature"/> the LMC is the third closest galaxy to the Milky Way, with the [[Sagittarius Dwarf Elliptical Galaxy|Sagittarius Dwarf Spheroidal]] (~ 16 kiloparsecs) and the putative [[Canis Major Dwarf Galaxy]] (~ 12.9 kiloparsecs, though its status as a galaxy is under [[Canis Major Dwarf Galaxy#Dispute|dispute]]) lying closer to the center of the Milky Way. It has a mass equivalent to approximately 10 billion times the mass of the Sun (10<sup>10</sup> [[solar mass]]es), making it roughly 1/100 as massive as the Milky Way, and a diameter of about 14,000 light-years (~ 4.3 [[kiloparsecs|kpc]]).<ref>"[http://www.britannica.com/EBchecked/topic/356551/Magellanic-Cloud Magellanic Cloud]." ''[[Encyclopædia Britannica]]''. 2009. Encyclopædia Britannica Online. 30 Aug. 2009.</ref> The LMC is the fourth largest galaxy in the [[Local Group]], after the [[Andromeda Galaxy]] (M31), the Milky Way, and the [[Triangulum Galaxy]] (M33).
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| While the LMC is often considered an irregular type galaxy (the [[NASA Extragalactic Database]] lists the [[Galaxy morphological classification|Hubble sequence]] type as Irr/SB(s)m), the LMC contains a very prominent bar in its center, suggesting that it may have previously been a barred spiral galaxy. The LMC's irregular appearance is possibly the result of tidal interactions with both the Milky Way and the [[Small Magellanic Cloud]] (SMC).
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| It is visible as a faint "cloud" in the night sky of the [[southern hemisphere]] straddling the border between the [[constellation]]s of [[Dorado]] and [[Mensa (constellation)|Mensa]], and it appears from [[Earth]] more than 20 times the width of the [[full moon]].<ref>{{cite web|url=http://earthsky.org/clusters-nebulae-galaxies/the-large-magellanic-cloud |title=Large Magellanic Cloud: spectacular from Earth's southern hemisphere | Clusters Nebulae Galaxies |publisher=EarthSky |date= |accessdate=2013-07-17}}</ref>
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| ==History==
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| The very first recorded mention of the Large Magellanic Cloud was by the [[Islamic astronomy|Persian astronomer]] [[Abd al-Rahman al-Sufi|`Abd al-Rahman al-Sufi]] (later known in Europe as "Azophi"), in his ''[[Book of Fixed Stars]]'' around 964 AD.<ref name="obspm" >{{cite web
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| | title=Observatoire de Paris (Abd-al-Rahman Al Sufi)
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| | url=http://messier.obspm.fr/xtra/Bios/alsufi.html
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| | accessdate=2007-04-19 }}</ref><ref name="obspm2" >{{cite web
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| | title=Observatoire de Paris (LMC)
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| | url=http://messier.obspm.fr/xtra/ngc/lmc.html
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| | accessdate=2007-04-19 }}</ref>
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| The next recorded observation was in 1503–4 by [[Amerigo Vespucci]] in a letter about his third voyage. In this letter he mentions "three Canopes, two bright and one obscure"; "bright" refers to the two [[Magellanic Clouds]], and "obscure" refers to the [[Coalsack]].<ref name="obspm3" >{{cite web
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| | title=Observatoire de Paris (Amerigo Vespucci)
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| | url=http://messier.obspm.fr/xtra/Bios/vespucci.html
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| | accessdate=2007-04-19 }}</ref>
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| [[Ferdinand Magellan]] sighted the LMC on his voyage in 1519, and his writings brought the LMC into common [[Western world|Western]] knowledge. The galaxy now bears his name.<ref name="obspm2" />
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| Announced in 2006, measurements with the Hubble Space Telescope suggest the Large and Small Magellanic Clouds may be moving too fast to be orbiting the [[Milky Way]].<ref>[http://phys.org/news87572515.html Magellanic Clouds May Be Just Passing Through January 9, 2007]</ref>
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| ==Geometry==
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| The Large Magellanic Cloud is usually considered an [[irregular galaxy]]. However, it shows signs of a bar structure, and is often reclassified as a [[Magellanic spiral|Magellanic-type]] [[dwarf spiral galaxy]]).
