Supernova neutrino fluxes in HALO-1kT, Super-Kamiokande, and JUNO

Abstract

When the next galactic core-collapse supernova occurs, we must be ready to obtain as much information as possible. Although many present and future detectors are well equipped to detect ${\overline{\nu }}_{\mathrm{e}}$ and ${\nu }_x$ neutrinos, the detection of the ${\nu }_{\mathrm{e}}$ species presents the biggest challenges. We assess the impact that a 1 ktonne lead-based detector, such as HALO-1kT, can have in constraining electron neutrino time-integrated fluxes. The study involves the detector taken alone as well as when combined with massive ${\overline{\nu }}_{\mathrm{e}}$-sensitive detectors such as Super-Kamiokande and JUNO. We find that HALO-1kT alone is not able to strongly constrain the emission parameters. When combined with other detectors, however, the orthogonal information might be helpful in improving the ${\nu }_{\mathrm{e}}$ total emitted energy and mean energy accuracy, up to about $50\%$, if no other ${\nu }_{\mathrm{e}}$-sensitive channel is implemented. A discussion on the reconstruction of ${\overline{\nu }}_{\mathrm{e}}$ and ${\nu }_x$ species, as well as the total emitted energy, is also presented.

Revised model 9.6 solar masses. Figures and tables updated, results unchanged

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