We made observations of H2O masers in the LkHα 234 star forming region using the Japanese domestic VLBI network (J-Net). We first present spatial and velocity structures of the maser sources of C1 and C3 which are detected by Tofani et al.(1995). The distribution of H2O maser components in C1 shows an extent of 300×150 AU. On the other hand, it shows a compact and linear extent of 15×3 AU in C3, and its position angle (RA.=232 °) roughly agrees with that of the H2 jet (PA.=226 °). Moreover, the most blue-shifted and red-shifted maser components are located at both ends of the linear extent, indicating that this might be a very small jet ejected from the deeply embedded protostar. However, it is difficult to explain the distribution of intermediate velocity components by a simple jet model. We will discuss whether the H2O masers originate in a jet or a disk.