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tokens: and, instead, seem to confirm the action of a predominantly “high-soft” radiation field. 9. Dust and molecular gas-to-stellar mass ratios that are typically much higher than can be explained by stellar recycling from the aging burst population. This indicates that the dust and gas reservoirs were not entirely expelled during burst truncation. 10. Negative trends of PAH/TIR and dust-to-stellar mass ratio as a function of post-burst age, consistent with observations of dusty ETGs, indicating the effect of accumulating grain destruction and an incipient transition to virialized early-type gas conditions. 11. Little evidence for significant AGN activity beyond potential low-level activity associated with their existing LINER classifications. The high-ionization emission line [O iv ] is only detected in one source (weakly), and PAH band ratios show no evidence of small-grain depletion. One galaxy (2360_167_53728) displays extreme AGN colors in the near-IR WISE bands, with evidence for a very hot dust component to its SED. The presumed AGN is likely deeply embedded. Three sources appear to display an excess at 1.4 GHz, relative to the radio–infrared correlation, potentially indicating the presence of radio AGN activity. One source, in particular, is clearly a radio galaxy—the same source that is detected in [O iv ]. 12. Low star formation rates and efficiencies. Offsets from the star-forming main sequence are typically >10 and reach factors of >100 in some cases, for a variety of tracers, characterizing these galaxies as truly quiescent. Offsets from the KS relation exist for most sources and range from ∼3 to >10 for reliable tracers, depending on the comparison sample considered. These results paint a compelling picture: one of galaxies whose star formation was, indeed, rapidly truncated, and which are transitioning away from compact starbursting systems, but in which the gas and dust have not been completely expelled and instead are supported against further star formation by turbulent or mechanical heating. The resulting dense, modestly aged burst stellar populations appear to provide a “high-soft” radiation field, which dominates the unusual ISM energetics of galaxies seen after the fall from a prior star-forming peak. Appendix A Photometric Tables and SDSS Spectra In Tables 5 – 7 we present the photometry for the sample from the Spitzer , Herschel , and WISE space observatories, respectively. Spitzer photometric data only exist for the original sample of 15 sources, while Herschel and WISE data are shown for the full sample of 33. Table 5 Spitzer Photometric Data Note. Column (1): galaxy ID. Columns (2)–(5): Spitzer IRAC flux densities. Column (6): IRAC 8 μ m FWHM. Computed as the geometric mean of the major and minor axes of 2D elliptical Gaussian. Column (7): ratio of synthetic IRAC 8 μ m, computed from the IRS spectrum, to global 8 μ m; used for spectral scaling of SL. Columns (8)–(10): Spitzer MIPS flux densities. Column (11):