Orion Nebula - Wikipedia Orion Nebula Orion Nebula Diffuse nebula The entire Orion Nebula in a composite image of visible light and infrared Observation data : J2000 epoch Subtype Reflection / Emission Right ascension 05 35 17.3 Declination − 05 ° 23 ′ 28 '' Distance 1,344 ± 20 ly ( 412 pc ) Apparent magnitude ( V ) + 4.0 Apparent dimensions ( V ) 65 × 60 arcmins Constellation Orion Physical characteristics Radius 12 ly Absolute magnitude ( V ) -- Notable features Trapezium cluster Designations NGC 1976, M42, LBN 974, Sharpless 281 See also : Lists of nebulae The Orion Nebula ( also known as Messier 42, M42, or NGC 1976 ) is a diffuse nebula situated in the Milky Way, being south of Orion 's Belt in the constellation of Orion. It is one of the brightest nebulae, and is visible to the naked eye in the night sky. M42 is located at a distance of 1,344 ± 20 light years and is the closest region of massive star formation to Earth. The M42 nebula is estimated to be 24 light years across. It has a mass of about 2,000 times that of the Sun. Older texts frequently refer to the Orion Nebula as the Great Nebula in Orion or the Great Orion Nebula. The Orion Nebula is one of the most scrutinized and photographed objects in the night sky, and is among the most intensely studied celestial features. The nebula has revealed much about the process of how stars and planetary systems are formed from collapsing clouds of gas and dust. Astronomers have directly observed protoplanetary disks, brown dwarfs, intense and turbulent motions of the gas, and the photo - ionizing effects of massive nearby stars in the nebula. Contents 1 Physical characteristics 1.1 Coloration 2 History 3 Structure 4 Star formation 4.1 Stellar wind and effects 5 Evolution 6 Image gallery 7 See also 8 Notes 9 References 10 External links Physical characteristics Play media Discussing the location of the Orion Nebula, what is seen within the star - formation region, and the effects of interstellar winds in shaping the nebula Amateur image of the Orion Nebula taken with a Sony Alpha a6300 camera Orion Nebula and the Running man Nebula with surrounding nebulosity. Composite of narrowband ( SII + Ha + OIII ) and RGB with a 80mm telescope. The constellation of Orion with the Orion Nebula ( lower middle ) The nebula is visible with the naked eye even from areas affected by some light pollution. It is seen as the middle `` star '' in the `` sword '' of Orion, which are the three stars located south of Orion 's Belt. The star appears fuzzy to sharp - eyed observers, and the nebulosity is obvious through binoculars or a small telescope. The peak surface brightness of the central region is about 17 Mag / arcsec ( about 14 milli nits ) and the outer bluish glow has a peak surface brightness of 21.3 Mag / arcsec ( about 0.27 millinits ). ( In the photos shown here the brightness, or luminance, is enhanced by a large factor. ) The Orion Nebula contains a very young open cluster, known as the Trapezium due to the asterism of its primary four stars. Two of these can be resolved into their component binary systems on nights with good seeing, giving a total of six stars. The stars of the Trapezium, along with many other stars, are still in their early years. The Trapezium is a component of the much larger Orion Nebula Cluster, an association of about 2,800 stars within a diameter of 20 light years. Two million years ago this cluster may have been the home of the runaway stars AE Aurigae, 53 Arietis, and Mu Columbae, which are currently moving away from the nebula at velocities greater than 100 km / s. Coloration Observers have long noted a distinctive greenish tint to the nebula, in addition to regions of red and of blue - violet. The red hue is a result of the Hα recombination line radiation at a wavelength