| Despite the different formation mechanisms that can yield brown dwarfs, understanding their formation requires observations at the earliest stages of these objects, when they are still embedded within a cold envelope of dust and gas, developing an outflow/jet-disk system, or forming within young protoplanetary disks. For this, we rely on radio to submillimeter facilities. Given that brown dwarfs are faint and relatively small, the use of sensitive radio interferometers is essential. ALMA and the VLA, with their current capabilities, have started to provide the first results in characterizing the early stages of brown dwarf formation. Nevertheless, future interferometers will significantly enhance our understanding of these formation mechanisms. In this talk, I will present a summary of the future capabilities that next-generation radio interferometers, such as the ngVLA, SKA, and ALMA with its Wideband Sensitivity Upgrade, will offer to expand our knowledge on how brown dwarfs form. |
