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São Gião Radio Telescope
The São Gião Radio Telescope is situated in the parish of São Gião Portugal. It was constructed in 2015, with first light in December 2015. The gregorian telescope has a diameter of 9.3 m. it is the biggest radio telescope in mainland Portugal. Two 3 phase motors drive the azimuth and elevation (or altitude) servo systems with an accuracy of 0.01 degree. The main reflector has a solid reflector surface that makes it suitable for observations of high frequencies up to 22 GHz. It is used to observe the hydrogen line from our galaxy and maser signals from star-forming regions and late evolution AGB or OH/IR stars. The frequencies used for the hydrogen line is 1.42 GHz and maser signals are measured on 1.612, and 12 GHz The data results obtained with the telescope were presented on EUCARA 2016 Dwingeloo Netherlands and on the ASTROFESTA 2018 in Constancia Portugal. The telescope data and methods are also referenced by universities like the Western Kentucky Unive ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
São Gião
São Gião is a parish (''freguesia'' in Portuguese), in the North of Portugal, on Serra da Estrela, the highest mountain range in Portugal. It belongs to the municipality of Oliveira do Hospital, and the district (''distrito'') of Coimbra. The population in 2011 was 425, in an area of 14.55 km2. It lies at an altitude of 704m, in the Beira region. It is an old Roman trading post. The old Roman bridge is still visible and in use to this day (to be confirmed). The town has a magnificent church - Igreja Matrix, also known as the Igreja Matriz de São Gião or the Catedral das Beiras. This is an excellent building in the Baroque style that dates back to 1795. It has 102 magnificent hand painted panels on the roof that are well worth the trip to this small, hidden village on the slopes of the Serra da Estrela. Situated in the countryside between São Gião and Carvalha is the São Gião Radio Telescope. The 9.3 meter diameter radio telescope is the largest radio telescope in ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Portugal
Portugal, officially the Portuguese Republic, is a country on the Iberian Peninsula in Southwestern Europe. Featuring Cabo da Roca, the westernmost point in continental Europe, Portugal borders Spain to its north and east, with which it shares Portugal-Spain border, the longest uninterrupted border in the European Union; to the south and the west is the North Atlantic Ocean; and to the west and southwest lie the Macaronesia, Macaronesian archipelagos of the Azores and Madeira, which are the two Autonomous Regions of Portugal, autonomous regions of Portugal. Lisbon is the Capital city, capital and List of largest cities in Portugal, largest city, followed by Porto, which is the only other Metropolitan areas in Portugal, metropolitan area. The western Iberian Peninsula has been continuously inhabited since Prehistoric Iberia, prehistoric times, with the earliest signs of Human settlement, settlement dating to 5500 BC. Celts, Celtic and List of the Pre-Roman peoples of the Iberia ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Gregorian Telescope
The Gregorian telescope is a type of reflecting telescope designed by Scottish mathematician and astronomer James Gregory in the 17th century, and first built in 1673 by Robert Hooke. James Gregory was a contemporary of Isaac Newton, and both often worked simultaneously on similar projects. Gregory's design was published in 1663 and pre-dates the first practical reflecting telescope, the Newtonian telescope, built by Sir Isaac Newton in 1668."Isaac Newton: adventurer in thought", by Alfred Rupert Hallpage 67 However, Gregory's design was only a theoretical description, and he never actually constructed the telescope. It was not successfully built until five years after Newton's first reflecting telescope. History The Gregorian telescope is named after the James Gregory design, which appeared in his 1663 publication (The Advance of Optics). Similar theoretical designs have been found in the writings of Bonaventura Cavalieri ( (On Burning Mirrors), 1632) and Marin Mersenne (, ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Azimuth
An azimuth (; from ) is the horizontal angle from a cardinal direction, most commonly north, in a local or observer-centric spherical coordinate system. Mathematically, the relative position vector from an observer ( origin) to a point of interest is projected perpendicularly onto a reference plane (the horizontal plane); the angle between the projected vector and a reference vector on the reference plane is called the azimuth. When used as a celestial coordinate, the azimuth is the horizontal direction of a star or other astronomical object in the sky. The star is the point of interest, the reference plane is the local area (e.g. a circular area with a 5 km radius at sea level) around an observer on Earth's surface, and the reference vector points to true north. The azimuth is the angle between the north vector and the star's vector on the horizontal plane. Azimuth is usually measured in degrees (°), in the positive range 0° to 360° or in the signed ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Altitude
Altitude is a distance measurement, usually in the vertical or "up" direction, between a reference datum (geodesy), datum and a point or object. The exact definition and reference datum varies according to the context (e.g., aviation, geometry, geographical survey, sport, or atmospheric pressure). Although the term ''altitude'' is commonly used to mean the height above sea level of a location, in geography the term elevation is often preferred for this usage. In aviation, altitude is typically measured relative to mean sea level or above ground level to ensure safe navigation and flight operations. In geometry and geographical surveys, altitude helps create accurate topographic maps and understand the terrain's elevation. For high-altitude trekking and sports, knowing and adapting to altitude is vital for performance and safety. Higher altitudes mean reduced oxygen levels, which can lead to altitude sickness if proper acclimatization measures are not taken. Vertical distance ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Hydrogen Line
