We study the radial velocity dependence in the spatial orientations of 10\,562 galaxies that have radial velocity $\leq$ 5\,000 km s$^{-1}$. The inclination angle and intrinsic flatness of galaxy are used to convert two- dimensional given parameters into three-dimensional spin vectors of the galaxy. We have performed Kolmogorov-Smirnov, Kuiper and Fourier tests in order to examine non-random effects in the expected isotropic distributions. No preferred alignment is noticed in the spatial orientation of total galaxies. However, the galaxies that have radial velocities 1\,500 to 2\,000 km s$^{-1}$ and 3\,000 to 3\,500 km s$^{-1}$ show preferred alignments in both the two and three dimensional analysis. Possible explanations of the results will be discussed. The spin vectors of high (low) radial velocity galaxies tend to be oriented parallel (perpendicular) the local supercluster planes. The spin vector projections of high radial velocity galaxies found to be oriented tangentially with respect to the local supercluster center. Thus, radial velocity dependence can be suspected in the spatial orientation of galaxies. In the total sample, our results supports the hierarchical clustering scenario which predicts that the directions of the spin vectors are entirely random. In the subsamples, we found radial velocity dependence in the spatial orientation of galaxies. Thus, we suspect a relationship between the origin of angular momentum and the Hubble recessional velocity of galaxies. We intend to extend our database upto the radial velocities $\sim$ 30\,000 km s$^{-1}$ and study the radial velocity dependence in the future.