We present the kinematical analysis of HI and HII gases within the disk of NGC 3359. There is a strong trend of non-circular gas flow as seen in the velocity field maps of both media. Specifically, the regions near the bar are marked by very skewed isovelocity contour lines. Within the area, velocity differences between the neutral atomic and ionized hydrogen up to 30 km s-1 can be seen. The large deviation from circular flow makes NGC 3359 an ideal candidate for us to test a new method of determining co-rotation radii of galaxies based on conspicuous features located at L4,5 Lagrangian points of the bar potential. The method and initial results will be discussed in this presentation. This work is supported by the pre-doctoral fellowship from the Florida Space Grant Consortium.