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faint, taking hours of exposure to capture. These nebulae clouds, an important component of the interstellar medium, are composed of dust particles, hydrogen and carbon monoxide and other elements." They are particularly prominent in the direction of both the north and south celestial poles. The vast nebula close to the south celestial pole is MW9, commonly known as the South
Celestial Serpent.
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2424:
188:
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140:. Earth's air has a density of approximately 10 molecules per cubic centimeter; by contrast, the densest nebulae can have densities of 10 molecules per cubic centimeter. Many nebulae are visible due to fluorescence caused by embedded hot stars, while others are so diffused that they can be detected only with long exposures and special filters. Some nebulae are variably illuminated by
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continued to collect the spectra from many different nebulae, finding 29 that showed emission spectra and 33 that had the continuous spectra of star light. In 1922, Hubble announced that nearly all nebulae are associated with stars and that their illumination comes from star light. He also discovered
333:
was published in 1786. A second catalog of a thousand was published in 1789, and the third and final catalog of 510 appeared in 1802. During much of their work, William
Herschel believed that these nebulae were merely unresolved clusters of stars. In 1790, however, he discovered a star surrounded by
892:
Planetary nebulae were given their name by the first astronomical observers who were initially unable to distinguish them from planets, and who tended to confuse them with planets, which were of more interest to them. The Sun is expected to spawn a planetary nebula about 12 billion years after
824:
Reflection nebulae themselves do not emit significant amounts of visible light, but are near stars and reflect light from them. Similar nebulae not illuminated by stars do not exhibit visible radiation, but may be detected as opaque clouds blocking light from luminous objects behind them; they are
772:
The term was coined by Steve Mandel who defined them as "high galactic latitude nebulae that are illuminated not by a single star (as most nebula in the plane of the Galaxy are) but by the energy from the integrated flux of all the stars in the Milky Way. As a result, these nebulae are incredibly
462:. Feedback from star-formation, in the form of supernova explosions of massive stars, stellar winds or ultraviolet radiation from massive stars, or outflows from low-mass stars may disrupt the cloud, destroying the nebula after several million years.
469:
explosions; the death throes of massive, short-lived stars. The materials thrown off from the supernova explosion are then ionized by the energy and the compact object that its core produces. One of the best examples of this is the
1000:
in the core of the star stops, the star collapses. The gas falling inward either rebounds or gets so strongly heated that it expands outwards from the core, thus causing the star to explode. The expanding shell of gas forms a
421:, the coldest, densest phase of interstellar gas, which can form by the cooling and condensation of more diffuse gas. Examples of the latter case are planetary nebulae formed from material shed by a star in late stages of its
665:
1248:
431:
are a class of emission nebula associated with giant molecular clouds. These form as a molecular cloud collapses under its own weight, producing stars. Massive stars may form in the center, and their
179:, and others. Edwin Hubble discovered that most nebulae are associated with stars and illuminated by starlight. He also helped categorize nebulae based on the type of light spectra they produced.
93:. In these regions, the formations of gas, dust, and other materials "clump" together to form denser regions, which attract further matter and eventually become dense enough to form
1495:
520:
650:
128:, can be viewed with the naked eye but was missed by early astronomers. Although denser than the space surrounding them, most nebulae are far less dense than any
790:
Most nebulae can be described as diffuse nebulae, which means that they are extended and contain no well-defined boundaries. Diffuse nebulae can be divided into
1620:
881:. Radiation from the hot white dwarf excites the expelled gases, producing emission nebulae with spectra similar to those of emission nebulae found in
877:
stars expel their outer layers outwards due to strong stellar winds, thus forming gaseous shells while leaving behind the star's core in the form of a
1594:
Halley, E. (1714–1716). "An account of several nebulae or lucid spots like clouds, lately discovered among the fixed stars by help of the telescope".