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| The Large Magellanic Cloud has a prominent central bar and a [[spiral arm]].<ref name=Nicolson >{{Cite book
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| | last = Nicolson
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| | first = Iain
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| | authorlink =
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| | coauthors =
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| | title = Unfolding our Universe
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| | publisher =
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| | year = 1999
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| | location = [[USA]]
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| | pages = 213–214
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| | url = http://books.google.com/?id=5iacbufd4kEC&printsec=frontcover&q=
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| | doi =
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| | isbn = 0-521-59270-4}}</ref> The central bar seems to be warped so that the east and west ends are nearer the Milky Way than the middle.<ref name=Subramaniam >{{Cite journal | last = Subramaniam
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| | first = Annapurni
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| | authorlink =
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| | coauthors =
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| | title = Large Magellanic Cloud Bar: Evidence of a Warped Bar
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| | journal = [[The Astrophysical Journal]]
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| | volume = 598
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| | pages = L19–L22
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| | publisher =
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| | location = [[USA]]
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| | date = 2003-11-03
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| | url = http://www.iop.org/EJ/article/1538-4357/598/1/L19/17609.web.pdf?request-id=97601007-bd6e-4a75-a90b-679dad73bf04
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| | issn =
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| | doi = 10.1086/380556
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| | accessdate = 2009-10-31
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| | bibcode=2003ApJ...598L..19S}}</ref>
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| The LMC was long considered to be a planar galaxy that could be assumed to lie at a single distance from us. However, in 1986, Caldwell and Coulson<ref>{{cite journal |last=Caldwell |first=J. A. R. |authorlink= |coauthors=Coulson, I. M. |year=1986 |month= |title=The geometry and distance of the Magellanic Clouds from Cepheid variables |journal=Royal Astronomical Society, Monthly Notices |volume=218 |issue= |pages=223–246 |bibcode=1986MNRAS.218..223C |url=}}</ref> found that field [[Cepheid]] variables in the northeast portion of the LMC lie closer to the Milky Way than Cepheids in the southwest portion. More recently, this inclined geometry for field stars in the LMC has been confirmed via observations of Cepheids,<ref>{{cite journal |last=Nikolaev |first=S. |authorlink= |coauthors=''et al.'' |year=2004 |month= |title=Geometry of the Large Magellanic Cloud Disk: Results from MACHO and the Two Micron All Sky Survey |journal=The Astrophysical Journal |volume=601 |issue=1 |pages=260–276 |doi=10.1086/380439 |url=|bibcode=2004ApJ...601..260N}}</ref> core helium-burning red clump stars<ref>{{cite journal | last=Olsen | first=K. A. G. | coauthors=Salyk, C. | year=2002 | title=A Warp in the Large Magellanic Cloud Disk? | journal=The [[Astronomical Journal]] | volume=124 | issue=4 | pages=2045–2053 | doi=10.1086/342739 | url=http://www.iop.org/EJ/article/1538-3881/124/4/2045/202206.html | bibcode=2002AJ....124.2045O}}</ref> and the tip of the red giant branch.<ref name="Marel2001" >{{cite journal | last=van der Marel | first=R. P. | coauthors=Cioni, M.