Abstract
An overview of the latest results of Dark Matter direct detection will be summarized, with particular care to the DAMA/LIBRA-phase1 results and the evidence with high confidence level obtained by exploiting the model independent Dark Matter annual modulation signature for the presence of Dark Matter particles in the galactic halo. Results from other experiments using different procedures, different techniques and different target-materials will be shortly discussed. Results, implications and experimental perspectives will be addressed.
Highlights
A century of experimental observations and theoretical arguments has pointed out that a large fraction of the Universe is composed by Dark Matter Particles and Dark Energy
Considering all the observational data coming from the study of the CMB, of the Supernovae Ia, of the Baryonic Acoustic Oscillations (BAO) and of the large-scale structures, the following contributions to are obtained[1, 2]: i) r ≈ 5 × 10−5 for the radiation density; ii) b ≈ 0.05 for the baryonic matter; iii) dm ≈ 0.27 for the non baryonic Dark Matter; iv)
A value b ≈ 0.05 for the baryonic matter is supported by the Big-Bang nucleosynthesis (BBN), that is based on the predictions of the abundances of the light elements
Summary
Considering all the observational data coming from the study of the CMB, of the Supernovae Ia, of the Baryonic Acoustic Oscillations (BAO) and of the large-scale structures, the following contributions to are obtained[1, 2]: i) r ≈ 5 × 10−5 for the radiation density; ii) b ≈ 0.05 for the baryonic matter; iii) dm ≈ 0.27 for the non baryonic Dark Matter; iv). Considering the richness of particle possibilities and the existing uncertainties on related astrophysical (e.g. halo model and related parameters, etc.), nuclear (e.g. form factors, spin factors, scaling laws, etc.) and particle physics (e.g. particle nature and interaction types, etc.), a widely-sensitive model independent approach is mandatory. The isothermal sphere model (which consists in a spherical infinite system with a flat rotational curve) is a widely used assumption for the DM density distribution, and in the evaluation of Dark Matter expected rates. Many other experimental and theoretical uncertainties exist and must be considered in a suitable comparison among the experiments of direct detection of DM particles
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