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A pulsar is a highly magnetized, rotating neutron star that emits beams of electromagnetic radiation out of its magnetic poles. This radiation is observable when the beam points towards Earth, often observed in radio frequencies.

A radiometer is a device used to measure the intensity and distribution of radiation, including radio waves. In radio astronomy, it is specifically used to measure the strength of the received radio waves from astronomical sources.

A radio telescope is a specialized antenna and radio receiver used to detect radio waves from astronomical radio sources in the sky. It operates on different frequencies than those for television and other communication systems.

Beamwidth is the angular width where the signal strength of a radio wave from an antenna falls to half its peak value. It determines the resolving power of a radio telescope.

Interferometry is a technique in radio astronomy where signals from multiple antennas are combined to create a virtual telescope with a size equal to the distance between the antennas, providing higher resolution images.

A spectral line in radio astronomy is a specific frequency of radio emission or absorption that corresponds to the transition of an atom or molecule from one energy level to another.

The radio window is the range of electromagnetic frequencies that pass through the Earth's atmosphere and reach the ground, allowing radio telescopes to observe astronomical phenomena without space-based receivers.

The Hydrogen Line, or 21 cm line, is the electromagnetic radiation spectral line that is created by a change in the energy state of neutral hydrogen atoms. It is vital for understanding the composition and structure of the universe.

Synchrotron Radiation is emitted when charged particles, like electrons, are accelerated in magnetic fields and emit radio frequency energy. It is a significant source of radio emission in the universe, from various astronomical objects.

Fast Radio Bursts are intense bursts of radio emission that last for a few milliseconds and come from unknown origins outside our galaxy. They are a recent discovery and the subject of active research in radio astronomy.

Cosmic rays are high-energy particles from space that can produce radio emissions when they interact with magnetic fields or the Earth's atmosphere, which can affect radio astronomical observations.

In the context of radio astronomy, cold fronts are relatively sharp boundary regions within galaxy clusters where there is a temperature gradient detected in radio frequencies, indicating various stages of cluster evolution.

The Cosmic Microwave Background is the thermal radiation left over from the time of recombination in Big Bang cosmology, observable today as a faint microwave glow present in all directions in the sky.

Redshift occurs when light or other electromagnetic radiation from an object is increased in wavelength, or shifted to the red end of the spectrum. In radio astronomy, it helps to determine the distance and velocity of distant galaxies.

The Spectral Index is a measure that characterizes how the intensity of radio emission from a celestial source varies with frequency. It is a key parameter in the study of the physical properties of radio sources.

Hertz is the unit of frequency in the International System of Units (SI), defined as one cycle per second. It is used in radio astronomy to describe the frequency of radio waves.

Faraday Rotation is the phenomenon where the polarization plane of electromagnetic waves, such as radio waves, is rotated as the waves pass through a magnetic field contained within an ionized medium, like a plasma.

A bolometer is a sensitive instrument that measures the energy of incident electromagnetic radiation via the heating of a material with a temperature-dependent electrical resistance. It can be used in radio astronomy to measure faint sources.

VLBI is a type of astronomical interferometry used in radio astronomy, in which data from separate radio telescopes are combined to create telescopes of the size of the separation distance for very high angular resolution.

Flux density is the measure of radio power per unit area from an astronomical source, measured in Jansky (Jy). It is a critical measure for understanding the luminosity and distance of celestial objects emitting radio waves.

Radio galaxies are types of galaxies that are very luminous at radio wavelengths, with radio emission coming from two large lobes on opposite sides of the galaxy's center, often associated with supermassive black holes.

The Doppler Effect in radio astronomy refers to the change in frequency or wavelength of radio waves from an emitting or reflecting object due to its relative motion towards or away from the observer.

In radio astronomy, an array refers to a collection of antennas or dishes that work together as a single instrument to observe radio waves. The combined data enhances the effective resolution and sensitivity of observations.

RFI refers to the disturbance caused by external sources of radio frequency energy in the operation of radio astronomical observations. It is a significant issue for radio astronomy given the sensitivity of the instruments.

Sky noise is the radio signal that comes from natural astronomical sources, both discrete objects and the background. It is a significant component of the noise that radio telescopes must detect signals against.

A quasar is an extremely bright and distant active galactic nucleus, with its radio emissions believed to be powered by accretion of material into supermassive black holes located at the center of galaxies.

LOFAR is a large network of radio telescopes primarily located in Europe, designed to observe the universe at low radio frequencies. It uses novel techniques to analyze signals and study astrophysical phenomena.

Continuum Emission refers to a wide and smooth spectrum of radiation emitted by astronomical sources. In radio astronomy, it encompasses a range of frequencies and is typically associated with thermal processes or synchrotron emission.

A radio source is any celestial body that emits significant amounts of radio frequency energy, such as stars, galaxies, quasars, and pulsars. They are of particular interest in radio astronomy studies.