of 656.3 nm. The blue - violet coloration is the reflected radiation from the massive O - class stars at the core of the nebula. The green hue was a puzzle for astronomers in the early part of the 20th century because none of the known spectral lines at that time could explain it. There was some speculation that the lines were caused by a new element, and the name nebulium was coined for this mysterious material. With better understanding of atomic physics, however, it was later determined that the green spectrum was caused by a low - probability electron transition in doubly ionized oxygen, a so - called `` forbidden transition ''. This radiation was all but impossible to reproduce in the laboratory at the time, because it depended on the quiescent and nearly collision - free environment found in the high vacuum of deep space. History Messier 's drawing of the Orion Nebula in his 1771 memoir, Mémoires de l'Académie Royale There has been speculation that the Mayans of Central America may have described the nebula within their `` Three Hearthstones '' creation myth ; if so, the three would correspond to two stars at the base of Orion, Rigel and Saiph, and another, Alnitak at the tip of the `` belt '' of the imagined hunter, the vertices of a nearly perfect equilateral triangle with Orion 's Sword ( including the Orion Nebula ) in the middle of the triangle seen as the smudge of smoke from copal incense in a modern myth, or, in ( the translation it suggests of ) an ancient one, the literal or figurative embers of a fiery creation. Neither Ptolemy 's Almagest nor Al Sufi 's Book of Fixed Stars noted this nebula, even though they both listed patches of nebulosity elsewhere in the night sky ; nor did Galileo mention it, even though he also made telescopic observations surrounding it in 1610 and 1617. This has led to some speculation that a flare - up of the illuminating stars may have increased the brightness of the nebula. The first discovery of the diffuse nebulous nature of the Orion Nebula is generally credited to French astronomer Nicolas - Claude Fabri de Peiresc, on 26 November 1610 when he made a record of observing it with a refracting telescope purchased by his patron Guillaume du Vair. The first published observation of the nebula was by the Jesuit mathematician and astronomer Johann Baptist Cysat of Lucerne in his 1619 monograph on the comets ( describing observations of the nebula that may date back to 1611 ). He made comparisons between it and a bright comet seen in 1618 and described how the nebula appeared through his telescope as : `` one sees how in like manner some stars are compressed into a very narrow space and how round about and between the stars a white light like that of a white cloud is poured out '' His description of the center stars as different from a comet 's head in that they were a `` rectangle '' may have been an early description of the Trapezium Cluster ( The first detection of three of the four stars of this cluster is credited to Galileo Galilei in a February 4, 1617 although he did not notice the surrounding nebula -- possibly due to the narrow field of vision of his early telescope. ) The nebula was independently discovered by several other prominent astronomers in the following years, including by Giovanni Battista Hodierna ( whose sketch was the first published in De systemate orbis cometici, deque admirandis coeli characteribus ). Charles Messier first noted the nebula on March 4, 1769, and he also noted three of the stars in Trapezium. Messier published the first edition of his catalog of deep sky objects in 1774 ( completed in 1771 ). As the Orion Nebula was the 42nd object in his list, it became identified as M42. Henry Draper 's 1880 photograph of the Orion Nebula, the first ever taken. One of Andrew