Vast quantities of dust observed in high red-shifted galaxies raise the
fundamental astrophysical question of the origin of dust in the early
Universe because the timescale of the primary source of dust formation, AGB
stars to release their dust is too long. Herschel and Spitzer observations
of two young supernova remnants (SNRs) G54.1+0.3 and Cas A provides the
total dust-mass estimates, which range 0.1-1 Msun and suggests that
supernovae are a significant source of dust in the early Universe. We
present Herschel FIR catalog of known SNRs in the Galactic
plane and the implication of their far-IR emission. Out of 190 SNR samples,
we detect dust signatures in 39 SNRs, including 13 core-collapse SNRs.

To understand the gaps of dust mass between supernovae (SNe) and young
SNRs, we have started a Gemini observing campaign to observe newly exploded
supernovae in nearby galaxies. We present the first example of eleven
near-infrared (0.8 − 2.5 microns) Gemini spectra of the Type II-P SN
2017eaw and a set of optical and IRTF spectra of SN 2018hna. The spectra
show the onset of CO formation and newly-formed hot dust, in addition to
numerous lines of hydrogen and metals, which reveal the change in
ionization as the density of much of the ejecta decreases. We will present
a plan of Gemini ToO SNe observations during 2020A and a perspective to
study dust formation in SN ejecta using GMT. We will also show  SOFIA
far-IR [O I] and [O III] maps and possibly polarization map of Cas A.
Lastly, I will show ground-based CO millimeter observations and molecular
hydrogen detection from SNRs, which are interacting with molecular clouds,
which are ideal for follow-up JCMT and ALMA observations.