too crude to use the galactic rotation curve in the present accuracy for discriminating the dark halo models, in so far as available observational kinematics using stars and interstellar gases are used.

Pseudo Rotation Curve of the Local Group
========================================

In order to discuss the dark halo and its mass distribution, kinematics beyond the Galactic disk is essential. There have been various works to use satellite and member galaxies in the Local Group for deriving the mass structure in the Local Group (the literature cited in Section 1). We, here, examine a possibility to use radial velocities of the Local Group of galaxies as an extension of the rotation curve of the Galaxy. We use the observed radial velocities in a direct way for continuing the dynamical mass analysis of Galactic rotation curve.

In figure \[fig-150\] we plot the absolute values of the galacto-centric radial velocities $V_r=|V_{\rm GC}|$ of outer globular clusters and members of the Local Group against their galacto-centric distances $R_{\rm GC}$ for objects within a distance of 150 kpc. Calculated rotation curves for the NFW model is shown by the thick line, and individual components are shown by dashed lines. The isothermal halo model is shown by 