The history of spectroscopy starts with the use of the lens by Aristophanes about 423 B.C.; and the studies of mirrors by Euclid (300 B.C.) and Hero (100 B.C.). Seneca (40 A.D.) observed the light scattering properties of prisms, and in 100 A.D. Ptolemy studied incidence and refraction.
Alhazen in 1038 studied reflection and refraction of light, and in 1250 Roger Bacon determined the focal points of concave mirros.
Around 1600, the telescope was developed in Holland and by 1610, Galileo had made improvements on the telescope design. Sir Isaac Newton (1642-1727) performed many experiments on the separation of light to obtain a spectrum and the indices of refraction of different colors of light; he applied those principles to the telescope.
Fraunhofer, about 1814-15, observed diffraction phenomena and was able to measure wavelength instead of angles of refraction. Herschel (1823) and Talbot (1825) discovered atomic emission when certain atoms were placed in a flame. Wheatstone concluded in 1835 that metals could be distinguished from one another on basis on the wavelengths of this emission. In 1848, Foucault observed atomic emission from sodium and discovered that the element would absorb the same rays from an electric arc.
In the later 1800, scientists such as Kirchoff, Bunsen, Angstr�m, Rowland, Michelson and Balmer studied the composition of the sun based on their emissions at different wavelengths. Kirchoff summarized the law which states that, "Matter absorbs light at the same wavelength at which it emits light". It is under this law that atomic absorption spectroscopy works.
Woodson was one of the first to apply this principle to the detection of mercury. In 1955, Walsh suggested the use of cathode lamps to provide an emission of appropriate wavelength; and the use of a flame to produce neutral atoms that would absorb the emission as they crossed its path. Instrumentation and applications for atomic absorption greatly expanded after the 1950s.
Alhazen in 1038 studied reflection and refraction of light, and in 1250 Roger Bacon determined the focal points of concave mirros.
Around 1600, the telescope was developed in Holland and by 1610, Galileo had made improvements on the telescope design. Sir Isaac Newton (1642-1727) performed many experiments on the separation of light to obtain a spectrum and the indices of refraction of different colors of light; he applied those principles to the telescope.
Fraunhofer, about 1814-15, observed diffraction phenomena and was able to measure wavelength instead of angles of refraction. Herschel (1823) and Talbot (1825) discovered atomic emission when certain atoms were placed in a flame. Wheatstone concluded in 1835 that metals could be distinguished from one another on basis on the wavelengths of this emission. In 1848, Foucault observed atomic emission from sodium and discovered that the element would absorb the same rays from an electric arc.
In the later 1800, scientists such as Kirchoff, Bunsen, Angstr�m, Rowland, Michelson and Balmer studied the composition of the sun based on their emissions at different wavelengths. Kirchoff summarized the law which states that, "Matter absorbs light at the same wavelength at which it emits light". It is under this law that atomic absorption spectroscopy works.
Woodson was one of the first to apply this principle to the detection of mercury. In 1955, Walsh suggested the use of cathode lamps to provide an emission of appropriate wavelength; and the use of a flame to produce neutral atoms that would absorb the emission as they crossed its path. Instrumentation and applications for atomic absorption greatly expanded after the 1950s.
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