The luminosity deficit in core galaxies may be estimated by taking the integrated difference between a model of the prescoured profile and the observed surface brightness profile. Shown here is an example for the galaxy NGC 4486 (M87). Here, we model the surface brightness profile with the Nuker Law, shown in solid blue (see Equation (1)). Our estimate for the prescoured profile, shown in dashed–dotted purple, is a power law with inner logarithmic slope equal to that at the break radius (R_b, see Equation (3)). The break radius indicates the distance from the galaxy center where the profile transitions from the shallow inner region to the steep outer region and represents the size of the core.