Stars like our Sun and their sub-stellar counterparts known as brown dwarfs form in large and complex cosmic clouds of molecular gas and dust. During their formation, the molecular cloud undergoes a hierarchical collapse such that this large cloud shrinks down in size by orders of magnitude, and its mass concentrated into a small central object. This object then evolves to become either a young star or a brown dwarf. Atomic and molecular outflows in the form of high velocity collimated jets and slower wide angled winds play a critical role during this formation process. Bipolar jets act to remove the excess angular momentum that the central object inherits from its birth environment. Meanwhile, the low velocity winds are thought to remove angular momentum from the circumstellar disc surrounding the central source, hence enabling the accretion of mass into the central object. The aim of this thesis is to explore unanswered questions in regard to this process. Namely, do these low velocity winds, which are thought to be traced by optical forbidden emission lines actually remove significant angular momentum from the disc, are these winds variable in time? And, what is the role of outflows at sub-stellar masses, particularly at the earliest stages of the formation process? The work presented in this thesis addresses these questions by utilising the forefront observational techniques of optical spectro-astrometry and radio interferometry in order to extract information about the morphology and kinematics of these flows. This thesis finds that despite variable kinematics, the spatial properties of these low velocity winds in low-mass stars remains stable. Assuming these winds magnetically driven, they don’t appear to remove a significant portion of excess angular momentum from the star-disc system, however, there are substantial uncertainties on these values due to the unconstrained temperature of the outflowing material. Lastly, in the substellar regime, outflows are observed via molecular gas alongside accretion, pointing to a "star-like" formation pathway for the young brown dwarf presented here.