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The velocity distribution function (VDF) of the hypothetical WeaklyInteracting Massive Particles (WIMPs), currently the most favored candidate forthe Dark Matter (DM) in the Galaxy, is determined directly from the circularspeed ("rotation") curve data of the Galaxy assuming isotropic VDF. This isdone by "inverting" --- using Eddington's method --- the Navarro-Frenk-Whiteuniversal density profile of the DM halo of the Galaxy, the parameters of whichare determined, by using Markov Chain Monte Carlo (MCMC) technique, from arecently compiled set of observational data on the Galaxy's rotation curveextended to distances well beyond the visible edge of the disk of the Galaxy.The derived most-likely local isotropic VDF strongly differs from theMaxwellian form assumed in the "Standard Halo Model" (SHM) customarily used inthe analysis of the results of WIMP direct-detection experiments. Aparametrized (non-Maxwellian) form of the derived most-likely local VDF isgiven. The astrophysical "g-factor" that determines the effect of the WIMP VDFon the expected event rate in a direct-detection experiment can be lower forthe derived most-likely VDF than that for the best Maxwellian fit to it by asmuch two orders of magnitude at the lowest WIMP mass threshold of a typicalexperiment.

Deriving the velocity distribution of Galactic Dark Matter particles from rotation curve data