First, we taper the data to 5, but still do not detect either galaxy in HCN (1–0). Second, we use a matched filter technique [@Loomis2018] using the prior information from the CO observations, but do not find any significant detections just below our sensitivity limit.

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Star Formation Rates {#sec:sfr}
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Determining SFRs for post-starburst galaxies is complicated by the recent starburst, possible AGN activity, and heating from the young A-star population. In @French2015 [§2.5], we explored many possible methods for calculating SFRs in the post-starburst galaxies using the available archival optical and radio data. Recent work by @Smercina2018 has explored a number of infrared tracers for these same galaxies. Here, we discuss the constraints on the SFRs of the two galaxies considered here from various measures.

In @French2015, we compared the SFRs derived from H$\alpha$ emission and the 4000Å Balmer break D$_n(4000)$, corrected for dust based on the Balmer decrement and for aperture based on their SDSS colors. A decreased SFE in the CO-traced gas was seen for both measures, which is conservative because both SFR indicators are likely upper limits: the high incidence of LINER-like emission line ratios in post-starbursts suggest that the H$\alpha$ fluxes are likely to 