maximum bulge and disk contributions (Sofue et al. 2008). Scale radius on the order of 3.5 to 10 kpc have been used for NFW profiles by other authors (e.g. Hayashi and Chiba 2006; Seljak 2002). We adopt $h=10$ kpc commonly for the three models throughout this paper, as it is not a sensitive parameter for discussing the outer Galaxy.

Figure \[fig-rho\] shows the density distributions for individual components of the bulge and disk, as well as those for the three different models of the dark halo. The parameters are the same as those adopted in Sofue et al. (2008) except for the halo scale radius ($h=10$ kpc). Figure \[fig-mass\] shows the corresponding masses enclosed within a sphere of radius $R$. In these figures, the total masses of the disk and halo are adjusted so that they become equal to each other at a radius $R_{\rm c}$, which we call the disk-halo critical radius. We take $R_{\rm c}=15$ kpc in the present calculation. Obviously, the circular velocities corresponding to the disk and halo become approximately equal to each other at the critical radius.

The circular velocity of the Galaxy is calculated by V(R)\^2=V\_[b]{} (R)\^2+V\_[d]{} (R)\^2+V\_[h]{} (R)\^2, \[eq\_rc\] where $V_{\rm b} (R)$, 