the upper thin line, which is horizontal at large radii. The upper boundaries of the plot is well fitted by the rotation curve for the NFW model. In figure \[fig-vgc\] we plot the same for entire region of the Local Group up to 1 Mpc. For each object, the galacto-centric distance $R_{\rm GC}$ was calculated from galactic coordinates and helio-centric distance for $R_0=8$ kpc, and $V_r$ was calculated from observed helio-centric radial velocity by correcting for the solar motion of $V_0=200$ after transforming to LSR velocity. We call these diagrams the “pseudo rotation curve” of the Local Group, or “Galacto-LG (GLG) rotation curve”. These may be compared to similar plots of velocity differences against spatial separations of satellite galaxies for many pair galaxies as obtained by Zaritsky et al. (1997) and Prada et al. (2003).

Used galaxies and globular clusters with their longitude, latitude, distances and velocities are listed in table 1. The velocity and position data were adopted from Kulessa and Lynden-Bell (1992), Sawa and Fujimoto (2005) which is mainly based on those of Mateo (1998), Kochanek et al. (1996), and Kopylov et al. (2008).

![image](fig-150kpc.eps){width="16cm"}\

![image](fig-vgc.eps){width="16cm"}\

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Name & $l $ & $b$ & $R_{\rm helio}$ & $v_{\rm 