Spectral Resolution

The spectral resolution of a spectrograph, or, more generally, of a frequency spectrum, is a measure of its ability to resolve features in the electromagnetic spectrum. It is usually denoted by $\Delta\lambda$, and is closely related to the resolving power of the spectrograph, defined as
$R = \frac,$
where $\Delta\lambda$ is the smallest difference in wavelengths that can be distinguished at a wavelength of $\lambda$. For example, the Space Telescope Imaging Spectrograph (STIS) can distinguish features 0.17 nm apart at a wavelength of 1000 nm, giving it a resolution of 0.17 nm and a resolving power of about 5,900. An example of a high resolution spectrograph is the ''Cryogenic High-Resolution IR Echelle Spectrograph'' (CRIRES+) installed at ESO's Very Large Telescope, which has a spectral resolving power of up to 100,000.

Doppler effect

The spectral resolution can also be expressed in terms of physical quantities, such as velocity; then it describes the difference between velocities $\Delta v$ that can be distinguished through the Doppler effect. Then, the resolution is $\Delta v$ and the resolving power is
$R = \frac,$
where $c$ is the speed of light. The STIS example above then has a spectral resolution of 51 km/s.

IUPAC definition

IUPAC defines resolution in optical spectroscopy as the minimum wavenumber, wavelength or frequency difference between two lines in a spectrum that can be distinguished. Resolving power, ''R'', is given by the transition wavenumber, wavelength or frequency, divided by the resolution.

See also

*Angular resolution
*Resolution (mass spectrometry)

References

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Further reading

*Kim Quijano, J., et al. (2003), ''STIS Instrument Handbook'', Version 7.0, (Baltimore: STScI)
*Frank L. Pedrotti, S.J. (2007), ''Introduction to optics'', 3rd version, (San Francisco)

Spectroscopy