Ainslie Common 's 1883 photograph of the Orion Nebula, the first to show that a long exposure could record new stars and nebulae invisible to the human eye. In 1865 English amateur astronomer William Huggins used his visual spectroscopy method to examine the nebula showing it, like other nebulae he had examined, was made up of `` luminous gas ''. On September 30, 1880 Henry Draper used the new dry plate photographic process with an 11 - inch ( 28 cm ) refracting telescope to make a 51 - minute exposure of the Orion Nebula, the first instance of astrophotography of a nebula in history. Another set of photographs of the nebula in 1883 saw breakthrough in astronomical photography when amateur astronomer Andrew Ainslie Common used the dry plate process to record several images in exposures up to 60 minutes with a 36 - inch ( 91 cm ) reflecting telescope that he constructed in the backyard of his home in Ealing, outside London. These images for the first time showed stars and nebula detail too faint to be seen by the human eye. In 1902, Vogel and Eberhard discovered differing velocities within the nebula and by 1914 astronomers at Marseilles had used the interferometer to detect rotation and irregular motions. Campbell and Moore confirmed these results using the spectrograph, demonstrating turbulence within the nebula. In 1931, Robert J. Trumpler noted that the fainter stars near the Trapezium formed a cluster, and he was the first to name them the Trapezium cluster. Based on their magnitudes and spectral types, he derived a distance estimate of 1,800 light years. This was three times farther than the commonly accepted distance estimate of the period but was much closer to the modern value. In 1993, the Hubble Space Telescope first observed the Orion Nebula. Since then, the nebula has been a frequent target for HST studies. The images have been used to build a detailed model of the nebula in three dimensions. Protoplanetary disks have been observed around most of the newly formed stars in the nebula, and the destructive effects of high levels of ultraviolet energy from the most massive stars have been studied. In 2005, the Advanced Camera for Surveys instrument of the Hubble Space Telescope finished capturing the most detailed image of the nebula yet taken. The image was taken through 104 orbits of the telescope, capturing over 3,000 stars down to the 23rd magnitude, including infant brown dwarfs and possible brown dwarf binary stars. A year later, scientists working with the HST announced the first ever masses of a pair of eclipsing binary brown dwarfs, 2MASS J05352184 -- 0546085. The pair are located in the Orion Nebula and have approximate masses of 0.054 M and 0.034 M respectively, with an orbital period of 9.8 days. Surprisingly, the more massive of the two also turned out to be the less luminous. Structure Optical images reveal clouds of gas and dust in the Orion Nebula ; an infrared image ( right ) reveals the new stars shining within. The entirety of the Orion Nebula extends across a 1 ° region of the sky, and includes neutral clouds of gas and dust, associations of stars, ionized volumes of gas, and reflection nebulae. The Nebula is part of a much larger nebula that is known as the Orion Molecular Cloud Complex. The Orion Molecular Cloud Complex extends throughout the constellation of Orion and includes Barnard 's Loop, the Horsehead Nebula, M43, M78, and the Flame Nebula. Stars are forming throughout the entire Cloud Complex, but most of the young stars are concentrated in dense clusters like the one illuminating the Orion Nebula. Orion A molecular cloud from VISTA reveals many young stars and other objects. The current astronomical model for the nebula consists of an ionized ( H II ) region, roughly centered on Theta Orionis C, which lies