Combining neutrino experimental light-curves for pointing to the next galactic core-collapse supernova

Abstract

The multi-messenger observation of the next galactic core-collapse supernova will shed light on the different physical processes involved in these energetic explosions. Good timing and pointing capabilities of neutrino detectors would help in the search for an electromagnetic or gravitational-wave counterparts. An approach for the determination of the arrival time delay of the neutrino signal at different experiments using a direct detected neutrino light-curve matching is discussed. A simplified supernova model and detector simulation are used for its application. The arrival time delay and its uncertainty between two neutrino detectors are estimated with chi-square and cross-correlation methods. The direct comparison of the detected light-curves offers the advantage to be model-independent. Millisecond time resolution on the arrival time delay at two different detectors is needed. Using the computed time delay between different combinations of currently operational and future detectors, a triangulation method is used to infer the supernova localisation in the sky. The combination of IceCube, Hyper-Kamiokande, JUNO and KM3NeT/ARCA provides a 90% confidence area of $$140\pm 20\,\hbox {deg}^2$$ 140 ± 20 deg 2 . These low-latency analysis methods can be implemented in the SNEWS alert system.

The KM3NeT potential for the next core-collapse supernova observation with neutrinos

“…In case of a high-significance detection, the large event statistics collected by KM3NeT can be exploited in a detailed analysis of the time profile of the neutrino burst with a potential millisecond time resolution. The reconstruction of the time profile of the signal can enable the triangulation of the source, either by the independent estimation of the burst arrival times at different detectors [40] or by directly comparing the experimental neutrino light curves [41]. The analysis of the time profile can also be a powerful tool for model discrimination, especially when considering black-hole forming scenarios that exhibit an abrupt interruption of the neutrino emission.…”

Exploring the Potential of Multi-Detector Analyses for Core-Collapse Supernova Neutrino Detection

“…Several efforts have already been carried out to triangulate the position of the CCSN using neutrino telescope data. We hereby use the approach described in [11], which estimates the time delay between the light curves recorded by different detectors during a CCSN to infer its position in the sky. In this study, we have used detectors sensitive to the same flavor, i.e.…”

“…This approach allows us to reduce the 90% confidence area of the source localization by more than 55%, depending on the combination of neutrino telescopes which is used, as shown in Fig 1. [11] with and without using the prior for a CCSN located at the Galactic Center.…”

“…Figure 1: Comparison of the confidence areas obtained by the CCSN triangulation method[11] with and without using the prior for a CCSN located at the Galactic Center.…”

Implementation and first results of the KM3NeT real-time core-collapse supernova neutrino search

“…Vice versa, a search for a neutrino counterpart can be performed as a follow-up of candidate gravitational-wave alerts. Furthermore, the detected neutrino light-curves can be combined to estimate the relative delays between the arrival times at each detector, allowing for the triangulation of the source location [14].…”