Crab Nebula - wikipedia Crab Nebula Crab Nebula Supernova remnant Hubble Space Telescope mosaic image assembled from 24 individual Wide Field and Planetary Camera 2 exposures taken in October 1999, January 2000, and December 2000 Observation data : J2000. 0 epoch Right ascension 05 34 31.94 Declination + 22 ° 00 ′ 52.2 '' Distance 7003650000000000000 ♠ 6500 ± 1600 ly ( 7003200000000000000 ♠ 2000 ± 500 pc ) Apparent magnitude ( V ) + 8.4 Apparent dimensions ( V ) 420 '' × 290 '' Constellation Taurus Physical characteristics Radius ~ 5.5 ly ( ~ 1.7 pc ) Absolute magnitude ( V ) 7000310000000000000 ♠ − 3.1 ± 0.5 Notable features Optical pulsar Designations Messier 1, NGC 1952, Taurus A, Sh 2 - 244 See also : Lists of nebulae The Crab Nebula ( catalogue designations M 1, NGC 1952, Taurus A ) is a supernova remnant in the constellation of Taurus. The now - current name is due to William Parsons, 3rd Earl of Rosse, who observed the object in 1840 using a 36 - inch telescope and produced a drawing that looked somewhat like a crab. Corresponding to a bright supernova recorded by Chinese astronomers in 1054, the nebula was observed later by English astronomer John Bevis in 1731. The nebula was the first astronomical object identified with a historical supernova explosion. At an apparent magnitude of 8.4, comparable to that of Saturn 's moon Titan, it is not visible to the naked eye but can be made out using binoculars under favourable conditions. The nebula lies in the Perseus Arm of the Milky Way galaxy, at a distance of about 2.0 kiloparsecs ( 6,500 ly ) from Earth. It has a diameter of 3.4 parsecs ( 11 ly ), corresponding to an apparent diameter of some 7 arcminutes, and is expanding at a rate of about 1,500 kilometres per second ( 930 mi / s ), or 0.5 % of the speed of light. At the center of the nebula lies the Crab Pulsar, a neutron star 28 -- 30 kilometres ( 17 -- 19 mi ) across with a spin rate of 30.2 times per second, which emits pulses of radiation from gamma rays to radio waves. At X-ray and gamma ray energies above 30 keV, the Crab Nebula is generally the brightest persistent source in the sky, with measured flux extending to above 10 TeV. The nebula 's radiation allows for the detailed studying of celestial bodies that occult it. In the 1950s and 1960s, the Sun 's corona was mapped from observations of the Crab Nebula 's radio waves passing through it, and in 2003, the thickness of the atmosphere of Saturn 's moon Titan was measured as it blocked out X-rays from the nebula. The inner part of the nebula is a much smaller pulsar wind nebula that appears as a shell surrounding the pulsar. Some sources consider the Crab Nebula to be an example of both a pulsar wind nebula as well as a supernova remnant, while others separate the two phenomena based on the different sources of energy production and behaviour. For the Crab Nebula, the divisions are superficial but remain meaningful to researchers and their lines of study. Contents 1 Observational history 1.1 First identification 1.2 Connection to SN 1054 1.3 Crab Pulsar 2 Physical conditions 2.1 Distance 2.2 Mass 2.3 Helium - rich torus 3 Central star 4 Progenitor star 5 Transits by Solar System bodies 5.1 Lunar 5.2 Solar 5.3 Other objects 6 Gallery 7 See also 8 Notes 9 References 10 External links Observational History HaRGB image of the Crab Nebula from the Liverpool Telescope, exposures totalling 1.4 hours. Further information : SN 1054 Modern understanding that the Crab Nebula was created by a supernova dates to 1921, when Carl Otto Lampland announced he had seen changes in its structure. This eventually led to the conclusion that the creation of the Crab Nebula corresponds to the bright SN 1054 supernova recorded by Chinese astronomers in AD 1054. There is also a 13th - century Japanese reference to this `` guest star '' in Meigetsuki. The event was long considered unrecorded in Islamic astronomy, but in 1978 a reference was found in