-R. L. | year=2001 | title=Magellanic Cloud Structure from Near-Infrared Surveys. I. The Viewing Angles of the Large Magellanic Cloud | journal=The Astronomical Journal | volume=122 | issue=4 | pages=1807–1826 | doi=10.1086/323099 | url=http://www.iop.org/EJ/article/1538-3881/122/4/1807/201194.html | bibcode=2001AJ....122.1807V|arxiv = astro-ph/0105339 }}</ref> All three of these papers find an inclination of ~35°, 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>{{cite journal |last=Alves |first=D. R. |authorlink= |coauthors=Nelson, C. A. |year=2000 |month= |title=The Rotation Curve of the Large Magellanic Cloud and the Implications for Microlensing |journal= The Astrophysical Journal|volume=542 |issue=2 |pages=789–803 |doi=10.1086/317023 |url=|bibcode=2000ApJ...542..789A|arxiv = astro-ph/0006018 }}</ref> Regarding the distribution of [[star clusters]] in the LMC, [[Robert Schommer|Schommer]] ''et al.''<ref>{{cite journal |last=Schommer |first=R. A. |authorlink= |coauthors=''et al.'' |year=1992 |month= |title=Spectroscopy of giants in LMC clusters. II - Kinematics of the cluster sample |journal=Astronomical Journal |volume=103 |issue= |pages=447–459 |doi=10.1086/116074 |url=|bibcode=1992AJ....103..447S}}</ref> measured velocities for ~80 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>{{cite journal |last=Grocholski |first=A. J. |authorlink= |coauthors=''et al.'' |year=2007 |month= |title=Distances to Populous Clusters in the Large Magellanic Cloud via the K-band Luminosity of the Red Clump |journal=The Astronomical Journal |volume=134 |issue=2 |pages=680–693 |doi=10.1086/519735 |url=|bibcode=2007AJ....134..680G|arxiv = 0705.2039 }}</ref> who calculated distances to a number of clusters and showed that the LMC's cluster system is in fact distributed in the same plane as the field stars.
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| ==Distance==
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| [[Image:Satellite Galaxies.JPG|thumb|250px|Location of the '''Large Magellanic Cloud''' with respect to the [[Milky Way]] and other satellite galaxies]]
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| Determining a precise distance to the LMC, as with any other galaxy, was challenging due to the use of [[standard candle]]s for calculating distances, with the primary problem being that many of the standard candles are not as 'standard' as one would like; in many cases, the age and/or [[metallicity]] of the standard candle plays a role in determining the intrinsic luminosity of the object. The distance to the LMC has been calculated using a variety of standard candles, with [[Cepheid]] variables being one of the most popular. Cepheids have been shown to have a relationship between their absolute luminosity and the period over which their brightness varies. However, Cepheids appear to suffer from a metallicity effect, where Cepheids of different metallicities have different period–luminosity relations. Unfortunately, the Cepheids in the Milky Way typically used to calibrate the period–luminosity relation are more metal rich than those found in the LMC.<ref name=mottini2006>Mottini, M.; Romaniello, M.; Primas, F.; Bono, G.; Groenewegen, M. A. T.; François, P. [http://adsabs.harvard.edu/abs/2006MmSAI..77..156M "The chemical composition of Cepheids in the Milky Way and the Magellanic Clouds"], ''MmSAI'', 2006</ref>
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| In the era of 8-meter-class telescopes, [[eclipsing binaries]] have been found throughout the [[Local Group]]. Parameters of these systems can be measured without mass or compositional assumptions. The [[light echoes]] of [[SN 1987A|supernova 1987A]] are also geometric measurements, without any stellar models or assumptions.
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| Recently, the Cepheid absolute luminosity has been re-calibrated using Cepheid variables in the galaxy NGC 4258 that cover a range of metallicities.<ref name="Macrietal2006" >{{cite journal |last=Macri |first=L. M. |authorlink= |coauthors=''et al.'' |year=2006 |month= |title=A New Cepheid Distance to the Maser-Host Galaxy NGC 4258 and Its Implications for the Hubble Constant |journal=The Astrophysical Journal |volume=652 |issue=2 |pages=1133–1149 |doi=10.1086/508530 |url=|bibcode=2006ApJ...652.1133M|arxiv = astro-ph/0608211 }}</ref> Using this improved calibration, they find an absolute distance modulus of <math>(m-M)_0 = </math>18.41, or 48 kpc (~157,000 light years). This distance, which is slightly shorter than the typically assumed distance of 50 kpc, has been confirmed by other authors.<ref name=freedman2010/><ref name=majaess2010/>
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| 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. Further work involves measuring the position of a target star or star system within the galaxy (i.e. toward or away from the observer).
