Program: GN-2023A-Q-218

We propose a systematic near-infrared (NIR) survey using sToO observations of core-collapse supernovae (ccSNe) to produce an unprecedented uniform near-IR spectral database, which will be complemented with the Keck Infrared Transients Survey (KITS). Both JWST and Nancy Grace Roman Telescope aim to detect the early universe’s first stars and supernovae, for which a NIR spectroscopic census of ccSNe (explosions of very massive stars) is vital. To significantly impact the astronomy community, we will waive the 1-year data-right period as it is for KITS. We aim to settle the question of whether ccSNe are major dust producers in the early universe. High-z galaxies contain large quantities of dust, which AGB stars cannot have been produced since they did not exist in the early universe. A few ccSN remnants have already been shown to create copious amounts of dust, which could explain the amount of dust seen in high-z. However, the dust masses detected in ccSNe are not well-known and understood. Using Gemini, we find that CO and dust formation in SNe IIP and SNe Ic begins on approximately days 100 and 60, respectively, but the dust mass is uncertain because the time coverage is still limited. We propose to continue the Gemini NIR program to study the temporal evolution of CO- and dust in ccSNe. Our immediate goals are (1) to obtain time series of NIR spectroscopy of SNe Ibc after day 70 to test if the dust is newly formed, pre-existing, or both, and (2) to detect CO and dust in super-luminous SNe, SNe Ibn, and SNe IIn. Our campaign will determine the timescale of CO and dust formation for each type of ccSNe and enable us to estimate dust mass with time, SN type, and progenitor mass.