a 13th - century copy made by Ibn Abi Usaibia of a work by Ibn Butlan, a Nestorian Christian physician active in Baghdad at the time of the supernova. First identification Reproduction of the first depiction of the nebula by Lord Rosse ( 1844 ) ( colour - inverted to appear white - on - black ) The Crab Nebula was first identified in 1731 by John Bevis. The nebula was independently rediscovered in 1758 by Charles Messier as he was observing a bright comet. Messier catalogued it as the first entry in his catalogue of comet - like objects ; in 1757, Alexis Clairaut reexamined the calculations of Edmund Halley and predicted the return of Halley 's Comet in late 1758. The exact time of the comet 's return required the consideration of perturbations to its orbit caused by planets in the Solar System such as Jupiter, which Clairaut and his two colleagues Jérôme Lalande and Nicole - Reine Lepaute carried out more precisely than Halley, finding that the comet should appear in the constellation of Taurus. It is in searching in vain for the comet that Charles Messier found the Crab nebula, which he at first thought to be Halley 's comet. After some observation, noticing that the object that he was observing was not moving across the sky, Messier concluded that the object was not a comet. Messier then realised the usefulness of compiling a catalogue of celestial objects of a cloudy nature, but fixed in the sky, to avoid incorrectly cataloguing them as comets. William Herschel observed the Crab Nebula numerous times between 1783 and 1809, but it is not known whether he was aware of its existence in 1783, or if he discovered it independently of Messier and Bevis. After several observations, he concluded that it was composed of a group of stars. The 3rd Earl of Rosse observed the nebula at Birr Castle in 1844 using a 36 - inch ( 0.9 m ) telescope, and referred to the object as the `` Crab Nebula '' because a drawing he made of it looked like a crab. He observed it again later, in 1848, using a 72 - inch ( 1.8 m ) telescope and could not confirm the supposed resemblance, but the name stuck nevertheless. Connection to SN 1054 The nebula is seen in the visible spectrum at 550 nm ( green light ). In 1913, when Vesto Slipher registered his spectroscopy study of the sky, the Crab Nebula was again one of the first objects to be studied. In the early twentieth century, the analysis of early photographs of the nebula taken several years apart revealed that it was expanding. Tracing the expansion back revealed that the nebula must have become visible on Earth about 900 years ago. Historical records revealed that a new star bright enough to be seen in the daytime had been recorded in the same part of the sky by Chinese astronomers in 1054. Changes in the cloud, suggesting its small extent, were discovered by Carl Lampland in 1921. That same year, John Charles Duncan demonstrated that the remnant is expanding, while Knut Lundmark noted its proximity to the guest star of 1054. In 1928, Edwin Hubble proposed associating the cloud to the star of 1054, an idea which remained controversial until the nature of supernovae was understood, and it was Nicholas Mayall who indicated that the star of 1054 was undoubtedly the supernova whose explosion produced the Crab Nebula. The search for historical supernovae started at that moment : seven other historical sightings have been found by comparing modern observations of supernova remnants with astronomical documents of past centuries. Given its great distance, the daytime `` guest star '' observed by the Chinese could only have been a supernova -- a massive, exploding star, having exhausted its supply of energy from nuclear fusion and collapsed in on itself. Recent analysis of historical records have found that the supernova that created the Crab Nebula probably appeared in April or early May, rising to its maximum brightness of between apparent magnitude − 7 and − 4.5 ( brighter