Luminosity function

﻿
Luminosity function

The luminosity function or luminous efficiency function describes the average sensitivity of the human eye to light of different wavelengths. It should not be considered perfectly accurate in every case, but it is a very good representation of human eye sensitivity and it is valuable as a baseline for experimental purposes. It is a standard function established by the Commission Internationale de l'Éclairage (CIE) and may be used to convert radiant energy into luminous (i.e., visible) energy. It also forms the central color matching function in the CIE 1931 color space.

Details

There are actually two luminosity functions in common use. For everyday light levels, the photopic luminosity function best approximates the response of the human eye. For low light levels, the response of the human eye changes, and the scotopic curve applies. The photopic curve is the CIE standard curve used in the CIE 1931 color space.

The luminous flux (or visible energy) in a light source is defined by the photopic luminosity function. The following equation calculates the total luminous flux in a source of light.

:$F=683.002 mathrm\left\{lm/W\right\}cdot int^infin_0 overline\left\{y\right\}\left(lambda\right) J\left(lambda\right) dlambda$

where:$F,$ is the luminous flux in lumens,:$J\left(lambda\right),$ is the power spectral density of the radiation (power per unit wavelength), in watts per metre.:$overline\left\{y\right\}\left(lambda\right)$ (also known as $V\left(lambda\right),$) is the standard luminosity function (which is dimensionless).:$lambda,$ is wavelength in metres.

Formally, the integral is the inner product of the luminosity function with the light spectrum. [cite book | title = Digital Video and HDTV: Algorithms and Interfaces | author = Charles A. Poynton | publisher = Morgan Kaufmann | year = 2003 | isbn = 1558607927 | url = http://books.google.com/books?id=ra1lcAwgvq4C&pg=RA1-PA205&dq=luminance+dot-product&as_brr=0&ei=-vxYR5SVBIyctAOh1czEDw&sig=QcrHfyk-R_b4hKf4YUOYhAT6Sss ] In practice, the functions of wavelength are discretized, and the inner product is computed as an ordinary vector dot product; the CIE distributes standard tables discretized into 5 nm samples from 380 nm to 780 nm. [cite web | url = http://www.cie.co.at/main/freepubs.html | title = CIE Free Documents for Download]

The standard luminosity function is normalized to a peak value of unity at 555 nm (see luminous coefficient). The value of the constant in front of the integral is usually rounded off to 683 lm/W. The small excess fractional value comes from the slight mismatch between the definition of the lumen and the peak of the luminosity function. The lumen is defined to be unity for a radiant energy of 1/683 watt at a frequency of 540 THz, which corresponds to a standard air wavelength of 555.016 nm rather than 555 nm, which is the peak of the luminosity curve. The value of $overline\left\{y\right\}\left(lambda\right)$ is 0.999997 at 555.016 nm, so that a value of 683/0.999997 = 683.002 is the multiplicative constant. [cite book | author=Wyszecki, Günter and Stiles, W.S. | title=Color Science - Concepts and Methods, Quantitative Data and Formulae |edition=2nd edition | publisher=Wiley-Interscience | year=2000 | id =ISBN 0-471-39918-3 ] The number 683 is connected to the modern (1979) definition of the candela, the unit of luminous intensity. [16th Conférence générale des poids et mesures Resolution 3, CR, 100 (1979), and "Metrologia", 16, 56 (1980).] This arbitrary number made the new definition give numbers equivalent to those from the old definition of the candela.

Improvements to the standard

The CIE 1924 photopic $V\left(lambda\right)$ luminosity function, [cite book | author=CIE | title=Commission internationale de l'Eclairage proceedings, 1924 | publisher=Cambridge University Press, Cambridge | year=1926 | id = ] which is included in the CIE 1931 color-matching functions as the "y" function, has long been acknowledged to underestimate the contribution of the blue end of the spectrum to perceived luminance. There have been numerous attempts to improve the standard function, to make it more representative of human vision. Judd in 1951, [cite book | author=Judd, Deane B. and Wyszecki, Günter | title=Color in Business, Science and Industry |edition=3rd edition| publisher=John Wiley | year=1975 | id =ISBN 0-471-45212-2] improved by Vos in 1978, [cite journal | author=Vos, J. J. | title=Colorimetric and photometric properties of a 2° fundamental observer | journal=Color Research and Application | year=1978 | volume=3 | issue=3|pages=125–128|doi=10.1002/col.5080030309] resulted in a function known as CIE $V_M\left(lambda\right)$. [cite journal | author=Stiles, W. S., & Burch, J. M. | title=Interim report to the Commission Internationale de l'Eclairage Zurich 1955, on the National Physical Laboratory's investigation of colour-matching | journal=Optica Acta | year=1955 | volume=2 | pages=168–181] More recently, Sharpe, Stockman, Jagla & Jägle (2005) developed a function consistent with the [http://www.cvrl.org/cones.htm Stockman & Sharpe cone fundamentals] ; [Sharpe, L. T., Stockman, A., Jagla, W., & Jägle, H. (2005). "A luminous efficiency function, V*(λ), for daylight adaptation". Journal of Vision, 5(11), 948-968, ] their curves are plotted in the figure above.

