Timing the Neutrino Signal of a Galactic Supernova. (arXiv:1904.11461v2 [hep-ph] UPDATED)
<a href="http://arxiv.org/find/hep-ph/1/au:+Hansen_R/0/1/0/all/0/1">Rasmus S. L. Hansen</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Lindner_M/0/1/0/all/0/1">Manfred Lindner</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Scholer_O/0/1/0/all/0/1">Oliver Scholer</a>
We study several methods for timing the neutrino signal of a Galactic
supernova (SN) for different detectors via Monte Carlo simulations. We find
that, for the methods we studied, at a distance of $10,$kpc both
Hyper-Kamiokande and IceCube can reach precisions of $sim1,$ms for the
neutrino burst, while a potential IceCube Gen2 upgrade will reach
submillisecond precision. In the case of a failed SN, we find that detectors
such as SK and JUNO can reach precisions of $sim0.1,$ms while HK could
potentially reach a resolution of $sim 0.01,$ms so that the impact of the
black hole formation process itself becomes relevant. Two possible applications
for this are the triangulation of a (failed) SN as well as the possibility to
constrain neutrino masses via a time-of-flight measurement using a potential
gravitational wave signal as reference.
We study several methods for timing the neutrino signal of a Galactic
supernova (SN) for different detectors via Monte Carlo simulations. We find
that, for the methods we studied, at a distance of $10,$kpc both
Hyper-Kamiokande and IceCube can reach precisions of $sim1,$ms for the
neutrino burst, while a potential IceCube Gen2 upgrade will reach
submillisecond precision. In the case of a failed SN, we find that detectors
such as SK and JUNO can reach precisions of $sim0.1,$ms while HK could
potentially reach a resolution of $sim 0.01,$ms so that the impact of the
black hole formation process itself becomes relevant. Two possible applications
for this are the triangulation of a (failed) SN as well as the possibility to
constrain neutrino masses via a time-of-flight measurement using a potential
gravitational wave signal as reference.
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