873:
Planetary nebulae are the remnants of the final stages of stellar evolution for mid-mass stars (varying in size between 0.5-~8 solar masses). Evolved
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497:
and slowly lose their outer layers during pulsations in their atmospheres. When a star has lost enough material, its temperature increases and the
228:
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are a relatively recently identified astronomical phenomenon. In contrast to the typical and well known gaseous nebulae within the plane of the
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601:
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that the emission spectrum nebulae are nearly always associated with stars having spectral classifications of B or hotter (including all
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the surrounding nebula that it has thrown off. The Sun will produce a planetary nebula and its core will remain behind in the form of a
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349:. The rest showed a continuous spectrum and were thus thought to consist of a mass of stars. A third category was added in 1912 when
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There are a variety of formation mechanisms for the different types of nebulae. Some nebulae form from gas that is already in the
1350:
272:
889:, because mostly hydrogen is ionized, but planetary are denser and more compact than nebulae found in star formation regions.
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1422:
493:. This is the final stage of a low-mass star's life, like Earth's Sun. Stars with a mass up to 8–10 solar masses evolve into
636:
2228:
1243:
821:, H II referring to ionized hydrogen), and reflection nebulae which are visible primarily due to the light they reflect.
2164:
2584:
2182:
1274:
482:. The compact object that was created after the explosion lies in the center of the Crab Nebula and its core is now a
959:. It is the second-from-the-last high-luminosity evolution phase in the life cycle of intermediate-mass stars (1–8
2441:
2371:
2012:
Kastner, J. H. (2005), "Near-death
Transformation: Mass Ejection in Planetary Nebulae and Protoplanetary Nebulae",
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in general as "spiral nebulae") before the true nature of galaxies was confirmed in the early 20th century by
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31:
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Although these nebulae have different visibility at optical wavelengths, they are all bright sources of
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236:
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2014:
American
Astronomical Society Meeting 206, #28.04; Bulletin of the American Astronomical Society
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in 1618. However, the first detailed study of the Orion Nebula was not performed until 1659 by
124:, the brightest nebula in the sky and occupying an area twice the angular diameter of the full
37:
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2123:
1971:
1950:
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nebulosity and concluded that this was a true nebulosity rather than a more distant cluster.
132:
created on Earth (10 to 10 molecules per cubic centimeter) – a nebular cloud the size of the
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102:
1524:"Suspected New Stars Recorded in the Old Chronicles and Among Recent Meridian Observations"
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1223:
791:
553:
338:
307:
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compiling a list of 20 (including eight not previously known) in 1746. From 1751 to 1753,
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published a list of six nebulae. This number steadily increased during the century, with
168:
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1990:
1787:
1756:
1729:
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1663:
1633:
1580:
1539:
1508:
1443:
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too distant to be resolved as stars were also classified as nebulae, but no longer are.
687:
Objects named nebulae belong to four major groups. Before their nature was understood,
391:
concluded that the nebulae surrounding the hotter stars are transformed in some manner.
341:
examined the spectra of about 70 nebulae. He found that roughly a third of them had the
314:, which included what are now known to be galaxies) by 1781; his interest was detecting
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1006:
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882:
867:
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311:
54:
1618:
Hoskin, Michael (2005). "Unfinished
Business: William Herschel's Sweeps for Nebulae".
208:, five stars that appeared nebulous. He also noted a region of nebulosity between the
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1918:
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emission from supernova remnants originates from ionized gas, a great amount of the
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387:), while nebulae with continuous spectra appear with cooler stars. Both Hubble and
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141:
121:
90:
1811:
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1493:
Harrison, T. G. (March 1984). "The Orion Nebula – where in
History is it".
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http://www.aicccd.com/archive/aic2005/The_unexplored_nebula_project-smandel.pdf
1641:
916:
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1198:
1039:
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while the shells of neutral hydrogen surrounding the H II region are known as
442:. The region of ionized hydrogen surrounding the massive stars is known as an
439:
212:
109:
1395:
993:
764:
494:
466:
372:
253:
156:
113:
1716:
Struve, Otto (1937). "Recent
Progress in the Study of Reflection Nebulae".
854:
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287:, who also believed he was the first person to discover this nebulosity.
17:
1022:
952:
859:
833:
814:
656:
371:, it became clear that many "nebulae" were in fact galaxies far from the
358:
204:
137:
78:
1743:
Slipher, V. M. (1912). "On the spectrum of the nebula in the
Pleiades".
