655:
510:
739:
640:
389:
27:
551:
906:
532:
626:
2393:
772:
591:
571:
2533:
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611:
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844:
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2403:
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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.
129:. 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
2452:
371:
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
322:
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
881:
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
813:
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
761:
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
451:. 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.
458:
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
989:
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
410:, 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
420:
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
168:, 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.
654:
1237:
82:. 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
117:, 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
779:
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
1484:
870:. Radiation from the hot white dwarf excites the expelled gases, producing emission nebulae with spectra similar to those of emission nebulae found in
866:
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
1583:
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".
862:
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
1553:
486:
and slowly lose their outer layers during pulsations in their atmospheres. When a star has lost enough material, its temperature increases and the
752:
are a relatively recently identified astronomical phenomenon. In contrast to the typical and well known gaseous nebulae within the plane of the
509:
639:
372:
that the emission spectrum nebulae are nearly always associated with stars having spectral classifications of B or hotter (including all
2539:
494:
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
1609:
338:. 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
590:
522:
518:
402:
There are a variety of formation mechanisms for the different types of nebulae. Some nebulae form from gas that is already in the
217:
1339:
878:, because mostly hydrogen is ionized, but planetary are denser and more compact than nebulae found in star formation regions.
570:
550:
1411:
1170:
482:. 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
531:
2504:
1175:
810:, H II referring to ionized hydrogen), and reflection nebulae which are visible primarily due to the light they reflect.
1845:
1159:
471:. The compact object that was created after the explosion lies in the center of the Crab Nebula and its core is now a
2069:
1943:
1918:
1463:
1368:
948:. It is the second-from-the-last high-luminosity evolution phase in the life cycle of intermediate-mass stars (1–8
2001:
Kastner, J. H. (2005), "Near-death
Transformation: Mass Ejection in Planetary Nebulae and Protoplanetary Nebulae",
1861:
1824:
261:
625:
2568:
2354:
738:
160:
in general as "spiral nebulae") before the true nature of galaxies was confirmed in the early 20th century by
2217:
1232:
2153:
2573:
2171:
1263:
821:
Although these nebulae have different visibility at optical wavelengths, they are all bright sources of
610:
2430:
2360:
1585:
2348:
1083:
373:
288:
284:
436:
357:
1679:
1658:
2406:
2343:
2338:
1202:
1197:
933:
863:
234:
20:
2003:
American
Astronomical Society Meeting 206, #28.04; Bulletin of the American Astronomical Society
2563:
2207:
749:
731:
724:
712:
515:
464:
407:
272:
in 1618. However, the first detailed study of the Orion Nebula was not performed until 1659 by
113:, the brightest nebula in the sky and occupying an area twice the angular diameter of the full
1960:
1952:
2522:
2202:
2197:
2161:
2139:
2062:
1358:
917:
898:
891:
601:
487:
421:
323:
nebulosity and concluded that this was a true nebulosity rather than a more distant cluster.
220:
121:
created on Earth (10 to 10 molecules per cubic centimeter) – a nebular cloud the size of the
2010:
1975:
1772:
1741:
1714:
1618:
1565:
1524:
1513:"Suspected New Stars Recorded in the Old Chronicles and Among Recent Meridian Observations"
1493:
1428:
1007:
597:
377:
269:
238:
2412:
287:
compiling a list of 20 (including eight not previously known) in 1746. From 1751 to 1753,
283:
published a list of six nebulae. This number steadily increased during the century, with
8:
2492:
2273:
1043:
921:
577:
417:
403:
388:
225:
205:
137:
75:
63:
2014:
1979:
1776:
1745:
1718:
1673:
1652:
1622:
1569:
1528:
1497:
1432:
684:
too distant to be resolved as stars were also classified as nebulae, but no longer are.
676:
Objects named nebulae belong to four major groups. Before their nature was understood,
380:
concluded that the nebulae surrounding the hotter stars are transformed in some manner.
330:
examined the spectra of about 70 nebulae. He found that roughly a third of them had the
303:, which included what are now known to be galaxies) by 1781; his interest was detecting
2480:
2468:
2256:
2235:
2041:
1671:
1634:
1227:
1154:
273:
1607:
Hoskin, Michael (2005). "Unfinished
Business: William Herschel's Sweeps for Nebulae".