than everything in the night sky except the Moon ) by July. The supernova was visible to the naked eye for about two years after its first observation. Thanks to the recorded observations of Far Eastern and Middle Eastern astronomers of 1054, Crab Nebula became the first astronomical object recognized as being connected to a supernova explosion. Crab pulsar Image combining optical data from Hubble ( in red ) and X-ray images from Chandra X-ray Observatory ( in blue ). In the 1960s, because of the prediction and discovery of pulsars, the Crab Nebula again became a major centre of interest. It was then that Franco Pacini predicted the existence of the Crab Pulsar for the first time, which would explain the brightness of the cloud. The star was observed shortly afterwards in 1968. The discovery of the Crab pulsar, and the knowledge of its exact age ( almost to the day ) allows for the verification of basic physical properties of these objects, such as characteristic age and spin - down luminosity, the orders of magnitude involved ( notably the strength of the magnetic field ), along with various aspects related to the dynamics of the remnant. The role of this supernova to the scientific understanding of supernova remnants was crucial, as no other historical supernova created a pulsar whose precise age we can know for certain. The only possible exception to this rule would be SN 1181 whose supposed remnant, 3C 58, is home to a pulsar, but its identification using Chinese observations from 1181 is sometimes contested. Physical conditions Hubble image of a small region of the Crab Nebula, showing Rayleigh -- Taylor instabilities in its intricate filamentary structure. In visible light, the Crab Nebula consists of a broadly oval - shaped mass of filaments, about 6 arcminutes long and 4 arcminutes wide ( by comparison, the full moon is 30 arcminutes across ) surrounding a diffuse blue central region. In three dimensions, the nebula is thought to be shaped like a prolate spheroid. The filaments are the remnants of the progenitor star 's atmosphere, and consist largely of ionised helium and hydrogen, along with carbon, oxygen, nitrogen, iron, neon and sulfur. The filaments ' temperatures are typically between 11,000 and 18,000 K, and their densities are about 1,300 particles per cm. In 1953 Iosif Shklovsky proposed that the diffuse blue region is predominantly produced by synchrotron radiation, which is radiation given off by the curving motion of electrons in a magnetic field. The radiation corresponded to electrons moving at speeds up to half the speed of light. Three years later the theory was confirmed by observations. In the 1960s it was found that the source of the curved paths of the electrons was the strong magnetic field produced by a neutron star at the centre of the nebula. Distance Even though the Crab Nebula is the focus of much attention among astronomers, its distance remains an open question, owing to uncertainties in every method used to estimate its distance. In 2008, the consensus was that its distance from Earth is 2.0 ± 0.5 kpc ( 6,500 ± 1,600 ly ). Along its longest visible dimension, it thus measures about 4.1 ± 1 pc ( 13 ± 3 ly ) across. The Crab Nebula currently is expanding outward at about 1,500 km / s ( 930 mi / s ). Images taken several years apart reveal the slow expansion of the nebula, and by comparing this angular expansion with its spectroscopically determined expansion velocity, the nebula 's distance can be estimated. In 1973, an analysis of many methods used to compute the distance to the nebula had reached a conclusion of about 1.9 kpc ( 6,300 ly ), consistent with the currently cited value. The Crab Pulsar itself was discovered in 1968. Tracing back its expansion ( assuming a constant decrease of expansion speed due to the nebula 's mass ) yielded a date for the creation of the nebula several decades after 1054, implying that its outward velocity has