977:
1876:
1337:
1322:
1307:
1304:
Collins
English Dictionary – Complete and Unabridged, 12th Edition 2014
1292:
805:
Visible light nebulae may be divided into emission nebulae, which emit
754:
642:
479:
403:
261:
199:
2041:
248:
star cluster as a "nebulous star" and other nebulous objects, such as
1249:
Timeline of knowledge about the interstellar and intergalactic medium
767:
688:
152:
129:
98:
1683:
Watts, William
Marshall; Huggins, Sir William; Lady Huggins (1904).
417:
while others are produced by stars. Examples of the former case are
2462:
1998:
1970:
Sahai, Raghvendra; Sánchez Contreras, Carmen; Morris, Mark (2005).
1796:
1771:
1548:
1523:
1334:
The American Heritage Dictionary of Student Science, Second Edition
1289:
American Heritage Dictionary of the English Language, Fifth Edition
478:. The supernova event was recorded in the year 1054 and is labeled
321:
The number of nebulae was then greatly increased by the efforts of
1010:
976:
915:
853:
781:
748:
398:
315:
186:
133:
117:
36:
996:
occurs when a high-mass star reaches the end of its life. When
936:
753:
An example of faint integrated flux nebula surrounding the star
675:
353:
showed that the spectrum of the nebula that surrounded the star
220:
147:
Originally, the term "nebula" was used to describe any diffused
125:
94:
2062:
1949:(2nd ed.). Upper Saddle River, New Jersey: Prentice-Hall.
810:
502:
435:
346:
2509:
2047:
1351:"In Reality, Nebulae Offer No Place for Spaceships to Hide"
331:
Catalogue of One Thousand New Nebulae and Clusters of Stars
2058:
318:, and these were objects that might be mistaken for them.
120:
would appear larger, but no brighter, from close by. The
85:. Nebulae are often star-forming regions, such as in the
1528:
Publications of the Astronomical Society of the Pacific
77:, which can consist of ionized, neutral, or molecular
2439:
1924:. Mill Valley, California: University Science Books.
364:. Thus, the nebula radiates by reflected star light.
310:
then compiled a catalog of 103 "nebulae" (now called
279:
using a telescope. This nebula was also observed by
108:
Most nebulae are of vast size; some are hundreds of
2381:
2335:
2319:
2298:
2260:
2227:
2196:
2163:
2096:
1847:Chadwick, Stephen; Cooper, Ian (11 December 2012).
1496:
Quarterly Journal of the Royal Astronomical Society
1336:. S.v. "nebula." Retrieved November 23, 2019, from
1321:. S.v. "nebula." Retrieved November 23, 2019, from
1319:
Random House Kernerman Webster's College Dictionary
1306:. S.v. "nebula." Retrieved November 23, 2019, from
1291:. S.v. "nebula." Retrieved November 23, 2019, from
786:
The Carina Nebula is an example of a diffuse nebula
702:, large diffuse nebulae containing ionized hydrogen
1917:
1017:emission is a form of non-thermal emission called
438:the surrounding gas, making it visible at optical
1972:"A Starfish Preplanetary Nebula: IRAS 19024+0044"
1686:An introduction to the study of spectrum analysis
97:. The remaining material is then thought to form
931:or preplanetary nebula (PPN, plural PPNe) is an
770:, IFNs lie beyond the main body of the galaxy.
1772:"The source of luminosity in galactic nebulae"
1423:"A Medieval Reference to the Andromeda Nebula"
1021:. This emission originates from high-velocity
2074:
1947:Astronomy: a beginner's guide to the universe
1613:
1611:
935:which is at the short-lived episode during a
112:in diameter. A nebula that is visible to the
8:
1569:Astronomical Society of the Pacific Leaflets
223:. The first true nebula, as distinct from a
163:, for instance, was once referred to as the
1711:
1709:
1707:
722:Not all cloud-like structures are nebulae;
450:. Examples of star-forming regions are the
240:(964). He noted "a little cloud" where the
2337:
2081:
2067:
2059:
1911:
1909:
1907:
1905:
1903:
1901:
1899:
1897:
1895:
1893:
1621:British Journal for the History of Science
1488:
1486:
1374:. Cambridge University Press. p. 98.
