Luminosity distance

Astronomical measurement in mathematics

Luminosity distance DL is defined in terms of the relationship between the absolute magnitude M and apparent magnitude m of an astronomical object. M = m − 5 log 10 ⁡ D L 10 pc {\displaystyle M=m-5\log _{10}{\frac {D_{L}}{10\,{\text{pc}}}}\!\,} which gives: D L = 10 ( m − M) 5 + 1 {\displaystyle D_{L}=10^{{\frac {(m-M)}{5}}+1}} where DL is measured in parsecs. For nearby objects (say, in the Milky Way) the luminosity distance gives a good approximation to the natural notion of distance in Euclidean space.

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