method of Whitaker et al. (2012), who identified recently-quenched candidates at the blue end of the passive UVJ sequence.

![The distribution of stellar mass as a function of photometric redshift for the three primary galaxy populations. The curves show the corresponding 95% completeness limits, determined using the method of Pozzetti et al. (2010). Details of the galaxy classification and stellar mass determination can be found in Wild et al. (2016). In this paper we focus on the structural properties of galaxies in the redshift range $1<z<2$.[]{data-label="fig:zmass"}](zmass.pdf){width="0.9\linewidth"}

![A comparison of size measurements for galaxies measured with ground-based $K$-band imaging and HST $H$-band imaging, using the subsample of $\sim$9% of galaxies within the UDS CANDELS mosaic. The upper panel compares half-light radii for individual galaxies. We find that ground-based imaging can provide robust measurements of galaxy sizes, although the relationship is not precisely 1:1. A linear fit to all points suggests that ground-based sizes are $\sim$13% smaller on average (dashed line). A characteristic uncertainty on individual measurements is shown, representing the median error on the PSB sizes. The lower (binned) distribution compares mean sizes for the three key populations, with unfilled symbols representing mean values determined from fewer than 5 galaxies. We 