45:, showing complex gas and plasma structure
1795:
1547:
1469:. Cambridge University Press. p. 1.
306:, most of which were previously unknown.
1460:
1458:
2522:
2446:
1565:"The Crab Nebula, a Probable Supernova"
1260:
516:
2055:, digital library of Paris Observatory
1873:"The Messier Catalog: Diffuse Nebulae"
643:Tycho Supernova remnant in X-ray light
136:would have a total mass of only a few
951:(PN) phase. A PPN emits strongly in
7:
2413:
1689:. Longmans, Green, and Co. pp.
1338:https://thefreedictionary.com/nebula
1323:https://thefreedictionary.com/nebula
1308:https://thefreedictionary.com/nebula
1293:https://thefreedictionary.com/nebula
465:Other nebulae form as the result of
73:) is a distinct luminescent part of
1945:Chaisson, E.; McMillan, S. (1995).
1467:Messier's nebulae and star clusters
1009:. Although much of the optical and
202:recorded, in books VII–VIII of his
58:
1182:Lynds' Catalogue of Bright Nebulae
1171:Abell Catalog of Planetary Nebulae
244:is located. He also cataloged the
25:
674:in the northern constellation of
219:that was not associated with any
2542:
2525:
2497:
2485:
2473:
2461:
2449:
2422:
2412:
2403:
2402:
2336:
1371:Visual astronomy of the deep sky
1349:Howell, Elizabeth (2013-02-22).
1187:Lynds' Catalogue of Dark Nebulae
947:(LAGB) phase and the subsequent
908:This section is an excerpt from
866:located in the constellation of
741:This section is an excerpt from
664:
649:
635:
620:
600:
580:
560:
541:
519:
1770:Hubble, E. P. (December 1922).
273:Nicolas-Claude Fabri de Peiresc
2053:Historical pictures of nebulae
1816:ESA/Hubble Picture of the Week
302:cataloged 42 nebulae from the
1:
1244:Orion molecular cloud complex
264:, was observed by Arabic and
1465:Jones, Kenneth Glyn (1991).
955:radiation, and is a kind of
489:Still other nebulae form as
2183:Evaporating gaseous globule
1745:Lowell Observatory Bulletin
1275:Online Etymology Dictionary
357:matched the spectra of the
27:Body of interstellar clouds
2601:
1665:Philosophical Transactions
1642:10.1177/007327530504300303
1597:Philosophical Transactions
924:, a protoplanetary nebula.
907:
900:
847:
809:radiation from excited or
740:
733:
385:O-type main sequence stars
57:for 'cloud, fog';
29:
2397:
1979:The Astrophysical Journal
1851:. Springer. p. 248.
1095:Engraved Hourglass Nebula
817:); they are often called
300:Nicolas-Louis de Lacaille
296:Jean-Philippe de Cheseaux
229:Muslim Persian astronomer
1849:Imaging the Southern Sky
1812:"A stellar sneezing fit"
1368:Clark, Roger N. (1990).
448:photodissociation region
41:True color image of the
1214:List of diffuse nebulae
1209:List of largest nebulae
945:asymptotic giant branch
875:asymptotic giant branch
836:emission, chiefly from
761:Integrated flux nebulae
691:("spiral nebulae") and
367:In 1923, following the
227:, was mentioned by the
32:Nebula (disambiguation)
2219:Integrated Flux Nebula
1875:. SEDS. Archived from
1421:Kunitzsch, P. (1987),
989:
925:
897:Protoplanetary nebulae
870:
787:
757:
743:Integrated Flux Nebula
736:Integrated Flux Nebula
627:The delicate shell of
419:giant molecular clouds
410:
195:
46:
2580:Concepts in astronomy
2209:Protoplanetary nebula
2173:Giant molecular cloud
2151:Protoplanetary nebula
1920:The Physical Universe
1776:Astrophysical Journal
1668:. T.N. 1786. p.
1563:Mayall, N.U. (1939).
980:
929:protoplanetary nebula
919:
910:Protoplanetary nebula
903:Protoplanetary nebula
857:
785:
752:
613:protoplanetary nebula
499:ultraviolet radiation
433:ultraviolet radiation
402:
232:Abd al-Rahman al-Sufi
190:
183:Observational history
40:
2229:Post-stellar nebulae
2044:, SEDS Messier Pages
1522:Lundmark, K (1921).
