De Vaucouleurs’ law fits (red and dashed green lines) to the surface brightness μ profile of metal-rich (red symbols with red fit line) and metal-poor (green symbols with dashed green fit line) stars in the halo of NGC 5128. We show μ in magnitudes per square arcsecond of the NGC 5128 RGB stars as a function of (R/R_eff)^1/4, where R is the ellipticity corrected distance from the center of the galaxy and R_eff = 5.6 kpc (Dufour et al. 1979). Within this plane, μ versus (R/R_eff)^1/4, we use the least squares method to fit the data and solve for the slope a and y-intercept μ₀ of de Vaucouleurs’ profile (de Vaucouleurs 1948) μ = a (R/R_eff)^1/4 + μ₀, where R_eff is fixed at 5.6 kpc. We correct for incompleteness by doubling the number of sources in our VIMOS field. Note that we have had to use only one distance bin for the metal-poor stars in VIMOS (due to small number statistics) whereas the metal-rich are numerous enough to be placed into 5 distance bins across the VIMOS field. Poisson distribution errors are included, although none appear for the red metal-rich symbols (fit by the red line) because the errors are of order of the same size as the symbol size. See Sect. 5.2 for a full discussion of this figure. (See the electronic edition of the journal for a color version of this figure.)