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tokens: bin with observed rest-frame wavelength. Here, we supplement the FUV and NUV results from this study with data used in our previous study (Taylor-Mager et al. 2007 ), which includes HST WFPC2 mid- to near-UV (F255W, λ c = 255 nm and F300W, λ c = 293 nm) and NIR data (F814W, λ c = 823 nm), as well as ground-based UBVR ( λ c = 360, 436, 540, and 634 nm, respectively) data from the VATT. Solid error bars indicate the error on the median, while dashed error bars give the 25%–75% quartile ranges, which indicate the spread of the data. The number statistics in the FUV and NUV are vastly improved in this study, which has resulted in much smaller error bars for each of the spiral, irregular, and peculiar galaxy type categories. Figure 5. Median CAS values in each type bin as a function of wavelength. Solid error bars indicate the error on the median, and dashed error bars indicate the 25%–75% quartile range of the data. The GALEX data (two left-most data points in each panel) are supplemented with HST and ground-based data. Circled data points: low GALEX S values are due to its poor (5 arcsec stellar FWHM) resolution. Disregarding this effect results in higher S values more in line with the trend displayed at longer wavelengths. In general, galaxies are more asymmetric and more clumpy at shorter rest-frame wavelengths, especially in the UV. This causes them to appear overall later type than they would at longer wavelengths. Sa-Sc galaxies appear less concentrated at shorter wavelengths, while Sd-Im and pec/mer galaxies do not exhibit a strong concentration versus wavelength relationship. The effect in the UV is particularly pronounced for elliptical/lenticular galaxies, which have little difference in their CAS parameters in the near-UV through the NIR, but appear significantly less concentrated, more asymmetric, and slightly more clumpy in the far-UV. For Figure 5 we reprocessed the Taylor-Mager et al. ( 2007 ) data through the newest version of the CAS code, as it treats background removal differently (utilizing the entire image with objects masked out via SExtractor catalogs versus a small user-defined box of empty sky). This had a minor impact on a small number of data points as compared to our 2007 results from the previous version of the code, but the overall trends with wavelength remain the same. This demonstrates that the difference in background subtraction methods does not have a significant impact on our conclusions. We rejected any median data points derived from fewer than five HST galaxies, as these low number statistics would produce unreliable results. Most panels in Figure 5 show a consistent general trend in CAS values as a function of rest-frame wavelength. A major exception is the clumpiness ( S ) parameter for all galaxy types except E/SO, where S increases significantly with decreasing wavelength, then drops dramatically between the HST /VATT UV and the shorter GALEX NUV wavelength (the second data point from the left in each