decelerated less than assumed since the supernova explosion. This reduced deceleration is believed to be caused by energy from the pulsar that feeds into the nebula 's magnetic field, which expands and forces the nebula 's filaments outward. Mass Estimates of the total mass of the nebula are important for estimating the mass of the supernova 's progenitor star. The amount of matter contained in the Crab Nebula 's filaments ( ejecta mass of ionized and neutral gas ; mostly helium ) is estimated to be 7030914732999999999 ♠ 4.6 ± 1.8 M. Helium - rich torus One of the many nebular components ( or anomalies ) of the Crab Nebula is a helium - rich torus which is visible as an east - west band crossing the pulsar region. The torus composes about 25 % of the visible ejecta. However, it is suggested by calculation that about 95 % of the torus is helium. As yet, there has been no plausible explanation put forth for the structure of the torus. Central star Main article : Crab Pulsar Slow - motion movie of the Crab Pulsar, taken with OES Single - Photon - Camera. Play media Data from orbiting observatories show unexpected variations in the Crab Nebula 's X-ray output, likely tied to the environment around its central neutron star. Play media NASA 's Fermi spots ' superflares ' in the Crab Nebula. At the center of the Crab Nebula are two faint stars, one of which is the star responsible for the existence of the nebula. It was identified as such in 1942, when Rudolf Minkowski found that its optical spectrum was extremely unusual. The region around the star was found to be a strong source of radio waves in 1949 and X-rays in 1963, and was identified as one of the brightest objects in the sky in gamma rays in 1967. Then, in 1968, the star was found to be emitting its radiation in rapid pulses, becoming one of the first pulsars to be discovered. Pulsars are sources of powerful electromagnetic radiation, emitted in short and extremely regular pulses many times a second. They were a great mystery when discovered in 1967, and the team who identified the first one considered the possibility that it could be a signal from an advanced civilization. However, the discovery of a pulsating radio source in the centre of the Crab Nebula was strong evidence that pulsars were formed by supernova explosions. They now are understood to be rapidly rotating neutron stars, whose powerful magnetic field concentrates their radiation emissions into narrow beams. The Crab Pulsar is believed to be about 28 -- 30 km ( 17 -- 19 mi ) in diameter ; it emits pulses of radiation every 33 milliseconds. Pulses are emitted at wavelengths across the electromagnetic spectrum, from radio waves to X-rays. Like all isolated pulsars, its period is slowing very gradually. Occasionally, its rotational period shows sharp changes, known as ' glitches ', which are believed to be caused by a sudden realignment inside the neutron star. The energy released as the pulsar slows down is enormous, and it powers the emission of the synchrotron radiation of the Crab Nebula, which has a total luminosity about 75,000 times greater than that of the Sun. The pulsar 's extreme energy output creates an unusually dynamic region at the centre of the Crab Nebula. While most astronomical objects evolve so slowly that changes are visible only over timescales of many years, the inner parts of the Crab Nebula show changes over timescales of only a few days. The most dynamic feature in the inner part of the nebula is the point where the pulsar 's equatorial wind slams into the bulk of the nebula, forming a shock front. The shape and position of this feature shifts rapidly, with the equatorial wind appearing as a series of wisp - like features that steepen, brighten, then fade as they move away from the pulsar to well out into the main body of the nebula. Progenitor star This sequence of Hubble images shows features in the inner Crab Nebula changing over a period of four