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词条 Large Magellanic Cloud
释义

  1. History

  2. Geometry

  3. Distance

  4. Features

  5. X-ray sources

  6. See also

  7. Notes

  8. External links

{{Infobox galaxy
| name = Large Magellanic Cloud
| image =
| caption= The Large Magellanic Cloud
| epoch = J2000
| type = SB(s)m[1]
| ra = {{RA|05|23|34.5}}[1]
| dec = {{DEC|-69|45|22}}[1]
| dist_ly = 163.0 kly (49.97 kpc)[2]
| Radial Velocity = 278 ± 3 km/s[1]
| appmag_v = 0.9[1]
| size_v = 10.75° × 9.17°[1]
| mass = {{nowrap|1010}}[8]
| constellation name = Dorado/Mensa
| size = 14,000 ly in diameter
(~4.3 kpc)[8]
| names = LMC, ESO 56- G 115, PGC 17223,[1] Nubecula Major[3]
}}

The Large Magellanic Cloud (LMC) is a satellite galaxy of the Milky Way.[4] At a distance of about 50 kiloparsecs (≈163,000 light-years),[2][14][5][6] the LMC is the second- or third-closest galaxy to the Milky Way, after the Sagittarius Dwarf Spheroidal (~16 kpc) and the possible dwarf irregular galaxy known as the Canis Major Overdensity. Based on readily visible stars and a mass of approximately 10 billion solar masses, the diameter of the LMC is about {{convert|14000|ly|kpc}}, making it roughly one one-hundredth as massive as the Milky Way.[7] This makes the LMC 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.[9] It contains a stellar bar that is geometrically off-center, suggesting that it was a barred dwarf spiral galaxy before its spiral arms were disrupted, likely by tidal interactions from the Small Magellanic Cloud (SMC), and the Milky Way's gravity.[10]

With a declination of about -70°, the LMC is visible as a faint "cloud" only in the southern celestial hemisphere and from latitudes south of 20° N, straddling the border between the constellations of Dorado and Mensa, and appears longer than 20 times the Moon's diameter (about 10° across) from dark sites away from light pollution.[11]

The Milky Way and the LMC are expected to collide in approximately 2.4 billion years.[12]

History

Although both clouds have been easily visible for southern nighttime observers well back into prehistory, 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"), in his Book of Fixed Stars around 964 AD.[14][15]

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{{sic}}, two bright and one obscure"; "bright" refers to the two Magellanic Clouds, and "obscure" refers to the Coalsack.[16]

Ferdinand Magellan sighted the LMC on his voyage in 1519, and his writings brought the LMC into common Western knowledge. The galaxy now bears his name.[15]

Measurements with the Hubble Space Telescope, announced in 2006, suggest the Large and Small Magellanic Clouds may be moving too fast to be orbiting the Milky Way.[17]

Geometry

The Large Magellanic Cloud has a prominent central bar and a spiral arm.[18] The central bar seems to be warped so that the east and west ends are nearer the Milky Way than the middle.[19] In 2014, measurements from the Hubble Space Telescope made it possible to determine that the LMC has a rotation period of 250 million years.[20]

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[21] 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,[22] core helium-burning red clump stars[23] and the tip of the red giant branch.[24] 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[24] and flared.[25] Regarding the distribution of star clusters in the LMC, Schommer et al.[26] 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.,[27] 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.

Distance

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.[28]

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.

In 2006, the Cepheid absolute luminosity was re-calibrated using Cepheid variables in the galaxy Messier 106 that cover a range of metallicities.[29] Using this improved calibration, they find an absolute distance modulus of 18.41, or 48 kpc (~157,000 light-years). This distance has been confirmed by other authors.[5][6]

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 49.97 kpc (163,000 light-years) with an accuracy of 2.2% was obtained.[2]

Features

Like many irregular galaxies, the LMC is rich in gas and dust, and it is currently undergoing vigorous star formation activity.[31] It is home to 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 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.[33] 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.[34] Supernova 1987a—the nearest supernova in recent years—was also located 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, 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.[35]

There is a bridge of gas connecting the Small Magellanic Cloud (SMC) with the LMC, which is evidence of tidal interaction between the galaxies.[36] 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.[37]

X-ray sources

No X-rays above background were observed from the Magellanic Clouds during the September 20, 1966, Nike-Tomahawk flight.[38] 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.[39] The LMC was not detected in the X-ray range 8–80 keV.[39]

Another Nike-Tomahawk was launched from Johnston Atoll at 11:32 UTC on October 29, 1968, to scan the LMC for X-rays.[56] The first discrete X-ray source in Dorado was at RA {{RA|05|20}} Dec {{Dec|-69}},[40][41] and it was the Large Magellanic Cloud.[42] 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 4 x 1038 ergs/s.[40] An X-ray astronomy instrument was carried aboard a 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.[43] The source in the LMC appeared extended and contained the star ε Dor. The X-ray luminosity (Lx) over the range 1.5–12 keV was 6 × 1031 W (6 × 1038 erg/s).[43]

