BULLKID silicon detector array background rate matches simulations at (6.8 ± 0.4 stat. ± 0.1 syst.) × 10^4 counts/keV/kg/day from 2 keV to 600 eV, with excess below 600 eV unlike typical cryogenic low-energy excesses.
Silk et al.,Particle Dark Matter: Observations, Models and Searches
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Observation of neutron stars at 1000-1200 K could constrain asymmetric dark matter self-interaction cross-sections by two orders of magnitude beyond bullet cluster limits.
citing papers explorer
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Background of the BULLKID detector array operated with moderate shield on surface
BULLKID silicon detector array background rate matches simulations at (6.8 ± 0.4 stat. ± 0.1 syst.) × 10^4 counts/keV/kg/day from 2 keV to 600 eV, with excess below 600 eV unlike typical cryogenic low-energy excesses.
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Constraining dark matter self-interaction from kinetic heating in neutron stars
Observation of neutron stars at 1000-1200 K could constrain asymmetric dark matter self-interaction cross-sections by two orders of magnitude beyond bullet cluster limits.