197:, five stars that appeared nebulous. He also noted a region of nebulosity between the
2230:
2129:
2112:
1939:
1914:
1907:
1841:
1638:
1459:
1364:
1217:
1164:
1149:
1143:
1103:
1033:
991:
975:
945:
929:
784:
699:
479:
411:
396:
331:
315:
292:
254:
1002:
emission from supernova remnants originates from ionized gas, a great amount of the
2558:
2444:
2396:
2330:
2315:
2225:
2107:
2055:
1983:
1780:
1626:
1532:
1207:
1118:
1078:
1038:
937:
910:
852:
838:
694:
581:
557:
376:), while nebulae with continuous spectra appear with cooler stars. Both Hubble and
311:
230:
149:
91:
1800:
2299:
2266:
2261:
2134:
2102:
1212:
780:
542:
327:
296:
157:
1482:
Harrison, T. G. (March 1984). "The Orion Nebula – where in
History is it".
2294:
2097:
1825:
http://www.aicccd.com/archive/aic2005/The_unexplored_nebula_project-smandel.pdf
1630:
1222:
1113:
1098:
1068:
1015:
995:
986:
871:
856:
444:
300:
43:
26:
2416:
435:
while the shells of neutral hydrogen surrounding the H II region are known as
431:. The region of ionized hydrogen surrounding the massive stars is known as an
2552:
2377:
1419:
1137:
1088:
1063:
1058:
795:
617:
343:
339:
280:
198:
181:
161:
31:
1384:
2456:
2192:
2176:
2117:
1705:
Struve, Otto (1937). "Recent
Progress in the Study of Reflection Nebulae".
1093:
1073:
1053:
681:
538:
472:
448:
440:
368:
350:
265:
213:
165:
130:
110:
79:
1258:
276:, who also believed he was the first person to discover this nebulosity.
2240:
2166:
2122:
2092:
1192:
1131:
1108:
1048:
971:
875:
867:
826:
815:
807:
788:
705:
688:
660:
561:
495:
460:
432:
360:, it became clear that many "nebulae" were in fact galaxies far from the
246:
71:
1732:
Slipher, V. M. (1912). "On the spectrum of the nebula in the
Pleiades".
2278:
1865:
1326:
1311:
1296:
1293:
Collins
English Dictionary – Complete and Unabridged, 12th Edition 2014
1281:
1187:
1028:
1003:
949:
794:
Visible light nebulae may be divided into emission nebulae, which emit
771:
428:
201:
98:
2030:
237:
star cluster as a "nebulous star" and other nebulous objects, such as
1238:
Timeline of knowledge about the interstellar and intergalactic medium
982:
753:
483:
455:
361:
242:
145:
102:
1672:
Watts, William
Marshall; Huggins, Sir William; Lady Huggins (1904).
406:
while others are produced by stars. Examples of the former case are
176:
1987:
1959:
Sahai, Raghvendra; Sánchez Contreras, Carmen; Morris, Mark (2005).
1785:
1760:
1537:
1512:
1323:
The American Heritage Dictionary of Student Science, Second Edition
1278:
American Heritage Dictionary of the English Language, Fifth Edition
1011:
941:
905:
848:
822:
803:
645:
467:. The supernova event was recorded in the year 1054 and is labeled
347:
310:
The number of nebulae was then greatly increased by the efforts of
193:
126:
67:
1994:
743:
631:
468:
392:
250:
188:
985:
occurs when a high-mass star reaches the end of its life. When
843:
742:
An example of faint integrated flux nebula surrounding the star
342:
showed that the spectrum of the nebula that surrounded the star
136:
Originally, the term "nebula" was used to describe any diffused
1938:(2nd ed.). Upper Saddle River, New Jersey: Prentice-Hall.
756:
677:
141:
118:
87:
966:
2498:
999:
304:
122:
106:
1958:
2036:
1340:"In Reality, Nebulae Offer No Place for Spaceships to Hide"
925:
664:
320:
Catalogue of One Thousand New Nebulae and Clusters of Stars
209:
114:
83:
2451:
2047:
307:, and these were objects that might be mistaken for them.
1818:
799:
491:
424:
335:
109:
would appear larger, but no brighter, from close by. The
74:. Nebulae are often star-forming regions, such as in the
1933:
1517:
Publications of the Astronomical Society of the Pacific
66:, which can consist of ionized, neutral, or molecular
2428:
1913:. Mill Valley, California: University Science Books.
353:. Thus, the nebula radiates by reflected star light.
