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Radiometry
Radiometry is a set of techniques for measuring 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. Radiometry is distinct from quantum techniques such as photon counting.
The use of radiometers 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.^{[1]}
Contents
Radiometric quantities
Quantity | Unit | Dimension | Notes | |||||
---|---|---|---|---|---|---|---|---|
Name | Symbol^{[nb 1]} | Name | Symbol | Symbol | ||||
Radiant energy | Q_{e}^{[nb 2]} | joule | J | M⋅L^{2}⋅T^{−2} | Energy of electromagnetic radiation. | |||
Radiant energy density | w_{e} | joule per cubic metre | J/m^{3} | M⋅L^{−1}⋅T^{−2} | Radiant energy per unit volume. | |||
Radiant flux | Φ_{e}^{[nb 2]} | watt | W or J/s | M⋅L^{2}⋅T^{−3} | Radiant energy emitted, reflected, transmitted or received, per unit time. This is sometimes also called "radiant power". | |||
Spectral flux | Φ_{e,ν}^{[nb 3]} or Φ_{e,λ}^{[nb 4]} |
watt per hertz or watt per metre |
W/Hz or W/m |
M⋅L^{2}⋅T^{−2} or M⋅L⋅T^{−3} |
Radiant flux per unit frequency or wavelength. The latter is commonly measured in W⋅sr^{−1}⋅m^{−2}⋅nm^{−1}. | |||
Radiant intensity | I_{e,Ω}^{[nb 5]} | watt per steradian | W/sr | M⋅L^{2}⋅T^{−3} | Radiant flux emitted, reflected, transmitted or received, per unit solid angle. This is a directional quantity. | |||
Spectral intensity | I_{e,Ω,ν}^{[nb 3]} or I_{e,Ω,λ}^{[nb 4]} |
watt per steradian per hertz or watt per steradian per metre |
W⋅sr^{−1}⋅Hz^{−1} or W⋅sr^{−1}⋅m^{−1} |
M⋅L^{2}⋅T^{−2} or M⋅L⋅T^{−3} |
Radiant intensity per unit frequency or wavelength. The latter is commonly measured in W⋅sr^{−1}⋅m^{−2}⋅nm^{−1}. This is a directional quantity. | |||
Radiance | L_{e,Ω}^{[nb 5]} | watt per steradian per square metre | W⋅sr^{−1}⋅m^{−2} | M⋅T^{−3} | Radiant flux emitted, reflected, transmitted or received by a surface, per unit solid angle per unit projected area. This is a directional quantity. This is sometimes also confusingly called "intensity". | |||
Spectral radiance | L_{e,Ω,ν}^{[nb 3]} or L_{e,Ω,λ}^{[nb 4]} |
watt per steradian per square metre per hertz or watt per steradian per square metre, per metre |
W⋅sr^{−1}⋅m^{−2}⋅Hz^{−1} or W⋅sr^{−1}⋅m^{−3} |
M⋅T^{−2} or M⋅L^{−1}⋅T^{−3} |
Radiance of a surface per unit frequency or wavelength. The latter is commonly measured in W⋅sr^{−1}⋅m^{−2}⋅nm^{−1}. This is a directional quantity. This is sometimes also confusingly called "spectral intensity". | |||
Irradiance | E_{e}^{[nb 2]} | watt per square metre | W/m^{2} | M⋅T^{−3} | Radiant flux received by a surface per unit area. This is sometimes also confusingly called "intensity". | |||
Spectral irradiance | E_{e,ν}^{[nb 3]} or E_{e,λ}^{[nb 4]} |
watt per square metre per hertz or watt per square metre, per metre |
W⋅m^{−2}⋅Hz^{−1} or W/m^{3} |
M⋅T^{−2} or M⋅L^{−1}⋅T^{−3} |
Irradiance of a surface per unit frequency or wavelength. The former is commonly measured in 10^{−22} W⋅m^{−2}⋅Hz^{−1}, known as solar flux unit, and the latter in W⋅m^{−2}⋅nm^{−1}.^{[nb 6]} This is sometimes also confusingly called "spectral intensity". | |||
Radiosity | J_{e}^{[nb 2]} | watt per square metre | W/m^{2} | M⋅T^{−3} | Radiant flux leaving (emitted, reflected and transmitted by) a surface per unit area. This is sometimes also confusingly called "intensity". | |||
Spectral radiosity | J_{e,ν}^{[nb 3]} or J_{e,λ}^{[nb 4]} |
watt per square metre per hertz or watt per square metre, per metre |
W⋅m^{−2}⋅Hz^{−1} or W/m^{3} |
M⋅T^{−2} or M⋅L^{−1}⋅T^{−3} |
Radiosity of a surface per unit frequency or wavelength. The latter is commonly measured in W⋅m^{−2}⋅nm^{−1}. This is sometimes also confusingly called "spectral intensity". | |||
Radiant exitance | M_{e}^{[nb 2]} | watt per square metre | W/m^{2} | M⋅T^{−3} | Radiant flux emitted by a surface per unit area. This is the emitted component of radiosity. "Radiant emittance" is an old term for this quantity. This is sometimes also confusingly called "intensity". | |||
Spectral exitance | M_{e,ν}^{[nb 3]} or M_{e,λ}^{[nb 4]} |
watt per square metre per hertz or watt per square metre, per metre |
W⋅m^{−2}⋅Hz^{−1} or W/m^{3} |
M⋅T^{−2} or M⋅L^{−1}⋅T^{−3} |
Radiant exitance of a surface per unit frequency or wavelength. The latter is commonly measured in W⋅m^{−2}⋅nm^{−1}. "Spectral emittance" is an old term for this quantity. This is sometimes also confusingly called "spectral intensity". | |||
