Recently , Gauza et al . ( 2015 ) reported the discovery of a companion to the late M-dwarf , VHS J125601.92-125723.9 ( VHS 1256-1257 ) . The companion ’ s absolute photometry suggests its mass and atmosphere are similar to the HR 8799 planets . However , as a wide companion to a late-type star , it is more accessible to spectroscopic characterization . We discovered that the primary of this system is an equal-magnitude binary . For an age \sim 300 Myr the A and B components each have a mass of 64.6 ^ { +0.8 } _ { -2.0 } ~ { } M _ { \mathrm { Jup } } , and the b component has a mass of 11.2 ^ { +9.7 } _ { -1.8 } , making VHS 1256-1257 only the third brown dwarf triple system . There exists some tension between the spectrophotometric distance of 17.2 \pm 2.6 pc and the parallax distance of 12.7 \pm 1.0 pc . At 12.7 pc VHS 1256-1257 A and B would be the faintest known M7.5 objects , and are even faint outliers among M8 types . If the larger spectrophotmetric distance is more accurate than the parallax , then the mass of each component increases . In particular , the mass of the b component increases well above the deuterium burning limit to \sim 35 ~ { } M _ { \mathrm { Jup } } and the mass of each binary component increases to 73 ^ { +20 } _ { -17 } ~ { } M _ { \mathrm { Jup } } . At 17.1 pc , the UVW kinematics of the system are consistent with membership in the AB Dor moving group . The architecture of the system resembles a hierarchical stellar multiple suggesting it formed via an extension of the star-formation process to low masses . Continued astrometric monitoring will resolve this distance uncertainty and will provide dynamical masses for a new benchmark system .