luminosity function

This response of the eye is represented by the luminosity function.

One then fits the observed luminosity function to some standard law.

The curve which measures the response of the human eye to light is a defined standard, known as the luminosity function.

The figure to the right shows two luminosity functions for an example population of stars that is magnitude-limited.

In reality, individual eyes vary slightly in their luminosity functions.

There are two luminosity functions in common use.

The weighting factor is known as the luminosity function.

Malmquist bias drastically changes the shape of the luminosity function.

Formally, the integral is the inner product of the luminosity function with the light spectrum.

Most mammals other than primates have the same luminosity function as people with protanopia.

The luminosity function falls to zero for wavelengths outside the visible spectrum.

The luminosity function (Φ) is independent of the distance (r).

An oscilloscope trace can be any color without loss of information, so a phosphor with Luminosity function is usually used.

For everyday light levels, the photopic luminosity function best approximates the response of the human eye.

There is no universal globular cluster luminosity function that applies to all galaxies.

Observations of the faintest objects will provide a more complete view of the stellar luminosity function.

(also known as ) is the standard luminosity function (which is dimensionless).

In astronomy, the luminosity function gives the number of stars or galaxies per luminosity interval.

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

The formula reflects the luminosity function: green light contributes the most to the intensity perceived by humans, and blue light the least.

In practice, the integral is replaced by a sum over discrete wavelengths for which tabulated values of the luminosity function are available.

The standardized model of the eye's response to light as a function of wavelength is given by the luminosity function.

The standard luminosity function is normalized to a peak value of unity at 555 nm (see luminous coefficient).

In photometry, the radiant power at each wavelength is weighted by a luminosity function that models human brightness sensitivity.

The galaxy luminosity function may have different parameters for different populations and environments; it is not a universal function.