To determine whether the stars and the gas within 3 kpc of the sun share the same motions, the radial velocities of 1461 O-BS stars, |& n | < 11°, r<3.0 kpc, have been investigated by methods which approximate the procedures used in analyzing the 21-cm observations of neutral hydrogen. The radial velocities come principally from Wilson's catalogue and observations of Feast and Thackeray. For 896 stars, absolute magnitudes M from MK classifications or from Petrie, and B-V colors (or colors which could be converted to B-V) are available. Of the remaining, 156 stars have known values of M, but no absorption; 177 have absorption measures, but no M ; and 232 have neither. These latter stars are sufficiently bright so that it can be shown that they are within 3 kpc of the sun. The stars in the sample were divided into 5° zones by longitude. In each zone a plot of the frequency distribution in radial velocity results in a curve which can be compared with the corresponding 21-cm curve, modified to include only radiation from within 3 kpc of the sun. Although for many zones the stellar curve is similar to the hydrogen curve, the spread in radial velocity is often larger than that predicted by the Oort model. The region 190 0 n <280 0 exhibits an excess of negative radial velocities, even after the application of a +10 km/sec correction to the Lick radial velocities (Feast and Thackery, Monthly Notices Roy. Astron. Soc. 118, 1958). Deviations from circular motion and random velocities larger than the random gas velocities must exist.
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