months. The star that exploded as a supernova is referred to as the supernova 's progenitor star. Two types of stars explode as supernovae : white dwarfs and massive stars. In the so - called Type Ia supernovae, gases falling onto a ' dead ' white dwarf raise its mass until it nears a critical level, the Chandrasekhar limit, resulting in a runaway nuclear fusion explosion that obliterates the star ; in Type Ib / c and Type II supernovae, the progenitor star is a massive star whose core runs out of fuel to power its nuclear fusion reactions and collapses in on itself, releasing gravitational potential energy in a form that blows away the star 's outer layers. The presence of a pulsar in the Crab Nebula means that it must have formed in a core - collapse supernova ; Type Ia supernovae do not produce pulsars. Theoretical models of supernova explosions suggest that the star that exploded to produce the Crab Nebula must have had a mass of between 9 and 11 M. Stars with masses lower than 8 M are thought to be too small to produce supernova explosions, and end their lives by producing a planetary nebula instead, while a star heavier than 12 M would have produced a nebula with a different chemical composition from that observed in the Crab Nebula. Recent studies, however, suggest the progenitor could have been a super-asymptotic giant branch star in the 8 to 10 M range that would have exploded in an electron - capture supernova. A significant problem in studies of the Crab Nebula is that the combined mass of the nebula and the pulsar add up to considerably less than the predicted mass of the progenitor star, and the question of where the ' missing mass ' is, remains unresolved. Estimates of the mass of the nebula are made by measuring the total amount of light emitted, and calculating the mass required, given the measured temperature and density of the nebula. Estimates range from about 1 -- 5 M, with 2 -- 3 M being the generally accepted value. The neutron star mass is estimated to be between 1.4 and 2 M. The predominant theory to account for the missing mass of the Crab Nebula is that a substantial proportion of the mass of the progenitor was carried away before the supernova explosion in a fast stellar wind, a phenomenon commonly seen in Wolf - Rayet stars. However, this would have created a shell around the nebula. Although attempts have been made at several wavelengths to observe a shell, none has yet been found. Transits by Solar System bodies Chandra image showing Saturn 's moon Titan transiting the nebula. The Crab Nebula lies roughly 1.5 degrees away from the ecliptic -- the plane of Earth 's orbit around the Sun. This means that the Moon -- and occasionally, planets -- can transit or occult the nebula. Although the Sun does not transit the nebula, its corona passes in front of it. These transits and occultations can be used to analyse both the nebula and the object passing in front of it, by observing how radiation from the nebula is altered by the transiting body. Lunar Lunar transits have been used to map X-ray emissions from the nebula. Before the launch of X-ray - observing satellites, such as the Chandra X-ray Observatory, X-ray observations generally had quite low angular resolution, but when the Moon passes in front of the nebula, its position is very accurately known, and so the variations in the nebula 's brightness can be used to create maps of X-ray emission. When X-rays were first observed from the Crab Nebula, a lunar occultation was used to determine the exact location of their source. Solar The Sun 's corona passes in front of the Crab Nebula every June. Variations in the radio waves received from the Crab Nebula at this time can be used to infer details about the corona 's density and structure. Early observations established that the corona extended out to much greater distances than had previously been thought ; later observations found that the corona contained substantial