Encyclopedia … combined with a great Buyer's Guide!

Luminosity Functions

Definition: functions describing the spectral sensitivity of the human eye

German: Empfindlichkeitskurven

Category: vision, displays and imagingvision, displays and imaging


Cite the article using its DOI: https://doi.org/10.61835/ngk

Get citation code: Endnote (RIS) BibTex plain textHTML

Luminosity functions describe the spectral sensitivity of the human eye. Official versions of those have been published by CIE, the Commission Internationale de l'Éclairage (International Commission on Illumination); they are based on the average perceptions of human beings with healthy eyes under well-defined experimental conditions (for the CIE standard observer).

Importantly, the spectral dependence of the sensitivity of the human eye depends on the lighting conditions, more precisely on the incoming luminance. For luminance values below approximately 10−3 cd/m2, one has scotopic vision, which is monochrome. At better illumination conditions with a luminance of at least a couple of cd/m2, one has photopic vision with good color perception. The intermediate regime is called mesopic vision. For more details, see the article on scotopic and photopic vision.

There are substantially different luminosity functions for scotopic and photopic vision.

Luminosity Function for Photopic Vision

For photopic vision, i.e., at sufficiently highlighted levels, the human eye uses the cone receptors, of which it has three different kinds (L, M and S). Their output signals are combined to determine the total received brightness.

In the simple case of monochromatic light with some wavelength <$\lambda$>, the luminous flux produced by a light source can be calculated as 683 lm/W times the photopic luminosity function value y<$(\lambda )$> times the radiant flux (optical power). For polychromatic light, the luminous flux obtains contributions for all the spectral components, and can thus be calculated as a spectral integral:

$${\Phi _{\rm{v}}} = 683\;{\rm{lm/W}} \cdot \int {\bar y(\lambda )\;} {\Phi _{\rm{e}}}(\lambda )\;{\rm{d}}\lambda $$

where <$\Phi_\textrm{e}(\lambda )$> is the spectral radiant flux entering the eye (within the opening of the iris) and <$\Phi_\textrm{v}(\lambda )$> the resulting luminous flux. Figure 1 shows the values of the photopic luminosity function.

photopic response
Figure 1: The photopic response function according to CIE. Data source: Colour & Vision Research Laboratory of the University College London, page on luminous efficiency functions.

Losses of optical energy on the way from the cornea to the retina are included in the luminosity function. Due to aging of the eye, particularly shorter-wavelength components will experience increasing absorption and scattering losses, eventually resulting in lower luminosities than predicted by that function.

The luminosity function is scaled such that its maximum value, reached at a wavelength of approximately 555 nm, is unity; that results in the maximum response of 683 lm/W. For other wavelengths, and for any mixtures of different wavelengths, lower values result. In particular, white light sources, the output of which needs to contain some red and blue light, are more limited than green light sources in terms of luminous efficacy, even if the conversion from electrical energy to luminous flux is highly efficient.

Luminosity Function for Scotopic Vision

Scotopic vision occurs at low light levels, where only the rod photoreceptors are involved because the cones are unable to provide sufficiently strong signals. In this regime, a different luminosity function called <$V'(\lambda )$> (defined by CIE in 1951) must be applied. That function is peaked at 507 nm, and is again normalized to be unity at that point. The luminous flux resulting from a certain radiant flux can be calculated as

$${\Phi _{\rm{v}}} = 1700\;{\rm{lm/W}} \cdot \int {V'(\lambda )\;} {\Phi _{\rm{e}}}(\lambda )\;{\rm{d}}\lambda $$

where <$\Phi (\lambda )$> is again the spectral radiant flux. (Figure 2 shows the values of the scotopic luminosity function.) One can see that much less light is required in that regime to obtain a significant light perception. However, color vision is then not possible.

photopic response
Figure 2: The scotopic response function according to CIE (1951). Data source: Colour & Vision Research Laboratory of the University College London, page on luminous efficiency functions.

Determination of Luminosity Functions

For determining luminosity functions, relatively complicated procedures are required, where it is tested how a larger group of individuals reacts to certain types of optical stimulus. One of the used methods is heterochromatic flicker photometry. Here, one essentially adjusts the relative powers of two signals with different wavelengths, to which the eye is exposed alternatingly, such that no flicker is observed.

Applications of Luminosity Functions

Based on the known luminosity functions and the known optical spectrum of a light source, one can calculate how bright a light source or an illuminated object can be perceived. For example, that allows one to calculate the luminous efficacy and efficiency of a light source if its efficiency for the conversion from electrical power to light power is known.

One may also use luminosity functions for comparing the apparent brightness of monochromatic light sources at a different wavelengths – for example, of laser pointers. Note that the ratio of luminosity values at two different wavelengths can be very different between scotopic and photopic vision. For example, while for photopic vision a 650-nm laser pointer can achieve at least more than 10% of the brightness of a green laser pointer with the same output power, the difference is much larger for scotopic vision, where the sensitivity at 650 nm becomes very small.

Luminosity Functions of Galaxies

An entirely different meaning of the term luminosity function is used in astronomy. With optical telescopes and specific photodetectors, one measures luminosities (in the sense of spectral intensities) of many galaxies for different spectral bands. One can then define a luminosity function which reflects the number distribution of many galaxies over certain intervals of that kind of luminosity.

More to Learn

Encyclopedia articles:

Questions and Comments from Users

Here you can submit questions and comments. As far as they get accepted by the author, they will appear above this paragraph together with the author’s answer. The author will decide on acceptance based on certain criteria. Essentially, the issue must be of sufficiently broad interest.

Please do not enter personal data here. (See also our privacy declaration.) If you wish to receive personal feedback or consultancy from the author, please contact him, e.g. via e-mail.

Spam check:

By submitting the information, you give your consent to the potential publication of your inputs on our website according to our rules. (If you later retract your consent, we will delete those inputs.) As your inputs are first reviewed by the author, they may be published with some delay.


Share this with your network:

Follow our specific LinkedIn pages for more insights and updates: