be contaminated, and the D$_n(4000)$-based SFRs have greater uncertainties and trace a longer period of star formation, and are thus contaminated by the starburst itself. The SFRs derived from the extinction-corrected H$\alpha$ fluxes are 0.09, 0.58 M$_\sun$yr$^{-1}$ for H02 and S05 respectively. While the D$_n(4000)$-based SFRs have significantly higher uncertainties, the 68%ile ranges are $0.01-0.29$ M$_\sun$yr$^{-1}$ for H02 and $0.006-1.05$ M$_\sun$yr$^{-1}$ for S05, consistent with the H$\alpha$-based SFRs.

We also consider several other SFR indicators to account for the possibility that the Balmer decrement measurements underestimate the true dust obscuration. We use the VLA FIRST Survey [Faint Images of the Radio Sky at Twenty centimeters @Becker1995] to study the 1.4 GHz radio continuum emission as a SFR tracer. 1.4 GHz emission is often used as an extinction-free tracer of SFRs [@Condon1992], but LINERs are found to contribute to the 1.4 GHz emission [@deVries2007; @Moric2010] with greater scatter than for H$\alpha$ [@Moric2010]. Neither post-starburst galaxy considered here is detected in FIRST, and upper limits imply 1$\sigma$ upper limits on the SFRs of $<0.6$ and $0.5$ M$_\sun$yr$^{-1}$ for H02 and S05, respectively.

@Smercina2018 fit the dust continuum to estimate SFRs from the total infrared (TIR) flux, as well as the other infrared 