299:
then compiled a catalog of 103 "nebulae" (now called
268:
using a telescope. This nebula was also observed by
97:
Most nebulae are of vast size; some are hundreds of
1836:Chadwick, Stephen; Cooper, Ian (11 December 2012).
1485:
Quarterly Journal of the Royal Astronomical Society
1453:
1325:. S.v. "nebula." Retrieved November 23, 2019, from
1310:. S.v. "nebula." Retrieved November 23, 2019, from
1308:
Random House Kernerman Webster's College Dictionary
1295:. S.v. "nebula." Retrieved November 23, 2019, from
1280:. S.v. "nebula." Retrieved November 23, 2019, from
775:
The Carina Nebula is an example of a diffuse nebula
691:, large diffuse nebulae containing ionized hydrogen
1906:
1006:emission is a form of non-thermal emission called
427:the surrounding gas, making it visible at optical
1961:"A Starfish Preplanetary Nebula: IRAS 19024+0044"
1675:An introduction to the study of spectrum analysis
1337:
86:. The remaining material is then thought to form
2550:
920:or preplanetary nebula (PPN, plural PPNe) is an
1356:
759:, IFNs lie beyond the main body of the galaxy.
1835:
1761:"The source of luminosity in galactic nebulae"
1412:"A Medieval Reference to the Andromeda Nebula"
1010:. This emission originates from high-velocity
2063:
1936:Astronomy: a beginner's guide to the universe
1602:
1600:
924:which is at the short-lived episode during a
101:in diameter. A nebula that is visible to the
1558:Astronomical Society of the Pacific Leaflets
212:. The first true nebula, as distinct from a
152:, for instance, was once referred to as the
1700:
1698:
1696:
1582:
711:Not all cloud-like structures are nebulae;
439:. Examples of star-forming regions are the
229:(964). He noted "a little cloud" where the
2326:
2070:
2056:
1900:
1898:
1896:
1894:
1892:
1890:
1888:
1886:
1884:
1882:
1610:British Journal for the History of Science
1597:
1477:
1475:
1363:. Cambridge University Press. p. 98.
34:, showing complex gas and plasma structure
1904:
1784:
1536:
1458:. Cambridge University Press. p. 1.
1409:
885:
295:, most of which were previously unknown.
1693:
1510:
1504:
1481:
1449:
1447:
965:
904:
842:
770:
737:
387:
175:
171:
25:
2000:
1879:
1854:
1731:
1554:"The Crab Nebula, a Probable Supernova"
1472:
2551:
2044:, digital library of Paris Observatory
1862:"The Messier Catalog: Diffuse Nebulae"
1758:
1704:
1606:
1551:
1545:
632:Tycho Supernova remnant in X-ray light
125:would have a total mass of only a few
2051:
1444:
961:
940:(PN) phase. A PPN emits strongly in
2505:
2402:
1678:. Longmans, Green, and Co. pp.
1327:https://thefreedictionary.com/nebula
1312:https://thefreedictionary.com/nebula
1297:https://thefreedictionary.com/nebula
1282:https://thefreedictionary.com/nebula
832:
454:Other nebulae form as the result of
62:) is a distinct luminescent part of
1934:Chaisson, E.; McMillan, S. (1995).
1456:Messier's nebulae and star clusters
998:. Although much of the optical and
191:recorded, in books VII–VIII of his
47:
13:
1256:
1171:Lynds' Catalogue of Bright Nebulae
1160:Abell Catalog of Planetary Nebulae
766:
671:
233:is located. He also cataloged the
14:
2585:
2024:
1927:
663:in the northern constellation of
208:that was not associated with any
2531:
2514:
2486:
2474:
2462:
2450:
2438:
2411:
2401:
2392:
2391:
2325:
1360:Visual astronomy of the deep sky
1338:Howell, Elizabeth (2013-02-22).
1176:Lynds' Catalogue of Dark Nebulae
936:(LAGB) phase and the subsequent
897:This section is an excerpt from
855:located in the constellation of
730:This section is an excerpt from
653:
638:
624:
609:
589:
569:
549:
530:
508:
1829:
1793:
1759:Hubble, E. P. (December 1922).
1752:
1725:
1665:
1645:
1576:
718:
262:Nicolas-Claude Fabri de Peiresc
2042:Historical pictures of nebulae
1805:ESA/Hubble Picture of the Week
1403:
1377:
1350:
1331:
1316:
1301:
1286:
1271:
1250:
291:cataloged 42 nebulae from the
1:
1243:
1233:Orion molecular cloud complex
253:, was observed by Arabic and
1454:Jones, Kenneth Glyn (1991).
