scale radius $h=5.5$ kpc with the terminal flat rotation velocity of 200 .

In figure \[fig-rc30\] we plot calculated rotation curves for the three dark halo models as shown in figure \[fig-rcmodels\]. Thin solid line indicates isothermal dark halo model ([*iso*]{}), solid lines NFW model ([*nfw*]{}), and dashed lines Burkert model ([*bur*]{}). The curves are so adjusted that the velocity, or the enclosed mass, at $R_{\rm c}=15$ kpc is equal to each other, and the masses within $R_{\rm c}$ are taken to be equal to that of the exponential disk . For each model, the upper line indicates the sum of those for the dark halo and disk. The thin dashed lines are for the bulge and disk.

In the inner Galaxy at $R<\sim 10$ kpc, the rotation velocity is predominantly determined by the bulge and disk contributions, and $R<0.5$ kpc it is almost determined by the bulge alone. The dark halo contribution is negligible in any models at these radii. Thus, it is hard to discriminate the models by comparing them with the observations in the inner Galaxy, although the data are most accurately obtained there.

Near the Galactic Center at $R<1$ kpc, the volume density of the NFW 