8799bcd.

We calculated the absolute magnitude of 2M0355 from the new parallax as well as Mauna Kea Observatory (MKO; @Tokunaga02) apparent magnitudes converted from 2MASS photometry using the @Stephens04 relations. Comparing M$_{JHK}$ for 2M0355 to the predicted values for an equivalent spectral type object based on the @Faherty12 polynomial, we find it to be \[-0.9,-0.5,-0.1\] magnitude underluminous at M$_{J}$,M$_{H}$, and M$_{K}$, respectively. As noted in @Faherty12, the population of low surface gravity L dwarfs is consistently red and underluminous–by up to 1.0 mag in M$_{JHK}$– compared to equivalent spectral type objects. As demonstrated in Figure  \[fig:spt\], 2M0355 clearly follows this trend. As discussed in @Faherty12 evolutionary models trace low-surface gravity objects at temperatures several hundred degrees lower than expected for equivalent spectral type objects on near-IR color magnitude diagrams, providing a potential explanation for the deviation in absolute magnitudes of low-gravity L dwarfs. Extending this analysis to 2M0355 we conclude that one explanation for its peculiar near-IR absolute magnitudes is that this source is cooler than normal L5 field dwarfs.

In Figure \[fig:SED\] we compare the full spectral energy distribution (SED) of 2M0355 to the field L5 dwarf 2MASSJ1507476-162738 (2M1507-@Reid00; @Dahn02). Combining the optical spectra, MKO $JHK$, and WISE $W1,W2,W3$ 