1400:Space Center Houston
1019:synchrotron emission
840:within the nebulae.
813:gas (mostly ionized
657:Southern Ring Nebula
609:Red Rectangle Nebula
429:Star-forming regions
389:Henry Norris Russell
281:Johann Baptist Cysat
30:For other uses, see
2320:Intergalactic blobs
2285:High-velocity cloud
2165:Pre-stellar nebulae
2026:2005AAS...206.2804K
1991:2005ApJ...620..948S
1788:1922ApJ....56..400H
1757:1912LowOB...2...26S
1730:1937PA.....45....9S
1634:2005HisSc..43..305H
1581:1939ASPL....3..145M
1540:1921PASP...33..225L
1509:1984QJRAS..25...65H
1444:1987Msngr..49...42K
1396:"What is a nebula?"
1025:oscillating within
933:astronomical object
724:Herbig–Haro objects
713:(e.g., Crab Nebula)
552:, an example of an
415:interstellar medium
337:Beginning in 1864,
266:Chinese astronomers
237:Book of Fixed Stars
149:astronomical object
87:Pillars of Creation
75:interstellar medium
2585:Interstellar media
2372:Supernova remnants
2268:Interstellar cloud
2247:Pulsar wind nebula
1916:F. H. Shu (1982).
1239:Nebular hypothesis
1166:Caldwell Catalogue
1157:(emission nebulae)
1151:(emission nebulae)
1145:(emission nebulae)
990:
985:, an example of a
973:Supernova remnants
926:
885:regions. They are
871:
796:reflection nebulae
788:
758:
711:Supernova remnants
659:, Planetary Nebula
611:, an example of a
591:, an example of a
571:, an example of a
411:
406:, a nebula in the
285:Christiaan Huygens
196:
47:
2437:
2436:
2242:Supernova remnant
2214:Wolf–Rayet nebula
2141:Reflection nebula
2124:Supernova remnant
2048:Fusedweb.pppl.gov
1718:Popular Astronomy
1268:Harper, Douglas.
1229:Magellanic Clouds
1176:Barnard Catalogue
1161:Messier Catalogue
1155:Sharpless catalog
1115:Red Square Nebula
1003:supernova remnant
987:supernova remnant
957:reflection nebula
943:between the late
844:Planetary nebulae
706:Planetary nebulae
491:planetary nebulae
423:stellar evolution
408:Triangulum Galaxy
343:emission spectrum
327:Caroline Herschel
304:Cape of Good Hope
256:that created the
250:Brocchi's Cluster
16:(Redirected from
2592:
2555:
2547:
2546:
2545:
2538:
2530:
2529:
2528:
2518:
2502:
2501:
2500:
2490:
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2488:
2478:
2477:
2476:
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2465:
2454:
2453:
2452:
2445:
2426:
2416:
2415:
2406:
2405:
2340:
2339:
2327:Lyman-alpha blob
2237:Planetary nebula
2119:Planetary nebula
2083:
2076:
2069:
2060:
2029:
2028:
2009:
2003:
2002:
1976:
1967:
1961:
1960:
1942:
1936:
1935:
1923:
1913:
1888:
1887:
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1884:
1869:
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1605:
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1560:
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1519:
1513:
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1480:
1462:
1453:
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1451:
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1427:
1418:
1412:
1411:
1409:
1407:
1402:. March 19, 2020
1392:
1386:
1385:
1365:
1359:
1358:
1346:
1340:
1331:
1325:
1316:
1310:
1301:
1295:
1286:
1280:
1279:
1265:
1219:Lists of nebulae
1130:Tarantula Nebula
1090:Horsehead Nebula
1055:Cat's Eye Nebula
1050:Boomerang Nebula
949:planetary nebula
922:Westbrook Nebula
864:planetary nebula
850:Planetary nebula
792:emission nebulae
726:are an example.
668:
653:
639:
624:
604:
593:planetary nebula
589:Cat's Eye Nebula
584:
569:Horsehead Nebula
564:
545:
523:
325:and his sister,
323:William Herschel
242:Andromeda Galaxy
165:Andromeda Nebula
161:Andromeda Galaxy
144:variable stars.