The hydrogen line, 21 centimeter line, or H I line is a spectral line that is created by a change in the energy state of solitary, electrically neutral hydrogen atoms. It is produced by a spin-flip transition, which means the direction of the electron's spin is reversed relative to the spin of the proton. This is a quantum state change between the two hyperfine levels of the hydrogen 1 s ground state. The electromagnetic radiation producing this line has a frequency of (1.42 GHz), which is equivalent to a wavelength of in a vacuum. According to the Planck–Einstein relation , the photon emitted by this transition has an energy of []. The constant of proportionality, , is known as the Planck constant. The hydrogen line frequency lies in the L band, which is located in the lower end of the microwave region of the electromagnetic spectrum. It is frequently observed in radio astronomy because those radio waves can penetrate the large clouds of interstellar ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Maser Source
An astrophysical maser is a naturally occurring source of stimulated spectral line emission, typically in the microwave portion of the electromagnetic spectrum. This emission may arise in molecular clouds, comets, planetary atmospheres, stellar atmospheres, or various other conditions in interstellar space. Background Discrete transition energy Like a laser, the emission from a maser is stimulated (or ''seeded'') and monochromatic, having the frequency corresponding to the energy difference between two quantum-mechanical energy levels of the species in the gain medium which have been pumped into a non-thermal population distribution. However, naturally occurring masers lack the resonant cavity engineered for terrestrial laboratory masers. The emission from an astrophysical maser is due to a single pass through the gain medium and therefore generally lacks the spatial coherence and mode purity expected from a laboratory maser. Nomenclature It is often stated that astroph ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Star-forming Region
Star formation is the process by which dense regions within molecular clouds in interstellar space—sometimes referred to as "stellar nurseries" or "star-forming regions"— collapse and form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function. Most stars do not form in isolation but as part of a group of stars referred as star clusters or stellar associations. First stars Star formation is divided into three groups called "Populations". Population III stars formed from primordial hydrogen after the Big Bang. These stars are poorly understo ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Asymptotic Giant Branch
The asymptotic giant branch (AGB) is a region of the Hertzsprung–Russell diagram populated by evolved cool luminous stars. This is a period of stellar evolution undertaken by all low- to intermediate-mass stars (about 0.5 to 8 solar masses) late in their lives. Observationally, an asymptotic-giant-branch star will appear as a bright red giant with a luminosity ranging up to thousands of times greater than the Sun. Its interior structure is characterized by a central and largely inert core of carbon and oxygen, a shell where helium is undergoing fusion to form carbon (known as helium burning), another shell where hydrogen is undergoing fusion forming helium (known as hydrogen burning), and a very large envelope of material of composition similar to main-sequence stars (except in the case of carbon stars). Stellar evolution When a star exhausts the supply of hydrogen by nuclear fusion processes in its core, the core contracts and its temperature increases, causing the oute ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
OH/IR Star
__notoc__ An OH/IR star is an asymptotic giant branch (AGB), a red supergiant (RSG), or a red hypergiant (RHG) star that shows strong OH maser emission and is unusually bright at near-infrared wavelengths. In the very late stages of AGB evolution, a star develops a ''super-wind'' with extreme mass loss. The gas in the stellar wind condenses as it cools away from the star, forming molecules such as water (H2O) and silicon monoxide (SiO). This can form grains of dust, mostly silicates, which obscure the star at shorter wavelengths, leading to a strong infrared source. Hydroxyl (OH) radicals can be produced by photodissociation or collisional dissociation. H2O and OH can both be pumped to produce maser emission. OH masers in particular can give rise to a powerful maser action at 1612 MHz and this is regarded as a defining feature of the OH/IR stars. Many other AGB stars, such as Mira variables, show weaker OH masers at other wavelengths, such as 1667MHz or 22MHz. Examples ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Maser
A maser is a device that produces coherent electromagnetic waves ( microwaves), through amplification by stimulated emission. The term is an acronym for microwave amplification by stimulated emission of radiation. Nikolay Basov, Alexander Prokhorov and Joseph Weber introduced the concept of the maser in 1952, and Charles H. Townes, James P. Gordon, and Herbert J. Zeiger built the first maser at Columbia University in 1953. Townes, Basov and Prokhorov won the 1964 Nobel Prize in Physics for theoretical work leading to the maser. Masers are used as timekeeping devices in atomic clocks, and as extremely low-noise microwave amplifiers in radio telescopes and deep-space spacecraft communication ground-stations. Modern masers can be designed to generate electromagnetic waves at microwave frequencies and radio and infrared frequencies. For this reason, Townes suggested replacing "microwave" with "molecular" as the first word in the acronym "maser". The ''laser'' works by the sa ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Western Kentucky University
Western Kentucky University (WKU) is a public university in Bowling Green, Kentucky, United States. It was founded by the Commonwealth of Kentucky in 1906, though its roots reach back a few decades earlier. It operates regional campuses in Glasgow, Kentucky, Glasgow, Elizabethtown, Kentucky, Elizabethtown-Fort Knox, and Owensboro, Kentucky, Owensboro. The main campus sits atop a hill overlooking the Barren River valley. History The roots of Western Kentucky University go back to 1876 with the founding by A. W. Mell of the privately owned Glasgow Normal School and Business College in Glasgow, Kentucky. This moved to Bowling Green in 1884 and became the Southern Normal School and Business College. In 1890, Potter College was opened as a private women's college by Pleasant J. Potter. In 1906, Henry Hardin Cherry sold the Southern Normal School and became president of the Western Kentucky State Normal School, which had just been created by an act of the Kentucky General Assembly. ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
