a, Star counts of the intermediate metallicity subpopulation25 at different radial bins (symbols with 1-σ error bars) and the best-fit soliton solution (red solid line) with mB = 8.0 × 10−23 eV, rc = 0.93 kpc and σ‖ = 11.3 km s−1, together with the 1-σ variation (red shaded). Star counts are normalized to the total number of sample stars within ∼2.1 kpc. Also shown are the best-fit empirical formula of Burkert35 (green dashed line) and the NFW profile (blue dot-dashed line) representing standard CDM. The scale radius of NFW is restricted to be no larger than 3.0 kpc during the fit to exclude unreasonably small concentration parameters. b, 1-σ contours of the total enclosed mass estimated from each of the three subpopulations5 (ovals), overplotted with the model curves using the same best-fit parameters adopted in a. Clearly, in both panels the soliton profile of ψDM provides an accurate fit, matched only by the empirical fitting function of the Burkert profile, whereas NFW is not favoured by the data.