The paper by Andrew M. Hopkins and John F. Beacom explores the normalization of the cosmic star formation history (SFH) using ultraviolet and far-infrared measurements, refining previous results over the past decade. The authors fit the most robust data to simple analytical forms and derive conservative bands to indicate possible variations from the best fits. They investigate the sequence of assumptions and corrections affecting the SFH normalization, testing their accuracy in the redshift range $z \lesssim 1$. The lower limits on the SFH normalization are derived from the evolution in stellar mass density, metal mass density, and supernova rate density, suggesting that the SFH normalization is unlikely to be much lower than indicated by the direct fit. The upper limit is set by the Super-Kamiokande (SK) limit on the electron antineutrino flux from past core-collapse supernovae, which applies primarily to $z \lesssim 1$. The authors find consistency with the SFH only if the neutrino temperatures from SN events are relatively modest. Constraints on the assumed initial mass function (IMF) are also discussed, showing that the traditional Salpeter IMF is not a robust model and that shallower or top-heavy IMFs may be preferred. The paper emphasizes the need for improved data on supernova rate density evolution, stellar mass ranges leading to core-collapse and type Ia supernovae, and antineutrino and neutrino backgrounds from core-collapse supernovae to resolve outstanding issues.The paper by Andrew M. Hopkins and John F. Beacom explores the normalization of the cosmic star formation history (SFH) using ultraviolet and far-infrared measurements, refining previous results over the past decade. The authors fit the most robust data to simple analytical forms and derive conservative bands to indicate possible variations from the best fits. They investigate the sequence of assumptions and corrections affecting the SFH normalization, testing their accuracy in the redshift range $z \lesssim 1$. The lower limits on the SFH normalization are derived from the evolution in stellar mass density, metal mass density, and supernova rate density, suggesting that the SFH normalization is unlikely to be much lower than indicated by the direct fit. The upper limit is set by the Super-Kamiokande (SK) limit on the electron antineutrino flux from past core-collapse supernovae, which applies primarily to $z \lesssim 1$. The authors find consistency with the SFH only if the neutrino temperatures from SN events are relatively modest. Constraints on the assumed initial mass function (IMF) are also discussed, showing that the traditional Salpeter IMF is not a robust model and that shallower or top-heavy IMFs may be preferred. The paper emphasizes the need for improved data on supernova rate density evolution, stellar mass ranges leading to core-collapse and type Ia supernovae, and antineutrino and neutrino backgrounds from core-collapse supernovae to resolve outstanding issues.