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 {{RA|05|40|05}} Dec {{Dec|-69|45|51}}, and is a high mass X-ray binary source (HMXB).[45] 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 only one that is a bright low-mass X-ray binary system (LMXB) in the LMC.[46]

DEM L316 in the Large Magellanic Cloud consists of two supernova remnants.[47] Chandra X-ray spectra show that the hot gas shell on the upper left contains a high abundance of iron. This implies that the upper-left SNR is the product of a Type Ia supernova. The much lower iron abundance in the lower SNR indicates a Type II supernova.[47]

A 16 ms X-ray pulsar is associated with SNR 0538-69.1.[48] SNR 0540-697 was resolved using ROSAT.[49]

See also

{{Portal|Astronomy}}
  • Large Magellanic Cloud in fiction

Notes

1. ^1 2 3 4 5 6 {{cite web | title=NASA/IPAC Extragalactic Database | work=Results for Large Magellanic Cloud | url=http://nedwww.ipac.caltech.edu/ | accessdate=2006-10-29 }}
2. ^1 2 {{cite journal|last=Pietrzyński|first=G|author2=D. Graczyk |author3=W. Gieren |author4=I. B. Thompson |author5=B. Pilecki |author6=A. Udalski |author7=I. Soszyński |display-authors=etal |title=An eclipsing-binary distance to the Large Magellanic Cloud accurate to two per cent|journal=Nature|date=7 March 2013|volume=495|issue=7439|pages=76–79|doi=10.1038/nature11878|pmid=23467166|arxiv = 1303.2063 |bibcode = 2013Natur.495...76P }}
3. ^{{cite journal|title=Astronomical Society of the Pacific Leaflets, The Magellanic Clouds|journal=Astronomical Society of the Pacific Leaflets|author1=Buscombe, William|volume=7|page=9|year=1954|bibcode=1954ASPL....7....9B}}
4. ^{{cite journal|bibcode=2009MNRAS.392L..21S|title=Implications of recent measurements of the Milky Way rotation for the orbit of t|journal=Monthly Notices of the Royal Astronomical Society: Letters|volume=392|pages=L21|author1=Shattow|first1=Genevieve|last2=Loeb|first2=Abraham|year=2009|doi=10.1111/j.1745-3933.2008.00573.x|arxiv = 0808.0104 }}
5. ^1 {{cite journal|bibcode=2010ARA&A..48..673F|title=The Hubble Constant|journal=Annual Review of Astronomy and Astrophysics|year=2010|arxiv = 1004.1856 |doi = 10.1146/annurev-astro-082708-101829|volume=48|pages=673–710|last1=Freedman|first1=Wendy L|last2=Madore|first2=Barry F}}
6. ^1 {{cite journal|author1=Majaess, Daniel J. |author2=Turner, David G. |author3=Lane, David J. |author4=Henden, Arne |author5=Krajci, Tom|bibcode=2011JAVSO..39..122M|title=Anchoring the Universal Distance Scale via a Wesenheit Template|journal=Journal of the American Association of Variable Star Observers|volume=|year=2010|arxiv=1007.2300}}
7. ^1 2 "Magellanic Cloud." Encyclopædia Britannica. 2009. Encyclopædia Britannica Online. 30 Aug. 2009.
8. ^{{cite paper|last1=Peñarrubia|first1=Jorge|display-authors=etal|title=A timing constraint on the total mass of the Large Magellanic Cloud|journal=Monthly Notices of the Royal Astronomical Society|volume=456|year=2016|issue=1|pages=54–58|url=https://arxiv.org/pdf/1507.03594.pdf|doi=10.1093/mnrasl/slv160|first=|date=|via=|arxiv=1507.03594|bibcode=2016MNRAS.456L..54P}}
9. ^{{cite book|last1=Peterson|first1=Barbara Ryden, Bradley M.|title=Foundations of astrophysics|date=2009|publisher=Pearson Addison-Wesley|location=New York|isbn=9780321595584|page=471}}
10. ^{{Cite journal|last=Besla|first=Gurtina|last2=Martínez-Delgado|first2=David|last3=Marel|first3=Roeland P. van der|last4=Beletsky|first4=Yuri|last5=Seibert|first5=Mark|last6=Schlafly|first6=Edward F.|last7=Grebel|first7=Eva K.|last8=Neyer|first8=Fabian|date=2016|title=Low Surface Brightness Imaging of the Magellanic System: Imprints of Tidal Interactions between the Clouds in the Stellar Periphery|url=http://stacks.iop.org/0004-637X/825/i=1/a=20|journal=The Astrophysical Journal|language=en|volume=825|issue=1|pages=20|doi=10.3847/0004-637X/825/1/20|issn=0004-637X|arxiv=1602.04222|bibcode=2016ApJ...825...20B}}
11. ^{{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 |accessdate=2013-07-17}}
12. ^{{Cite journal|last=McAlpine|first=Stuart|last2=Frenk|first2=Carlos S.|last3=Deason|first3=Alis J.|last4=Cautun|first4=Marius|date=2019-02-21|title=The aftermath of the Great Collision between our Galaxy and the Large Magellanic Cloud|url=https://academic.oup.com/mnras/article/483/2/2185/5181341|journal=Monthly Notices of the Royal Astronomical Society|language=en|volume=483|issue=2|pages=2185–2196|doi=10.1093/mnras/sty3084|issn=0035-8711}}
