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FWHM

Atmospheric Research Center

Full Width

FWHM

Astronomy

Full Width At Half Maximum

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FWHM

Full width at half maximum

In a distribution, full width at half maximum (FWHM) is the difference between the two values of the independent variable at which the dependent variable

Scherrer equation

{\displaystyle \beta } is the line broadening at half the maximum intensity (FWHM), after subtracting the instrumental line broadening, in radians. This quantity

Gaussian function

full width at half maximum (FWHM) of the peak according to FWHM = 2 2 ln ⁡ 2 c ≈ 2.35482 c . {\displaystyle {\text{FWHM}}=2{\sqrt {2\ln 2}}\,c\approx

Beam diameter

the beam width are in common use: D4σ, 10/90 or 20/80 knife-edge, 1/e2, FWHM, and D86. The beam width can be measured in units of length at a particular

X-ray photoelectron spectroscopy

band has a FWHM of 0.43 eV, centered on 1,486.7 eV (E/ΔE = 3,457). If magnesium K-alpha X-rays are used, the intrinsic energy band has a FWHM of 0.36 eV

Spectral width

(FWHM). This is the same convention used in bandwidth, defined as the frequency range where power drops by less than half (at most −3 dB). The FWHM method

Gaussian beam

maximum (FWHM) of the intensity distribution at that position according to: w ( z ) = FWHM ( z ) 2 ln ⁡ 2 . {\displaystyle w(z)={\frac {{\text{FWHM}}(z)}{\sqrt

Astronomical seeing

astronomical seeing conditions at an observatory: The full width at half maximum (FWHM) of the seeing disc r0 (the size of a typical "lump" of uniform air within

Half flux diameter

maximum (FWHM), but is a more robust measurement especially for stars out of focus. For a perfect Gaussian shaped star image, both the FWHM and half flux

Cosmic microwave background

greater than half of its maximal value (the "full width at half maximum", or FWHM) over an interval of 115,000 years. By this measure, decoupling took place