2017/12/15 by A. Gallo Rosso, Andrea Gallo Rosso, Francesco Vissani +1
Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Cosmic Phenomena #Cherenkov detector #Cherenkov radiation #Detector #Electron neutrino #Galaxy #Luminosity #Muon #Neutral current #Neutrino #Neutrino Physics Research #Neutrino detector #Neutrino oscillation #Nuclear physics #Optics #Particle physics #Particle physics theoretical and experimental studies #Physics #Solar neutrino #Solar neutrino problem #Spectral line #Sterile neutrino #Super-Kamiokande #Supernova #astro-ph.HE #hep-ph
paper · pdf · doi:10.1088/1475-7516/2018/04/040
22 pages, 19 figures, 7 tables
arxiv created 2017/12/15 · openalex publication_date 2018/04/12 · arxiv updated 2018/04/25 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We investigate the precision with which the supernova neutrino spectra can be reconstructed in water Cherenkov detectors, in particular the large scale Hyper-Kamiokande and Super-Kamiokande. To this aim, we consider quasi-thermal neutrino spectra modified by the Mikheev-Smirnov-Wolfenstein effect for the case of normal ordering. We perform three 9 degrees of freedom likelihood analyses including first inverse-beta decay only, then the combination of inverse beta decay and elastic scattering on electrons and finally a third analysis that also includes neutral scattering neutrino-oxygen events. A tenth parameter is added in the analyses to account for the theoretical uncertainty on the neutral current neutrino-oxygen cross section. By assuming a 100% efficiency in Hyper-Kamiokande, we show that one can reconstruct the electron antineutrino average energy and pinching parameter with an accuracy of ∼2% and ∼7% percent respectively, while the antineutrino integrated luminosity can be pinned down at ∼3% percent level. As for the muon and tau neutrinos, the average energy and the integrated luminosity can be measured with ∼7% precision. These results represent a significant improvement with respect Super-Kamiokande, particularly for the pinching parameter defining the electron antineutrino spectra. As for electron neutrinos, the determination of the emission parameters requires the addition of supplementary detection channels.