density variations. Other objects Very rarely, Saturn transits the Crab Nebula. Its transit in 2003 was the first since 1296 ; another will not occur until 2267. Observers used the Chandra X-ray Observatory to observe Saturn 's moon Titan as it crossed the nebula, and found that Titan 's X-ray ' shadow ' was larger than its solid surface, due to absorption of X-rays in its atmosphere. These observations showed that the thickness of Titan 's atmosphere is 880 km ( 550 mi ). The transit of Saturn itself could not be observed, because Chandra was passing through the Van Allen belts at the time. Gallery The Crab Nebula seen in radio, infrared, visible light, ultraviolet, X-rays, and gamma - rays ( 8 March 2015 ) The Crab Nebula -- five observatories ( 10 May 2017 ) The Crab Nebula -- five observatories ( animation ; 10 May 2017 ) See also Crab Nebula in fiction Lists of nebulae Notes Size as measured on a very deep plate taken by Sidney van den Bergh in late 1969. Apparent Magnitude of 8.4 -- distance modulus of 7001115000000000000 ♠ 11.5 ± 0.5 = 7000310000000000000 ♠ − 3.1 ± 0.5 distance × tan ( diameter_angle = 420 '' ) = 7000409999999999999 ♠ 4.1 ± 1.0 pc diameter = 7001130000000000000 ♠ 13 ± 3 light year diameter References ^ Jump up to : `` M 1 -- SuperNova Remnant ''. SIMBAD. Observatory of Strasbourg. Retrieved 12 February 2012. Jump up ^ Kaplan, David L. ; Chatterjee, S. ; Gaensler, B.M. ; Anderson, J. ( 2008 ). `` A Precise Proper Motion for the Crab Pulsar, and the Difficulty of Testing Spin - Kick Alignment for Young Neutron Stars ''. 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Bibcode : 2005EAS... 16... 115D. doi : 10.1051 / eas : 2005070. Jump up ^ LaViolette, Paul A. ( April 2006 ). Decoding the Message of the Pulsars : Intelligent Communication from the Galaxy. Bear & Co. p. 73. ISBN 978 - 1 - 59143 - 062 - 9. Jump up ^ LaViolette, Paul A. ( April 2006 ). Decoding the Message of the Pulsars : Intelligent Communication from the Galaxy. Bear & Co. p. 135. ISBN 978 - 1 - 59143 - 062 - 9. Jump up ^ Bejger, M. ; Haensel, P. ( 2002 ). `` Moments of inertia for neutron and strange stars : Limits derived for the Crab pulsar ''. Astronomy and Astrophysics. 396 ( 3 ) : 917 -- 921. arXiv : astro - ph / 0209151. Bibcode : 2002A&A... 396... 917B. doi : 10.1051 / 0004 - 6361 : 20021241. Jump up ^ Harnden, F.R. ; Seward, F.D. ( 1984 ). `` Einstein observations of the Crab nebula pulsar ''. The Astrophysical Journal. 283 : 279 -- 285. Bibcode : 1984ApJ... 283... 279H. doi : 10.1086 / 162304. Jump up ^ Kaufmann, W.J. ( 1996 ). Universe ( 4th ed. ). W.H. Freeman. p. 428. ISBN 0 - 7167 - 2379 - 4. ^ Jump up to : Hester, J. Jeff ; Scowen, P.A. ; Sankrit, R. ; Michel, F.C. ; et al. ( 1996 ). `` The Extremely Dynamic Structure of the Inner Crab Nebula ''. Bulletin of the American Astronomical Society. 28 ( 2 ) : 950. Bibcode : 1996BAAS... 28... 950H. Jump up ^ Maoz, Dan ( December 2011 ). Astrophysics in a Nutshell. Princeton University Press. p. 90. ISBN 1 - 4008 - 3934 - 3. Jump up ^ Pasachoff, Jay M. ; Filippenko, Alex ( August 2013 ). The Cosmos : Astronomy in the New Millennium. Cambridge University Press. p. 357. ISBN 978 - 1 - 107 - 27695 - 6. Jump up ^ Nomoto, K. ( 1985 ). `` Evolutionary models of the Crab Nebula 's progenitor ''. The Crab Nebula and related supernova remnants ; Proceedings of the Workshop. Cambridge University Press. pp. 97 -- 113. Bibcode : 1985cnrs. work... 97N. ^ Jump up to : Davidson, K. ; Fesen, R.A. ( 1985 ). `` Recent developments concerning the Crab Nebula ''. Annual Review of Astronomy and Astrophysics. 23 ( 507 ) : 119 -- 146. Bibcode : 1985ARA&A... 23... 119D. doi : 10.1146 / annurev. aa. 23.090185. 001003. Jump up ^ Tominaga, N. ; Blinnikov, S.I. ; Nomoto, Ken'Ichi ( 2013 ). `` Supernova explosions of super-asymptotic giant branch stars : multicolor light curves of electron - capture supernovae ''. The Astrophysical Journal Letters. 