944:radiation, and is a kind of
478:Still other nebulae form as
383:
7:
2172:Evaporating gaseous globule
2077:
1734:Lowell Observatory Bulletin
1264:Online Etymology Dictionary
1181:
1125:
1021:
346:matched the spectra of the
16:Body of interstellar clouds
10:
2590:
1654:Philosophical Transactions
1631:10.1177/007327530504300303
1586:Philosophical Transactions
913:, a protoplanetary nebula.
896:
889:
836:
798:radiation from excited or
729:
722:
374:O-type main sequence stars
46:for 'cloud, fog';
18:
2386:
2370:
2324:
2308:
2287:
2249:
2216:
2185:
2152:
2085:
1968:The Astrophysical Journal
1840:. Springer. p. 248.
1084:Engraved Hourglass Nebula
806:); they are often called
289:Nicolas-Louis de Lacaille
285:Jean-Philippe de Cheseaux
218:Muslim Persian astronomer
1838:Imaging the Southern Sky
1801:"A stellar sneezing fit"
1357:Clark, Roger N. (1990).
501:
437:photodissociation region
30:True color image of the
1203:List of diffuse nebulae
1198:List of largest nebulae
934:asymptotic giant branch
864:asymptotic giant branch
825:emission, chiefly from
750:Integrated flux nebulae
680:("spiral nebulae") and
356:In 1923, following the
216:, was mentioned by the
21:Nebula (disambiguation)
2208:Integrated Flux Nebula
1864:. SEDS. Archived from
1410:Kunitzsch, P. (1987),
978:
914:
886:Protoplanetary nebulae
859:
776:
746:
732:Integrated Flux Nebula
725:Integrated Flux Nebula
616:The delicate shell of
408:giant molecular clouds
399:
184:
35:
2569:Concepts in astronomy
2198:Protoplanetary nebula
2162:Giant molecular cloud
2140:Protoplanetary nebula
1909:The Physical Universe
1765:Astrophysical Journal
1657:. T.N. 1786. p.
1552:Mayall, N.U. (1939).
969:
918:protoplanetary nebula
908:
899:Protoplanetary nebula
892:Protoplanetary nebula
846:
774:
741:
602:protoplanetary nebula
488:ultraviolet radiation
422:ultraviolet radiation
391:
221:Abd al-Rahman al-Sufi
179:
172:Observational history
29:
2218:Post-stellar nebulae
2033:, SEDS Messier Pages
1511:Lundmark, K (1921).
1389:Space Center Houston
1008:synchrotron emission
829:within the nebulae.
802:gas (mostly ionized
646:Southern Ring Nebula
598:Red Rectangle Nebula
418:Star-forming regions
378:Henry Norris Russell
270:Johann Baptist Cysat
19:For other uses, see
2309:Intergalactic blobs
2274:High-velocity cloud
2154:Pre-stellar nebulae
2015:2005AAS...206.2804K
1980:2005ApJ...620..948S
1777:1922ApJ....56..400H
1746:1912LowOB...2...26S
1719:1937PA.....45....9S
1623:2005HisSc..43..305H
1570:1939ASPL....3..145M
1529:1921PASP...33..225L
1498:1984QJRAS..25...65H
1433:1987Msngr..49...42K
1385:"What is a nebula?"
1014:oscillating within
922:astronomical object
713:Herbig–Haro objects
702:(e.g., Crab Nebula)
541:, an example of an
404:interstellar medium
326:Beginning in 1864,
255:Chinese astronomers
226:Book of Fixed Stars
138:astronomical object
76:Pillars of Creation
64:interstellar medium
2574:Interstellar media
2361:Supernova remnants
2257:Interstellar cloud
2236:Pulsar wind nebula
1905:F. H. Shu (1982).
1228:Nebular hypothesis
1155:Caldwell Catalogue
1146:(emission nebulae)
1140:(emission nebulae)
1134:(emission nebulae)
979:
974:, an example of a
962:Supernova remnants
915:
874:regions. They are
860:
785:reflection nebulae
777:
747:
700:Supernova remnants
648:, Planetary Nebula
600:, an example of a
580:, an example of a
560:, an example of a
400:
395:, a nebula in the
274:Christiaan Huygens
185:
36:
2426:
2425:
2231:Supernova remnant
2203:Wolf–Rayet nebula
2130:Reflection nebula
2113:Supernova remnant
2037:Fusedweb.pppl.gov
1707:Popular Astronomy
1257:Harper, Douglas.
