2020/07/06 by Riya, Vikram Rentala, Rentala, Vikram · 2 citations
Physics and Astronomy · #Astrophysics and Cosmic Phenomena #Astrophysics of Galaxies (astro-ph.GA) #Cosmology and Nongalactic Astrophysics (astro-ph.CO) #FOS: Physical sciences #Gamma-ray bursts and supernovae #High Energy Astrophysical Phenomena (astro-ph.HE) #High Energy Physics - Experiment (hep-ex) #High Energy Physics - Phenomenology (hep-ph) #Neutrino Physics Research #astro-ph.CO #astro-ph.GA #astro-ph.HE #hep-ex #hep-ph
paper · pdf · doi:10.48550/arxiv.2007.02951
14 pages, 4 figures, 5 tables
arxiv created 2020/07/06 · openalex publication_date 2020/07/06 · arxiv updated 2020/07/08 · openalex created_date 2020/07/10 · openalex updated_date 2026/07/28
Multiple astrophysical probes of the cosmic star formation history yield widely different inferences of this rate at redshifts z > 1. While all probes seem to indicate a period of peak star formation known as the cosmic noon between 1.5 < z < 3, the detailed inferences from these probes are in disagreement. In particular, the magnitude of the peak star formation rate density indicated by H-alpha data is higher by a factor of ~ 4 compared to the magnitude of the peak indicated by UV/IR data. In this work, we explore the potential of future measurements of the diffuse supernova neutrino background at the Hyper-Kamiokande (HK) experiment to resolve the discrepancy and help pin down the magnitude of the peak cosmic star formation rate. We find that, depending upon the cosmic core-collapse supernova neutrino spectrum, HK loaded with 0.1% Gadolinium by mass has the potential to discriminate between the different star formation histories with between 1.6-20 years of data collection.