103:planetary system
60:
21:
2600:
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2554:from Wikisource
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2517:sister projects
2516:
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2355:Largest Nebulae
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2311:Pinwheel nebula
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2278:Infrared cirrus
2273:Molecular cloud
2256:
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2146:Variable nebula
2114:Emission nebula
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975:
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969:
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852:
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778:Diffuse nebulae
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554:emission nebula
546:
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515:
397:
339:William Huggins
312:Messier objects
308:Charles Messier
275:discovered the
246:Omicron Velorum
198:Around 150 AD,
191:Portion of the
185:
169:spiral galaxies
35:
28:
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2197:Stellar nebula
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2109:Diffuse nebula
2106:
2100:
2098:
2097:Visible nebula
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2088:
2086:
2085:
2078:
2071:
2063:
2057:
2056:
2050:
2045:
2037:
2036:External links
2034:
2031:
2030:
2004:
1999:10.1086/426469
1985:(2): 948–960.
1962:
1955:
1937:
1930:
1889:
1864:
1858:978-1461447498
1857:
1839:
1828:
1803:
1797:10.1086/142713
1762:
1735:
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1675:
1655:
1628:(3): 305–320.
1607:
1586:
1555:
1549:10.1086/123101
1514:
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1387:
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1355:Universe Today
1341:
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1184:
1179:
1178:(dark nebulae)
1173:
1168:
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1146:
1138:
1135:
1133:
1132:
1127:
1125:Rosette Nebula
1122:
1117:
1112:
1110:Pelican Nebula
1107:
1102:
1097:
1092:
1087:
1082:
1080:Fox Fur Nebula
1077:
1072:
1067:
1062:
1057:
1052:
1047:
1045:Barnard's Loop
1042:
1036:
1034:
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1007:diffuse nebula
998:nuclear fusion
974:
971:
964:
961:
914:
906:
901:Main article:
898:
895:
883:star formation
868:Camelopardalis
848:Main article:
845:
842:
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734:Main article:
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629:SNR B0509-67.5
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456:Rosette Nebula
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210:constellations
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1149:RCW Catalogue
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1128:
1126:
1123:
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1118:
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1113:
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1100:Lagoon Nebula
1098:
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1075:Carina Nebula
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860:Oyster Nebula
856:
851:
843:
841:
839:
835:
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828:
822:
820:
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812:
808:
807:spectral line
803:
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784:
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771:
769:
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737:
729:
727:
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712:
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694:
693:star clusters
690:
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531:
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512:
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508:
504:
501:it emits can
500:
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351:Vesto Slipher
348:
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324:
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309:
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297:
293:
292:Edmond Halley
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243:
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238:
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230:
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218:
214:
211:
207:
206:
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194:
193:Carina Nebula
189:
182:
180:
178:
174:
173:Vesto Slipher
170:
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158:
154:
150:
145:
143:
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80:
76:
72:
68:
64:
56:
52:
44:
43:Trifid Nebula
39:
33:
19:
2549:
2537:from Commons
2532:
2511:
2504:Solar System
2204:Nova remnant
2188:Solar nebula
2129:Nova remnant
2089:
2017:
2013:
2007:
1982:
1978:
1965:
1946:
1940:
1919:
1881:. Retrieved
1877:the original
1867:
1848:
1842:
1831:
1819:. Retrieved
1815:
1806:
1779:
1775:
1765:
1748:
1744:
1738:
1721:
1717:
1695:. Retrieved
1685:
1678:
1664:
1658:
1625:
1619:
1601:
1595:
1589:
1575:(119): 145.
1572:
1568:
1558:
1534:(195): 225.
1531:
1527:
1517:
1503:(1): 70–73.
