Towards Probing the Diffuse Supernova Neutrino Background in All Flavors

Abstract

Fully understanding the average core-collapse supernova requires detecting the diffuse supernova neutrino background (DSNB) in all flavors. While the DSNB ${\bar{\nu }}_e$ flux is near detection, and the DSNB ${\nu }_e$ flux has a good upper limit and prospects for improvement, the DSNB ${\nu }_x$ (each of ${\nu }_{\mu },{\nu }_{\tau },{\bar{\nu }}_{\mu },{\bar{\nu }}_{\tau }$) flux has a poor limit and heretofore had no clear path for improved sensitivity. We show that a succession of xenon-based dark matter detectors -- XENON1T (completed), XENONnT/LUX-ZEPLIN (running), and DARWIN (proposed) -- can dramatically improve sensitivity to DSNB ${\nu }_x$ the neutrino-nucleus coherent scattering channel. XENON1T could match the present sensitivity of $\sim 10^3{\mathrm{cm}}^{-2}{\mathrm{s}}^{-1}$ per ${\nu }_x$ flavor, XENONnT/LUX-ZEPLIN would have linear improvement of sensitivity with exposure, and a long run of DARWIN could reach a flux sensitivity of $\sim 10{\mathrm{cm}}^{-2}{\mathrm{s}}^{-1}$. Together, these would also contribute to greatly improve bounds on non-standard scenarios. Ultimately, to reach the standard flux range of $\sim 1{\mathrm{cm}}^{-2}{\mathrm{s}}^{-1}$, even larger exposures will be needed, which we show may be possible with the series of proposed lead-based RES-NOVA detectors.

arXiv comment13 pages, 11 figures, 3 appendices. Minor clarifications added, matches version accepted for publication in Phys. Rev. D

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