Welcome to the new version of CaltechAUTHORS. Login is currently restricted to library staff. If you notice any issues, please email coda@library.caltech.edu
Published January 1, 2009 | Submitted + Published
Journal Article Open

New DAMA dark-matter window and energetic-neutrino searches


Recently, the DAMA/LIBRA Collaboration has repeated and reinforced their claim to have detected an annual modulation in their signal rate, and have interpreted this observation as evidence for dark-matter particles at the 8.2σ confidence level. Furthermore, it has also been noted that the effects of channeling may enable a weakly interacting massive particle (WIMP) that scatters elastically via spin-independent interactions from nuclei to produce the signal observed by DAMA/LIBRA without exceeding the limits placed by CDMS, XENON, CRESST, CoGeNT, and other direct-detection experiments. To accommodate this elastic-scattering explanation, however, the mass of the responsible dark-matter particle must be relatively light, mDM ≾ 10 GeV. Such dark-matter particles will become captured by and annihilate in the Sun at very high rates, leading to a potentially large flux of GeV-scale neutrinos. We calculate the neutrino spectrum resulting from WIMP annihilations in the Sun and show that existing limits from Super-Kamiokande can be used to close a significant portion of the DAMA region, especially if the dark-matter particles produce tau leptons or neutrinos in a sizable fraction of their annihilations. We also determine the spin-dependent WIMP-nuclei elastic-scattering parameter space consistent with DAMA. The constraints from Super-Kamiokande on the spin-dependent scenario are even more severe—they exclude any self-annihilating WIMP in the DAMA region that annihilates 1% of the time or more to any combination of neutrinos, tau leptons, or charm or bottom quarks.

Additional Information

© 2009 The American Physical Society. Received 5 September 2008; published 22 January 2009. D. H. is supported by the Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy and by NASA Grant No. NNX08AH34G. M. K. is supported by DOE Grant No. DE-FG03-92-ER40701 and the Gordon and Betty Moore Foundation. F. P. and K. M. Z. are supported by DOE Grant No. DE-FG02-95ER40896. F. P. and K. M. Z. thank the Aspen Center for Physics, where part of this work was completed.

Attached Files

Published - Hooper2009p25910.1103PhysRevD.79.015010.pdf

Submitted - 0808.2464.pdf


Files (621.8 kB)
Name Size Download all
333.1 kB Preview Download
288.7 kB Preview Download

Additional details

August 20, 2023
March 5, 2024