The surface brightness profiles of the galaxies were made by binning the image data with a minimum size of 3 pixels, equivalent to the seeing, exponentially growing from the center in the radial and vertical direction. We do this to smooth peaks and irregularities in the profile, but also so that in the outer parts, where the influence of the noise grows larger, more area contributes to the mean intensity. This is to retain an approximately constant overall and higher S/N ratio, thus making it able to follow the profiles further out [De Grijs and Peletier1997]. If a bin possessed a partial mask, the mask values were ignored and only the real data was used to calculate the average intensity. The vertical position of the bin was determined by weighting all used datapoints to their position. See figures 2 and 3 for examples of radial and vertical profiles.