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NGC 383
NGC 383 is a double radio galaxy with a quasar-like appearance located in the constellation Pisces. It was discovered by German-British astronomer William Herschel on 12 September 1784. It is listed as Arp 331 in Halton Arp's Atlas of Peculiar Galaxies. Recent discoveries by the National Radio Astronomy Observatory in 2006 reveal that NGC 383 is being bisected by high energy relativistic jets traveling at relatively high fractions of the speed of light. The relativistic electrons in the jets are detected as synchrotron radiation in the x-ray and radio wavelengths. The focus of this intense energy is the galactic center of NGC 383. The relativistic electron jets detected as synchrotron radiation extend for several thousand parsecs and then appear to dissipate at the ends in the form of streamers or filaments. There are four other nearby galaxies NGC 379, NGC 380, NGC 385, and NGC 384 which are suspected of being closely associated with NGC 383, as well as several other ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
New General Catalogue
The ''New General Catalogue of Nebulae and Clusters of Stars'' (abbreviated NGC) is an astronomical catalogue of deep-sky objects compiled by John Louis Emil Dreyer in 1888. The NGC contains 7,840 objects, including galaxy, galaxies, star clusters and emission nebulae. Dreyer published two supplements to the NGC in 1895 and 1908, known as the ''Index Catalogues'' (abbreviated IC), describing a further 5,386 astronomical objects. Thousands of these objects are best known by their NGC or IC numbers, which remain in widespread use. The NGC expanded and consolidated the cataloguing work of William Herschel, William and Caroline Herschel, and John Herschel's ''General Catalogue of Nebulae and Clusters of Stars''. Objects south of the Celestial sphere, celestial equator are catalogued somewhat less thoroughly, but many were included based on observation by John Herschel or James Dunlop. The NGC contained multiple errors, but attempts to eliminate them were made by the ''Revised New Ge ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Astrophysical Jet
An astrophysical jet is an astronomical phenomenon where outflows of ionised matter are emitted as extended beams along the axis of rotation. When this greatly accelerated matter in the beam approaches the speed of light, astrophysical jets become relativistic jets as they show effects from special relativity. The formation and powering of astrophysical jets are highly complex phenomena that are associated with many types of high-energy astronomical sources. They likely arise from dynamic interactions within accretion disks, whose active processes are commonly connected with compact central objects such as black holes, neutron stars or pulsars. One explanation is that tangled magnetic fields are organised to aim two diametrically opposing beams away from the central source by angles only several degrees wide Jets may also be influenced by a general relativity effect known as frame-dragging. Most of the largest and most active jets are created by supermassive black holes (SM ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Radio Galaxies
A radio galaxy is a galaxy with giant regions of radio emission extending well beyond its visible structure. These energetic radio lobes are powered by jets from its active galactic nucleus. They have luminosities up to 1039 watt, W at radio waves, radio wavelengths between 10 MHz and 100 GHz. The radio emission is due to the synchrotron radiation, synchrotron process. The observed structure in radio emission is determined by the interaction between twin relativistic jet, jets and the external medium, modified by the effects of relativistic beaming. The host galaxy, host galaxies are almost exclusively large elliptical galaxy, elliptical galaxies. ''Radio-loud'' active galaxies can be detected at large distances, making them valuable tools for observational cosmology. Recently, much work has been done on the effects of these objects on the intergalactic medium, particularly in galaxy groups and clusters. The term "radio galaxy" is often used to refer to the entire j ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Relativistic Beaming
In physics, relativistic beaming (also known as Doppler beaming, Doppler boosting, or the headlight effect) is the process by which relativistic effects modify the apparent luminosity of emitting matter that is moving at speeds close to the speed of light. In an astronomical context, relativistic beaming commonly occurs in two oppositely-directed relativistic jets of plasma that originate from a central compact object that is accreting matter. Accreting compact objects and relativistic jets are invoked to explain x-ray binaries, gamma-ray bursts, and, on a much larger scale, (AGN) active galactic nuclei (of which quasars are a particular variety). Beaming affects the apparent brightness of a moving object. Consider a cloud of gas moving relative to the observer and emitting electromagnetic radiation. If the gas is moving towards the observer, it will be brighter than if it were at rest, but if the gas is moving away, it will appear fainter. The magnitude of the effect ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Radio Galaxy 3C31
Radio is the technology of telecommunication, communicating using radio waves. Radio waves are electromagnetic waves of frequency between 3 hertz (Hz) and 300 gigahertz (GHz). They are generated by an electronic device called a transmitter connected to an antenna (radio), antenna which radiates the waves. They can be received by other antennas connected to a radio receiver; this is the fundamental principle of radio communication. In addition to communication, radio is used for radar, radio navigation, radio control, remote control, remote sensing, and other applications. In radio communication, used in radio and television broadcasting, cell phones, two-way radios, wireless networking, and satellite communication, among numerous other uses, radio waves are used to carry information across space from a transmitter to a receiver, by Modulation, modulating the radio signal (impressing an information signal on the radio wave by varying some aspect of the wave) in the tran ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Xingming Observatory
