of young brown dwarfs as a population can be used as an indicator of youth as they are distinctly different from the kinematics of the field brown dwarf population. As discussed in @Faherty09 [@Faherty12] low surface gravity brown dwarfs have significantly smaller tangential velocities and dispersions than the overall brown dwarf population. The young age (likely $<$ 1 Gyr) of these sources means they have spent less time in the disk so they have had minimal interactions with nearby stars and giant molecular clouds that will eventually increase their overall velocity dispersion (e.g. @Weinberg87; @Faherty10; @Dhital10). In the following subsections we compare the photometry, near-infrared spectral features, and kinematics of 2M0355 to known young brown dwarfs, directly-imaged exoplanets, and the field population in order to evaluate signatures of youth for this unusual object.

Photometry\[Photometry\]
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2M0355 is the reddest isolated L dwarf known. In Figure  \[fig:jmk\] we show the mean $J-K_{s}$ color and standard deviation for L dwarfs (binned by 0.5 subtype) calculated from a compilation of field objects[^3] with photometric uncertainties $<$ 0.1, excluding known young objects and subdwarfs. For comparison, other confirmed low-gravity L$\gamma$ dwarfs are plotted as filled circles and 2M0355 as a filled five-point star. In 