1218:Magellanic Clouds
1165:Barnard Catalogue
1150:Messier Catalogue
1144:Sharpless catalog
1104:Red Square Nebula
992:supernova remnant
976:supernova remnant
946:reflection nebula
932:between the late
833:Planetary nebulae
695:Planetary nebulae
480:planetary nebulae
412:stellar evolution
397:Triangulum Galaxy
332:emission spectrum
316:Caroline Herschel
293:Cape of Good Hope
245:that created the
239:Brocchi's Cluster
2581:
2544:
2536:
2535:
2534:
2527:
2519:
2518:
2517:
2507:
2491:
2490:
2489:
2479:
2478:
2477:
2467:
2466:
2465:
2455:
2454:
2443:
2442:
2441:
2434:
2415:
2405:
2404:
2395:
2394:
2329:
2328:
2316:Lyman-alpha blob
2226:Planetary nebula
2108:Planetary nebula
2072:
2065:
2058:
2049:
2048:
2018:
2017:
1998:
1992:
1991:
1965:
1956:
1950:
1949:
1931:
1925:
1924:
1912:
1902:
1877:
1876:
1874:
1873:
1858:
1852:
1851:
1833:
1827:
1822:
1816:
1815:
1813:
1811:
1797:
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1756:
1750:
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1729:
1723:
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1702:
1691:
1690:
1688:
1687:
1669:
1663:
1662:
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1391:. March 19, 2020
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1268:
1254:
1208:Lists of nebulae
1119:Tarantula Nebula
1079:Horsehead Nebula
1044:Cat's Eye Nebula
1039:Boomerang Nebula
938:planetary nebula
911:Westbrook Nebula
853:planetary nebula
839:Planetary nebula
781:emission nebulae
715:are an example.
657:
642:
628:
613:
593:
582:planetary nebula
578:Cat's Eye Nebula
573:
558:Horsehead Nebula
553:
534:
512:
314:and his sister,
312:William Herschel
231:Andromeda Galaxy
154:Andromeda Nebula
150:Andromeda Galaxy
133:variable stars.
92:planetary system
49:
2589:
2588:
2584:
2583:
2582:
2580:
2579:
2578:
2549:
2548:
2547:
2543:from Wikisource
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2513:
2510:
2506:sister projects
2503:at Knowledge's
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2366:
2344:Largest Nebulae
2320:
2304:
2300:Pinwheel nebula
2283:
2267:Infrared cirrus
2262:Molecular cloud
2245:
2212:
2181:
2148:
2135:Variable nebula
2103:Emission nebula
2081:
2076:
2027:
2022:
2021:
1999:
1995:
1963:
1957:
1953:
1946:
1932:
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1213:Molecular cloud
1184:
1128:
1123:
1024:
1016:magnetic fields
964:
959:
958:
955:
952:
902:
894:
888:
882:its formation.
841:
835:
769:
767:Diffuse nebulae
764:
763:
735:
727:
721:
674:
672:Classical types
667:
658:
649:
643:
634:
629:
620:
614:
605:
594:
585:
574:
565:
554:
545:
543:emission nebula
535:
526:
513:
504:
386:
328:William Huggins
301:Messier objects
297:Charles Messier
264:discovered the
235:Omicron Velorum
187:Around 150 AD,
180:Portion of the
174:
158:spiral galaxies
24:
17:
12:
11:
5:
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2355:Protoplanetary
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2322:
2321:
2319:
2318:
2312:
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2306:
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2297:
2295:Bipolar nebula
2291:
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2222:
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2200:
2195:
2189:
2187:
2186:Stellar nebula
2183:
2182:
2180:
2179:
2174:
2169:
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2137:
2127:
2126:
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2110:
2098:Diffuse nebula
2095:
2089:
2087:
2086:Visible nebula
2083:
2082:
2075:
2074:
2067:
2060:
2052:
2046:
2045:
2039:
2034:
2026:
2025:External links
2023:
2020:
2019:
1993:
1988:10.1086/426469
1974:(2): 948–960.
