2M0355 places the L5$\gamma$ dwarf at a distance of 8.2$^{+1.0}_{-0.8}$ pc. We list all astrometric and photometric properties in Table  \[properties\].

Moving Group Membership
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At a distance of 8.2 pc and with spectral and photometric differences from the field population resembling those of the $\sim$10 Myr 2M1207b, we investigate whether 2M0355 could be kinematically associated with one of the nearby young moving groups. Using the proper motion and parallax measured in this work with the most recent radial velocity from @Blake10, we calculate ($U,V,W$) = ($-$5.9$\pm$1.5, $-$23.6$\pm$2.0, $-$14.6$\pm$1.3) km s$^{-1}$ for 2M0355[^5]. These calculated space velocities are consistent with thin disk membership (age $<$ $\sim$2-3 Gyr), and the tangential velocity of 21.5$\pm$1.2 km s$^{-1}$ is consistent with the population of low gravity, kinematically young brown dwarfs (@Faherty09 [@Faherty12]; @Eggen89a [@Eggen89]). In Figure  \[fig:space\] we show the $UV$ velocities for a number of young stars or clusters within 200 pc of the Sun and find that 2M0355 is at the edge of a well populated region of velocity space. Figure \[fig:kinematics\] shows Galactic space velocities compared to $\beta$ Pictoris, and AB Doradus, the two closest moving groups to the Sun and the most likely groups of which 2M0355 might be 