DIRECT DETECTION OF DARK MAT TER

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Teraelectronvolt Astronomy (2010, background): “Possibilities for the detection of cosmological DM include challenging direct-detection experiments, where DM particles — typically assumed to have a local density of around 0.3 GeV cm−3 — scatter off nuclei, resulting in keVscale recoil energies (Gaitskell 2004).”
KINEMATICAL AND CHEMICAL VERTICAL STRUCTURE OF THE GALACTIC THICK DISK. II. A LACK OF DARK MATTER IN THE SOLAR NEIGHBORHOOD, (2012, background): “The results of these experiments are degenerate between the unknown interaction cross-section of the searched particles and their local density (e.g., Gaitskell 2004; Aprile et al. 2005).”
The Aquarius Project: the subhaloes of galactic haloes (2008, background): “…of dark matter substructure within halos is made more urgent by the prospect of observing dark matter particles in the near future, either by their annihilation radiation (e.g. Bergström et al., 1998), or through direct detection in experiments here on Earth (reviewed, e.g., by Gaitskell, 2004).”