1951:
1944:
1926:
1919:
1878:
1853:
1847:978-1461447498
1846:
1828:
1817:
1792:
1786:10.1086/142713
1751:
1724:
1692:
1664:
1644:
1617:(3): 305–320.
1596:
1575:
1544:
1538:10.1086/123101
1503:
1471:
1464:
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1402:
1376:
1369:
1349:
1344:Universe Today
1330:
1315:
1300:
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1242:
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1235:
1230:
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1223:Messier object
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1210:
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1200:
1195:
1190:
1183:
1180:
1179:
1178:
1173:
1168:
1167:(dark nebulae)
1162:
1157:
1152:
1147:
1141:
1135:
1127:
1124:
1122:
1121:
1116:
1114:Rosette Nebula
1111:
1106:
1101:
1099:Pelican Nebula
1096:
1091:
1086:
1081:
1076:
1071:
1069:Fox Fur Nebula
1066:
1061:
1056:
1051:
1046:
1041:
1036:
1034:Barnard's Loop
1031:
1025:
1023:
1020:
996:diffuse nebula
987:nuclear fusion
963:
960:
953:
950:
903:
895:
890:Main article:
887:
884:
872:star formation
857:Camelopardalis
837:Main article:
834:
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728:
723:Main article:
720:
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618:SNR B0509-67.5
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445:Rosette Nebula
385:
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199:constellations
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15:
9:
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2564:Space plasmas
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1465:0-521-37079-5
1461:
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1422:
1421:
1420:ESO Messenger
1413:
1406:
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1370:9780521361552
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1138:RCW Catalogue
1136:
1133:
1130:
1129:
1120:
1117:
1115:
1112:
1110:
1107:
1105:
1102:
1100:
1097:
1095:
1092:
1090:
1089:Lagoon Nebula
1087:
1085:
1082:
1080:
1077:
1075:
1072:
1070:
1067:
1065:
1064:Carina Nebula
1062:
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1059:Eskimo Nebula
1057:
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912:
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893:
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879:
877:
873:
869:
865:
858:
854:
850:
849:Oyster Nebula
845:
840:
830:
828:
824:
819:
817:
811:
809:
805:
801:
797:
796:spectral line
792:
790:
786:
782:
773:
760:
758:
755:
751:
745:
740:
733:
726:
716:
714:
707:
704:
701:
698:
696:
693:
690:
687:
686:
685:
683:
682:star clusters
679:
666:
662:
656:
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647:
641:
636:
633:
627:
622:
619:
612:
607:
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583:
579:
572:
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552:
547:
544:
540:
533:
528:
524:
520:
517:
511:
506:
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499:
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493:
490:it emits can
489:
485:
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476:
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457:
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390:
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379:
375:
370:
365:
363:
359:
354:
352:
349:
345:
341:
340:Vesto Slipher
337:
333:
329:
324:
321:
317:
313:
308:
306:
302:
298:
294:
290:
286:
282:
281:Edmond Halley
277:
275:
271:
267:
263:
258:
256:
252:
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244:
240:
236:
232:
228:
227:
222:
219:
215:
211:
207:
203:
200:
196:
195:
190:
183:
182:Carina Nebula
178:
169:
167:
163:
162:Vesto Slipher
159:
155:
151:
147:
143:
139:
134:
132:
128:
124:
120:
116:
112:
108:
104:
100:
95:
93:
89:
85:
81:
77:
73:
69:
65:
61:
57:
53:
45:
41:
33:
32:Trifid Nebula
28:
22:
2538:
2526:from Commons
2521:
2500:
2493:Solar System
2193:Nova remnant
2177:Solar nebula
2118:Nova remnant
2078:
2006:
2002:
1996:
1971:
1967:
1954:
1935:
1929:
1908:
1870:. Retrieved
1866:the original
1856:
1837:
1831:
1820:
1808:. Retrieved
1804:
1795:
1768:
1764:
1754:
1737:
1733:
1727:
1710:
1706:
1684:. Retrieved
1674:
1667:
1653:
1647:
1614:
1608:
1590:
1584:
1578:
1564:(119): 145.
1561:
1557:
1547:
1523:(195): 225.
1520:
1516:
1506:
1492:(1): 70–73.
