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Recently, Gauza et al. (2015) reported the discovery of a companion to thelate M-dwarf, VHS J125601.92-125723.9 (VHS 1256-1257). The companion's absolutephotometry 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 tospectroscopic characterization. We discovered that the primary of this systemis an equal-magnitude binary. For an age $\sim300$ Myr the A and B componentseach have a mass of $64.6^{+0.8}_{-2.0}~M_{\mathrm{Jup}}$, and the b componenthas a mass of $11.2^{+9.7}_{-1.8}$, making VHS 1256-1257 only the third browndwarf triple system. There exists some tension between the spectrophotometricdistance of $17.2\pm2.6$ pc and the parallax distance of $12.7\pm1.0$ pc. At12.7 pc VHS1256-1257 A and B would be the faintest known M7.5 objects, and areeven faint outliers among M8 types. If the larger spectrophotmetric distance ismore accurate than the parallax, then the mass of each component increases. Inparticular, the mass of the b component increases well above the deuteriumburning limit to $\sim35~M_{\mathrm{Jup}}$ and the mass of each binarycomponent increases to $73^{+20}_{-17}~M_{\mathrm{Jup}}$. At 17.1 pc, the UVWkinematics of the system are consistent with membership in the AB~Dor movinggroup. The architecture of the system resembles a hierarchical stellar multiplesuggesting it formed via an extension of the star-formation process to lowmasses. Continued astrometric monitoring will resolve this distance uncertaintyand will provide dynamical masses for a new benchmark system.

Adaptive Optics imaging of VHS 1256-1257: A Low Mass Companion to a Brown Dwarf Binary System