1500:
1494:
1466:
1447:, retrieved
1435:
1429:
1416:
1404:. Retrieved
1399:
1390:
1370:
1363:
1354:
1344:
1333:
1329:
1318:
1314:
1303:
1299:
1288:
1284:
1273:
1263:
1105:Orion Nebula
1085:Helix Nebula
1065:Eagle Nebula
1005:, a special
991:
891:
887:H II regions
872:
831:
827:dark nebulae
823:
819:H II regions
804:
800:dark nebulae
789:
759:
730:Flux Nebulae
721:
717:Dark nebulae
700:H II regions
686:
550:Omega Nebula
488:
484:neutron star
464:
460:Omega Nebula
452:Orion Nebula
427:
412:
380:Edwin Hubble
378:Slipher and
377:
369:Great Debate
366:
362:open cluster
336:
330:
320:
289:
277:Orion Nebula
270:
235:
225:star cluster
203:
197:
177:Edwin Hubble
164:
151:, including
146:
122:Orion Nebula
107:
91:Eagle Nebula
70:
66:
62:
50:
48:
2492:Outer space
2480:Spaceflight
2178:Bok globule
2134:H II region
2104:Dark nebula
1821:16 December
1782:: 400–438.
1204:H II region
1143:Gum catalog
1120:Ring Nebula
1060:Crab Nebula
983:Crab Nebula
879:white dwarf
672:Ring Nebula
573:dark nebula
527:Herbig–Haro
507:white dwarf
472:Crab Nebula
444:H II region
440:wavelengths
258:Crab Nebula
155:beyond the
110:light-years
83:cosmic dust
2564:Categories
2428:Wiktionary
2299:Morphology
2290:H I region
2252:Supershell
1883:2007-06-12
1697:2009-10-31
1449:2009-10-31
1255:References
1199:H I region
1040:Ant Nebula
495:red giants
213:Ursa Major
105:objects.
101:and other
18:Nebulosity
2456:Astronomy
2360:Planetary
1751:: 26–27.
1650:161558679
1604:: 390–92.
1438:: 42–43,
1023:electrons
994:supernova
941:evolution
939:'s rapid
765:Milky Way
467:supernova
395:Formation
373:Milky Way
290:In 1715,
271:In 1610,
268:in 1054.
254:supernova
157:Milky Way
138:kilograms
114:human eye
81:and also
2408:Category
1724:: 9–22.
1406:June 27,
1270:"nebula"
1193:See also
1137:Catalogs
1033:Examples
965:☉
953:infrared
834:infrared
815:hydrogen
689:galaxies
458:and the
359:Pleiades
329:. Their
205:Almagest
153:galaxies
79:hydrogen
2570:Nebulae
2442:Portals
2418:Commons
2382:Related
2350:Diffuse
2090:Nebulae
2042:Nebulae
2022:Bibcode
1987:Bibcode
1784:Bibcode
1753:Bibcode
1726:Bibcode
1630:Bibcode
1577:Bibcode
1536:Bibcode
1505:Bibcode
1440:Bibcode
825:called
811:ionized
755:Polaris
480:SN 1054
436:ionizes
404:NGC 604
262:SN 1054
234:in his
200:Ptolemy
142:T Tauri
99:planets
89:in the
71:nebulas
63:nebulae
2512:Nebula
2374:(SNRs)
2368:(PPNe)
2261:Clouds
1953:
1928:
1855:
1648:
1473:
1378:
768:galaxy
534:HH 164
530:HH 161
503:ionize
476:Taurus
454:, the
355:Merope
316:comets
252:. The
159:. The
130:vacuum
67:nebulæ
51:nebula
2551:Texts
2534:Media
2468:Stars
2362:(PNe)
2342:Lists
1975:(PDF)
1646:S2CID
1602:XXXIX
1426:(PDF)
1015:radio
1011:X-ray
862:is a
513:Types
474:, in
345:of a
167:(and
134:Earth
118:Earth
116:from
95:stars
69:, or
55:Latin
1951:ISBN
1926:ISBN
1853:ISBN
1823:2013
1471:ISBN
1408:2021
1376:ISBN
981:The
937:star
920:The
858:The
838:dust
798:and
676:Lyra
607:The
587:The
567:The
548:The
532:and
221:star
215:and
126:Moon
1995:doi
1983:620
1792:doi
1693:–85
1670:457
1638:doi
1544:doi
347:gas
217:Leo
59:pl.
2566::
2020:,
2018:37
2016:,
1993:.
1981:.
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