Near-Infrared observations of the classical T Tauri star RW Aurigae A taken using the OH-Suppressing Infrared Spectrograph (OSIRIS) on the KECK telescope have been used to investigate the morphology & kinematics of the jet, finding an extended knot from the main body of the blue jet. Diagnostics have been performed, with the extinction being found to be higher than previous measurement (Av = 4.6). The jets’ mass-loss rates have been found to be 1.022 ×10−9 M /year and 1.544 ×10−9 M /year for the blue and red jet, respectively. The mass accretion rate has been measured to be 8.93 ×10−9 M /year using the Brγ emission line, having determined that it is not a constituent of the jet. The wiggle for the RW Aur jet has been fit with a precession and orbital model, both pointing to a brown dwarf companion with mass between 0.07 — 0.23 M similar to independently derived results for RW Aur A and for other protostellar systems where wiggling has been used.