771 ( 1 ) : L12. arXiv : 1305.6813. Bibcode : 2013ApJ... 771L... 12T. doi : 10.1088 / 2041 - 8205 / 771 / 1 / L12. Jump up ^ Frail, D.A. ; Kassim, N.E. ; Cornwell, T.J. ; Goss, W.M. ( 1995 ). `` Does the Crab Have a Shell ? ''. The Astrophysical Journal Letters. 454 ( 2 ) : L129 -- L132. arXiv : astro - ph / 9509135. Bibcode : 1995ApJ... 454L. 129F. doi : 10.1086 / 309794. Jump up ^ Palmieri, T.M. ; Seward, F.D. ; Toor, A. ; van Flandern, T.C. ( 1975 ). `` Spatial distribution of X-rays in the Crab Nebula ''. The Astrophysical Journal. 202 : 494 -- 497. Bibcode : 1975ApJ... 202... 494P. doi : 10.1086 / 153998. Jump up ^ Erickson, W.C. ( 1964 ). `` The Radio - Wave Scattering Properties of the Solar Corona ''. The Astrophysical Journal. 139 : 1290. Bibcode : 1964ApJ... 139.1290 E. doi : 10.1086 / 147865. Jump up ^ Mori, K. ; Tsunemi, H. ; Katayama, H. ; Burrows, D.N. ; Garmire, G.P. ; Metzger, A.E. ( 2004 ). `` An X-Ray Measurement of Titan 's Atmospheric Extent from Its Transit of the Crab Nebula ''. The Astrophysical Journal. 607 ( 2 ) : 1065 -- 1069. arXiv : astro - ph / 0403283. Bibcode : 2004ApJ... 607.1065 M. doi : 10.1086 / 383521. Chandra images used by Mori et al. can be viewed here. Jump up ^ van den Bergh, Sidney ( 1970 ). `` A Jetlike Structure Associated with the Crab Nebula ''. The Astrophysical Journal Letters. 160 : L27. Bibcode : 1970ApJ... 160L... 27V. doi : 10.1086 / 180516. External links Wikimedia Commons has media related to Crab Nebula. Crab Nebula on WikiSky : DSS2, SDSS, GALEX, IRAS, Hydrogen α, X-Ray, Astrophoto, Sky Map, Articles and images Crab Nebula in the University of Cambridge Catalogue of Galactic Supernova Remnants Crab Nebula in the SEDS Messier index Crab Nebula in the Chandra X-ray Observatory Field Guide series Crab Nebula images by the Hubble Space Telescope 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 New General Catalogue 1500 to 1999 NGC 1500 NGC 1501 NGC 1502 NGC 1503 NGC 1504 NGC 1505 NGC 1506 NGC 1507 NGC 1508 NGC 1509 NGC 1510 NGC 1511 NGC 1512 NGC 1513 NGC 1514 NGC 1515 NGC 1516 NGC 1517 NGC 1518 NGC 1519 NGC 1520 NGC 1521 NGC 1522 NGC 1523 NGC 1524 NGC 1525 NGC 1526 NGC 1527 NGC 1528 NGC 1529 NGC 1530 NGC 1531 NGC 1532 NGC 1533 NGC 1534 NGC 1535 NGC 1536 NGC 1537 NGC 1538 NGC 1539 NGC 1540 NGC 1541 NGC 1542 NGC 1543 NGC 1544 NGC 1545 NGC 1546 NGC 1547 NGC 1548 NGC 1549 NGC 1550 NGC 1551 NGC 1552 NGC 1553 NGC 1554 NGC 1555 NGC 1556 NGC 1557 NGC 1558 NGC 1559 NGC 1560 NGC 1561 NGC 1562 NGC 1563 NGC 1564 NGC 1565 NGC 1566 NGC 1567 NGC 1568 NGC 1569 NGC 1570 NGC 1571 NGC 1572 NGC 1573 NGC 1574 NGC 1575 NGC 1576 NGC 1577 NGC 1578 NGC 1579 NGC 1580 NGC 1581 NGC 1582 NGC 1583 NGC 1584 NGC 1585 NGC 1586 NGC 1587 NGC 1588 NGC 1589 NGC 1590 NGC 1591 NGC 1592 NGC 1593 NGC 1594 NGC 1595 NGC 1596 NGC 1597 NGC 1598 NGC 1599 NGC 1600 NGC 1601 NGC 1602 NGC 1603 NGC 1604 NGC 1605 NGC 1606 NGC 1607 NGC 1608 NGC 1609 NGC 1610 NGC 1611 NGC 1612 NGC 1613 NGC 1614 NGC 1615 NGC 1616 NGC 1617 NGC 1618 NGC 1619 NGC 1620 NGC 1621 NGC 1622 NGC 1623 NGC 1624 NGC 1625 NGC 1626 NGC 1627 NGC 1628 NGC 1629 NGC 1630 NGC 1631 NGC 1632 NGC 1633 NGC 1634 NGC 1635 NGC 1636 NGC 1637 NGC 1638 NGC 1639 NGC 1640 NGC 1641 NGC 1642 NGC 1643 NGC 1644 NGC 1645 NGC 1646 NGC 1647 NGC 1648 NGC 1649 NGC 1650 NGC 1651 NGC 1652 NGC 1653 NGC 1654 NGC 1655 NGC 1656 NGC 1657 NGC 1658 NGC 1659 NGC 1660 NGC 1661 NGC 1662 NGC 1663 NGC 1664 NGC 1665 NGC 1666 NGC 1667 NGC 1668 NGC 1669 NGC 1670 NGC 1671 NGC 1672 NGC 1673 NGC 1674 NGC 1675 NGC 1676 NGC 1677 NGC 1678 NGC 1679 NGC 1680 NGC 1681 NGC 1682 NGC 1683 NGC 1684 NGC 1685 NGC 1686 NGC 1687 NGC 1688 NGC 1689 NGC 1690 NGC 1691 NGC 1692 NGC 1693 NGC 1694 NGC 1695 NGC 1696 NGC 1697 NGC 1698 NGC 1699 NGC 1700 NGC 1701 NGC 1702 NGC 1703 NGC 1704 NGC 1705 NGC 1706 NGC 1707 NGC 1708 NGC 1709 NGC 1710 NGC 1711 NGC 1712 NGC 1713 NGC 1714 NGC 1715 NGC 1716 NGC 1717 NGC 1718 NGC 1719 NGC 1720 NGC 1721 NGC 1722 NGC 1723 NGC 1724 NGC 1725 NGC 1726 NGC 1727 NGC 1728 