the target was $\pm$30 minutes off the meridian (Table  \[observing\]). Dark frames and lights on/off dome flats were obtained at the start of each evening. We used the Carnegie Astrometric Planet Search software to extract all point sources from each epoch and solve for relative parallaxes and proper motions (@Boss09). The full image reduction procedures as well as the description of the parallax pipeline are described in @Faherty12.

Evaluating Youth Indicators\[youth\]
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Youth indicators for isolated L dwarfs are not yet fully quantified or calibrated, but a number of distinguishing characteristics have been extrapolated from low-mass members (primarily late-type M dwarfs) of nearby young moving groups, open clusters and star forming regions or companions to young stars and confirmed by low-gravity atmosphere models (e.g. @Lucas01; @Gorlova03; @Luhman04; @McGovern04; @Allers07; @Rice10 [@Rice11], @Patience12).

Among the strongest indicators is the shape of the near-infrared spectra of young brown dwarfs which are subtly different than those of their field counterparts. Known brown dwarf members of the Chamaelleon II, Ophiuchus, Orion Nebula Cluster, TW Hydrae, and $\beta$ Pictoris groups demonstrate various degrees of sharply peaked $H$-band spectra compared to field aged objects. The shape of the near-infrared continuum induced by steam absorption is sensitive 