  The local stellar kinematics of the Milky Way, parameterized by the Oort
constants A and B, depend on the local gradient of the rotation curve, its
absolute value (Theta_0), and the distance to the Galactic center (R_0). The
surface density of interstellar gas in the Milky Way varies non-monotonically
with radius, and so contributes significantly to the local gradient of the
rotation curve, and the Oort constants. Because of this, the Oort functions
A(R) and B(R) differ significantly from the dominant ~Theta_0/R dependence, in
the Solar neighborhood and other locations in the Galaxy. These models may
explain the ~40% difference between the values for 2 A R_0 derived from radial
velocity data originating in the inner and outer Galaxy (Merrifield 1992).
Incorporating these local non-linearities explains the significant differences
between the Oort constants derived from nearby stars (d <= 1 kpc; Hanson 1987)
and distant Cepheids (d=0.5-6 kpc; Feast & Whitelock 1997). However, a
consistent picture only emerges if one adopts small values for the Galactic
constants: R_0 = 7.1 +/- 0.4 kpc, and Theta_0 = 184 +/- 8 km/s. These values
are consistent with most kinematical methods of determining R_0, including the
proper motion of Sgr A* (Backer 1996), the direct determination of R_0 using
water masers (7.2 +/- 0.7 kpc; Reid 1993), and constraints set by the shape of
the Milky Way's dark halo (Olling & Merrifield 1997b).
