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Fast Radio Burst Monitoring refers to the detection and study of the mysterious and brief flashes of radio light known as Fast Radio Bursts (FRBs). Monitoring these events helps to identify their origins and understand the extreme conditions in which they occur.

Solar Radio Observations involve the monitoring of radio emissions from the sun to study solar activity, such as solar flares and coronal mass ejections. This provides insights into space weather and the sun's influence on the solar system environment.

Pulsar Timing is a technique used to observe the regular radio pulses emitted by pulsars. By precisely measuring the timing of these pulses, astronomers can test theories of gravity, detect binary and exoplanet companions, and potentially observe gravitational waves.

Interferometric Imaging uses multiple telescopes to create higher-resolution images than is possible with a single telescope. It works on the principle of constructive and destructive interference, and allows astronomers to study fine detail in radio sources.

CMB Observations focus on detecting the faint microwave radiation left over from the Big Bang, providing insights into the early universe's conditions and the fundamental physics of cosmology.

Continuum Observation involves measuring the radio emissions from celestial bodies over a wide range of frequencies. This technique is used to create maps of large objects like galaxies or clusters, and can reveal structural and physical information.

21 cm Line Observations pertain to the radio emission at a wavelength of 21 cm, originating from neutral hydrogen atoms in space. These observations are crucial for mapping the structure and distribution of hydrogen in the Galaxy and for studying the early Universe.

Radio Polarimetry is a technique that measures the polarization of radio waves emitted from astronomical sources. It can uncover details about magnetic fields, radiation processes, and physical conditions within the observed regions.

Radio Recombination Line Studies focus on the analysis of specific electromagnetic transitions of electrons in ions that occur in space. These studies provide information on the density, temperature, and dynamics within ionized regions of space such as H II regions.

Single-Dish Observing refers to the use of an individual radio telescope for astronomical observations. Such observations can measure the total power from sources and are important for surveys and for observing large-scale structures in the sky. However, they typically have lower resolution compared to interferometric techniques.

Aperture Synthesis is a method that combines signals from a collection of smaller telescopes to produce images with a resolution equivalent to that of a larger telescope. This is a fundamental technique for radio interferometry and is key to the operation of arrays like the Very Large Array (VLA).

Spectral Line Observation uses radio telescopes to observe specific frequencies emitted or absorbed by atoms and molecules in space. This technique enables the study of chemical compositions, physical conditions, and velocities of celestial objects.

RFI Mitigation involves techniques to reduce or eliminate the noise in radio astronomical observations caused by human-made sources such as communication signals. Effective RFI mitigation is critical for acquiring clean, usable data in radio astronomy.

VLBI is a type of astronomical interferometry used in radio astronomy. It involves using multiple radio telescopes spread over large distances to simulate a telescope of that size. The technique allows for extremely high angular resolution, and is used to image distant cosmic radio sources, conduct astrometric measurements, and improve geodetic measurements.