The milky way total mass profile as inferred from Gaia DR2

We determine the Milky Way (MW) mass profile inferred from fitting physically motivated models to the Gala DR2 Galactic rotation curve and other data. Using various hydrodynamical simulations of MW-mass haloes, we show that the presence of baryons induces a contraction of the dark matter (DM) distribution in the inner regions, r less than or similar to 20 kpc. We provide an analytic expression that relates the baryonic distribution to the change in the DM halo profile. For our galaxy, the contraction increases the enclosed DM halo mass by factors of roughly 1.3, 2, and 4 at radial distances of 20, 8, and 1 kpc, respectively compared to an uncontracted halo. Ignoring this contraction results in systematic biases in the inferred halo mass and concentration. We provide a best-fitting contracted NFW halo model to the MW rotation curve that matches the data very well. 1 The best-fit has a DM halo mass, M-200(DM) = 0.97(-0.19)(+0.24) x 10(12) M-circle dot, and concentration before baryon contraction of 9.4(-2.6)(+1.9), which lie close to the median halo mass-concentration relation predicted in ACDM. The inferred total mass, M-200(total) = 1.08(-0.14)(+0.20) x 10(12) M-circle dot, is in good agreement with recent measurements. The model gives an MW stellar mass of 5.04(-0.52)(+0.43) x 10(10) M-circle dot and infers that the DM density at the Solar position is rho(DM)(circle dot) = 8.8(-0.5)(+0.5) x 10(-3) M-circle dot pc(-3) 0.33(-0.02)(+0.02) GeV cm(-3). The rotation curve data can also be fitted with an uncontracted NI-1V halo model, but with very different DM and stellar parameters. The observations prefer the physically motivated contracted NFW halo, but the measurement uncertainties are too large to rule out the uncontracted NFW halo.