on the side of an elongated molecular cloud in a cavity formed by the massive young stars. ( Theta Orionis C emits 3 - 4 times as much photoionizing light as the next brightest star, Theta Orionis A. ) The H II region has a temperature ranging up to 10,000 K, but this temperature falls dramatically near the edge of the nebula. The nebulous emission comes primarily from photoionized gas on the back surface of the cavity. The H II region is surrounded by an irregular, concave bay of more neutral, high - density cloud, with clumps of neutral gas lying outside the bay area. This in turn lies on the perimeter of the Orion Molecular Cloud. The gas in the molecular cloud displays a range of velocities and turbulence, particularly around the core region. Relative movements are up to 10 km / s ( 22,000 mi / h ), with local variations of up to 50 km / s and possibly more. Observers have given names to various features in the Orion Nebula. The dark lane that extends from the north toward the bright region is called the `` Fish 's Mouth ''. The illuminated regions to both sides are called the `` Wings ''. Other features include `` The Sword '', `` The Thrust '', and `` The Sail ''. Star formation View of several proplyds within the Orion Nebula taken by the Hubble Space Telescope Star Formation Fireworks in Orion The Orion Nebula is an example of a stellar nursery where new stars are being born. Observations of the nebula have revealed approximately 700 stars in various stages of formation within the nebula. Recent observations with the Hubble Space Telescope have yielded the major discovery of protoplanetary disks within the Orion Nebula, which have been dubbed proplyds. HST has revealed more than 150 of these within the nebula, and they are considered to be systems in the earliest stages of solar system formation. The sheer numbers of them have been used as evidence that the formation of star systems is fairly common in the universe. Stars form when clumps of hydrogen and other gases in an H II region contract under their own gravity. As the gas collapses, the central clump grows stronger and the gas heats to extreme temperatures by converting gravitational potential energy to thermal energy. If the temperature gets high enough, nuclear fusion will ignite and form a protostar. The protostar is ' born ' when it begins to emit enough radiative energy to balance out its gravity and halt gravitational collapse. Typically, a cloud of material remains a substantial distance from the star before the fusion reaction ignites. This remnant cloud is the protostar 's protoplanetary disk, where planets may form. Recent infrared observations show that dust grains in these protoplanetary disks are growing, beginning on the path towards forming planetesimals. Once the protostar enters into its main sequence phase, it is classified as a star. Even though most planetary disks can form planets, observations show that intense stellar radiation should have destroyed any proplyds that formed near the Trapezium group, if the group is as old as the low mass stars in the cluster. Since proplyds are found very close to the Trapezium group, it can be argued that those stars are much younger than the rest of the cluster members. Stellar wind and effects Once formed, the stars within the nebula emit a stream of charged particles known as a stellar wind. Massive stars and young stars have much stronger stellar winds than the Sun. The wind forms shock waves or hydrodynamical instabilities when it encounters the gas in the nebula, which then shapes the gas clouds. The shock waves from stellar wind also play a large part in stellar formation by compacting the gas clouds, creating density inhomogeneities that lead to gravitational collapse of the cloud. View of the ripples ( Kelvin -- Helmholtz instability ) formed by the action of stellar winds on the cloud. There are three different kinds of shocks in the Orion Nebula. Many are featured in Herbig -- Haro objects : Bow shocks are stationary and are formed when two particle streams collide with each other. They are present near the hottest stars in the nebula where the stellar wind speed is estimated to be thousands of kilometers per second and in the outer parts of the nebula where the speeds are tens of kilometers per second. Bow shocks can also form at the front end of stellar jets when the jet hits interstellar particles. Jet - driven shocks are formed from jets of material sprouting off newborn T Tauri stars. These narrow streams are traveling at hundreds of kilometers per second, and become shocks when they encounter relatively stationary gases. Warped shocks appear bow - like to an observer. They are produced when a jet - driven shock encounters gas moving in a cross-current. The interaction of the stellar wind with the surrounding cloud also forms `` waves '' which are believed to be due to the hydrodynamical Kelvin - Helmholtz instability. The dynamic gas motions in M42 are complex, but are trending out through the opening in the bay and toward the Earth. The large neutral area behind the ionized region is currently contracting under its own gravity. There are also supersonic `` bullets '' of gas piercing the hydrogen clouds of the Orion Nebula. Each bullet is ten times the diameter of Pluto 's orbit and tipped with iron atoms glowing in the infra - red. They were probably formed one thousand years ago from an unknown violent event. Evolution Panoramic image of the center of the nebula, taken by the Hubble Telescope. This view is about 2.5 light years across. The Trapezium is at center left. Interstellar clouds like the Orion Nebula are found throughout galaxies such as the Milky Way. They begin as gravitationally bound blobs of cold, neutral hydrogen, intermixed with traces of other elements. The cloud can contain hundreds of thousands of solar masses and extend for hundreds of light years. The tiny force of gravity that could compel the cloud to collapse is counterbalanced by the very faint pressure of the gas in the cloud. Whether due to collisions with a spiral arm, or through the shock wave emitted from supernovae, the atoms are precipitated into heavier molecules and the result is a molecular cloud. This presages the formation of stars within the cloud, usually thought to be within a period of 10 -- 30 million years, as regions pass the Jeans mass and the destabilized volumes collapse into disks. The disk concentrates at the core to form a star, which may be surrounded by a protoplanetary disk. This is the current stage of evolution of the nebula, with additional stars still forming from the collapsing molecular cloud. The youngest and brightest stars we now see in the Orion Nebula are thought to be less than 300,000 years old, and the brightest may be only 10,000 years in age. Some of these collapsing stars can be particularly massive, and can emit large quantities of ionizing ultraviolet radiation. An example of this is seen with the Trapezium cluster. Over time the ultraviolet light from the massive stars at the center of the nebula will push away the surrounding gas and dust in a process called photo evaporation. This process is responsible for creating the interior cavity of the nebula, allowing the stars at the core to be viewed from Earth. The largest of these stars have short life spans and will evolve to become supernovae. Within about 100,000 years, most of the gas and dust will be ejected. The remains will form a young open cluster, a cluster of bright, young stars surrounded by wispy filaments from the former cloud. Image gallery Web of filaments