Stellar rotation, parameterized by a star's projected rotational velocity v sin i, is a fundamental parameter linked to star formation, evolution, and dynamical interaction.These are still poorly understood for OB stars, which typically rotate faster than their lower-mass counterparts. We determine v sin i for 210 field OB stars in the Small Magellanic Cloud, 39 of which are classical Oe/Be stars due to the low-metallicity environment of the SMC. We use spectroscopic data from the RIOTS4 survey, employing Fourier analysis to derive v sin i from the rotational broadening of spectral lines, primarily He I and He II. We confirm that Be stars are typically much faster rotators than normal B stars, and their v sin i distribution is a single symmetric peak with a mean of 180 km / s and standard deviation of 50 km / s. We therefore suggest that stars linked to the Be phenomenon may correspond to the high-velocity peak of the well-known bimodal v sin i distribution of B stars. We will also correlate rotation with other stellar parameters, such as proper motion, galactic environment, degree of isolation, and radial velocity to probe physical properties of OB stars.