Abstract The selected 146 Cepheids, for which accurate photometric measurements and also radial velocity and/or proper motion data exist, were used to determine a set of values concerning the motion of the stars and the distance scale of the Galaxy. Distances of these Cepheids were determined by combining photometric data with the period-luminosity and period-color relations derived by KRAFT (1961), FERNIE (1967b), and GEYER (1970). We solved the radial velocity equation and tangential velocity equations to evaluate such kinematical parameters as the solar motion components, u⊙, v⊙, and w⊙, the K-term, K, the Oort constants, A and B, and the corrections to Newcomb’s constants of precession, Δp and Δl, and to the motion of equinox, Δe. Calculations were made in parallel for various values of the galactocentric distance, R0, and for three sets of the Cepheids distance r. The solution for the case where rKraft, determined with KRAFT’s (1961) period-luminosity and period-color relations, was used and R0 was taken as 10 kpc, was adopted as the most plausible result, after some consideration. The estimations of the quantities corresponding to this case are: u⊙=8.4 km/sec, v⊙=14.3 km/sec, w⊙=7.0 km/sec (adopted), and K = –2.0km/sec; A = 14.1 km/sec kpc and B = –9.4 km/sec kpc; Δp = 1.″2/century and Δl + Δe=0.″7/century, respectively. The residual motions, namely the peculiar velocities were also analyzed in an attempt to interpret the K-term. It was found that the negative K-term of the Cepheids seems not to be due to the general contracting motion of the Galaxy, but might be partly due to the local inward community motions of Cepheids.