Authors: Pan, Kasen, & Loeb
This paper discusses the observability of PISN, Core Collapse, and Type Ia Supernovae
with JWST. They use light curves and spectra of the explosions using a time dependent
radiative transfer code for a wide range of Pop III stellar masses and evolutionary states.
One key point they argue based on the luminosity of various explosions is that for detecting
large numbers of PISN, a wide rather than deep survey will be better with JWST. In addition,
spectra of the explosions will help determine the stellar progenitor and it's evolutionary
state prior to the explosion.
After obtaining the spectra, they attempt to quantify how many SN are produced by using a very
simple analytic argument for the SFR in the early universe. The SFR is calibrated to ensure
the Universe is reionized by z=6. They have two classes of models: one where only Pop III stars
reionize and one where only Pop II stars provide the reionizing photons. Two different IMF's are
assumed (Salpeter and a flat IMF) for the Pop III stars, and a Salpeter IMF is used for the Pop II
case. With this constraint, they make predictions for the detectability of PISN and CCSN, and find that
it would be possible with JWST to distinguish between the two Pop III IMF models used here.
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