Dark matter-electron scattering rates in isotropic materials are bounded from above by a universal expression depending only on plasma frequency, mass density, and static dielectric function.
Detectability of Weakly Interacting Massive Particles in the Sagittarius Dwarf Tidal Stream
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Tidal streams of the Sagittarius dwarf spheroidal galaxy (Sgr) may be showering dark matter onto the solar system and contributing approx (0.3--23)% of the local density of our Galactic Halo. If the Sagittarius galaxy contains WIMP dark matter, the extra contribution from the stream gives rise to a step-like feature in the energy recoil spectrum in direct dark matter detection. For our best estimate of stream velocity (300 km/sec) and direction (the plane containing the Sgr dwarf and its debris), the count rate is maximum on June 28 and minimum on December 27 (for most recoil energies), and the location of the step oscillates yearly with a phase opposite to that of the count rate. In the CDMS experiment, for 60 GeV WIMPs, the location of the step oscillates between 35 and 42 keV, and for the most favorable stream density, the stream should be detectable at the 11 sigma level in four years of data with 10 keV energy bins. Planned large detectors like XENON, CryoArray and the directional detector DRIFT may also be able to identify the Sgr stream.
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First-principles upper bounds on dark matter-electron scattering rates from condensed matter sum rules
Dark matter-electron scattering rates in isotropic materials are bounded from above by a universal expression depending only on plasma frequency, mass density, and static dielectric function.