Xingming Observatory () is a private amateur astronomical observatory located in Gangou Township, Ürümqi, Xinjiang, China. The observatory was founded by amateur astronomer Gao Xing in 2007. The name "Xingming" is chosen partly to commemorate Zhou Xingming, a pioneer of amateur astronomy in China. As of 2024, discoveries made by Xingming Observatory include 3 comets, 15 asteroids, 90 supernovae, 63 novae, and 111 dwarf novae. Research Programs The observatory conducts research in time-domain astronomy and solar system observations in collaboration with professional astronomers. It hosts XOSS (Xingming Observatory Sky Survey), an amateur sky survey that searches for transients, asteroids and comets. Observational data from Xingming Observatory contributed to published astronomy research since 2011. Public Outreach The observatory shares a number of telescopes with the public through the XPRO (Xingming Public Remote Observatory) program. It also operates PSP (Popular Superno ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
International Astronomical Union
The International Astronomical Union (IAU; , UAI) is an international non-governmental organization (INGO) with the objective of advancing astronomy in all aspects, including promoting astronomical research, outreach, education, and development through global cooperation. It was founded on 28 July 1919 in Brussels, Belgium and is based in Paris, France. The IAU is composed of individual members, who include both professional astronomers and junior scientists, and national members, such as professional associations, national societies, or academic institutions. Individual members are organised into divisions, committees, and working groups centered on particular subdisciplines, subjects, or initiatives. the Union had 85 national members and 12,734 individual members, spanning 90 countries and territories. Among the key activities of the IAU is serving as a forum for scientific conferences. It sponsors nine annual symposia and holds a triannual General Assembly that sets policy ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Type Ia Supernova
A Type Ia supernova (read: "type one-A") is a type of supernova that occurs in binary systems (two stars orbiting one another) in which one of the stars is a white dwarf. The other star can be anything from a giant star to an even smaller white dwarf. Physically, carbon–oxygen white dwarfs with a low rate of rotation are limited to below 1.44 solar masses (). Beyond this "Chandrasekhar limit, critical mass", they reignite and in some cases trigger a supernova explosion; this critical mass is often referred to as the Chandrasekhar mass, but is marginally different from the absolute Chandrasekhar limit, where electron degeneracy pressure is unable to prevent catastrophic collapse. If a white dwarf gradually accretes mass from a binary companion, or merges with a second white dwarf, the general hypothesis is that a white dwarf's core will reach the ignition temperature for Carbon burning process, carbon fusion as it approaches the Chandrasekhar mass. Within a few seconds of ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Supernova
A supernova (: supernovae or supernovas) is a powerful and luminous explosion of a star. A supernova occurs during the last stellar evolution, evolutionary stages of a massive star, or when a white dwarf is triggered into runaway nuclear fusion. The original object, called the ''progenitor'', either collapses to a neutron star or black hole, or is completely destroyed to form a diffuse nebula. The peak optical luminosity of a supernova can be comparable to that of an entire galaxy before fading over several weeks or months. The last supernova directly observed in the Milky Way was Kepler's Supernova in 1604, appearing not long after Tycho's Supernova in 1572, both of which were visible to the naked eye. The supernova remnant, remnants of more recent supernovae have been found, and observations of supernovae in other galaxies suggest they occur in the Milky Way on average about three times every century. A supernova in the Milky Way would almost certainly be observable through mo ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
NGC 384
NGC 384 is an elliptical galaxy located in the constellation Pisces. It was discovered on November 4, 1850, by Bindon Stoney. It was described by Dreyer as "pretty faint, pretty small, southwestern of 2.", the other being NGC 385. Along with galaxies NGC 375, NGC 379, NGC 382, NGC 383 NGC 383 is a double radio galaxy with a quasar-like appearance located in the constellation Pisces. It was discovered by German-British astronomer William Herschel on 12 September 1784. It is listed as Arp 331 in Halton Arp's Atlas of Peculi ..., NGC 385, NGC 386, NGC 387 and NGC 388, NGC 384 forms a galaxy cluster called Arp 331. References External links * Elliptical galaxies 0384 18501104 Pisces (constellation) 003983 {{elliptical-galaxy-stub ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
NGC 385
NGC 385 is an unbarred lenticular galaxy located in the constellation Pisces. It was discovered on November 4, 1850, by Bindon Stoney. It was described by Dreyer as "pretty faint, pretty small, round, northeastern of 2.", the other being NGC 384. Along with galaxies NGC 375, NGC 379, NGC 382, NGC 383 NGC 383 is a double radio galaxy with a quasar-like appearance located in the constellation Pisces. It was discovered by German-British astronomer William Herschel on 12 September 1784. It is listed as Arp 331 in Halton Arp's Atlas of Peculi ..., NGC 384, NGC 386, NGC 387 and NGC 388, NGC 385 forms a galaxy cluster called Arp 331. References External links * 0385 18501104 Pisces (constellation) Unbarred lenticular galaxies 003984 {{lenticular-galaxy-stub ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
NGC 380
NGC 380 is an elliptical galaxy located in the constellation Pisces. It was discovered on September 12, 1784 by William Herschel. It was described by Dreyer as "pretty faint, small, round, suddenly brighter middle." Along with galaxies NGC 375, NGC 379, NGC 382, NGC 383, NGC 384, NGC 385 NGC 385 is an unbarred lenticular galaxy located in the constellation Pisces. It was discovered on November 4, 1850, by Bindon Stoney. It was described by Dreyer as "pretty faint, pretty small, round, northeastern of 2.", the other being NGC 38 ..., NGC 386, NGC 387 and NGC 388, NGC 380 forms a galaxy cluster called Arp 331. References External links * 0380 17840912 Pisces (constellation) Elliptical galaxies 003969 {{Elliptical-galaxy-stub ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