13. ^{{cite news|title=Cloaked in red|url=http://www.spacetelescope.org/images/potw1408a/|accessdate=12 March 2014|newspaper=ESA / HUBBLE}}
14. ^{{cite web | title=Observatoire de Paris (Abd-al-Rahman Al Sufi) | url=http://messier.obspm.fr/xtra/Bios/alsufi.html | accessdate=2007-04-19 }}
15. ^1 {{cite web | title=Observatoire de Paris (LMC) | url=http://messier.obspm.fr/xtra/ngc/lmc.html | accessdate=2007-04-19 }}
16. ^{{cite web | title=Observatoire de Paris (Amerigo Vespucci) | url=http://messier.obspm.fr/xtra/Bios/vespucci.html | accessdate=2007-04-19 }}
17. ^{{cite web|title=Press release: Magellanic Clouds May Be Just Passing Through|url=https://www.cfa.harvard.edu/news/2007-02|publisher=Harvard University|date=January 9, 2007}}
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22. ^{{cite journal |last=Nikolaev |first=S. |display-authors=etal |date=2004 |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|bibcode=2004ApJ...601..260N|citeseerx=10.1.1.409.5235}}
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25. ^{{cite journal |last=Alves |first=D. R. |authorlink= |author2=Nelson, C. A. |date=2000 |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 |bibcode=2000ApJ...542..789A|arxiv = astro-ph/0006018 }}
26. ^{{cite journal |last=Schommer |first=R. A. |display-authors=etal |date=1992 |title=Spectroscopy of giants in LMC clusters. II – Kinematics of the cluster sample |journal=The Astronomical Journal |volume=103 |issue= |pages=447–459 |doi=10.1086/116074|bibcode=1992AJ....103..447S}}
27. ^{{cite journal |last=Grocholski |first=A. J. |display-authors=etal |date=2007 |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 |bibcode=2007AJ....134..680G|arxiv = 0705.2039 }}
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29. ^1 {{cite journal |last=Macri |first=L. M. |display-authors=etal |date=2006 |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 |bibcode=2006ApJ...652.1133M|arxiv = astro-ph/0608211 }}
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32. ^{{cite news|title=A youthful cluster|url=http://www.spacetelescope.org/images/potw1534a/|accessdate=24 August 2015|newspaper=ESA/Hubble Picture of the Week}}
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37. ^{{cite journal |doi=10.1051/0004-6361:20031360 |title=The stellar environment of SMC N81|date=2003 |journal=Astronomy and Astrophysics |volume=411 |issue=3 |pages=427–435 |bibcode=2003A&A...411..427H|arxiv = astro-ph/0309126 |last1=Heydari-Malayeri |first1=M |last2=Meynadier |first2=F |last3=Charmandaris |first3=V |last4=Deharveng |first4=L |last5=Le Bertre |first5=Th |last6=Rosa |first6=M. R |last7=Schaerer |first7=D }}
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40. ^1 2 {{cite journal |doi=10.1086/180322 |title=Detection of X-rays from the large magellanic cloud |date=Mar 1969 |journal=Astrophysical Journal Letters |volume=155 |issue=3 |pages=L143–4 |bibcode=1969ApJ...155L.143M |last1=Mark |first1=Hans |last2=Price |first2=R |last3=Rodrigues |first3=R |last4=Seward |first4=F. D |last5=Swift |first5=C. D }}
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47. ^1 {{cite journal |title=Supernova Remnants in the Magellanic Clouds. VI. The DEM L316 Supernova Remnants |journal=The Astrophysical Journal |date=Dec 2005 |volume=635 |issue=2 |pages=1077–86 |doi=10.1086/497681 |bibcode=2005ApJ...635.1077W|arxiv = astro-ph/0509696 |last1=Williams |first1=R. M |last2=Chu |first2=Y.‐H }}
48. ^{{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|date=1998|pages=L179–L182|issn=0004-637X|doi=10.1086/311381|arxiv = astro-ph/9803214 |bibcode = 1998ApJ...499L.179M }}
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External links

{{commons category|Large Magellanic Cloud}}
  • NASA Extragalactic Database
  • Encyclopedia of Astronomy entry
  • SEDS LMC page
  • Large Magellanic Cloud at Constellation Guide
{{Milky Way}}{{Sky|05|23|34.5|-|69|45|22|157000}}{{Authority control}}

9 : Dwarf barred irregular galaxies|Large Magellanic Cloud|Principal Galaxies Catalogue objects|Astronomical objects known since antiquity|ESO objects|Magellanic Clouds|Dorado (constellation)|Mensa (constellation)|Local Group
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