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We present a novel study on the problem of constructing mass models for theMilky Way, concentrating on features regarding the dark matter halo component.We have considered a variegated sample of dynamical observables for the Galaxy,including several results which have appeared recently, and studied a 7- or8-dimensional parameter space - defining the Galaxy model - by implementing aBayesian approach to the parameter estimation based on a Markov Chain MonteCarlo method. The main result of this analysis is a novel determination of thelocal dark matter halo density which, assuming spherical symmetry and either anEinasto or an NFW density profile is found to be around 0.39 GeV cm$^{-3}$ witha 1-$\sigma$ error bar of about 7%; more precisely we find a $\rho_{DM}(R_0) =0.385 \pm 0.027 \rm GeV cm^{-3}$ for the Einasto profile and $\rho_{DM}(R_0) =0.389 \pm 0.025 \rm GeV cm^{-3}$ for the NFW. This is in contrast to thestandard assumption that $\rho_{DM}(R_0)$ is about 0.3 GeV cm$^{-3}$ with anuncertainty of a factor of 2 to 3. A very precise determination of the localhalo density is very important for interpreting direct dark matter detectionexperiments. Indeed the results we produced, together with the recent accuratedetermination of the local circular velocity, should be very useful toconsiderably narrow astrophysical uncertainties on direct dark matterdetection.

A novel determination of the local dark matter density