Radiant exposure | H_{e} | joule per square metre | J/m^{2} | M⋅T^{−2} | Radiant energy received by a surface per unit area, or equivalently irradiance of a surface integrated over time of irradiation. This is sometimes also called "radiant fluence". | |||
Spectral exposure | H_{e,ν}^{[nb 3]} or H_{e,λ}^{[nb 4]} |
joule per square metre per hertz or joule per square metre, per metre |
J⋅m^{−2}⋅Hz^{−1} or J/m^{3} |
M⋅T^{−1} or M⋅L^{−1}⋅T^{−2} |
Radiant exposure of a surface per unit frequency or wavelength. The latter is commonly measured in J⋅m^{−2}⋅nm^{−1}. This is sometimes also called "spectral fluence". | |||
Hemispherical emissivity | ε | 1 | Radiant exitance of a surface, divided by that of a black body at the same temperature as that surface. | |||||
Spectral hemispherical emissivity | ε_{ν} or ε_{λ} |
1 | Spectral exitance of a surface, divided by that of a black body at the same temperature as that surface. | |||||
Directional emissivity | ε_{Ω} | 1 | Radiance emitted by a surface, divided by that emitted by a black body at the same temperature as that surface. | |||||
Spectral directional emissivity | ε_{Ω,ν} or ε_{Ω,λ} |
1 | Spectral radiance emitted by a surface, divided by that of a black body at the same temperature as that surface. | |||||
Hemispherical absorptance | A | 1 | Radiant flux absorbed by a surface, divided by that received by that surface. This should not be confused with "absorbance". | |||||
Spectral hemispherical absorptance | A_{ν} or A_{λ} |
1 | Spectral flux absorbed by a surface, divided by that received by that surface. This should not be confused with "spectral absorbance". | |||||
Directional absorptance | A_{Ω} | 1 | Radiance absorbed by a surface, divided by the radiance incident onto that surface. This should not be confused with "absorbance". | |||||
Spectral directional absorptance | A_{Ω,ν} or A_{Ω,λ} |
1 | Spectral radiance absorbed by a surface, divided by the spectral radiance incident onto that surface. This should not be confused with "spectral absorbance". | |||||
Hemispherical reflectance | R | 1 | Radiant flux reflected by a surface, divided by that received by that surface. | |||||
Spectral hemispherical reflectance | R_{ν} or R_{λ} |
1 | Spectral flux reflected by a surface, divided by that received by that surface. | |||||
Directional reflectance | R_{Ω} | 1 | Radiance reflected by a surface, divided by that received by that surface. | |||||
Spectral directional reflectance | R_{Ω,ν} or R_{Ω,λ} |
1 | Spectral radiance reflected by a surface, divided by that received by that surface. | |||||
Hemispherical transmittance | T | 1 | Radiant flux transmitted by a surface, divided by that received by that surface. | |||||
Spectral hemispherical transmittance | T_{ν} or T_{λ} |
1 | Spectral flux transmitted by a surface, divided by that received by that surface. | |||||
Directional transmittance | T_{Ω} | 1 | Radiance transmitted by a surface, divided by that received by that surface. | |||||
Spectral directional transmittance | T_{Ω,ν} or T_{Ω,λ} |
1 | Spectral radiance transmitted by a surface, divided by that received by that surface. | |||||
Hemispherical attenuation coefficient | μ | reciprocal metre | m^{−1} | L^{−1} | Radiant flux absorbed and scattered by a volume per unit length, divided by that received by that volume. | |||
Spectral hemispherical attenuation coefficient | μ_{ν} or μ_{λ} |
reciprocal metre | m^{−1} | L^{−1} | Spectral radiant flux absorbed and scattered by a volume per unit length, divided by that received by that volume. | |||
Directional attenuation coefficient | μ_{Ω} | reciprocal metre | m^{−1} | L^{−1} | Radiance absorbed and scattered by a volume per unit length, divided by that received by that volume. | |||
Spectral directional attenuation coefficient | μ_{Ω,ν} or μ_{Ω,λ} |
reciprocal metre | m^{−1} | L^{−1} | Spectral radiance absorbed and scattered by a volume per unit length, divided by that received by that volume. | |||
See also: SI · Radiometry · Photometry |
- ^ Standards organizations recommend that radiometric quantities should be denoted with suffix "e" (for "energetic") to avoid confusion with photometric or photon quantities.
