found to identify approximately 60% of galaxies that would be spectroscopically classified as PSBs. Overall, these figures confirm that photometric PCA techniques can be used to identify large and relatively clean samples of recently quenched galaxies. So far the spectroscopic confirmation is restricted to $z<1.4$, given the requirement to detect H$\delta$ with optical spectroscopy. Future near-infrared spectroscopy (e.g. with the [*James Webb Space Telescope*]{}) will allow a detailed investigation of the population at higher redshift.

The identification of large PSB samples has allowed the first study of the PSB galaxy mass function and its evolution to $z=2$ (Wild et al. 2016). Strong evolution was observed, with the implication that a large fraction of massive galaxies are rapidly quenched and pass through a PSB phase. In this paper we use the unique PCA sample described in Wild et al. (2016) to explore the structural properties of post-starburst galaxies. As newly quenched systems, our primary aim is to investigate if this population is structurally similar to star-forming galaxies at the same epoch, or if they already show evidence for the compact spheroid-dominated morphology of well-established quiescent galaxies.

We assume a cosmology with $\Omega_M=0.3$, $\Omega_\Lambda=0.7$ and $h=0.7$. All magnitudes are given in the 