Radio astronomy Radio astronomy The Astronomical Image Processing System provides facilities for calibration, editing, image formation, image enhancement, and analysis of images and other astronomical data. A major focus is on reduction of data from both single-dish and aperture synthesis radio telescopes. Although the tools provided in AIPS/AIPS++ are mainly designed for processing data from varieties of radio telescopes, the package is expected to also be useful for processing other types of astronomical data and images. However, the reduction of most data from imaging array detectors is performed using IRAF instead. ...more on Wikipedia about "AIPS"
The Allen Telescope Array (ATA), formerly known as the One Hectare Telescope (1hT), is a joint effort by the SETI Institute and the Radio Astronomy Laboratory at the University of California, Berkeley to construct a radio interferometer that will be dedicated to astronomical and simultaneous search for extra-terrestrial intelligence observations. It is being constructed at the Hat Creek Radio Observatory, 290 miles northeast of San Francisco, California and will be composed of 350 antennas at completion. ...more on Wikipedia about "Allen Telescope Array"
Auroral kilometric radiation (AKR) is the intense radio radiation emitted in the acceleration zone (at a height of three times the radius of the Earth) of the polar lights. The radiation mainly comes from cyclotron radiation from electrons orbiting around the magnetic field lines of the Earth. The radiation has a frequency of between 50 and 5000 kHz and a total power of between about 1 million and 10 million Watts. The radiation is absorbed by the ionosphere and therefore can only be measured by satellites positioned at vast heights, such as the Fast Auroral Snapshot Explorer (FAST). ...more on Wikipedia about "Auroral kilometric radiation"
In cosmology, the cosmic microwave background radiation (most often abbreviated CMB but occasionally CMBR, CBR or MBR) is a form of electromagnetic radiation discovered in 1965. It has a thermal black-body spectrum which peaks in the microwave range. Most cosmologists consider the cosmic microwave background radiation to be the best evidence for the hot big bang model of the universe. ...more on Wikipedia about "Cosmic microwave background radiation"
The hydrogen line refers to the spectral line created by changes in the energy state of neutral hydrogen and occurs at 1420.40575 MHz, or a wavelength of around 21 cm. The line is used extensively in astronomy, particularly radio astronomy. ...more on Wikipedia about "Hydrogen line"
The Istituto di Radioastronomia di Bologna (Institute for Radio Astronomy of Bologna) is one of the Italian institutes that had already been part of the Consiglio Nazionale delle Ricerche (National Association for Research), now part of the Istituto Nazionale di Astrofisica (National Institute for Astrophysics). ...more on Wikipedia about "Istituto di Radioastronomia di Bologna"
Pulsars are rotating neutron stars that are observable as sources of electromagnetic radiation. The radiation intensity varies with a regular period, believed to correspond to the rotation period of the star. ...more on Wikipedia about "Pulsar"
A quasar (contraction of QUASi-stellAR radio sources) is an astronomical source of electromagnetic energy, including light, that dwarfs the energy output of the brightest stars. A Quasar may readily release energy in levels equal to the output of dozens of average galaxies combined. In optical telescopes, a quasar looks like a very faint star (i.e. it is a point source), and has a very high redshift. The general consensus is that this high redshift is cosmological, the result of Hubble's law, which implies that quasars must be very distant and must emit more energy than dozens of normal galaxies. ...more on Wikipedia about "Quasar"
Radio astronomy is the study of celestial phenomena through measurement of the characteristics of radio waves emitted by physical processes occurring in space. Radio waves are much longer than light waves. In order to receive good signals, radio astronomy requires large antennas, or arrays of smaller antennas all working together (The Very Large Array near Socorro, New Mexico is an example of this). Most telescopes use a parabolic dish to reflect the waves to a receiver which detects and amplifies the signal into usable data. This allows astronomers to see a region of the radio sky. If they take multiple scans of overlaping strips of the sky they can piece together an image ('mosaicing'). Radio astronomy is a relatively new field of astronomical research that still has much more to be discovered. ...more on Wikipedia about "Radio astronomy"
The Sunyaev-Zel'dovich effect (occasionally abbreviated as the SZ effect) is due to high energy electrons distorting the cosmic microwave background radiation (CMB) through inverse Compton scattering, in which some of the energy of the electrons is transferred to the low energy photons. Observed distortions of the cosmic microwave background spectrum are used to detect the density perturbations of the universe. Using the Sunyaev-Zeldovich effect, dense clusters of galaxies have been observed. ...more on Wikipedia about "Sunyaev-Zel'dovich effect"
Very Long Baseline Interferometry (VLBI) is a type of interferometry used in radio astronomy, in which the data received at each antenna in the array is paired with timing information, usually from a local atomic clock, and then stored for later analysis on magnetic tape or hard disk. At that later time, the data are correlated with data from other antennas similarly recorded, to produce the resulting image. The resolution achievable using interferometry is proportional to the distance between the antennas furthest apart in the array. The VLBI technique enables this distance to be much greater than that possible with conventional interferometry, which requires antennas to be physically connected by coaxial cable, waveguide, optical fiber, or other type of transmission line. The greater telescope separations are possible in VLBI due to the development of the closure phase imaging technique by Roger Jennison in the 1950s, allowing VLBI to produce images with superior resolution. VLBI is most often performed at radio wavelengths; however, the technique has recently been extended to optics. ...more on Wikipedia about "Very Long Baseline Interferometry"
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