Ref Arxiv: 1507.08827
DOI: 10.1103/PhysRevD.92.053011
Ref. & Cit.: NASA ADS
Commentaires: 19 pages, 36 figures, version accepted in Phys. Rev. D. Réf Journal: Phys. Rev. D 92, 053011 (2015)

Ref Arxiv: 1510.00246
Ref. & Cit.: NASA ADS

Ref Arxiv: 1502.05836
Ref INSPIRE: 1345450
DOI: 10.1103/PhysRevD.92.015006
Ref. & Cit.: NASA ADS
18 citations

Ref Arxiv: 1411.1325
Ref INSPIRE: 1326121
DOI: 10.1103/PhysRevD.91.023510
Ref. & Cit.: NASA ADS
16 citations

Ref HAL: hal-01982710_v1
Ref Arxiv: 1407.1797
DOI: 10.1103/PhysRevD.90.035026
Ref. & Cit.: NASA ADS
Exporter : BibTex | endNote

Résumé:

Direct detection (DD) of dark matter (DM) candidates in the $\lesssim$10 GeV mass range is very sensitive to the tail of their velocity distribution. The important quantity is the maximum WIMP speed in the observer's rest frame, i.e. in average the sum of the local Galactic escape speed $v_{\rm esc}$ and of the circular velocity of the Sun $v_c$. While the latter has been receiving continuous attention, the former is more difficult to constrain. The RAVE Collaboration has just released a new estimate of $v_{\rm esc}$ (Piffl {\em et al.}, 2014 --- P14) that supersedes the previous one (Smith {\em et al.}, 2007), which is of interest in the perspective of reducing the astrophysical uncertainties in DD. Nevertheless, these new estimates cannot be used blindly as they rely on assumptions in the dark halo modeling which induce tight correlations between the escape speed and other local astrophysical parameters. We make a self-consistent study of the implications of the RAVE results on DD assuming isotropic DM velocity distributions, both Maxwellian and ergodic. Taking as references the experimental sensitivities currently achieved by LUX, CRESST-II, and SuperCDMS, we show that: (i) the exclusion curves associated with the best-fit points of P14 may be more constraining by up to $\sim 40$\% with respect to standard limits, because the underlying astrophysical correlations induce a larger local DM density; (ii) the corresponding relative uncertainties inferred in the low WIMP mass region may be moderate, down to 10-15\% below 10 GeV. We finally discuss the level of consistency of these results with other independent astrophysical constraints. This analysis is complementary to others based on rotation curves.