Radiometry

 ( Measurement ) 

Radiometry is a set of techniques for measurement electromagnetic radiation, including visible light. Radiometric techniques in optics characterize the distribution of the radiation's power in space, as opposed to photometric techniques, which characterize the light's interaction with the human eye. The fundamental difference between radiometry and photometry is that radiometry gives the entire optical radiation spectrum, while photometry is limited to the visible spectrum. Radiometry is distinct from quantum optics techniques such as photon counting.

The use of to determine the temperature of objects and gasses by measuring radiation flux is called pyrometry. Handheld pyrometer devices are often marketed as infrared thermometers.

Radiometry is important in astronomy, especially radio astronomy, and plays a significant role in Earth remote sensing. The measurement techniques categorized as radiometry in optics are called photometry in some astronomical applications, contrary to the optics usage of the term.

Spectroradiometry is the measurement of absolute radiometric quantities in narrow bands of wavelength.

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Radiometric quantities

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Integral and spectral radiometric quantities Integral quantities (like radiant flux) describe the total effect of radiation of all or frequency, while spectral quantities (like spectral power) describe the effect of radiation of a single wavelength or frequency . To each integral quantity there are corresponding spectral quantities, defined as the quotient of the integrated quantity by the range of frequency or wavelength considered. For example, the radiant flux Φ_e corresponds to the spectral power Φ_e, and Φ_e,.

Getting an integral quantity's spectral counterpart requires a limit transition. This comes from the idea that the precisely requested wavelength photon existence probability is zero. Let us show the relation between them using the radiant flux as an example:

Integral flux, whose unit is watt: $$\backslash Phi\_\backslash mathrm\{e\}.$$ Spectral flux by wavelength, whose unit is : $$\backslash Phi\_\{\backslash mathrm\{e\},\backslash lambda\}\; =\; \{d\backslash Phi\_\backslash mathrm\{e\}\; \backslash over\; d\backslash lambda\},$$ where $d\backslash Phi\_\backslash mathrm\{e\}$ is the radiant flux of the radiation in a small wavelength interval $\backslash lambda$. The area under a plot with wavelength horizontal axis equals to the total radiant flux.

Spectral flux by frequency, whose unit is : $$\backslash Phi\_\{\backslash mathrm\{e\},\backslash nu\}\; =\; \{d\backslash Phi\_\backslash mathrm\{e\}\; \backslash over\; d\backslash nu\},$$ where $d\backslash Phi\_\backslash mathrm\{e\}$ is the radiant flux of the radiation in a small frequency interval $\backslash nu$. The area under a plot with frequency horizontal axis equals to the total radiant flux.

The spectral quantities by wavelength and frequency are related to each other, since the product of the two variables is the speed of light ($\backslash lambda\; \backslash cdot\; \backslash nu\; =\; c$):

$\backslash Phi\_\{\backslash mathrm\{e\},\backslash lambda\}\; =\; \{c\; \backslash over\; \backslash lambda^2\}\; \backslash Phi\_\{\backslash mathrm\{e\},\backslash nu\},$ or $\backslash Phi\_\{\backslash mathrm\{e\},\backslash nu\}\; =\; \{c\; \backslash over\; \backslash nu^2\}\; \backslash Phi\_\{\backslash mathrm\{e\},\backslash lambda\},$ or $\backslash lambda\; \backslash Phi\_\{\backslash mathrm\{e\},\backslash lambda\}\; =\; \backslash nu\; \backslash Phi\_\{\backslash mathrm\{e\},\backslash nu\}.$

The integral quantity can be obtained by the spectral quantity's integration:

$$\backslash Phi\_\backslash mathrm\{e\}\; =\; \backslash int\_0^\backslash infty\; \backslash Phi\_\{\backslash mathrm\{e\},\backslash lambda\}\backslash ,\; d\backslash lambda\; =\; \backslash int\_0^\backslash infty\; \backslash Phi\_\{\backslash mathrm\{e\},\backslash nu\}\backslash ,\; d\backslash nu\; =\; \backslash int\_0^\backslash infty\; \backslash lambda\; \backslash Phi\_\{\backslash mathrm\{e\},\backslash lambda\}\backslash ,\; d\; \backslash ln\; \backslash lambda\; =\; \backslash int\_0^\backslash infty\; \backslash nu\; \backslash Phi\_\{\backslash mathrm\{e\},\backslash nu\}\backslash ,\; d\; \backslash ln\; \backslash nu.$$

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See also

• Reflectivity
• Microwave radiometer
• Measurement of ionizing radiation
• Radiometric calibration
• Radiometric resolution

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External links

• Radiometry and photometry FAQ Professor Jim Palmer's Radiometry FAQ page (The University of Arizona College of Optical Sciences).

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