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We present far-infrared (FIR) spectroscopy of supernova remnants (SNRs) basedon the archival data of the Infrared Space Observatory ($ISO$) taken with theLong Wavelength Spectrometer (LWS). Our sample includes previously unpublishedprofiles of line and continuum spectra for 20 SNRs in the Galaxy and MagellanicClouds. In several SNRs including G21.5-0.9, G29.7-0.3, the Crab Nebula, andG320.4-1.2, we find evidence for broad [O I], [O III], [N II], and [C II] lineswith velocity dispersions up to a few 10$^3$ km s$^{-1}$, indicating that theyare associated with high-velocity SN ejecta. Our detection of Doppler-broadenedatomic emission lines and a bright FIR continuum hints at the presence of newlyformed dust in SN ejecta. For G320.4-1.2, we present the first estimate of anejecta-dust mass of 0.1 - 0.2 M$_\odot$, which spatially coincides with thebroad line emission, by applying a blackbody model fit with components of theSNR and background emission. Our sample includes raster maps of 63, 145 $\mu$m[O I] and 158 $\mu$m [C II] lines toward SNRs Kes 79, CTB 109, and IC 443.Based on these line intensities, we suggest interacting shock types in theseSNRs. Finally, we compare our LWS spectra of our sample SNRs with the spectraof several HII regions, and discuss their FIR line intensity ratios andcontinuum properties. Follow-up observations with modern instruments (e.g.$JWST$ and $SOFIA$) with higher spatial and spectral resolution are encouragedfor an extensive study of the SN ejecta and the SN dust.

A Spectroscopic Study of Supernova Remnants with the Infrared Space Observatory