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Ammonia inversion lines are crucial for measuring temperatures in dense molecular clouds and are an excellent thermometer for the cold, dense gas where stars are born.

This line corresponds to the hyperfine transition of neutral hydrogen. It helps in mapping the structure and density of hydrogen in the Milky Way and other galaxies, which aids our understanding of cosmic structure, star formation, and the dynamics of galaxies.

The regular radio pulses emitted at this frequency provide insights into neutron star properties, including magnetic field strength, age, and rotation. They also contribute to the understanding of matter under extreme conditions and tests of general relativity.

The fine-structure line of C II at 157µm provides information on the state and distribution of the interstellar medium, and is a major coolant of the cold interstellar gas.

Water masers are found around young stellar objects and in the jets ejected by these objects. They play a key role in understanding the early stages of star formation and the dynamics of water vapor in space.

The CO J=1-0 transition at 2.6mm is crucial for tracing molecular gas in the galaxy, which is a precursor to star formation. It often acts as a substitute for H$_2$ which doesn't emit readily in cold interstellar environments.

These lines are emitted when an electron recombines with a proton to form an atom of hydrogen. They are used to determine the physical conditions of ionized gas phases in the interstellar medium and are especially important in HII regions.

The CN radical lines are valuable for studying magnetic fields in molecular clouds and circumstellar environments, providing insights into star formation and the dynamics of stellar environments.

OH masers are associated with star-forming regions and the envelopes of late-type stars. Observations of these lines provide valuable information on the kinematics and magnetic fields in these regions.

By measuring the splitting of spectral lines caused by the Zeeman Effect, the magnetic field strength in different astronomical environments such as the surfaces of stars, accretion disks, and molecular clouds can be deduced.

Methanol masers occur in regions of high-mass star formation. They are important for tracing shock regions within molecular clouds and indicating early indicators of star-forming activities.