in the Orion Nebula. Orion over ALMA. An APEX view of star formation in the Orion Nebula. Orion Nebula was captured using the Wide Field Imager camera on the MPG / ESO 2.2 - metre telescope. RGB image of the Orion Nebula ( M42 ) and Running Man Nebula ( Sh2 - 279 ) taken with a 5 '' apochromatic refractor and a DSLR. Orion Nebula Complex including M42, M43, Running Man Nebula ( NGC 1973, 1975, and 1977 ) and much of the surrounding nebulosity. Panoramic image of the Orion Nebula, taken by Ioannidis Panos with an 8 Inch Newtonian telescope and a Nikon D70 camera. Infant stars, image from NASA 's Spitzer Space Telescope. The Orion Nebula imaged with the 2.2 m ESO / MPG telescope. The central part of the Orion Nebula. This wide - field view of the Orion Nebula ( Messier 42 ), was taken with the VISTA infrared survey telescope at ESO 's Paranal Observatory in Chile. Orion by Spitzer. The Orion Nebula 's biggest stars. An infrared image showing fledgling stars located in the Orion Nebula. Core detail of the nebula with all the stars identified. A shot of the core details of the Orion Nebula. H - alpha image of the nebula with amateur telescope. X-rays produced by the young Orion stars penetrate the gas and dust clouds, producing this image as seen by the Chandra X-ray Observatory Orion Nebula, photographed with amateur equipment See also Barnard 's Loop Flame Nebula ( NGC 2024 ) Horsehead Nebula Hubble 3D ( 2010 ), an IMAX film with an elaborate CGI fly - through of the Orion Nebula List of diffuse nebulae List of Messier objects M43, which is part of the Orion Nebula M78, a reflection nebula New General Catalogue Orion correlation theory Orion Molecular Cloud Complex Orion Nebula in fiction Orion OB1 Association Notes 1,270 × tan ( 66 ′ / 2 ) = 12 ly. radius From temperate zones in the Northern Hemisphere, the nebula appears below the Belt of Orion ; from temperate zones in the Southern Hemisphere the nebula appears above the Belt. C. Robert O'Dell commented about this Wikipedia article, `` The only egregious error is the last sentence in the Stellar Formation section. 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External links Wikimedia Commons has media related to Orion Nebula. Wikisource has original text related to this article : The Great Nebula in Orion Wikisource has original text related to this article : Telescopic Research on the Nebula of Orion `` Animated tour of the Orion Nebula '', University of South Wales Orion Nebula observed by Chandra / HST Orion Nebula observed by Gemini Observatory Orion Nebula at ESA / Hubble Messier 42, SEDS Messier pages and specifically NGC 1976. January 2006 Hubble Space Telescope image of the Orion Nebula January 2006 Hubble Space Telescope image of the Trapezium cluster Orion Nebula M42, Hubble Images Remarkable new views captured of Orion Nebula, SpaceFlight Now, 2001. NightSkyInfo.com -- The Great Orion Nebula Astronomy Picture of the Day Spitzer 's Orion 2010 April 10 Planetary Systems Now Forming in Orion 2009 December 22 Great Orion Nebulae 2008 October 23 Gray, Meghan ; et al. `` M42 -- Orion Nebula ''. Deep Sky Videos. Brady Haran. The Orion Nebula on WikiSky : DSS2, SDSS, GALEX, IRAS, Hydrogen α, X-Ray, Astrophoto, Sky Map, Articles and images ESO : Hidden Secrets of Orion 's Clouds incl. Photos & Animations Messier objects List M1 M2 M3 M4 M5 M6 M7 M8 M9 M10 M11 M12 M13 M14 M15 M16 M17 M18 M19 M20 M21 M22 M23 M24 M25 M26 M27 M28 M29 M30 M31 M32 M33 M34 M35 M36 M37 M38 M39 M40 M41 M42 M43 M44 M45 M46 M47 M48 M49 M50 M51 M52 M53 M54 M55 M56 M57 M58 M59 M60 M61 M62 M63 M64 M65 M66 M67 M68 M69 M70 M71 M72 M73 M74 M75 M76 M77 M78 M79 M80 M81 M82 M83 M84 M85 M86 M87 M88 M89 M90 M91 M92 M93 M94 M95 M96 M97 M98 M99 M100 M101 M102 M103 M104 M105 M106 M107 M108 M109 M110 See also Caldwell catalogue