(1) sample size and selection: as you reference in the paper, there have been several recent studies with large sample sizes that look at the surface brightness profiles of nearby galaxies. It is not clear that analysis of an additional 15 galaxies is significant in this context. And, furthermore, the specific galaxies included in this study, many of which are highly inclined, are neither optimized for the project (in fact, they are poorly suited for this type of analysis due to their small axial ratios) nor a random (statistical) sample. We do have optical (B and R) images available for almost all of the EDGES galaxies at this point. Would it be possible to extend the sample size to include all of the GALEX sub-set (approximately 40 galaxies)? I realize that this would be significantly more work. While my optical images have been masked and edited, we would need to mask the GALEX data, and also pull the infrared data from the archives. Nonetheless, I think it is worth thinking about the impact of the paper: a statistical sample would be more significant. At the very least, we should mention that it would be possible to extend this work to a larger sub-set of the EDGES sample... ** The heart of this paper is the SED fitting and the inferred radial star formation histories, not the surface brightness profiles. By no means do I think this work can compete with or supersede other, larger efforts. I included a section on surface brightness because it seemed appropriate and a nice way to showcase the data. I looked into using your B and R data. As expected, they are much shallower than my WIRO data, and since one of the main goals is to characterize the outskirts I decided to not utilize your imaging. I have added a note to the text about extending this work to a larger subset of the EDGES sample. (2) psf issues: It is not clear that the annuli represent independent measurements for the small and/or edge-on systems. "Beam smearing" is particularly a problem for highly inclined galaxies and could significantly effect your derived colors. Have you considered the effect of the psf for the various data sets? For the small edge-on systems, where most of the light along the minor axis is contaminated by the psf, you might want to consider using small circular apertures measured along the major axis only. (You could try this analysis for one or two of the worst case scenarios, such as UGC07301, to see if it makes any difference in the radial color plots). In any event, the paper needs to acknowledge the effect of the psf on surface brightness profiles and colors. ** Good point. I've done your suggested analysis and added some text and a figure to demonstrate that the impact is not large. (3) robustness of the analysis: I agree with your approach of using a limited suite of star formation histories to match the observed SEDs, as many SFHs are degenerate in this parameter space. However, the paper would be significantly improved if there was more discussion about the possible degeneracies. Would adding a 3rd (intermediate-age) stellar population make much of a difference in terms of the derived ages of the dominant (recent) stellar population? Are the radial gradients in stellar metallicities to be believed? Overall, how robust is this analysis? ** CIGALE currently allows for a single exponential SFH, a double exponential SFH, and a delayed SFH, so it's not straightforward to analyze a triple exponential SFH. However, I have modified Figure 6 to show the similarity in the tau values for the main stellar population under both a single and a double exponential SFH. ** I have carried out a Monte Carlo-type analysis to assess the robustness of the fitted parameters. The metallicity is the least reliable output. I have removed the figure on metallicity and extinction. Concerns about the data analysis: - how did you separate the light from NGC4485 and NGC4490? - are you concerned about systemics introduced by poor sky subtraction in any of the data sets? ** Good points. I have added some text that explains in the analysis I edited the overlap region between 4485 and 4490. Fortunately this region is fractionally small compared to the total areas within the outermost elliptical annuli (1/4th for N4485 and 1/8th for N4490). ** I spent a lot of time looking into sky subtraction. In fact, I revised my initial approach, which was to edit away all stars near the galaxy outskirts where I placed sky apertures. I quickly realized that approach artificially underestimates the sky level for my aperture photometry, since I wasn't equally ruthless in my star editing for foreground stars superposed on top of the galaxy. On the minor detail side: para 1, section 5.1: usually b/a is quoted, not a/b ** Fixed. Tables - I know that this paper is mainly about radial profiles, but I assume that you also derived integrated fluxes for each galaxy at each passband. You may wish to include the integrated fluxes in a table, and reference as to whether or not these newly measured integrated fluxes agree with the LVL published values. ** I have added a table of the fluxes within the 1.50 2a_25x2b_25 ellipses. For the subset of the sample that has published data (9 galaxies at 7 wavelengths), these fluxes agree quite well with published values: the average ratio of my fluxes to literature fluxes is 0.98+/-0.02. Two notable exceptions are for the GALEX measurements of N4625, a known XUV galaxy with extended UV emission (Thilker et al. 2007).