Course : Εισαγωγή στη Ραδιοστρονομία
Course code : PH338C
Definition
The ability of a telescope to detect signals. Better sensitivity means weaker sources can be observed.
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Secondary response regions outside the main beam. Bright sources entering sidelobes can contaminate observations.
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The strength of a signal compared with the level of noise. Higher S/N means a more reliable detection.
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Observation using one radio telescope antenna. Useful for total power measurements, pulsar timing, spectral lines, and large-scale emission.
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Noise contribution from the sky itself, including the atmosphere, Galactic emission, and cosmic background.
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How fast a telescope can move from one pointing direction to another.
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Emission at a specific frequency caused by transitions between energy levels. The most famous radio example is the 21-cm hydrogen line.
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A systematic observation of a large area of the sky.
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Radiation emitted by charged particles, usually electrons, spiralling around magnetic field lines at relativistic speeds. Common in supernova remnants, jets, pulsars, and radio galaxies.
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The effective beam of an interferometric array, determined by the uv coverage and weighting scheme.
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A measure of the total noise in a radio telescope system, including receiver noise, sky noise, atmosphere, ground spillover, and other contributions.
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