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| The results of a study using late-type eclipsing binaries to determine the distance more accurately was published in [[Nature magazine|Nature]] in March 2013. A distance of 49.97 kpc (162,983 light-years) with an accuracy of 2.2% was obtained.<ref name="Nature"/>
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| ==Features==
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| [[File:Two very different glowing gas clouds in the Large Magellanic Cloud.jpg|thumb|Two very different glowing gas clouds in the Large Magellanic Cloud<ref>{{cite news|title=The Odd Couple|url=http://www.eso.org/public/news/eso1335/|accessdate=8 August 2013|newspaper=ESO Press Release}}</ref>]]
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| Like many [[irregular galaxy|irregular galaxies]], the LMC is rich in gas and dust, and it is currently undergoing vigorous [[star formation]] activity.<ref>{{cite book |title=Explorations: An Introduction to Astronomy |last=Arny |first=Thomas T. |authorlink= |coauthors= |year=2000 |edition=2nd |publisher=McGraw-Hill |location=Boston |isbn=0-07-228249-5 |page=479 |url= }}</ref> It is home to the [[Tarantula Nebula]], the most active star-forming region in the Local Group.
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| The LMC is full of a wide range of galactic objects and phenomena that make it aptly known as an "astronomical treasure-house, a great celestial laboratory for the study of the growth and evolution of the stars," as described by [[Robert Burnham, Jr.]]<ref>{{cite book |title=Burnham's Celestial Handbook: Volume Two |last=Burnham |first=Robert, Jr. |authorlink= |coauthors= |year=1978 |publisher=Dover |location=New York |isbn=0-486-23567-X |page=837 |url= }}</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 star|giant]] and [[supergiant]] stars.<ref>Burnham (1978), 840–848.</ref> [[Supernova 1987a]]—the nearest [[supernova]] in recent years—was also located in the Large Magellanic Cloud. The '''Lionel-Murphy SNR''' is [[nitrogen]]-abundant [[supernova remnant]] (SNR) N86 in the Large Magellanic Cloud named by [[astronomers]] at the [[Australian National University]]'s [[Mount Stromlo Observatory]] in acknowledgement of [[Australian High Court]] Justice [[Lionel Murphy]]'s interest in science and because of SNR N86's perceived resemblance to his large nose.<ref>Dopita MA, Mathewson DS, Ford VL. Optical emission from shock waves. III. Abundances in supernova remnants. The Astrophysical Journal. 1977; 214: 179-188 plate 4</ref>
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| There is a [[Magellanic Bridge|bridge of gas]] connecting the Small Magellanic Cloud (SMC) with the LMC, which is evidence of tidal interaction between the galaxies.<ref name=Mathewson>{{cite journal |author=Mathewson DS, Ford VL |journal=IAUS |month= |year=1984 |volume=108 |page=125 }}</ref> The Magellanic Clouds have a common envelope of neutral hydrogen indicating they have been gravitationally bound for a long time. This bridge of gas is a star-forming site.<ref name=Heydari>{{cite journal |doi=10.1051/0004-6361:20031360 |author=Heydari-Malayeri M, Meynadier F, Charmandaris V, Deharveng L, Le Bertre T, Rosa MR, Schaerer D |month= |title=The stellar environment of SMC N81|year=2003 |journal=Astron Astrophys. |volume=411 |issue=3 |page=427 |bibcode=2003A&A...411..427H|arxiv = astro-ph/0309126 }}</ref>
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| ==X-ray sources==