- ^ ^{a} ^{b} ^{c} ^{d} ^{e} Alternative symbols sometimes seen: W or E for radiant energy, P or F for radiant flux, I for irradiance, W for radiant exitance.
- ^ ^{a} ^{b} ^{c} ^{d} ^{e} ^{f} ^{g} Spectral quantities given per unit frequency are denoted with suffix "ν" (Greek)—not to be confused with suffix "v" (for "visual") indicating a photometric quantity.
- ^ ^{a} ^{b} ^{c} ^{d} ^{e} ^{f} ^{g} Spectral quantities given per unit wavelength are denoted with suffix "λ" (Greek).
- ^ ^{a} ^{b} Directional quantities are denoted with suffix "Ω" (Greek).
- ^ NOAA / Space Weather Prediction Center includes a definition of the solar flux unit (SFU).
Integral and spectral radiometric quantities
Integral quantities (like radiant flux) describe the total effect of radiation of all wavelengths or frequencies, while spectral quantities (like spectral power) describe the effect of radiation of a single wavelength λ or frequency ν. To each integral quantity there are corresponding spectral quantities, for example the radiant flux Φ_{e} corresponds to the spectral power Φ_{e,λ} and Φ_{e,ν}.
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 W:
- <math>\Phi_\mathrm{e}.</math>
Spectral flux by wavelength, whose unit is W/m:
- <math>\Phi_{\mathrm{e},\lambda} = {\mathrm{d}\Phi_\mathrm{e} \over \mathrm{d}\lambda},</math>
where <math>\mathrm{d}\Phi_\mathrm{e}</math> is the radiant flux of the radiation in a small wavelength interval [λ, λ + dλ]. The area under a plot with wavelength horizontal axis equals to the total radiant flux.
Spectral flux by frequency, whose unit is W/Hz:
- <math>\Phi_{\mathrm{e},\nu} = {\mathrm{d}\Phi_\mathrm{e} \over \mathrm{d}\nu},</math>
where <math>\mathrm{d}\Phi_\mathrm{e}</math> is the radiant flux of the radiation in a small frequency interval [ν, ν + dν]. The area under a plot with frequency horizontal axis equals to the total radiant flux.
Spectral flux multiplied by wavelength or frequency, whose unit is W, i.e. the same as the integral quantity:
- <math>\lambda \Phi_{\mathrm{e},\lambda} = \nu \Phi_{\mathrm{e},\nu}.</math>
The area under a plot with logarithmic wavelength or frequency horizontal axis equals to the total radiant flux.
The spectral quantities by wavelength λ and frequency ν are related by equations featuring the speed of light c:
- <math>\Phi_{\mathrm{e},\lambda} = {c \over \lambda^2} \Phi_{\mathrm{e},\nu},</math>
- <math>\Phi_{\mathrm{e},\nu} = {c \over \nu^2} \Phi_{\mathrm{e},\lambda},</math>
- <math>\lambda = {c \over \nu}.</math>
The integral quantity can be obtained by the spectral quantity's integration:
- <math>\Phi_\mathrm{e} = \int_0^\infty \Phi_{\mathrm{e},\lambda}\, \mathrm{d}\lambda = \int_0^\infty \Phi_{\mathrm{e},\nu}\, \mathrm{d}\nu = \int_0^\infty \lambda \Phi_{\mathrm{e},\lambda}\, \mathrm{d} \ln \lambda = \int_0^\infty \nu \Phi_{\mathrm{e},\nu}\, \mathrm{d} \ln \nu.</math>
See also
References
- ^ Leslie D. Stroebel & Richard D. Zakia (1993). Focal Encyclopedia of Photography (3rd ed.). Focal Press. p. 115. ISBN 0-240-51417-3.
External links
- Radiometry and photometry FAQ Professor Jim Palmer's Radiometry FAQ page (The University of Arizona College of Optical Sciences).