we compared the full spectral energy distribution of 2M0355 with the field L5 dwarf 2M1507-16. We find that 2M0355 is underluminous in optical through $K$ band then switches to overluminous through at least 12$\mu$m compared to 2M1507-16. Calculating the bolometric luminosity by integrating over the optical and near-IR spectra as well as WISE photometry, shows that the overall luminosity of 2M0355 is overluminous compared to the field object. We conclude that enhanced photospheric dust, thought to be correlated with young, low-temperature, low-luminosity brown dwarfs and giant exoplanets, shifts flux to longer wavelengths creating the red SED. The position of 2M0355 on the near-IR color magnitude diagram supports this conclusion as it appears redward and underluminous of the known population in a similar region as 2M1207b and HR8799bcd.

Combining new proper motion and parallax measurements we calculate UVW velocities to evaluate membership in nearby young moving groups. We find the kinematics consistent with the young thin disk and the UV velocities for 2M0355 place it in a busy part of velocity space for young objects. A careful kinematic comparison with nearby young groups and the field population leads us to conclude that 2M0355 has a 42% chance of membership in AB 