Sensitivity of future liquid argon dark matter search experiments to core-collapse supernova neutrinos. (arXiv:2011.07819v2 [astro-ph.HE] UPDATED)
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Future liquid-argon DarkSide-20k and ARGO detectors, designed for direct dark
matter search, will be sensitive also to core-collapse supernova neutrinos, via
coherent elastic neutrino-nucleus scattering. This interaction channel is
flavor-insensitive with a high-cross section, enabling for a high-statistics
neutrino detection with target masses of $sim$50~t and $sim$360~t for
DarkSide-20k and ARGO, respectively.
Thanks to the low-energy threshold of $sim$0.5~keV$_{nr}$ achievable by
exploiting the ionization channel, DarkSide-20k and ARGO have the potential to
discover supernova bursts throughout our galaxy and up to the Small Magellanic
Cloud, respectively, assuming a 11-M$_{odot}$ progenitor star. We report also
on the sensitivity to the neutronization burst, whose electron neutrino flux is
suppressed by oscillations when detected via charged current and elastic
scattering. Finally, the accuracies in the reconstruction of the average and
total neutrino energy in the different phases of the supernova burst, as well
as its time profile, are also discussed, taking into account the expected
background and the detector response.
Future liquid-argon DarkSide-20k and ARGO detectors, designed for direct dark
matter search, will be sensitive also to core-collapse supernova neutrinos, via
coherent elastic neutrino-nucleus scattering. This interaction channel is
flavor-insensitive with a high-cross section, enabling for a high-statistics
neutrino detection with target masses of $sim$50~t and $sim$360~t for
DarkSide-20k and ARGO, respectively.
Thanks to the low-energy threshold of $sim$0.5~keV$_{nr}$ achievable by
exploiting the ionization channel, DarkSide-20k and ARGO have the potential to
discover supernova bursts throughout our galaxy and up to the Small Magellanic
Cloud, respectively, assuming a 11-M$_{odot}$ progenitor star. We report also
on the sensitivity to the neutronization burst, whose electron neutrino flux is
suppressed by oscillations when detected via charged current and elastic
scattering. Finally, the accuracies in the reconstruction of the average and
total neutrino energy in the different phases of the supernova burst, as well
as its time profile, are also discussed, taking into account the expected
background and the detector response.
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