NGC 1729 NGC 1730 NGC 1731 NGC 1732 NGC 1733 NGC 1734 NGC 1735 NGC 1736 NGC 1737 NGC 1738 NGC 1739 NGC 1740 NGC 1741 NGC 1742 NGC 1743 NGC 1744 NGC 1745 NGC 1746 NGC 1747 NGC 1748 NGC 1749 NGC 1750 NGC 1751 NGC 1752 NGC 1753 NGC 1754 NGC 1755 NGC 1756 NGC 1757 NGC 1758 NGC 1759 NGC 1760 NGC 1761 NGC 1762 NGC 1763 NGC 1764 NGC 1765 NGC 1766 NGC 1767 NGC 1768 NGC 1769 NGC 1770 NGC 1771 NGC 1772 NGC 1773 NGC 1774 NGC 1775 NGC 1776 NGC 1777 NGC 1778 NGC 1779 NGC 1780 NGC 1781 NGC 1782 NGC 1783 NGC 1784 NGC 1785 NGC 1786 NGC 1787 NGC 1788 NGC 1789 NGC 1790 NGC 1791 NGC 1792 NGC 1793 NGC 1794 NGC 1795 NGC 1796 NGC 1797 NGC 1798 NGC 1799 NGC 1800 NGC 1801 NGC 1802 NGC 1803 NGC 1804 NGC 1805 NGC 1806 NGC 1807 NGC 1808 NGC 1809 NGC 1810 NGC 1811 NGC 1812 NGC 1813 NGC 1814 NGC 1815 NGC 1816 NGC 1817 NGC 1818 NGC 1819 NGC 1820 NGC 1821 NGC 1822 NGC 1823 NGC 1824 NGC 1825 NGC 1826 NGC 1827 NGC 1828 NGC 1829 NGC 1830 NGC 1831 NGC 1832 NGC 1833 NGC 1834 NGC 1835 NGC 1836 NGC 1837 NGC 1838 NGC 1839 NGC 1840 NGC 1841 NGC 1842 NGC 1843 NGC 1844 NGC 1845 NGC 1846 NGC 1847 NGC 1848 NGC 1849 NGC 1850 NGC 1851 NGC 1852 NGC 1853 NGC 1854 NGC 1855 NGC 1856 NGC 1857 NGC 1858 NGC 1859 NGC 1860 NGC 1861 NGC 1862 NGC 1863 NGC 1864 NGC 1865 NGC 1866 NGC 1867 NGC 1868 NGC 1869 NGC 1870 NGC 1871 NGC 1872 NGC 1873 NGC 1874 NGC 1875 NGC 1876 NGC 1877 NGC 1878 NGC 1879 NGC 1880 NGC 1881 NGC 1882 NGC 1883 NGC 1884 NGC 1885 NGC 1886 NGC 1887 NGC 1888 NGC 1889 NGC 1890 NGC 1891 NGC 1892 NGC 1893 NGC 1894 NGC 1895 NGC 1896 NGC 1897 NGC 1898 NGC 1899 NGC 1900 NGC 1901 NGC 1902 NGC 1903 NGC 1904 NGC 1905 NGC 1906 NGC 1907 NGC 1908 NGC 1909 NGC 1910 NGC 1911 NGC 1912 NGC 1913 NGC 1914 NGC 1915 NGC 1916 NGC 1917 NGC 1918 NGC 1919 NGC 1920 NGC 1921 NGC 1922 NGC 1923 NGC 1924 NGC 1925 NGC 1926 NGC 1927 NGC 1928 NGC 1929 NGC 1930 NGC 1931 NGC 1932 NGC 1933 NGC 1934 NGC 1935 NGC 1936 NGC 1937 NGC 1938 NGC 1939 NGC 1940 NGC 1941 NGC 1942 NGC 1943 NGC 1944 NGC 1945 NGC 1946 NGC 1947 NGC 1948 NGC 1949 NGC 1950 NGC 1951 NGC 1952 NGC 1953 NGC 1954 NGC 1955 NGC 1956 NGC 1957 NGC 1958 NGC 1959 NGC 1960 NGC 1961 NGC 1962 NGC 1963 NGC 1964 NGC 1965 NGC 1966 NGC 1967 NGC 1968 NGC 1969 NGC 1970 NGC 1971 NGC 1972 NGC 1973 NGC 1974 NGC 1975 NGC 1976 NGC 1977 NGC 1978 NGC 1979 NGC 1980 NGC 1981 NGC 1982 NGC 1983 NGC 1984 NGC 1985 NGC 1986 NGC 1987 NGC 1988 NGC 1989 NGC 1990 NGC 1991 NGC 1992 NGC 1993 NGC 1994 NGC 1995 NGC 1996 NGC 1997 NGC 1998 NGC 1999 Astronomical catalog List of NGC objects Coordinates : 5 34 31.97, + 22 ° 00 ′ 52.1 '' Astronomy portal Cosmology portal Star portal VIAF : 315126060 LCCN : sh85033695 GND : 4148360 - 1 Retrieved from `` https://en.wikipedia.org/w/index.php?title=Crab_Nebula&oldid=808963978 '' Categories : Astronomical objects discovered in 1731 Crab Nebula Messier objects NGC objects Perseus Arm Pulsar wind nebulae Sharpless objects Supernova remnants Taurus ( constellation ) Hidden categories : Use British English from February 2015 Use dmy dates from January 2015 Pages using deprecated image syntax All articles with unsourced statements Articles with unsourced statements from March 2017 Wikipedia articles with VIAF identifiers Wikipedia articles with LCCN identifiers Wikipedia articles with GND identifiers Articles containing video clips Talk Contents About Wikipedia Afrikaans Asturianu Azərbaycanca Bân - lâm - gú Беларуская Беларуская ( тарашкевіца ) ‎ Български Bosanski Català Čeština Corsu Dansk Deutsch Eesti Ελληνικά Español Esperanto Euskara فارسی Français Gaeilge Galego 한국어 हिन्दी Hrvatski Ido Bahasa Indonesia Interlingua Íslenska Italiano עברית ಕನ್ನಡ ქართული Latviešu Lëtzebuergesch Lietuvių Magyar Македонски മലയാളം مازِرونی Bahasa Melayu မြန်မာဘာသာ Nederlands 日本 語 Norsk Norsk nynorsk Novial Occitan Oʻzbekcha / ўзбекча ਪੰਜਾਬੀ پنجابی Polski Português Română Русский 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Question: where is the crab nebula located in the sky
Answer: in the constellation of Taurus