Empirical capture cross sections for cosmic neutrino detection with $^{151}{\rm \bf Sm}$ and $^{171}{\rm \bf Tm}$

TL;DR

This paper predicts neutrino capture cross sections for $^{151}$Sm and $^{171}$Tm isotopes, demonstrating their potential for cosmic neutrino background detection with minimal theoretical uncertainties.

Contribution

It introduces a robust method to calculate neutrino capture cross sections for these isotopes, avoiding reliance on endpoint spectral data and accounting for relevant nuclear effects.

Findings

Predicted cross sections: $^{171}$Tm: $(1.12 ext{±}0.01) imes 10^{-46}$ cm$^2$, $^{151}$Sm: $(4.77 ext{±}0.01) imes 10^{-48}$ cm$^2$

Method applicable within 1% accuracy, independent of atomic physics contamination

Supports feasibility of cosmic neutrino detection using these isotopes in the PTOLEMY project.

Abstract

The nuclei $^{151}$Sm and $^{171}$Tm have been identified as attractive candidates for the detection of the cosmic neutrino background. Both isotopes undergo first-forbidden non-unique beta decays which inhibits a prediction of their spectral shape using symmetries alone and this has, so far, obstructed a definitive prediction of their neutrino capture cross sections. In this work we point out that for both elements the so-called "$\xi$-approximation" is applicable and this effectively reduces the spectral shape to deviate by at most $1\%$ from the one that would arise if beta decays were of the allowed type. Using measured half-lives we extract the relevant nuclear matrix element and predict the neutrino capture cross sections for both isotopes at $1\%$ level, accounting for a number of relevant effects including radiative corrections and the finite size of the nuclei. We obtained $(1.12\pm 0.01)\times 10^{-46}{\rm cm}^2$ for $^{171}$Tm and $(4.77\pm 0.01)\times 10^{-48}{\rm cm}^2$ for $^{151}$Sm. This method is robust as it does not rely on the data points near the end-point of the beta spectrum which may be contaminated by atomic physics effects, namely shake-up and shake-off. Finally, we calculate the target mass which is necessary for cosmic neutrino discovery and discuss several bottlenecks and respective solutions associated to the experimental program. We conclude that the detection of cosmic neutrino background by neutrino capture on $^{151}$Sm and $^{171}$Tm is achievable and free from theoretical limitations but still subject to technical issues that should be further investigated by the experimentalists in the context of the proposed PTOLEMY project.