The width of a spectral line, often measured at half its maximum intensity, indicating the range of frequencies absorbed or emitted.A spectral line is a dark or bright feature in a spectrum, corresponding to the absorption or emission of light at a specific frequency. The linewidth is the range of frequencies over which this feature extends, typically measured at half its maximum intensity (full width at half maximum, FWHM). A narrow linewidth means the light is highly monochromatic, while a broad linewidth indicates a spread of frequencies. The linewidth is a fundamental property that encodes information about the physical conditions of the emitting or absorbing material, such as temperature, pressure, and velocity.
The concept of spectral linewidth was established in the late 19th and early 20th centuries with the development of high-resolution spectroscopy. Albert Michelson and others measured the fine structure of spectral lines, and the theoretical framework was later refined by Hendrik Lorentz and others.
The linewidth arises from several broadening mechanisms. Natural broadening is due to the finite lifetime of quantum states, as described by the Heisenberg uncertainty principle. Doppler broadening occurs because atoms or molecules in a gas move at different velocities, shifting the absorbed or emitted frequencies via the Doppler effect. Pressure (collisional) broadening results from interactions between particles that perturb energy levels. The observed line profile is a convolution of these effects, and measuring its shape and width allows physicists to infer the temperature, density, and motion of the source.
Linewidth is crucial in laser technology, where narrow linewidths enable precision measurements, optical clocks, and high-resolution spectroscopy. It is also used in astronomy to determine the composition, temperature, and velocity of celestial objects, as well as in telecommunications to increase the data capacity of optical fibers.
The narrowest spectral lines ever measured are in ultra-cold trapped ions, with linewidths of less than one hertz, corresponding to a frequency stability that would only drift by one second over the age of the universe.









