Supernova cooling excludes fermionic dark matter produced by neutrino scattering down to cross sections of about 10^-58 cm^2 for electrons and 10^-56 cm^2 for nucleons across the keV to 100 MeV mass range.
Observation of low-lying isomeric states in $^{136}$Cs: a new avenue for dark matter and solar neutrino detection in xenon detectors
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abstract
We report on new measurements establishing the existence of low-lying isomeric states in $^{136}$Cs using $\gamma$ rays produced in $^{136}$Xe(p,n)$^{136}$Cs reactions. Two states with $\mathcal{O}(100)$~ns lifetimes are placed in the decay sequence of the $^{136}$Cs levels that are populated in charged-current interactions of solar neutrinos and fermionic dark matter with $^{136}$Xe. Xenon-based experiments can therefore exploit a delayed-coincidence tag of these interactions, greatly suppressing backgrounds to enable spectroscopic studies of solar neutrinos and dark matter.
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Supernova cooling from neutrino-devouring dark matter
Supernova cooling excludes fermionic dark matter produced by neutrino scattering down to cross sections of about 10^-58 cm^2 for electrons and 10^-56 cm^2 for nucleons across the keV to 100 MeV mass range.