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| No X-rays above background were observed from the Magellanic Clouds during the September 20, 1966, [[Nike-Tomahawk]] flight.<ref name=Chodil >{{cite journal |author=Chodil G, Mark H, Rodrigues R, Seward FD, Swift CD |title=X-Ray Intensities and Spectra from Several Cosmic Sources |journal=Ap J. |date=Oct 1967 |volume=150 |issue=10 |pages=57–65 |url= | bibcode=1967ApJ...150...57C |doi=10.1086/149312}}</ref> A second Nike-Tomahawk rocket was launched from [[Johnston Atoll]] on September 22, 1966, at 17:13 UTC and reached an apogee of {{convert|160|km|0|abbr=on}}, with spin-stabilization at 5.6 rps.<ref name=Seward >{{cite journal |doi=10.1086/149343 |author=Seward FD, Toor A |title=Search for 8-80 KEV X-Rays from the Large Magellanic Cloud and the Crab Nebula |journal=Ap J. |date=Nov 1967 |volume=150 |issue=11 |pages=405–12 |bibcode=1967ApJ...150..405S }}</ref> The LMC was not detected in the X-ray range 8-80 keV.<ref name=Seward />
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| Another Nike-Tomahawk was launched from Johnston 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 (constellation)|Dorado]] was at [[Right ascension|RA]] {{RA|05|20}} [[Declination|Dec]] {{Dec|-69}},<ref name=Mark >{{cite journal |doi=10.1086/180322 |author=Mark H, Price R, Rodrigues R, Seward FD, Swift CD |title=Detection of X-rays from the large magellanic cloud |date=Mar 1969 |journal=Ap J Lett. |volume=155 |issue=3 |pages=L143–4 |bibcode=1969ApJ...155L.143M }}</ref><ref name=Lewin >{{cite journal |author=Lewin WHG, Clark GW, Smith WB |year=1968 |journal=Nature. |volume=220 |page=249 |bibcode = 1968Natur.220..249L |doi = 10.1038/220249b0 |issue=5164}}</ref> and it was the Large Magellanic Cloud.<ref name=Dolan>{{cite journal |doi=10.1086/110966 |author=Dolan JF |title=A Catalogue of Discrete Celestial X-Ray Sources |journal=Astron J. |date=Apr 1970 |issue=4 |volume=75 |pages=223–30 |bibcode=1970AJ.....75..223D }}</ref> This X-ray source extended over about 12° and is consistent with the Cloud.<ref name=Mark /> Its emission rate between 1.5-10.5 keV for a distance of 50 kpc is 4 x 10<sup>38</sup> ergs/s.<ref name=Mark /> An [[X-ray astronomy]] instrument was carried aboard a [[Thor (rocket family)|Thor missile]] launched from [[Johnston Atoll]] on September 24, 1970, at 12:54 UTC and altitudes above {{convert|300|km|0|abbr=on}}, to search for the [[Small Magellanic Cloud]] and to extend previous observations of the LMC.<ref name=PriceThor>{{cite journal |doi=10.1086/180773 |author=Price RE, Groves DJ, Rodrigues RM, Seward FD, Swift CD, Toor A |title=X-Rays from the Magellanic Clouds |journal=Ap J. |date=Aug 1971 |volume=168 |issue=8 |pages=L7–9 |bibcode=1971ApJ...168L...7P }}</ref> The source in the LMC appeared extended and contained the star ε Dor.<ref name=PriceThor/> The X-ray luminosity (L<sub>x</sub>) over the range 1.5–12 keV was 6 × 10<sup>31</sup> W (6 × 10<sup>38</sup> erg/s).<ref name=PriceThor/>
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| The Large Magellanic Cloud (LMC) is in the constellations [[Mensa (constellation)|Mensa]] and [[Dorado (constellation)|Dorado]]. LMC X-1 (the first X-ray source in the LMC) is at [[Right ascension|RA]] {{RA|05|40|05}} [[Declination|Dec]] {{Dec|-69|45|51}}, and is a high mass X-ray binary source ([[HMXB]]).<ref name=Rapley>{{cite journal |author=Rapley, Tuohy|title=X-Ray Observations of the Large Magellanic Cloud by the Copernicus Satellite|journal=Astrophysical Journal |volume=191 |page=L113 |year=1974 |bibcode=1974ApJ...191L.113R|doi=10.1086/181564}}</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); [[Large Magellanic Cloud X-2|LMC X-2]] is the only one that is a bright low-mass X-ray binary system ([[LMXB]]) in the LMC.<ref name=Bonnet>{{cite journal |author=Bonnet-Bidaud JM, Motch C, Beuermann K, Pakull M, Parmar AN, van der Klis M |title=LMC X-2: an extragalactic bulge-type source |journal=Astron Astrophys. |date=Apr 1989 |volume=213 |issue=1-2 |pages=97–106 |bibcode=1989A&A...213...97B }}</ref>
