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The formation mechanism of brown dwarfs (BDs) is one of the long-standingproblems in star formation because the typical Jeans mass in molecular cloudsis too large to form these substellar objects. To answer this question, it iscrucial to study a BD at the embedded phase. IRAS 16253-2429 is classified as avery low luminosity object (VeLLO) with internal luminosity 0.1 Lsun. VeLLOsare believed to be very low-mass protostars or even proto-BDs. We observed thejet/outflow driven by IRAS 16253-2429 in CO (2-1), (6-5), and (7-6) using theIRAM 30 m and APEX telescopes and the SMA in order to study its dynamicalfeatures and physical properties. Our SMA map reveals two protostellar jets,indicating the existence of a proto-binary system as implied by the precessingjet detected in H2 emission. We detect a wiggling pattern in theposition-velocity diagrams along the jet axes, which is likely due to thebinary orbital motion. Based on this, we derive the current mass of the binaryas ~0.032 Msun. Given the low envelope mass, IRAS 16253-2429 will form a binarythat probably consist of one or two BDs. Furthermore, we found that the outflowforce as well as the mass accretion rate are very low based on themulti-transition CO observations, which suggests that the final masses of thebinary components are at the stellar/substellar boundary. Since IRAS 16253 islocated in an isolated environment, we suggest that BDs can form throughfragmentation and collapse like low-mass stars.

IRAS 16253-2429: the First Proto-Brown Dwarf Binary Candidate Identified through Dynamics of Jets