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

A Coleiro,V Kulikovskiy,M Lincetto,M Colomer Molla,D Dornic

doi:10.1140/epjc/s10052-020-8407-7

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 140pm 20,hbox {deg}^2. These low-latency analysis methods can be implemented in the SNEWS alert system.

Highlights

Gravitational binding energy of the stellar collapse is released through neutrinos [1]
Because of the weak anisotropy, pointing to CoreCollapse Supernovae (CCSN) with inverse beta decay (IBD) is difficult in water Cherenkov detectors and it is more promising for liquid scintillator detectors [8]
The JUNO scintillator detector is sensitive to both IBD and elastic scattering (ES) [9]

Summary

Introduction

Gravitational binding energy of the stellar collapse is released through neutrinos [1]. In the triangulation method proposed in [13], the uncertainty on the arrival time delay between a pair of detectors is inferred from the number of the detected neutrinos in the bulk of the emission and its duration. In [15], the triangulation method is revisited and a rough estimate of the arrival time uncertainty for each detector is computed assuming a generic neutrino light-curve with an exponential rise. The use of the time delay estimate between the first detected events in each experiment is proposed in [17] The latter method can be implemented for real-time CCSN localisation. A model-independent approach that relies on matching the detected neutrino light-curves is elaborated Such an approach requires data sharing between the detectors. The codes for the detected neutrino light-curves simulation, their matching and skymaps creations are publicly available [20]

Methods

Results

Conclusion