absolute photometry for each we confirm that the SED for 2M0355 is underluminous compared to the field object through $K$ band. However, redward of $\sim$ 2.5$\mu$m, 2M0355 switches to being overluminous through at least 12 $\mu$m. Following the method described in @Cushing05, we combine the flux-calibrated optical and near-IR spectra as well as WISE photometry and calculate bolometric luminosities for both 2M0355 and 2M1507. We linearly interpolate between the centers of each WISE bandpass (W1: 3.4; W2: 4.6; W3: 11.6) and assume a Rayleigh-Jeans tail for $\lambda>$11.6 $\mu$m. We find that 2M0355 is slightly more luminous than 2M1507 by $\Delta$ log$_{10}$ (L$_{2M0355}$/L$_{2M1507}$)=0.12$\pm$0.1. The overall luminosity of our source is further evidence that it is young, and we surmise that enhanced photospheric dust which weakens molecular bands and shifts flux to longer wavelengths is the most likely cause of the red SED.

In Figure \[fig:TM0355\] we show the near-infrared color-magnitude diagram for the field brown dwarf population (color-coded by spectral type), 2M1207b, the HR8799bcd planets, and 2M0355. The low luminosity and extremely red $J-K$ color of 2M0355 place it at the red edge of the brown dwarf population, in a similar region as 2M1207b. @Barman11 find the positions of the giant 