One believes there is a huge amount of dark matter particles in our Galaxy which manifest themselves only gravitationally. There is a big challenge to prove their existence in a laboratory experiment. To this end, it is not sufˇcient toˇght only for the best exclusion curve, one has to see an annual recoil spectrum modulation Å the only available positive direct dark matter detection signature. A necessity to measure the recoil spectra is stressed. 95.35.+d; 14.80.Ly; 12.60.Jv Galactic Dark Matter (DM) particles do not emit (or re ect) any detectable electromagnetic radiation and manifest themselves only gravitationally by affecting other astrophysical objects. According to the estimates based on a detailed model of our Galaxy [1], the local density of DM (nearby the Solar System) amounts to about ρ −25 g/cm 3 (see also recent reviews , where m χ is the DM particle mass. This value is often considered as a promising basis for direct laboratory dark matter search experiments. The problem of the DM in the Universe is a challenge for modern physics and experimental technology. To solve the problem, i.e., at least to detect the DM particles, one simultaneously needs to apply the front-end knowledge of modern particle physics, astrophysics, cosmology and nuclear physics and to develop and use over long time extremely high-sensitive experimental setups and complex data analysis methods (see, for example, recent discussion in Weakly Interacting Massive Particles (WIMPs) are among the most popular candidates for the relic DM. These particles are nonbaryonic and there is no room for them in the Standard Model of particle physics (SM). The Lightest Supersymmetric (SUSY) Particle (LSP), neutralino (being massive, neutral and stable), is currently often assumed to be a favorite WIMP dark matter particle.