Catalogue of Nebulae and Clusters of Stars Herschel 400 Catalogue Index Catalogue New General Catalogue Revised New General Catalogue Book Commons Portal Sharpless catalog Sh2 - 1 Sh2 - 2 Sh2 - 3 Sh2 - 4 Sh2 - 5 Sh2 - 6 Sh2 - 7 Sh2 - 8 Sh2 - 9 Sh2 - 10 Sh2 - 11 Sh2 - 12 Sh2 - 13 Sh2 - 14 Sh2 - 15 Sh2 - 16 Sh2 - 17 Sh2 - 18 Sh2 - 19 Sh2 - 20 Sh2 - 21 Sh2 - 22 Sh2 - 23 Sh2 - 24 Sh2 - 25 Sh2 - 26 Sh2 - 27 Sh2 - 28 Sh2 - 29 Sh2 - 30 Sh2 - 31 Sh2 - 32 Sh2 - 33 Sh2 - 34 Sh2 - 35 Sh2 - 36 Sh2 - 37 Sh2 - 38 Sh2 - 39 Sh2 - 40 Sh2 - 41 Sh2 - 42 Sh2 - 43 Sh2 - 44 Sh2 - 45 Sh2 - 46 Sh2 - 47 Sh2 - 48 Sh2 - 49 Sh2 - 50 Sh2 - 51 Sh2 - 52 Sh2 - 53 Sh2 - 54 Sh2 - 55 Sh2 - 56 Sh2 - 57 Sh2 - 58 Sh2 - 59 Sh2 - 60 Sh2 - 61 Sh2 - 62 Sh2 - 63 Sh2 - 64 Sh2 - 65 Sh2 - 66 Sh2 - 67 Sh2 - 68 Sh2 - 69 Sh2 - 70 Sh2 - 71 Sh2 - 72 Sh2 - 73 Sh2 - 74 Sh2 - 75 Sh2 - 76 Sh2 - 77 Sh2 - 78 Sh2 - 79 Sh2 - 80 Sh2 - 81 Sh2 - 82 Sh2 - 83 Sh2 - 84 Sh2 - 85 Sh2 - 86 Sh2 - 87 Sh2 - 88 Sh2 - 89 Sh2 - 90 Sh2 - 91 Sh2 - 92 Sh2 - 93 Sh2 - 94 Sh2 - 95 Sh2 - 96 Sh2 - 97 Sh2 - 98 Sh2 - 99 Sh2 - 100 Sh2 - 101 Sh2 - 102 Sh2 - 103 Sh2 - 104 Sh2 - 105 Sh2 - 106 Sh2 - 107 Sh2 - 108 Sh2 - 109 Sh2 - 110 Sh2 - 111 Sh2 - 112 Sh2 - 113 Sh2 - 114 Sh2 - 115 Sh2 - 116 Sh2 - 117 Sh2 - 118 Sh2 - 119 Sh2 - 120 Sh2 - 121 Sh2 - 122 Sh2 - 123 Sh2 - 124 Sh2 - 125 Sh2 - 126 Sh2 - 127 Sh2 - 128 Sh2 - 129 Sh2 - 130 Sh2 - 131 Sh2 - 132 Sh2 - 133 Sh2 - 134 Sh2 - 135 Sh2 - 136 Sh2 - 137 Sh2 - 138 Sh2 - 139 Sh2 - 140 Sh2 - 141 Sh2 - 142 Sh2 - 143 Sh2 - 144 Sh2 - 145 Sh2 - 146 Sh2 - 147 Sh2 - 148 Sh2 - 149 Sh2 - 150 Sh2 - 151 Sh2 - 152 Sh2 - 153 Sh2 - 154 Sh2 - 155 Sh2 - 156 Sh2 - 157 Sh2 - 158 Sh2 - 159 Sh2 - 160 Sh2 - 161 Sh2 - 162 Sh2 - 163 Sh2 - 164 Sh2 - 165 Sh2 - 166 Sh2 - 167 Sh2 - 168 Sh2 - 169 Sh2 - 170 Sh2 - 171 Sh2 - 172 Sh2 - 173 Sh2 - 174 Sh2 - 175 Sh2 - 176 Sh2 - 177 Sh2 - 178 Sh2 - 179 Sh2 - 180 Sh2 - 181 Sh2 - 182 Sh2 - 183 Sh2 - 184 Sh2 - 185 Sh2 - 186 Sh2 - 187 Sh2 - 188 Sh2 - 189 Sh2 - 190 Sh2 - 191 Sh2 - 192 Sh2 - 193 Sh2 - 194 Sh2 - 195 Sh2 - 196 Sh2 - 197 Sh2 - 198 Sh2 - 199 Sh2 - 201 Sh2 - 202 Sh2 - 203 Sh2 - 204 Sh2 - 205 Sh2 - 206 Sh2 - 207 Sh2 - 208 Sh2 - 209 Sh2 - 210 Sh2 - 211 Sh2 - 212 Sh2 - 213 Sh2 - 214 Sh2 - 215 Sh2 - 216 Sh2 - 217 Sh2 - 218 Sh2 - 219 Sh2 - 220 Sh2 - 221 Sh2 - 222 Sh2 - 223 Sh2 - 224 Sh2 - 225 Sh2 - 226 Sh2 - 227 Sh2 - 228 Sh2 - 229 Sh2 - 230 Sh2 - 231 Sh2 - 232 Sh2 - 233 Sh2 - 234 Sh2 - 235 Sh2 - 236 Sh2 - 237 Sh2 - 238 Sh2 - 239 Sh2 - 240 Sh2 - 241 Sh2 - 242 Sh2 - 243 Sh2 - 244 Sh2 - 245 Sh2 - 246 Sh2 - 247 Sh2 - 248 Sh2 - 249 Sh2 - 250 Sh2 - 251 Sh2 - 252 Sh2 - 253 Sh2 - 254 Sh2 - 255 Sh2 - 256 Sh2 - 257 Sh2 - 258 Sh2 - 259 Sh2 - 260 Sh2 - 261 Sh2 - 262 Sh2 - 263 Sh2 - 264 Sh2 - 265 Sh2 - 266 Sh2 - 267 Sh2 - 268 Sh2 - 269 Sh2 - 270 Sh2 - 271 Sh2 - 272 Sh2 - 273 Sh2 - 274 Sh2 - 275 Sh2 - 276 Sh2 - 277 Sh2 - 278 Sh2 - 279 Sh2 - 280 Sh2 - 281 Sh2 - 282 Sh2 - 283 Sh2 - 284 Sh2 - 285 Sh2 - 286 Sh2 - 287 Sh2 - 288 Sh2 - 289 Sh2 - 290 Sh2 - 291 Sh2 - 292 Sh2 - 293 Sh2 - 294 Sh2 - 295 Sh2 - 296 Sh2 - 297 Sh2 - 298 Sh2 - 299 Sh2 - 301 Sh2 - 302 Sh2 - 303 Sh2 - 304 Sh2 - 305 Sh2 - 306 Sh2 - 307 Sh2 - 308 Sh2 - 309 Sh2 - 310 Sh2 - 311 Sh2 - 312 Sh2 - 313 See also : Gum catalog Nebula RCW Catalogue Stewart Sharpless BNF : cb122613708 ( data ) GND : 4172839 - 7 LCCN : sh85095658 Coordinates : 05 35 17.3, − 05 ° 23 ′ 28 '' Retrieved from `` https://en.wikipedia.org/w/index.php?title=Orion_Nebula&oldid=837105385 '' Categories : Messier objects H II regions NGC objects Orion Molecular Cloud Complex Orion -- Cygnus Arm Diffuse nebulae Astronomical objects discovered in 1610 Astronomical objects known since antiquity Star - 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Question: where is the nebula in the orion located
Answer: south of Orion's Belt in the constellation of Orion