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We present and analyze Subaru/IRCS L' and M' images of the nearby M dwarf VHSJ125601.92-125723.9 (VHS 1256), which was recently claimed to have a ~11 M_Jupcompanion (VHS 1256 b) at ~102 au separation. Our AO images partially resolvethe central star into a binary, whose components are nearly equal in brightnessand separated by 0.106" +/- 0.001". VHS 1256 b occupies nearly the same near-IRcolor-magnitude diagram position as HR 8799 bcde and has a comparable L'brightness. However, it has a substantially redder H - M' color, implying arelatively brighter M' flux density than for the HR 8799 planets and suggestingthat non-equilibrium carbon chemistry may be less significant in VHS 1256 b. Wesuccessfully match the entire SED (optical through thermal infrared) for VHS1256 b to atmospheric models assuming chemical equilibrium, models which failedto reproduce HR 8799 b at 5 microns. Our modeling favors slightly thick cloudsin the companion's atmosphere, although perhaps not quite as thick as thosefavored recently for HR 8799 bcde. We estimate that the system is at leastolder than 200 Myr and the masses of the stars comprising the central binaryare at least 58 M_Jup each. Moreover, we find some of the properties of VHS1256 are inconsistent with the recent suggestion that it is a member of the ABDor moving group. Given the possible ranges in distance (12.7 pc vs. 17.1 pc),the lower mass limit for VHS 1256 b ranges from 10.5 - 26.2 M_Jup. Ourdetection limits rule out companions more massive than VHS 1256 b exterior to6-8 au, placing significant limits on and providing some evidence against asecond, more massive companion that may have scattered the wide-separationcompanion to its current location. VHS 1256 is most likely a very low masshierarchical triple system, and could be the third such system in which allcomponents reside in the brown dwarf mass regime.

astrophysical journal/the astrophysical journal

Thermal Infrared Imaging and Atmospheric Modeling of VHS  J125601.92-125723.9 b: Evidence for Moderately Thick Clouds and Equilibrium  Carbon Chemistry in a Hierarchical Triple System