they are smoothly connected to the inner composite rotation curve for the best-fit bulge and disk models, and that the flat part at $R\sim 10-20$ kpc is approximately reproduced. The scale radius of the dark halo is taken to be $h=10$ kpc. The total mass of the dark halo within the critical radius $R_{\rm c}=15$ kpc in each model is taken to be equal to the disk mass in the same radius.

As equations (\[eq-nfw\]) and (\[eq-bur\]) indicate, the NFW and Burkert profiles are similar to each other at radii sufficiently greater than the scale radius $h$, e.g. at $R\gg h=10$ kpc. Accordingly, the rotation curves corresponding to these two models are similar at $R>30$ kpc, except for a small difference arising from the difference in the profiles, and therefore the total masses, at $R< \sim h$.

If we look into the local area around the Galaxy at $R<\sim 150$ kpc as in figure \[fig-150\], the NFW well traces the upper envelope of the pseudo rotation curve. On the other hand, if look into the plot at larger scales as in figure \[fig-vgc\], the isothermal model can approximately trace the upper boundary of the entire observations in the Local Group. 