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| DEM L316 in the Large Magellanic Cloud consists of two supernove remnants.<ref name=Williams>{{cite journal |author=Williams RM, Chu YH |title=Supernova Remnants in the Magellanic Clouds. VI. The DEM L316 Supernova Remnants |journal=Ap J. |date=Dec 2005 |volume=635 |issue=2 |pages=1077–86 |url=http://iopscience.iop.org/0004-637X/635/2/1077/pdf/0004-637X_635_2_1077.pdf |doi=10.1086/497681 |bibcode=2005ApJ...635.1077W|arxiv = astro-ph/0509696 }}</ref> [[Chandra X-ray Observatory|Chandra]] X-ray spectra show that the hot gas shell on the upper left contains a high abundance of iron.<ref name=Williams/> This implies that the upper left [[Supernova remnant|SNR]] is the product of a [[Type Ia supernova]].<ref name=Williams/> The much lower iron abundance in the lower SNR indicates a [[Type II supernova]].<ref name=Williams/>
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| A 16 ms X-ray pulsar is associated with SNR 0538-69.1.<ref name="MarshallGotthelf1998">{{cite journal|last1=Marshall|first1=F. E.|last2=Gotthelf|first2=E. V|last3=Zhang|first3=W.|last4=Middleditch|first4=J.|last5=Wang|first5=Q. D.|title=Discovery of an Ultrafast X-Ray Pulsar in the Supernova Remnant N157B|journal=The Astrophysical Journal|volume=499|issue=2|year=1998|pages=L179–L182|issn=0004637X|doi=10.1086/311381|url=https://hea-www.harvard.edu/ChandraSNR/SNR0538-69.1/|arxiv = astro-ph/9803214 |bibcode = 1998ApJ...499L.179M }}</ref> SNR 0540-697 was resolved using [[ROSAT]].<ref name="ChuKennicutt1997">{{cite journal|last1=Chu|first1=Y.-H.|last2=Kennicutt|first2=R. C.|last3=Snowden|first3=S. L.|last4=Smith|first4=R. C.|last5=Williams|first5=R. M.|last6=Bomans|first6=D. J.|title=Uncovering a Supernova Remnant Hidden Near LMCX-1|journal=Publications of the Astronomical Society of the Pacific|volume=109|year=1997|page=554|issn=0004-6280|doi=10.1086/133913|bibcode = 1997PASP..109..554C }}</ref>
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| ==View from the LMC==
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| {{Refimprove section|date=August 2012}}
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| From a viewpoint in the LMC, the Milky Way would be a spectacular sight. The galaxy's total [[apparent magnitude]] would be −2.0—over 14 times brighter than the LMC appears to us on Earth—and it would span about 36[[degree (angle)|°]] across the sky, which is the width of over 70 full moons. Furthermore, because of the LMC's high [[Galactic coordinate system|galactic latitude]], an observer there would get an oblique view of the entire galaxy, free from the interference of [[interstellar dust]] which makes studying in the Milky Way's plane difficult from Earth.<ref>Some of the figures in the "View" section were extrapolated from data in the Appendix of Chaisson and McMillan's ''Astronomy Today'' (Englewood Cliffs: Prentice-Hall, Inc., 1993).</ref> The [[Small Magellanic Cloud]] would be about magnitude 0.6, substantially brighter than the LMC appears to us.
