The measurement of the Galactic rotation curve provides a powerful tool for constraining the mass distribution in the Milky Way and enters various branches of Galactic kinematics as an essential ingredient. The Galactic rotation curves obtained by different methods are still not in a prefect agreement. In our work we investigate the shape of the rotation curve in the extended solar neighborhood and test it for presence of any peculiarities just outside the solar orbit as has been reported by some authors. We use RAVE data to determine the solar peculiar velocity and the radial scalelengths for the three populations of different metallicities representing the Galactic thin disc. For the same metallicity populations we construct the rotation curve in the range of Galactocentric distances 7-10 kpc for the sample of G-dwarfs from SEGUE. This work demonstrates the importance and non-triviality of the asymmetric drift correction while inferring the rotation velocity from the dynamically heated tracers. We find that the local rotation curve is essentially flat, thus the presence of any peculiarities in the rotation curve shape just outside the solar radius can be disproved.