1489:
1483:
1455:
1436:, retrieved
1424:
1418:
1405:
1393:. Retrieved
1388:
1379:
1359:
1352:
1343:
1333:
1322:
1318:
1307:
1303:
1292:
1288:
1277:
1273:
1262:
1252:
1094:Orion Nebula
1074:Helix Nebula
1054:Eagle Nebula
994:, a special
980:
880:
876:H II regions
861:
820:
816:dark nebulae
812:
808:H II regions
793:
789:dark nebulae
778:
748:
719:Flux Nebulae
710:
706:Dark nebulae
689:H II regions
675:
539:Omega Nebula
477:
473:neutron star
453:
449:Omega Nebula
441:Orion Nebula
416:
401:
369:Edwin Hubble
367:Slipher and
366:
358:Great Debate
355:
351:open cluster
325:
319:
309:
278:
266:Orion Nebula
259:
224:
214:star cluster
192:
186:
166:Edwin Hubble
153:
140:, including
135:
111:Orion Nebula
96:
80:Eagle Nebula
59:
55:
51:
39:
37:
2481:Outer space
2469:Spaceflight
2167:Bok globule
2123:H II region
2093:Dark nebula
1810:16 December
1771:: 400–438.
1193:H II region
1132:Gum catalog
1109:Ring Nebula
1049:Crab Nebula
972:Crab Nebula
868:white dwarf
661:Ring Nebula
562:dark nebula
516:Herbig–Haro
496:white dwarf
461:Crab Nebula
433:H II region
429:wavelengths
247:Crab Nebula
144:beyond the
99:light-years
72:cosmic dust
2553:Categories
2417:Wiktionary
2288:Morphology
2279:H I region
2241:Supershell
1872:2007-06-12
1686:2009-10-31
1438:2009-10-31
1244:References
1188:H I region
1029:Ant Nebula
484:red giants
202:Ursa Major
94:objects.
90:and other
2445:Astronomy
2349:Planetary
1740:: 26–27.
1639:161558679
1593:: 390–92.
1427:: 42–43,
1012:electrons
983:supernova
930:evolution
928:'s rapid
754:Milky Way
456:supernova
384:Formation
362:Milky Way
279:In 1715,
260:In 1610,
257:in 1054.
243:supernova
146:Milky Way
127:kilograms
103:human eye
70:and also
2397:Category
1713:: 9–22.
1395:June 27,
1259:"nebula"
1182:See also
1126:Catalogs
1022:Examples
954:☉
942:infrared
823:infrared
804:hydrogen
678:galaxies
447:and the
348:Pleiades
318:. Their
194:Almagest
142:galaxies
68:hydrogen
2559:Nebulae
2431:Portals
2407:Commons
2371:Related
2339:Diffuse
2079:Nebulae
2031:Nebulae
2011:Bibcode
1976:Bibcode
1773:Bibcode
1742:Bibcode
1715:Bibcode
1619:Bibcode
1566:Bibcode
1525:Bibcode
1494:Bibcode
1429:Bibcode
814:called
800:ionized
744:Polaris
469:SN 1054
425:ionizes
393:NGC 604
251:SN 1054
223:in his
189:Ptolemy
131:T Tauri
88:planets
78:in the
60:nebulas
52:nebulae
2501:Nebula
2363:(SNRs)
2357:(PPNe)
2250:Clouds
1942:
1917:
1844:
1637:
1462:
1367:
757:galaxy
523:HH 164
519:HH 161
492:ionize
465:Taurus
443:, the
344:Merope
305:comets
241:. The
148:. The
119:vacuum
56:nebulæ
40:nebula
2540:Texts
2523:Media
2457:Stars
2351:(PNe)
2331:Lists
1964:(PDF)
1635:S2CID
1591:XXXIX
1415:(PDF)
1004:radio
1000:X-ray
851:is a
502:Types
463:, in
334:of a
156:(and
123:Earth
107:Earth
105:from
84:stars
58:, or
44:Latin
1940:ISBN
1915:ISBN
1842:ISBN
1812:2013
1460:ISBN
1397:2021
1365:ISBN
970:The
926:star
909:The
847:The
827:dust
787:and
665:Lyra
596:The
576:The
556:The
537:The
521:and
210:star
204:and
115:Moon
1984:doi
1972:620
1781:doi
1682:–85
1659:457
1627:doi
1533:doi
336:gas
206:Leo
48:pl.
2555::
2009:,
2007:37
2005:,
1982:.
1970:.
1966:.
1881:^
1803:.
1779:.
1769:56
1767:.
1763:.
1736:.
1711:45
1709:.
1695:^
1680:84
1633:.
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