Editing Fourier-transform spectroscopy (section)

===Measuring an emission spectrum===
[[File:Spectrum of blue flame.svg|thumb|300 px| An example of a [[spectrum]]: The spectrum of light emitted by the blue flame of a [[butane torch]]. The horizontal axis is the [[wavelength]] of light, and the vertical axis represents how much light is emitted by the torch at that wavelength.]]
One of the most basic tasks in [[spectroscopy]] is to characterize the [[spectrum]] of a light source: how much light is emitted at each different wavelength. The most straightforward way to measure a spectrum is to pass the light through a [[monochromator]], an instrument that blocks all of the light ''except'' the light at a certain wavelength (the un-blocked wavelength is set by a knob on the monochromator). Then the intensity of this remaining (single-wavelength) light is measured. The measured intensity directly indicates how much light is emitted at that wavelength. By varying the monochromator's wavelength setting, the full spectrum can be measured. This simple scheme in fact describes how ''some'' spectrometers work.

Fourier-transform spectroscopy is a less intuitive way to get the same information. Rather than allowing only one wavelength at a time to pass through to the detector, this technique lets through a beam containing many different wavelengths of light at once, and measures the ''total'' beam intensity. Next, the beam is modified to contain a ''different'' combination of wavelengths, giving a second data point. This process is repeated many times. Afterwards, a computer takes all this data and works backwards to infer how much light there is at each wavelength.

To be more specific, between the light source and the detector, there is a certain configuration of mirrors that allows some wavelengths to pass through but blocks others (due to [[wave interference]]). The beam is modified for each new data point by moving one of the mirrors; this changes the set of wavelengths that can pass through.

As mentioned, computer processing is required to turn the raw data (light intensity for each mirror position) into the desired result (light intensity for each wavelength). The processing required turns out to be a common algorithm called the [[Fourier transform]] (hence the name, "Fourier-transform spectroscopy"). The raw data is sometimes called an "interferogram". Because of the existing computer equipment requirements, and the ability of light to analyze very small amounts of substance, it is often beneficial to automate many aspects of the sample preparation. The sample can be better preserved and the results are much easier to replicate. Both of these benefits are important, for instance, in testing situations that may later involve legal action, such as those involving drug specimens.<ref>Semiautomated depositor for infrared microspectrometry
http://www.opticsinfobase.org/viewmedia.cfm?uri=as-57-9-1078&seq=0</ref>