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A technique used to study the composition of celestial objects by analyzing the light absorbed by elements as it passes through a medium or an object's atmosphere.

Dark or bright lines seen within the spectrum that are signatures of the presence of specific elements or molecules in a star or galaxy, revealing information about their chemical composition, temperature, and density.

The change in frequency or wavelength of light from an object moving relative to the observer, used to determine the velocity of stars and galaxies moving towards or away from Earth.

Specific dark lines in the solar spectrum used to identify the presence of various elements in the Sun's atmosphere, named after the German physicist who first observed them.

The measurement of the reflection or scattering of light by surfaces or particles, used in astronomy to determine the surface composition of planets, moons, and asteroids.

Observes the specific wavelengths of light emitted by an element or compound when it undergoes excitation, used in astronomy to identify the composition of stars and galaxies.

Three rules that describe the creation of spectral lines: a luminous solid, liquid, or dense gas emits light of all wavelengths; a low-density gas emits light at specific wavelengths; and a continuous spectrum viewed through a cool, low-density gas has dark lines.

This form of spectroscopy looks at the X-ray part of the electromagnetic spectrum, providing information about high-energy processes in the universe, such as those involving black holes and neutron stars.

Astronomical technique used to study objects that are too cool to emit visible light, such as dust clouds, brown dwarfs, and planets, by observing the infrared part of the spectrum.

A series of absorption lines in the spectra of distant galaxies and quasars caused by hydrogen in the intergalactic medium and used to study the distribution and evolution of hydrogen gas over cosmic time.

A technique that relies on the emission of light by a substance that has absorbed light, often of a different wavelength, used to study cosmic phenomena with fluorescing materials like certain nebulae.

A spectroscopic technique used to observe vibrational, rotational, and other low-frequency modes in a system, which can provide information on molecular composition and structure in astronomical objects.

A correction factor that is applied to convert observed magnitudes of celestial objects into bolometric (total emitted energy) magnitudes, taking into account light emitted across all wavelengths.

Analysis of radio wavelength emissions from celestial objects that can provide information about molecular clouds, cosmic microwave background radiation, and the dynamics of galaxies.