Brightness

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The brightness distance (DL) and angular distance are distance definitions based on the physical properties of astronomical objects - on a given object's radiation stream and on the physical size of the object. The brightness distance is closely related to the distance of the motion that we can not directly measure, but we can calculate it for the object of redness with, for the given Hubble constant and the components of the universe Ωm0 and Ωλ0 at the moment t0. We can measure the brightness of a specific object using objects called standard candles. The most spectacular success was achieved with the use of supernova type Ia in 1998 (group Saul Perlmutter). The measured brightness distances from the supernovae allowed us to determine the components of the Universe Ωm0 and Ωλ0. Surprisingly, the result of the study was the finding of a non-permanent cosmological constant.

The relationship between the brightness, the angular distance and other distances from cosmological scales is described in the co-ordinate coordinates.

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