De Vaucouleur's law
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In astrophysics, de Vaucouleurs' law describes the surface luminosity profile of an elliptical galaxy as a function of radius R
- lnI(R) = lnI0 − kR1 / 4
By defining Re as the radius of the isophote containing half the luminosity (i.e., the radius of the inner disk contributing half the brightness of the galaxy), de Vaucouleur's law may be written as
![\ln I(R) = \ln I_{e} + 7.67 \left[ 1 - \left( \frac{R}{R_{e}} \right)^{1/4} \right]](../../../../math/0/3/a/03aae9027dda4fb97c2f56bf9246815b.png)
where Ie is the surface luminosity at Re.
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