(Figure \[fig:sersic-test\]), and we find a significant degree of scatter when comparing ground-based and CANDELS measurements. Formally, the characteristic scatter in $\delta n/n$, given by the normalized median absolute deviation ($\sigma_{{\rm
    NMAD}}$) is 45%, 39%, and 35% for the star-forming, passive and PSB populations respectively. Nevertheless, there is a clear correlation, and we find that ground-based determinations are sufficient to distinguish populations with “high” Sérsic indices (e.g. $n>2$) from those with “low” Sérsic indices ($n<2$). Comparing the three primary galaxy types, we find consistent results; the passive and post-starburst populations show consistently high Sérsic indices (from ground or spaced-based measurements), while star-forming galaxies are concentrated at lower values. The binned distribution demonstrates that the correlation between ground and space-based Sérsic indices is not perfectly 1:1, but we see no systematic differences in this relation between the three populations. We conclude that ground-based measurements can be used to broadly compare the Sérsic indices for our galaxy populations. In addition, we will use the subset of galaxies with HST measurements ($\sim$9%) to verify any conclusions drawn from the larger ground-based sample. The Sérsic distributions will be compared further (and as a function of stellar mass) in Section \[sec:sersic\].

The sizes of post-starburst 