cotopic luminosity

For very low levels of intensity (scotopic vision), the sensitivity of the eye is mediated by rods, not cones, and shifts toward the violet, peaking around 507 nm for young eyes; the sensitivity is equivalent to 1699 lm/W [cite book | title = Light Pollution Handbook | author = Kohei Narisada and Duco Schreuder | publisher = Springer | year = 2004 | isbn = 140202665X] or 1700 lm/W [cite book | title = Handbook of Applied Photometry | author = Casimer DeCusatis | publisher = Springer | year = 1998 | isbn = 1563964163] at this peak.

The standard scotopic luminosity function or $V^prime\left(lambda\right)$ was adopted by the CIE in 1951, based on measurements by Wald (1945) and by Crawford (1949). [http://www.cvrl.org/database/text/lum/scvl.htm]

*Color vision
*A-weighting, the sound equivalent
*Quantum efficiency, the image sensor equivalent

References

* [http://cvision.ucsd.edu/lumindex.htm UCSD Color Vision — tables of luminosity functions]

Wikimedia Foundation. 2010.

Look at other dictionaries:

• luminosity function — noun a) A standard measure of the response of the human eye to light of different wavelengths b) A relative measure of the relationship between stellar magnitude and the distribution of stars between magnitudes …   Wiktionary

• Luminosity function (astronomy) — In astronomy, the luminosity function gives the number of stars or galaxies with a given luminosity. [ [http://www.daviddarling.info/encyclopedia/L/lumfunc.html luminosity function] , David Darling, entry in The Internet Encyclopedia of Science …   Wikipedia

• Planetary nebula luminosity function — (PNLF) is a secondary distance indicator used in astronomy. It makes use of the [O III| [O III] λ5007 forbidden line found in all planetary nebula which are members of the old stellar populations (Population… …   Wikipedia

• Luminosity — has different meanings in several different fields of science.In photometry and color imagingIn photometry, luminosity is sometimes incorrectly used to refer to luminance, which is the density of luminous intensity in a given direction. The SI… …   Wikipedia

• Initial mass function — The initial mass function (IMF) is an empirical function that describes the mass distribution (the histogram of stellar masses) of a population of stars in terms of their theoretical initial mass (the mass they were formed with). The properties… …   Wikipedia

• Milky Way Galaxy — Large spiral galaxy (roughly 150,000 light years in diameter) that contains Earth s solar system. It includes the multitude of stars whose light is seen as the Milky Way, the irregular luminous band that encircles the sky defining the plane of… …   Universalium

• Malmquist bias — For other uses of Malmquist, see Malmquist (disambiguation). The Malmquist bias refers to an effect in observational astronomy which leads to the preferential detection of intrinsically bright objects. It was first popularized in 1922 by Swedish… …   Wikipedia

• Cosmic distance ladder — * Light green boxes: Technique applicable to star forming galaxies. * Light blue boxes: Technique applicable to Population II galaxies. * Light Purple boxes: Geometric distance technique. * Light Red box: The planetary nebula luminosity function… …   Wikipedia

• star — starless, adj. /stahr/, n., adj., v., starred, starring. n. 1. any of the heavenly bodies, except the moon, appearing as fixed luminous points in the sky at night. 2. Astron. any of the large, self luminous, heavenly bodies, as the sun, Polaris,… …   Universalium

• Extragalactic distance scale — The extragalactic distance scale is a series of techniques used today by astronomers to determine the distance of cosmological bodies (beyond our own galaxy) not easily obtained with traditional methods. Some procedures utilize properties of… …   Wikipedia