turbulence from stellar feedback is unlikely. Secular sources of turbulence like morphological quenching act over $>1$ Gyr, so are unlikely to play a role during this short transitional phase.

We have selected the post-starburst galaxies on a lack of emission lines, which selects against strong AGN. Nevertheless, LINER-like activity is currently seen in many post-starburst galaxies [@Yan2006; @Yang2006; @French2015]. Obscured AGN activity in a small number of sources, including H02, is suggested by the dust spectral fitting done by @Smercina2018. Smercina et al. also observe H$_2$ rotational lines in S05 in the mid-IR, satisfying the turbulent heating threshold of H$_2$/7.7$\mu$m $>0.04$ seen in molecular hydrogen emission-line galaxies [MOHEGs; @Ogle2010]. Further evidence of AGN activity affecting the molecular gas reservoirs is seen in the rapid decline of the CO-traced gas during the post-starburst phase, on a timescale too rapid to be explained by star formation (French et al. 2018 submitted to ApJ), with timescales and inferred outflow rates similar to those seen in LINERs [@Cicone2013].

We also may be observing the post-starburst galaxies in the non-active phase of a trend of AGN variability. AGN activity is possible during the post-starburst phase [@Davies2007; @Schawinski2009; @Wild2010; @Cales2015], and varies with timescales short enough 