and low-surface brightness galaxies, which are thought to be dark matter dominant (e.g. van den Bosch et al. 2000; Gentil et al. 2007; Jiminez et al. 2003). However, the major dynamical constituents of the Local Group are M31 and our Galaxy, two orders of magnitude more massive than dwarfs, where the bulge and disk are dominant within the optical radii at $<R_{\rm c} \sim 15$ kpc. It is, therefore, essential to investigate outer halo kinematics in order to discuss the dark halo in such a big galaxy as the Milky Way. For this purpose, we constructed a Galacto-Local Group rotation curve as shown in figures \[fig-vgc\] and \[fig-150\].

NFW/Burkert model and the Mass of the Galaxy
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The upper boundary of the pseudo rotation curve within $\sim150$ kpc radius is well fitted by the NFW and Burkert models, as shown in figure \[fig-150\]. In these models, the total mass of the Galaxy involved within a radius 770 kpc, the distance to M31, is $8.7\times 10^{11}\Msun$, and the mass within 385 kpc is $4.4 \times 10^{11}\Msun$, respectively. These values may be adjustable within a range less than $10^{12}\Msun$ by tuning the parameters $h$ and $R_{\rm c}$, so that the flat galactic 