
The distribution of light intensity across wavelengths, used to identify elements and physical conditions.Spectra refer to the distribution of electromagnetic radiation (such as light) emitted, absorbed, or scattered by matter, as a function of wavelength or frequency. Each element and molecule has a unique spectral fingerprint, like a barcode, that reveals its composition, temperature, density, and motion. Spectra are the primary tool astronomers use to understand the universe, from the composition of distant stars to the expansion of galaxies.
The foundation of spectroscopy was laid in the 19th century by Joseph von Fraunhofer, who mapped dark lines in the solar spectrum, and later by Gustav Kirchhoff and Robert Bunsen, who established that each element has a unique spectral signature. The quantum mechanical explanation of spectral lines was developed by Niels Bohr in 1913.
When atoms or molecules absorb or emit energy, they do so at specific wavelengths corresponding to transitions between quantized energy levels. The resulting spectrum consists of discrete lines (emission or absorption lines) or continuous bands, depending on the material and conditions. By analyzing the positions, intensities, and widths of these lines, scientists can deduce the chemical composition, temperature, pressure, and velocity (via the Doppler effect) of the source.
Spectra are used in astronomy to determine the chemical composition of stars and exoplanets, in chemistry for material analysis, and in medicine for non-invasive diagnostics such as pulse oximetry.
The element helium was discovered in 1868 in the spectrum of the Sun's corona before it was ever found on Earth — its name comes from the Greek word 'helios', meaning sun.