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| == Gallery ==
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| <gallery style="margin:auto;">
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| Image:The star formation region NGC 2035 imaged by the ESO Very Large Telescope.jpg|The star formation region [[NGC 2035]] imaged by the [[ESO]] [[Very Large Telescope|VLT]]<ref>{{cite news|title=A Fiery Drama of Star Birth and Death|url=http://www.eso.org/public/news/eso1348/|accessdate=29 November 2013|newspaper=ESO Press Release}}</ref>
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| Image:LHA 120-N11 in the Large Magellanic Cloud.jpg|LHA 120-N11 in the Large Magellanic Cloud. Credit: [[NASA]]/[[ESA]]
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| Image:LH 95.jpg|[[LH 95]] stellar nursery in Large Magellanic Cloud. Credit: [[NASA]]/[[ESA]]
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| Image:ESO-SNR B0544-6910 in the LMC-phot-34d-04-fullres.jpg|SNR B0544-6910 in the LMC. Credit: [[ESO]]
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| Image:ESO-SNR 0543-689 in the LMC-phot-34c-04-fullres.jpg|SNR 0543-689 in the LMC. Credit: [[ESO]]
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| Image:Southern part of the spectacular N44 H II region in the Large Magellanic Cloud.jpg|N44 region in the Large Magellanic Cloud. Credit: [[ESO]]
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| Image:ESO-DEM L 159 Nebula KMHK 840 and 831 clusters LMC-phot-31c-03-fullres.jpg| DEM L 159 and two clusters KMHK 840 (top left) and KMHK 831 (bottom right). Credit: [[ESO]]
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| Image:Image from ESO’s La Silla Observatory of part of the Large Magellanic Cloud.jpg| Image from the Wide Field Imager on the MPG/ESO 2.2-metre telescope at ESO's La Silla Observatory in Chile. Credit: [[ESO]]
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| Image:Large and small magellanic cloud from new zealand.jpg|Large and Small Magellanic Clouds as viewed in the Southern Hemisphere sky
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| Image:Large Magellanic Cloud.jpg|The Large Magellanic Cloud galaxy in [[infrared]] light.
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| File:Large Magellanic Cloud-8sec.jpg|Large Magellanic Cloud 12 frames stacked each frame taken 8 sec. with steady camera. [[Canon EOS 7D]] with [[Canon EF 85mm lens#EF 85mm f/1.8 USM|85mm f/1.8]] squeezed to f/2.5, at ASA 3200.
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| </gallery>
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| ==See also==
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| *[[Galaxies in fiction#Large Magellanic Cloud|Large Magellanic Cloud in fiction]]
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| == Notes ==
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| {{Reflist|colwidth=30em}}
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| ==External links==
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| {{commons category|Large Magellanic Cloud}}
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| *[http://nedwww.ipac.caltech.edu/index.html NASA Extragalactic Database]
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| *[http://www.daviddarling.info/encyclopedia/L/LMC.html Encyclopedia of Astronomy entry]
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| *[http://www.seds.org/messier/xtra/ngc/lmc.html SEDS LMC page]
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| {{Milky Way}}
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| {{Sky|05|23|34.5|-|69|45|22|157000}}
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| [[Category:Dwarf barred irregular galaxies]]
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| [[Category:Large Magellanic Cloud| ]]
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| [[Category:PGC objects|17223]]
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| {{link FA|it}}
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