13:00 – 13:10
Yosuke Ashida (University of Utah)
13:10 – 13:50
Sonia El Hedri (Laboratoire Astroparticules et Cosmologie)
Core-collapse supernovae (CCSNe) are important actors in the dynamics of galaxies but their underlying mechanism is still only partially understood. The detection of neutrinos from SN1987A confirmed that these particles play a key role in supernova explosions and that their detection would provide a complete recording of the behavior of the core of the star during the collapse. Moreover, CCSN neutrinos could be detected minutes to hours before the electromagnetic signal, thus providing an advance warning for telescopes. However, the CCSN detection range of current and upcoming neutrino experiments only covers our Galaxy and its immediate neighborhood, where supernovae take place only 2-3 times per century. The rarity and unpredictability of close-by supernovae has motivated the development of CCSN search strategies at a wide variety of neutrino detectors, sometimes extending their nominal energy range. Furthermore, a centralized real time analysis system, the Supernova Early Warning System (SNEWS), has been developed in order to combine observations from multiple experiments and send relevant information to telescopes within minutes after a CCSN neutrino detection. This contribution will illustrate the current challenges of CCSN neutrino detection through two topics. First, I will describe the CCSN search program of the KM3NeT neutrino experiment, originally aimed at studying neutrino oscillations and high-energy neutrinos from cosmic ray sources. Second, I will describe how to locate a supernova using neutrino observations, and will show how exploiting novel features of next-generation neutrino and dark matter experiments could improve SNEWS’s current strategies.
13:50 – 14:15
Yosuke Ashida (University of Utah)
The IceCube Neutrino Observatory is a cubic km detector using the Antarctic ice as a medium and with 5,160 optical modules deployed in 86 drilling holes. It has been releasing important science results, highlighting the first discovery of the astrophysical neutrino flux. In this talk, I will shed light on an aspect of supernova neutrino studies at IceCube as well as show prospects at IceCube-Upgrade which will equip optical detectors with a better performance and in a dense array.
Break 14:15 – 14:30
14:30 – 15:00
Guillaume Pronost (The University of Tokyo)
Since SN1987A, we know that supernovae (SNs) produce burst of neutrinos which can be detected several minutes to hours before the electromagnetic burst. Detecting this neutrino burst can provide an early warning to the astronomer community of the imminent SN. The Super-Kamiokande experiment, with its 50 ktons water Cerenkov detector, is currently the world's most sensitive neutrino detector able to provide this warning. Two main interactions are expected from the neutrino bursts in a water Cerenkov detector : inverse β decay (IBD) for ~90 % and electron scattering for ~5 %, this last one providing a direct indication of the SN direction. The recent gadolinium loading in the Super-Kamiokande detector allows a quasi-background-free selection of the IBD in the detector, providing a clear signature of potential SN burst, and allowing separation between IBD and ES to improve the SN direction pointing accuracy. In this presentation, we will present the status of the Super-Kamiokande supernova monitoring system.
15:00 – 15:30
Yudai Suwa (The University of Tokyo)
Neutrinos are pivotal signals in multi-messenger observations of supernovae. Recent advancements in the methods of analyzing supernova neutrinos, particularly in quantitative analysis, have significantly broadened scientific possibilities. In this talk, I will introduce the developments achieved by the nuLC collaboration over the past several years. First, we perform numerous numerical simulations of neutrino emissions from the supernova core. Second, we derive analytical solutions by solving the neutrino transfer equation, which closely approximate the numerical solutions. Finally, we have developed an analysis pipeline code that enables us to conduct quantitative data analysis of supernova neutrinos.
Break 15:30 – 15:45
15:45 – 16:00
Masamitsu Mori (National Astronomical Observatory of Japan)
16:00 – 16:15
Ryo Sawada (The University of Tokyo)
16:15 – 18:00
Everyone
Banquet 18:30 – 21:00